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Lifetimes and Branching Ratios Apparatus (LIBRA)
L. J. Sun, J. Dopfer, A. Adams, C. Wrede, A. Banerjee, B. A. Brown, J. Chen, E. A. M. Jensen, R. Mahajan, T. Rauscher, C. Sumithrarachchi, L. E. Weghorn, D. Weisshaar, T. Wheeler
Oct 23 2024 physics.ins-det astro-ph.IM nucl-ex arXiv:2410.16446v1

@misc{2410.16446, author = {L.~J.~Sun and J.~Dopfer and A.~Adams and C.~Wrede and A.~Banerjee and B.~A.~Brown and J.~Chen and E.~A.~M.~Jensen and R.~Mahajan and T.~Rauscher and C.~Sumithrarachchi and L.~E.~Weghorn and D.~Weisshaar and T.~Wheeler}, title = {{L}ifetimes and {B}ranching {R}atios {A}pparatus ({LIBRA})}, year = {2024}, eprint = {2410.16446}, note = {arXiv:2410.16446v1} }
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The Particle X-ray Coincidence Technique (PXCT) was originally developed to measure average lifetimes in the $10^{-17}-10^{-15}$~s range for proton-unbound states populated by electron capture (EC). We have designed and built the Lifetimes and Branching Ratios Apparatus (LIBRA) to be used in the stopped-beam area at the Facility for Rare Isotope Beams that extends PXCT to measure both lifetimes and decay branching ratios of resonances populated by EC/$\beta^+$ decay. The first application of LIBRA aims to obtain essential nuclear data from $^{60}$Ga EC/$\beta^+$ decay to constrain the thermonuclear rates of the $^{59}$Cu$(p,\gamma)^{60}$Zn and $^{59}$Cu$(p,\alpha)^{56}$Ni reactions, and in turn, the strength of the NiCu nucleosynthesis cycle, which is predicted to significantly impact the modeling of Type I X-ray burst light curves and the composition of the burst ashes. Detailed theoretical calculations, Monte Carlo simulations, and performance tests with radioactive sources have been conducted to validate the feasibility of employing LIBRA for the $^{60}$Ga experiment. The method introduced with LIBRA has the potential to measure nearly all essential ingredients for thermonuclear reaction rate calculations in a single experiment, in the absence of direct measurements, which are often impractical for radioactive reactants.
Search for gravitational waves emitted from SN 2023ixf
LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, A. G. Abac, R. Abbott, I. Abouelfettouh, F. Acernese, K. Ackley, S. Adhicary, N. Adhikari, R. X. Adhikari, V. K. Adkins, D. Agarwal, M. Agathos, M. Aghaei Abchouyeh, O. D. Aguiar, I. Aguilar, L. Aiello, A. Ain, T. Akutsu, et al (1763)
Oct 23 2024 astro-ph.HE arXiv:2410.16565v1

@misc{2410.16565, author = {LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration and A.~G.~Abac and R.~Abbott and I.~Abouelfettouh and F.~Acernese and K.~Ackley and S.~Adhicary and N.~Adhikari and R.~X.~Adhikari and V.~K.~Adkins and D.~Agarwal and M.~Agathos and M.~Aghaei Abchouyeh and O.~D.~Aguiar and I.~Aguilar and L.~Aiello and A.~Ain and T.~Akutsu and S.~Albanesi and R.~A.~Alfaidi and A.~Al-Jodah and C.~Alléné and A.~Allocca and S.~Al-Shammari and P.~A.~Altin and S.~Alvarez-Lopez and A.~Amato and L.~Amez-Droz and A.~Amorosi and C.~Amra and A.~Ananyeva and S.~B.~Anderson and W.~G.~Anderson and M.~Andia and M.~Ando and T.~Andrade and N.~Andres and M.~Andrés-Carcasona and T.~Andrić and J.~Anglin and S.~Ansoldi and J.~M.~Antelis and S.~Antier and M.~Aoumi and E.~Z.~Appavuravther and S.~Appert and S.~K.~Apple and K.~Arai and A.~Araya and M.~C.~Araya and J.~S.~Areeda and L.~Argianas and N.~Aritomi and F.~Armato and N.~Arnaud and M.~Arogeti and S.~M.~Aronson and G.~Ashton and Y.~Aso and M.~Assiduo and S.~Assis de Souza Melo and S.~M.~Aston and P.~Astone and F.~Attadio and F.~Aubin and K.~AultONeal and G.~Avallone and S.~Babak and F.~Badaracco and C.~Badger and S.~Bae and S.~Bagnasco and E.~Bagui and J.~G.~Baier and L.~Baiotti and R.~Bajpai and T.~Baka and M.~Ball and G.~Ballardin and S.~W.~Ballmer and S.~Banagiri and B.~Banerjee and D.~Bankar and P.~Baral and J.~C.~Barayoga and B.~C.~Barish and D.~Barker and P.~Barneo and F.~Barone and B.~Barr and L.~Barsotti and M.~Barsuglia and D.~Barta and A.~M.~Bartoletti and M.~A.~Barton and I.~Bartos and S.~Basak and A.~Basalaev and R.~Bassiri and A.~Basti and D.~E.~Bates and M.~Bawaj and P.~Baxi and J.~C.~Bayley and A.~C.~Baylor and P.~A.~Baynard II and M.~Bazzan and V.~M.~Bedakihale and F.~Beirnaert and M.~Bejger and D.~Belardinelli and A.~S.~Bell and V.~Benedetto and W.~Benoit and J.~D.~Bentley and M.~Ben Yaala and S.~Bera and M.~Berbel and F.~Bergamin and B.~K.~Berger and S.~Bernuzzi and M.~Beroiz and D.~Bersanetti and A.~Bertolini and J.~Betzwieser and D.~Beveridge and N.~Bevins and R.~Bhandare and U.~Bhardwaj and R.~Bhatt and D.~Bhattacharjee and S.~Bhaumik and S.~Bhowmick and A.~Bianchi and I.~A.~Bilenko and G.~Billingsley and A.~Binetti and S.~Bini and O.~Birnholtz and S.~Biscoveanu and A.~Bisht and M.~Bitossi and M.-A.~Bizouard and J.~K.~Blackburn and L.~A.~Blagg and C.~D.~Blair and D.~G.~Blair and F.~Bobba and N.~Bode and G.~Boileau and M.~Boldrini and G.~N.~Bolingbroke and A.~Bolliand and L.~D.~Bonavena and R.~Bondarescu and F.~Bondu and E.~Bonilla and M.~S.~Bonilla and A.~Bonino and R.~Bonnand and P.~Booker and A.~Borchers and V.~Boschi and S.~Bose and V.~Bossilkov and V.~Boudart and A.~Boudon and A.~Bozzi and C.~Bradaschia and P.~R.~Brady and M.~Braglia and A.~Branch and M.~Branchesi and J.~Brandt and I.~Braun and M.~Breschi and T.~Briant and A.~Brillet and M.~Brinkmann and P.~Brockill and E.~Brockmueller and A.~F.~Brooks and B.~C.~Brown and D.~D.~Brown and M.~L.~Brozzetti and S.~Brunett and G.~Bruno and R.~Bruntz and J.~Bryant and F.~Bucci and J.~Buchanan and O.~Bulashenko and T.~Bulik and H.~J.~Bulten and A.~Buonanno and K.~Burtnyk and R.~Buscicchio and D.~Buskulic and C.~Buy and R.~L.~Byer and G.~S.~Cabourn Davies and G.~Cabras and R.~Cabrita and V.~Cáceres-Barbosa and L.~Cadonati and G.~Cagnoli and C.~Cahillane and J.~Calderón Bustillo and T.~A.~Callister and E.~Calloni and J.~B.~Camp and M.~Canepa and G.~Caneva Santoro and K.~C.~Cannon and H.~Cao and L.~A.~Capistran and E.~Capocasa and E.~Capote and G.~Carapella and F.~Carbognani and M.~Carlassara and J.~B.~Carlin and M.~Carpinelli and G.~Carrillo and J.~J.~Carter and G.~Carullo and J.~Casanueva Diaz and C.~Casentini and S.~Y.~Castro-Lucas and S.~Caudill and M.~Cavaglià and R.~Cavalieri and G.~Cella and P.~Cerdá-Durán and E.~Cesarini and W.~Chaibi and P.~Chakraborty and S.~Chalathadka Subrahmanya and J.~C.~L.~Chan and M.~Chan and K.~Chandra and R.-J.~Chang and S.~Chao and E.~L.~Charlton and P.~Charlton and E.~Chassande-Mottin and C.~Chatterjee and Debarati Chatterjee and Deep Chatterjee and M.~Chaturvedi and S.~Chaty and A.~Chen and A.~H.-Y.~Chen and D.~Chen and H.~Chen and H.~Y.~Chen and J.~Chen and K.~H.~Chen and Y.~Chen and Yanbei Chen and Yitian Chen and H.~P.~Cheng and P.~Chessa and H.~T.~Cheung and S.~Y.~Cheung and F.~Chiadini and G.~Chiarini and R.~Chierici and A.~Chincarini and M.~L.~Chiofalo and A.~Chiummo and C.~Chou and S.~Choudhary and N.~Christensen and S.~S.~Y.~Chua and P.~Chugh and G.~Ciani and P.~Ciecielag and M.~Cieślar and M.~Cifaldi and R.~Ciolfi and F.~Clara and J.~A.~Clark and J.~Clarke and T.~A.~Clarke and P.~Clearwater and S.~Clesse and E.~Coccia and E.~Codazzo and P.-F.~Cohadon and S.~Colace and M.~Colleoni and C.~G.~Collette and J.~Collins and S.~Colloms and A.~Colombo and M.~Colpi and C.~M.~Compton and G.~Connolly and L.~Conti and T.~R.~Corbitt and I.~Cordero-Carrión and S.~Corezzi and N.~J.~Cornish and A.~Corsi and S.~Cortese and C.~A.~Costa and R.~Cottingham and M.~W.~Coughlin and A.~Couineaux and J.-P.~Coulon and S.~T.~Countryman and J.-F.~Coupechoux and P.~Couvares and D.~M.~Coward and M.~J.~Cowart and R.~Coyne and K.~Craig and R.~Creed and J.~D.~E.~Creighton and T.~D.~Creighton and P.~Cremonese and A.~W.~Criswell and J.~C.~G.~Crockett-Gray and S.~Crook and R.~Crouch and J.~Csizmazia and J.~R.~Cudell and T.~J.~Cullen and A.~Cumming and E.~Cuoco and M.~Cusinato and P.~Dabadie and T.~Dal Canton and S.~Dall'Osso and S.~Dal Pra and G.~Dálya and B.~D'Angelo and S.~Danilishin and S.~D'Antonio and K.~Danzmann and K.~E.~Darroch and L.~P.~Dartez and A.~Dasgupta and S.~Datta and V.~Dattilo and A.~Daumas and N.~Davari and I.~Dave and A.~Davenport and M.~Davier and T.~F.~Davies and D.~Davis and L.~Davis and M.~C.~Davis and P.~J.~Davis and M.~Dax and J.~De Bolle and M.~Deenadayalan and J.~Degallaix and M.~De Laurentis and S.~Deléglise and F.~De Lillo and D.~Dell'Aquila and W.~Del Pozzo and F.~De Marco and F.~De Matteis and V.~D'Emilio and N.~Demos and T.~Dent and A.~Depasse and N.~DePergola and R.~De Pietri and R.~De Rosa and C.~De Rossi and R.~DeSalvo and R.~De Simone and A.~Dhani and R.~Diab and M.~C.~Díaz and M.~Di Cesare and G.~Dideron and N.~A.~Didio and T.~Dietrich and L.~Di Fiore and C.~Di Fronzo and M.~Di Giovanni and T.~Di Girolamo and D.~Diksha and A.~Di Michele and J.~Ding and S.~Di Pace and I.~Di Palma and F.~Di Renzo and Divyajyoti and A.~Dmitriev and Z.~Doctor and E.~Dohmen and P.~P.~Doleva and D.~Dominguez and L.~D'Onofrio and F.~Donovan and K.~L.~Dooley and T.~Dooney and S.~Doravari and O.~Dorosh and M.~Drago and J.~C.~Driggers and J.-G.~Ducoin and L.~Dunn and U.~Dupletsa and D.~D'Urso and H.~Duval and P.-A.~Duverne and S.~E.~Dwyer and C.~Eassa and M.~Ebersold and T.~Eckhardt and G.~Eddolls and B.~Edelman and T.~B.~Edo and O.~Edy and A.~Effler and J.~Eichholz and H.~Einsle and M.~Eisenmann and R.~A.~Eisenstein and A.~Ejlli and R.~M.~Eleveld and M.~Emma and K.~Endo and A.~J.~Engl and E.~Enloe and L.~Errico and R.~C.~Essick and H.~Estellés and D.~Estevez and T.~Etzel and M.~Evans and T.~Evstafyeva and B.~E.~Ewing and J.~M.~Ezquiaga and F.~Fabrizi and F.~Faedi and V.~Fafone and S.~Fairhurst and A.~M.~Farah and B.~Farr and W.~M.~Farr and G.~Favaro and M.~Favata and M.~Fays and M.~Fazio and J.~Feicht and M.~M.~Fejer and R.~Felicetti and E.~Fenyvesi and D.~L.~Ferguson and S.~Ferraiuolo and I.~Ferrante and T.~A.~Ferreira and F.~Fidecaro and P.~Figura and A.~Fiori and I.~Fiori and M.~Fishbach and R.~P.~Fisher and R.~Fittipaldi and V.~Fiumara and R.~Flaminio and S.~M.~Fleischer and L.~S.~Fleming and E.~Floden and E.~M.~Foley and H.~Fong and J.~A.~Font and B.~Fornal and P.~W.~F.~Forsyth and K.~Franceschetti and N.~Franchini and S.~Frasca and F.~Frasconi and A.~Frattale Mascioli and Z.~Frei and A.~Freise and O.~Freitas and R.~Frey and W.~Frischhertz and P.~Fritschel and V.~V.~Frolov and G.~G.~Fronzé and M.~Fuentes-Garcia and S.~Fujii and T.~Fujimori and P.~Fulda and M.~Fyffe and B.~Gadre and J.~R.~Gair and S.~Galaudage and V.~Galdi and H.~Gallagher and S.~Gallardo and B.~Gallego and R.~Gamba and A.~Gamboa and D.~Ganapathy and A.~Ganguly and B.~Garaventa and J.~García-Bellido and C.~García Núñez and C.~García-Quirós and J.~W.~Gardner and K.~A.~Gardner and J.~Gargiulo and A.~Garron and F.~Garufi and C.~Gasbarra and B.~Gateley and V.~Gayathri and G.~Gemme and A.~Gennai and V.~Gennari and J.~George and R.~George and O.~Gerberding and L.~Gergely and Archisman Ghosh and Sayantan Ghosh and Shaon Ghosh and Shrobana Ghosh and Suprovo Ghosh and Tathagata Ghosh and L.~Giacoppo and J.~A.~Giaime and K.~D.~Giardina and D.~R.~Gibson and D.~T.~Gibson and C.~Gier and P.~Giri and F.~Gissi and S.~Gkaitatzis and J.~Glanzer and F.~Glotin and J.~Godfrey and P.~Godwin and N.~L.~Goebbels and E.~Goetz and J.~Golomb and S.~Gomez Lopez and B.~Goncharov and Y.~Gong and G.~González and P.~Goodarzi and S.~Goode and A.~W.~Goodwin-Jones and M.~Gosselin and A.~S.~Göttel and R.~Gouaty and D.~W.~Gould and K.~Govorkova and S.~Goyal and B.~Grace and A.~Grado and V.~Graham and A.~E.~Granados and M.~Granata and V.~Granata and S.~Gras and P.~Grassia and A.~Gray and C.~Gray and R.~Gray and G.~Greco and A.~C.~Green and S.~M.~Green and S.~R.~Green and A.~M.~Gretarsson and E.~M.~Gretarsson and D.~Griffith and W.~L.~Griffiths and H.~L.~Griggs and G.~Grignani and A.~Grimaldi and C.~Grimaud and H.~Grote and D.~Guerra and D.~Guetta and G.~M.~Guidi and A.~R.~Guimaraes and H.~K.~Gulati and F.~Gulminelli and A.~M.~Gunny and H.~Guo and W.~Guo and Y.~Guo and Anchal Gupta and Anuradha Gupta and Ish Gupta and N.~C.~Gupta and P.~Gupta and S.~K.~Gupta and T.~Gupta and N.~Gupte and J.~Gurs and N.~Gutierrez and F.~Guzman and H.-Y.~H and D.~Haba and M.~Haberland and S.~Haino and E.~D.~Hall and E.~Z.~Hamilton and G.~Hammond and W.-B.~Han and M.~Haney and J.~Hanks and C.~Hanna and M.~D.~Hannam and O.~A.~Hannuksela and A.~G.~Hanselman and H.~Hansen and J.~Hanson and R.~Harada and A.~R.~Hardison and K.~Haris and T.~Harmark and J.~Harms and G.~M.~Harry and I.~W.~Harry and J.~Hart and B.~Haskell and C.-J.~Haster and J.~S.~Hathaway and K.~Haughian and H.~Hayakawa and K.~Hayama and R.~Hayes and A.~Heffernan and A.~Heidmann and M.~C.~Heintze and J.~Heinze and J.~Heinzel and H.~Heitmann and F.~Hellman and P.~Hello and A.~F.~Helmling-Cornell and G.~Hemming and O.~Henderson-Sapir and M.~Hendry and I.~S.~Heng and E.~Hennes and C.~Henshaw and T.~Hertog and M.~Heurs and A.~L.~Hewitt and J.~Heyns and S.~Higginbotham and S.~Hild and S.~Hill and Y.~Himemoto and N.~Hirata and C.~Hirose and S.~Hoang and S.~Hochheim and D.~Hofman and N.~A.~Holland and K.~Holley-Bockelmann and Z.~J.~Holmes and D.~E.~Holz and L.~Honet and C.~Hong and J.~Hornung and S.~Hoshino and J.~Hough and S.~Hourihane and E.~J.~Howell and C.~G.~Hoy and C.~A.~Hrishikesh and H.-F.~Hsieh and C.~Hsiung and H.~C.~Hsu and W.-F.~Hsu and P.~Hu and Q.~Hu and H.~Y.~Huang and Y.-J.~Huang and A.~D.~Huddart and B.~Hughey and D.~C.~Y.~Hui and V.~Hui and S.~Husa and R.~Huxford and T.~Huynh-Dinh and L.~Iampieri and G.~A.~Iandolo and M.~Ianni and A.~Iess and H.~Imafuku and K.~Inayoshi and Y.~Inoue and G.~Iorio and M.~H.~Iqbal and J.~Irwin and R.~Ishikawa and M.~Isi and M.~A.~Ismail and Y.~Itoh and H.~Iwanaga and M.~Iwaya and B.~R.~Iyer and V.~JaberianHamedan and C.~Jacquet and P.-E.~Jacquet and S.~J.~Jadhav and S.~P.~Jadhav and T.~Jain and A.~L.~James and P.~A.~James and R.~Jamshidi and J.~Janquart and K.~Janssens and N.~N.~Janthalur and S.~Jaraba and P.~Jaranowski and R.~Jaume and W.~Javed and A.~Jennings and W.~Jia and J.~Jiang and J.~Kubisz and C.~Johanson and G.~R.~Johns and N.~A.~Johnson and M.~C.~Johnston and R.~Johnston and N.~Johny and D.~H.~Jones and D.~I.~Jones and R.~Jones and S.~Jose and P.~Joshi and L.~Ju and K.~Jung and J.~Junker and V.~Juste and T.~Kajita and I.~Kaku and C.~Kalaghatgi and V.~Kalogera and M.~Kamiizumi and N.~Kanda and S.~Kandhasamy and G.~Kang and J.~B.~Kanner and S.~J.~Kapadia and D.~P.~Kapasi and S.~Karat and C.~Karathanasis and R.~Kashyap and M.~Kasprzack and W.~Kastaun and T.~Kato and E.~Katsavounidis and W.~Katzman and R.~Kaushik and K.~Kawabe and R.~Kawamoto and A.~Kazemi and D.~Keitel and J.~Kelley-Derzon and J.~Kennington and R.~Kesharwani and J.~S.~Key and R.~Khadela and S.~Khadka and F.~Y.~Khalili and F.~Khan and I.~Khan and T.~Khanam and M.~Khursheed and N.~M.~Khusid and W.~Kiendrebeogo and N.~Kijbunchoo and C.~Kim and J.~C.~Kim and K.~Kim and M.~H.~Kim and S.~Kim and Y.-M.~Kim and C.~Kimball and M.~Kinley-Hanlon and M.~Kinnear and J.~S.~Kissel and S.~Klimenko and A.~M.~Knee and N.~Knust and K.~Kobayashi and M.~Obergaulinger and P.~Koch and S.~M.~Koehlenbeck and G.~Koekoek and K.~Kohri and K.~Kokeyama and S.~Koley and P.~Kolitsidou and M.~Kolstein and K.~Komori and A.~K.~H.~Kong and A.~Kontos and M.~Korobko and R.~V.~Kossak and X.~Kou and A.~Koushik and N.~Kouvatsos and M.~Kovalam and D.~B.~Kozak and S.~L.~Kranzhoff and V.~Kringel and N.~V.~Krishnendu and A.~Królak and K.~Kruska and G.~Kuehn and P.~Kuijer and S.~Kulkarni and A.~Kulur Ramamohan and A.~Kumar and Praveen Kumar and Prayush Kumar and Rahul Kumar and Rakesh Kumar and J.~Kume and K.~Kuns and N.~Kuntimaddi and S.~Kuroyanagi and N.~J.~Kurth and S.~Kuwahara and K.~Kwak and K.~Kwan and J.~Kwok and G.~Lacaille and P.~Lagabbe and D.~Laghi and S.~Lai and A.~H.~Laity and M.~H.~Lakkis and E.~Lalande and M.~Lalleman and P.~C.~Lalremruati and M.~Landry and B.~B.~Lane and R.~N.~Lang and J.~Lange and B.~Lantz and A.~La Rana and I.~La Rosa and A.~Lartaux-Vollard and P.~D.~Lasky and J.~Lawrence and M.~N.~Lawrence and M.~Laxen and A.~Lazzarini and C.~Lazzaro and P.~Leaci and Y.~K.~Lecoeuche and H.~M.~Lee and H.~W.~Lee and K.~Lee and R.-K.~Lee and R.~Lee and S.~Lee and Y.~Lee and I.~N.~Legred and J.~Lehmann and L.~Lehner and M.~Le Jean and A.~Lemaître and M.~Lenti and M.~Leonardi and M.~Lequime and N.~Leroy and M.~Lesovsky and N.~Letendre and M.~Lethuillier and S.~E.~Levin and Y.~Levin and K.~Leyde and A.~K.~Y.~Li and K.~L.~Li and T.~G.~F.~Li and X.~Li and Z.~Li and A.~Lihos and C-Y.~Lin and C.-Y.~Lin and E.~T.~Lin and F.~Lin and H.~Lin and L.~C.-C.~Lin and Y.-C.~Lin and F.~Linde and S.~D.~Linker and T.~B.~Littenberg and A.~Liu and G.~C.~Liu and Jian Liu and F.~Llamas Villarreal and J.~Llobera-Querol and R.~K.~L.~Lo and J.-P.~Locquet and L.~T.~London and A.~Longo and D.~Lopez and M.~Lopez Portilla and M.~Lorenzini and A.~Lorenzo-Medina and V.~Loriette and M.~Lormand and G.~Losurdo and T.~P.~Lott IV and J.~D.~Lough and H.~A.~Loughlin and C.~O.~Lousto and M.~J.~Lowry and N.~Lu and H.~Lück and D.~Lumaca and A.~P.~Lundgren and A.~W.~Lussier and L.-T.~Ma and S.~Ma and M.~Ma'arif and R.~Macas and A.~Macedo and M.~MacInnis and R.~R.~Maciy and D.~M.~Macleod and I.~A.~O.~MacMillan and A.~Macquet and D.~Macri and K.~Maeda and S.~Maenaut and I.~Magaña Hernandez and S.~S.~Magare and C.~Magazzù and R.~M.~Magee and E.~Maggio and R.~Maggiore and M.~Magnozzi 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B.~F.~Whiting and C.~Whittle and J.~B.~Wildberger and O.~S.~Wilk and D.~Wilken and A.~T.~Wilkin and D.~J.~Willadsen and K.~Willetts and D.~Williams and M.~J.~Williams and N.~S.~Williams and J.~L.~Willis and B.~Willke and M.~Wils and J.~Winterflood and C.~C.~Wipf and G.~Woan and J.~Woehler and J.~K.~Wofford and N.~E.~Wolfe and H.~T.~Wong and H.~W.~Y.~Wong and I.~C.~F.~Wong and J.~L.~Wright and M.~Wright and C.~Wu and D.~S.~Wu and H.~Wu and E.~Wuchner and D.~M.~Wysocki and V.~A.~Xu and Y.~Xu and N.~Yadav and H.~Yamamoto and K.~Yamamoto and T.~S.~Yamamoto and T.~Yamamoto and S.~Yamamura and R.~Yamazaki and S.~Yan and T.~Yan and F.~W.~Yang and F.~Yang and K.~Z.~Yang and Y.~Yang and Z.~Yarbrough and H.~Yasui and S.-W.~Yeh and A.~B.~Yelikar and X.~Yin and J.~Yokoyama and T.~Yokozawa and J.~Yoo and H.~Yu and S.~Yuan and H.~Yuzurihara and A.~Zadrożny and M.~Zanolin and M.~Zeeshan and T.~Zelenova and J.-P.~Zendri and M.~Zeoli and M.~Zerrad and M.~Zevin and A.~C.~Zhang and L.~Zhang and R.~Zhang and T.~Zhang and Y.~Zhang and C.~Zhao and Yue Zhao and Yuhang Zhao and Y.~Zheng and H.~Zhong and R.~Zhou and X.-J.~Zhu and Z.-H.~Zhu and A.~B.~Zimmerman and M.~E.~Zucker and J.~Zweizig}, title = {{S}earch for gravitational waves emitted from {SN} 2023ixf}, year = {2024}, eprint = {2410.16565}, note = {arXiv:2410.16565v1} }
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We present the results of a search for gravitational-wave transients associated with core-collapse supernova SN 2023ixf, which was observed in the galaxy Messier 101 via optical emission on 2023 May 19th, during the LIGO-Virgo-KAGRA 15th Engineering Run. We define a five-day on-source window during which an accompanying gravitational-wave signal may have occurred. No gravitational waves have been identified in data when at least two gravitational-wave observatories were operating, which covered $\sim 14\%$ of this five-day window. We report the search detection efficiency for various possible gravitational-wave emission models. Considering the distance to M101 (6.7 Mpc), we derive constraints on the gravitational-wave emission mechanism of core-collapse supernovae across a broad frequency spectrum, ranging from 50 Hz to 2 kHz where we assume the GW emission occurred when coincident data are available in the on-source window. Considering an ellipsoid model for a rotating proto-neutron star, our search is sensitive to gravitational-wave energy $1 \times 10^{-5} M_{\odot} c^2$ and luminosity $4 \times 10^{-5} M_{\odot} c^2/\text{s}$ for a source emitting at 50 Hz. These constraints are around an order of magnitude more stringent than those obtained so far with gravitational-wave data. The constraint on the ellipticity of the proto-neutron star that is formed is as low as $1.04$, at frequencies above $1200$ Hz, surpassing results from SN 2019ejj.
Deep kiloparsec view of the molecular gas in a massive star-forming galaxy at cosmic noon
Sebastián Arriagada-Neira, Rodrigo Herrera-Camus, Vicente Villanueva, Natascha M. Förster Schreiber, Minju Lee, Alberto Bolatto, Jianhang Chen, Reinhard Genzel, Daizhong Liu, Alvio Renzini, Linda J. Tacconi, Giulia Tozzi, Hannah Übler
Oct 22 2024 astro-ph.GA arXiv:2410.14781v2

@misc{2410.14781, author = {Sebastián Arriagada-Neira and Rodrigo Herrera-Camus and Vicente Villanueva and Natascha M.~Förster Schreiber and Minju Lee and Alberto Bolatto and Jianhang Chen and Reinhard Genzel and Daizhong Liu and Alvio Renzini and Linda J.~Tacconi and Giulia Tozzi and Hannah Übler}, title = {{D}eep kiloparsec view of the molecular gas in a massive star-forming galaxy at cosmic noon}, year = {2024}, eprint = {2410.14781}, note = {arXiv:2410.14781v2} }
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We present deep ($\sim$ 20 hr), high-angular resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations of the $\rm CO ~ (4-3)$ and $\rm [CI] ~ (1-0)$ transitions, along with the rest-frame 630 $\mu$m dust continuum, in BX610 --a massive, main-sequence galaxy at the peak epoch of cosmic star formation $(z = 2.21)$. Combined with deep Very Large Telescope (VLT) SINFONI observations of the H$\alpha$ line, we characterize the molecular gas and star formation activity on kiloparsec scales. Our analysis reveals that the excitation of the molecular gas, as traced by the $L'_{\rm CO ~ (4-3)} / L'_{\rm [CI] ~ (1-0)}$ line luminosity ratio, decreases with increasing galactocentric radius. While the line luminosity ratios in the outskirts are similar to those typically found in main-sequence galaxies at $z \sim 1$, the ratios in the central regions of BX610 are comparable to those observed in local starbursts. There is also a giant extra-nuclear star-forming clump in the southwest of BX610 that exhibits high star formation activity, molecular gas abundance, and molecular gas excitation. Furthermore, the central region of BX610 is rich in molecular gas $(M_{\rm mol} / M_{\rm \star} \approx 1)$; however, at the current level of star formation activity, such molecular gas is expected to be depleted in $\sim$ 450 Myr. This, along with recent evidence for rapid inflow toward the center, suggests that BX610 may be experiencing an evolutionary phase often referred to as wet compaction, which is expected to lead to central gas depletion and subsequent inside-out quenching of star formation activity.
Optimising the Processing and Storage of Visibilities using lossy compression
Richard Dodson, Alex Williamson, Qian Gong, Pascal Elahi, Andreas Wicenec, Maria J. Rioja, Jieyang Chen, Norbert Podhorszki, Scott Klasky
Oct 22 2024 astro-ph.IM arXiv:2410.15683v1

@misc{2410.15683, author = {Richard Dodson and Alex Williamson and Qian Gong and Pascal Elahi and Andreas Wicenec and Maria J.~Rioja and Jieyang Chen and Norbert Podhorszki and Scott Klasky}, title = {{O}ptimising the {P}rocessing and {S}torage of {V}isibilities using lossy compression}, year = {2024}, eprint = {2410.15683}, note = {arXiv:2410.15683v1} }
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The next-generation radio astronomy instruments are providing a massive increase in sensitivity and coverage, through increased stations in the array and frequency span. Two primary problems encountered when processing the resultant avalanche of data are the need for abundant storage and I/O. An example of this is the data deluge expected from the SKA Telescopes of more than 60PB per day, all to be stored on the buffer filesystem. Compressing the data is an obvious solution. We used MGARD, an error-controlled compressor, and applied it to simulated and real visibility data, in noise-free and noise-dominated regimes. As the data has an implicit error level in the system temperature, using an error bound in compression provides a natural metric for compression. Measuring the degradation of images reconstructed using the lossy compressed data, we explore the trade-off between these error bounds and the corresponding compression ratios, as well as the impact on science quality derived from the lossy compressed data products through a series of experiments. We studied the global and local impacts on the output images. We found relative error bounds of as much as $10\%$, which provide compression ratios of about 20, have a limited impact on the continuum imaging as the increased noise is less than the image RMS. For extremely sensitive observations and for very precious data, we would recommend a $0.1\%$ error bound with compression ratios of about 4. These have noise impacts two orders of magnitude less than the image RMS levels. At these levels, the limits are due to instabilities in the deconvolution methods. We compared the results to the alternative compression tool DYSCO. MGARD provides better compression for similar results, and has a host of potentially powerful additional features.
Enhanced $S$-factor for the $^{14}$N$(p,\gamma)^{15}$O reaction and its impact on the solar composition problem
X. Chen, J. Su, Y. P. Shen, L. Y. Zhang, J. J. He, S. Z. Chen, S. Wang, Z. L. Shen, S. Lin, L. Y. Song, H. Zhang, L. H. Wang, X. Z. Jiang, L. Wang, Y. T. Huang, Z. W. Qin, F. C. Liu, Y. D. Sheng, Y. J. Chen, Y. L. Lu, et al (28)
Oct 22 2024 nucl-ex astro-ph.SR arXiv:2410.16086v1

@misc{2410.16086, author = {X.~Chen and J.~Su and Y.~P.~Shen and L.~Y.~Zhang and J.~J.~He and S.~Z.~Chen and S.~Wang and Z.~L.~Shen and S.~Lin and L.~Y.~Song and H.~Zhang and L.~H.~Wang and X.~Z.~Jiang and L.~Wang and Y.~T.~Huang and Z.~W.~Qin and F.~C.~Liu and Y.~D.~Sheng and Y.~J.~Chen and Y.~L.~Lu and X.~Y.~Li and J.~Y.~Dong and Y.~C.~Jiang and Y.~Q.~Zhang and Y.~Zhang and J.~W.~Tian and D.~Xiao and Y.~Zhang and Z.~M.~Li and X.~C.~Han and J.~J.~Wei and H.~Li and Z.~An and W.~P.~Lin and B.~Liao and H.~N.~Liu and F.~S.~Zhang and M.~L.~Qiu and C.~Xu and S.~L.~Jin and F.~Lu and J.~F.~Chen and W.~Nan and Y.~B.~Wang and Z.~H.~Li and B.~Guo and Y.~Q.~Gu and W.~P.~Liu}, title = {{E}nhanced ${S}$-factor for the $^{14}${N}$(p,\gamma)^{15}${O} reaction and its impact on the solar composition problem}, year = {2024}, eprint = {2410.16086}, note = {arXiv:2410.16086v1} }
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The solar composition problem has puzzled astrophysicists for more than 20 years. Recent measurements of carbon-nitrogen-oxygen (CNO) neutrinos by the Borexino experiment show a $\sim2\sigma$ tension with the "low-metallicity" determinations. $^{14}$N$(p,\gamma)^{15}$O, the slowest reaction in the CNO cycle, plays a crucial role in the standard solar model (SSM) calculations of CNO neutrino fluxes. Here we report a direct measurement of the $^{14}$N$(p,\gamma)^{15}$O reaction, in which $S$-factors for all transitions were simultaneously determined in the energy range of $E_p=110-260$ keV for the first time. Our results resolve previous discrepancies in the ground-state transition, yielding a zero-energy $S$-factor $S_{114}(0) = 1.92\pm0.08$ keV b which is 14% higher than the $1.68\pm0.14$ keV b recommended in Solar Fusion III (SF-III). With our $S_{114}$ values, the SSM B23-GS98, and the latest global analysis of solar neutrino measurements, the C and N photospheric abundance determined by the Borexino experiment is updated to $N_{\mathrm{CN}}=({4.45}^{+0.69}_{-0.61})\times10^{-4}$. This new $N_{\mathrm{CN}}$ value agrees well with latest "high-metallicity" composition, however, is also consistent with the "low-metallicity" determination within $\sim 1\sigma$ C.L., indicating that the solar metallicity problem remains an open question. In addition, the significant reduction in the uncertainty of $S_{114}$ paves the way for the precise determination of the CN abundance in future large-volume solar neutrino measurements.
A search using GEO600 for gravitational waves coincident with fast radio bursts from SGR 1935+2154
LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, A. G. Abac, R. Abbott, I. Abouelfettouh, F. Acernese, K. Ackley, S. Adhicary, N. Adhikari, R. X. Adhikari, V. K. Adkins, D. Agarwal, M. Agathos, M. Aghaei Abchouyeh, O. D. Aguiar, I. Aguilar, L. Aiello, A. Ain, P. Ajith, et al (1763)
Oct 15 2024 astro-ph.HE arXiv:2410.09151v1

@misc{2410.09151, author = {LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration and A.~G.~Abac and R.~Abbott and I.~Abouelfettouh and F.~Acernese and K.~Ackley and S.~Adhicary and N.~Adhikari and R.~X.~Adhikari and V.~K.~Adkins and D.~Agarwal and M.~Agathos and M.~Aghaei Abchouyeh and O.~D.~Aguiar and I.~Aguilar and L.~Aiello and A.~Ain and P.~Ajith and T.~Akutsu and S.~Albanesi and R.~A.~Alfaidi and A.~Al-Jodah and C.~Alléné and A.~Allocca and S.~Al-Shammari and P.~A.~Altin and S.~Alvarez-Lopez and A.~Amato and L.~Amez-Droz and A.~Amorosi and C.~Amra and A.~Ananyeva and S.~B.~Anderson and W.~G.~Anderson and M.~Andia and M.~Ando and T.~Andrade and N.~Andres and M.~Andrés-Carcasona and T.~Andrić and J.~Anglin and S.~Ansoldi and J.~M.~Antelis and S.~Antier and M.~Aoumi and E.~Z.~Appavuravther and S.~Appert and S.~K.~Apple and K.~Arai and A.~Araya and M.~C.~Araya and J.~S.~Areeda and L.~Argianas and N.~Aritomi and F.~Armato and N.~Arnaud and M.~Arogeti and S.~M.~Aronson and G.~Ashton and Y.~Aso and M.~Assiduo and S.~Assis de Souza Melo and S.~M.~Aston and P.~Astone and F.~Attadio and F.~Aubin and K.~AultONeal and G.~Avallone and D.~Azrad and S.~Babak and F.~Badaracco and C.~Badger and S.~Bae and S.~Bagnasco and E.~Bagui and J.~G.~Baier and L.~Baiotti and R.~Bajpai and T.~Baka and M.~Ball and G.~Ballardin and S.~W.~Ballmer and S.~Banagiri and B.~Banerjee and D.~Bankar and P.~Baral and J.~C.~Barayoga and B.~C.~Barish and D.~Barker and P.~Barneo and F.~Barone and B.~Barr and L.~Barsotti and M.~Barsuglia and D.~Barta and A.~M.~Bartoletti and M.~A.~Barton and I.~Bartos and S.~Basak and A.~Basalaev and R.~Bassiri and A.~Basti and D.~E.~Bates and M.~Bawaj and P.~Baxi and J.~C.~Bayley and A.~C.~Baylor and P.~A.~Baynard II and M.~Bazzan and V.~M.~Bedakihale and F.~Beirnaert and M.~Bejger and D.~Belardinelli and A.~S.~Bell and V.~Benedetto and W.~Benoit and J.~D.~Bentley and M.~Ben Yaala and S.~Bera and M.~Berbel and F.~Bergamin and B.~K.~Berger and S.~Bernuzzi and M.~Beroiz and D.~Bersanetti and A.~Bertolini and J.~Betzwieser and D.~Beveridge and N.~Bevins and R.~Bhandare and U.~Bhardwaj and R.~Bhatt and D.~Bhattacharjee and S.~Bhaumik and S.~Bhowmick and A.~Bianchi and I.~A.~Bilenko and G.~Billingsley and A.~Binetti and S.~Bini and O.~Birnholtz and S.~Biscoveanu and A.~Bisht and M.~Bitossi and M.-A.~Bizouard and J.~K.~Blackburn and L.~A.~Blagg and C.~D.~Blair and D.~G.~Blair and F.~Bobba and N.~Bode and G.~Boileau and M.~Boldrini and G.~N.~Bolingbroke and A.~Bolliand and L.~D.~Bonavena and R.~Bondarescu and F.~Bondu and E.~Bonilla and M.~S.~Bonilla and A.~Bonino and R.~Bonnand and P.~Booker and A.~Borchers and V.~Boschi and S.~Bose and V.~Bossilkov and V.~Boudart and A.~Boudon and A.~Bozzi and C.~Bradaschia and P.~R.~Brady and M.~Braglia and A.~Branch and M.~Branchesi and J.~Brandt and I.~Braun and M.~Breschi and T.~Briant and A.~Brillet and M.~Brinkmann and P.~Brockill and E.~Brockmueller and A.~F.~Brooks and B.~C.~Brown and D.~D.~Brown and M.~L.~Brozzetti and S.~Brunett and G.~Bruno and R.~Bruntz and J.~Bryant and F.~Bucci and J.~Buchanan and O.~Bulashenko and T.~Bulik and H.~J.~Bulten and A.~Buonanno and K.~Burtnyk and R.~Buscicchio and D.~Buskulic and C.~Buy and R.~L.~Byer and G.~S.~Cabourn Davies and G.~Cabras and R.~Cabrita and V.~Cáceres-Barbosa and L.~Cadonati and G.~Cagnoli and C.~Cahillane and J.~Calderón Bustillo and T.~A.~Callister and E.~Calloni and J.~B.~Camp and M.~Canepa and G.~Caneva Santoro and K.~C.~Cannon and H.~Cao and L.~A.~Capistran and E.~Capocasa and E.~Capote and G.~Carapella and F.~Carbognani and M.~Carlassara and J.~B.~Carlin and M.~Carpinelli and G.~Carrillo and J.~J.~Carter and G.~Carullo and J.~Casanueva Diaz and C.~Casentini and S.~Y.~Castro-Lucas and S.~Caudill and M.~Cavaglià and R.~Cavalieri and G.~Cella and P.~Cerdá-Durán and E.~Cesarini and W.~Chaibi and P.~Chakraborty and S.~Chalathadka Subrahmanya and J.~C.~L.~Chan and M.~Chan and K.~Chandra and R.-J.~Chang and S.~Chao and E.~L.~Charlton and P.~Charlton and E.~Chassande-Mottin and C.~Chatterjee and Debarati Chatterjee and Deep Chatterjee and M.~Chaturvedi and S.~Chaty and A.~Chen and A.~H.-Y.~Chen and D.~Chen and H.~Chen and H.~Y.~Chen and J.~Chen and K.~H.~Chen and Y.~Chen and Yanbei Chen and Yitian Chen and H.~P.~Cheng and P.~Chessa and H.~T.~Cheung and S.~Y.~Cheung and F.~Chiadini and G.~Chiarini and R.~Chierici and A.~Chincarini and M.~L.~Chiofalo and A.~Chiummo and C.~Chou and S.~Choudhary and N.~Christensen and S.~S.~Y.~Chua and P.~Chugh and G.~Ciani and P.~Ciecielag and M.~Cieślar and M.~Cifaldi and R.~Ciolfi and F.~Clara and J.~A.~Clark and J.~Clarke and T.~A.~Clarke and P.~Clearwater and S.~Clesse and E.~Coccia and E.~Codazzo and P.-F.~Cohadon and S.~Colace and M.~Colleoni and C.~G.~Collette and J.~Collins and S.~Colloms and A.~Colombo and M.~Colpi and C.~M.~Compton and G.~Connolly and L.~Conti and T.~R.~Corbitt and I.~Cordero-Carrión and S.~Corezzi and N.~J.~Cornish and A.~Corsi and S.~Cortese and C.~A.~Costa and R.~Cottingham and M.~W.~Coughlin and A.~Couineaux and J.-P.~Coulon and S.~T.~Countryman and J.-F.~Coupechoux and P.~Couvares and D.~M.~Coward and M.~J.~Cowart and R.~Coyne and K.~Craig and R.~Creed and J.~D.~E.~Creighton and T.~D.~Creighton and P.~Cremonese and A.~W.~Criswell and J.~C.~G.~Crockett-Gray and S.~Crook and R.~Crouch and J.~Csizmazia and J.~R.~Cudell and T.~J.~Cullen and A.~Cumming and E.~Cuoco and M.~Cusinato and P.~Dabadie and T.~Dal Canton and S.~Dall'Osso and S.~Dal Pra and G.~Dálya and B.~D'Angelo and S.~Danilishin and S.~D'Antonio and K.~Danzmann and K.~E.~Darroch and L.~P.~Dartez and A.~Dasgupta and S.~Datta and V.~Dattilo and A.~Daumas and N.~Davari and I.~Dave and A.~Davenport and M.~Davier and T.~F.~Davies and D.~Davis and L.~Davis and M.~C.~Davis and P.~J.~Davis and M.~Dax and J.~De Bolle and M.~Deenadayalan and J.~Degallaix and M.~De Laurentis and S.~Deléglise and F.~De Lillo and D.~Dell'Aquila and W.~Del Pozzo and F.~De Marco and F.~De Matteis and V.~D'Emilio and N.~Demos and T.~Dent and A.~Depasse and N.~DePergola and R.~De Pietri and R.~De Rosa and C.~De Rossi and R.~DeSalvo and R.~De Simone and A.~Dhani and R.~Diab and M.~C.~Díaz and M.~Di Cesare and G.~Dideron and N.~A.~Didio and T.~Dietrich and L.~Di Fiore and C.~Di Fronzo and M.~Di Giovanni and T.~Di Girolamo and D.~Diksha and A.~Di Michele and J.~Ding and S.~Di Pace and I.~Di Palma and F.~Di Renzo and Divyajyoti and A.~Dmitriev and Z.~Doctor and E.~Dohmen and P.~P.~Doleva and D.~Dominguez and L.~D'Onofrio and F.~Donovan and K.~L.~Dooley and T.~Dooney and S.~Doravari and O.~Dorosh and M.~Drago and J.~C.~Driggers and J.-G.~Ducoin and L.~Dunn and U.~Dupletsa and D.~D'Urso and H.~Duval and P.-A.~Duverne and S.~E.~Dwyer and C.~Eassa and M.~Ebersold and T.~Eckhardt and G.~Eddolls and B.~Edelman and T.~B.~Edo and O.~Edy and A.~Effler and J.~Eichholz and H.~Einsle and M.~Eisenmann and R.~A.~Eisenstein and A.~Ejlli and R.~M.~Eleveld and M.~Emma and K.~Endo and A.~J.~Engl and E.~Enloe and L.~Errico and R.~C.~Essick and H.~Estellés and D.~Estevez and T.~Etzel and M.~Evans and T.~Evstafyeva and B.~E.~Ewing and J.~M.~Ezquiaga and F.~Fabrizi and F.~Faedi and V.~Fafone and S.~Fairhurst and A.~M.~Farah and B.~Farr and W.~M.~Farr and G.~Favaro and M.~Favata and M.~Fays and M.~Fazio and J.~Feicht and M.~M.~Fejer and R.~.~Felicetti and E.~Fenyvesi and D.~L.~Ferguson and S.~Ferraiuolo and I.~Ferrante and T.~A.~Ferreira and F.~Fidecaro and P.~Figura and A.~Fiori and I.~Fiori and M.~Fishbach and R.~P.~Fisher and R.~Fittipaldi and V.~Fiumara and R.~Flaminio and S.~M.~Fleischer and L.~S.~Fleming and E.~Floden and E.~M.~Foley and H.~Fong and J.~A.~Font and B.~Fornal and P.~W.~F.~Forsyth and K.~Franceschetti and N.~Franchini and S.~Frasca and F.~Frasconi and A.~Frattale Mascioli and Z.~Frei and A.~Freise and O.~Freitas and R.~Frey and W.~Frischhertz and P.~Fritschel and V.~V.~Frolov and G.~G.~Fronzé and M.~Fuentes-Garcia and S.~Fujii and T.~Fujimori and P.~Fulda and M.~Fyffe and B.~Gadre and J.~R.~Gair and S.~Galaudage and V.~Galdi and H.~Gallagher and S.~Gallardo and B.~Gallego and R.~Gamba and A.~Gamboa and D.~Ganapathy and A.~Ganguly and B.~Garaventa and J.~García-Bellido and C.~García Núñez and C.~García-Quirós and J.~W.~Gardner and K.~A.~Gardner and J.~Gargiulo and A.~Garron and F.~Garufi and C.~Gasbarra and B.~Gateley and V.~Gayathri and G.~Gemme and A.~Gennai and V.~Gennari and J.~George and R.~George and O.~Gerberding and L.~Gergely and S.~Ghonge and Archisman Ghosh and Sayantan Ghosh and Shaon Ghosh and Shrobana Ghosh and Suprovo Ghosh and Tathagata Ghosh and L.~Giacoppo and J.~A.~Giaime and K.~D.~Giardina and D.~R.~Gibson and D.~T.~Gibson and C.~Gier and P.~Giri and F.~Gissi and S.~Gkaitatzis and J.~Glanzer and F.~Glotin and J.~Godfrey and P.~Godwin and N.~L.~Goebbels and E.~Goetz and J.~Golomb and S.~Gomez Lopez and B.~Goncharov and Y.~Gong and G.~González and P.~Goodarzi and S.~Goode and A.~W.~Goodwin-Jones and M.~Gosselin and A.~S.~Göttel and R.~Gouaty and D.~W.~Gould and K.~Govorkova and S.~Goyal and B.~Grace and A.~Grado and V.~Graham and A.~E.~Granados and M.~Granata and V.~Granata and S.~Gras and P.~Grassia and A.~Gray and C.~Gray and R.~Gray and G.~Greco and A.~C.~Green and S.~M.~Green and S.~R.~Green and A.~M.~Gretarsson and E.~M.~Gretarsson and D.~Griffith and W.~L.~Griffiths and H.~L.~Griggs and G.~Grignani and A.~Grimaldi and C.~Grimaud and H.~Grote and D.~Guerra and D.~Guetta and G.~M.~Guidi and A.~R.~Guimaraes and H.~K.~Gulati and F.~Gulminelli and A.~M.~Gunny and H.~Guo and W.~Guo and Y.~Guo and Anchal Gupta and Anuradha Gupta and Ish Gupta and N.~C.~Gupta and P.~Gupta and S.~K.~Gupta and T.~Gupta and N.~Gupte and J.~Gurs and N.~Gutierrez and F.~Guzman and H.-Y.~H and D.~Haba and M.~Haberland and S.~Haino and E.~D.~Hall and E.~Z.~Hamilton and G.~Hammond and W.-B.~Han and M.~Haney and J.~Hanks and C.~Hanna and M.~D.~Hannam and O.~A.~Hannuksela and A.~G.~Hanselman and H.~Hansen and J.~Hanson and R.~Harada and A.~R.~Hardison and K.~Haris and T.~Harmark and J.~Harms and G.~M.~Harry and I.~W.~Harry and J.~Hart and B.~Haskell and C.-J.~Haster and J.~S.~Hathaway and K.~Haughian and H.~Hayakawa and K.~Hayama and R.~Hayes and A.~Heffernan and A.~Heidmann and M.~C.~Heintze and J.~Heinze and J.~Heinzel and H.~Heitmann and F.~Hellman and P.~Hello and A.~F.~Helmling-Cornell and G.~Hemming and O.~Henderson-Sapir and M.~Hendry and I.~S.~Heng and E.~Hennes and C.~Henshaw and T.~Hertog and M.~Heurs and A.~L.~Hewitt and J.~Heyns and S.~Higginbotham and S.~Hild and S.~Hill and Y.~Himemoto and N.~Hirata and C.~Hirose and W.~C.~G.~Ho and S.~Hoang and S.~Hochheim and D.~Hofman and N.~A.~Holland and K.~Holley-Bockelmann and Z.~J.~Holmes and D.~E.~Holz and L.~Honet and C.~Hong and J.~Hornung and S.~Hoshino and J.~Hough and S.~Hourihane and E.~J.~Howell and C.~G.~Hoy and C.~A.~Hrishikesh and H.-F.~Hsieh and C.~Hsiung and H.~C.~Hsu and W.-F.~Hsu and P.~Hu and Q.~Hu and H.~Y.~Huang and Y.-J.~Huang and A.~D.~Huddart and B.~Hughey and D.~C.~Y.~Hui and V.~Hui and S.~Husa and R.~Huxford and T.~Huynh-Dinh and L.~Iampieri and G.~A.~Iandolo and M.~Ianni and A.~Iess and H.~Imafuku and K.~Inayoshi and Y.~Inoue and G.~Iorio and M.~H.~Iqbal and J.~Irwin and R.~Ishikawa and M.~Isi and M.~A.~Ismail and Y.~Itoh and H.~Iwanaga and M.~Iwaya and B.~R.~Iyer and V.~JaberianHamedan and C.~Jacquet and P.-E.~Jacquet and S.~J.~Jadhav and S.~P.~Jadhav and T.~Jain and A.~L.~James and P.~A.~James and R.~Jamshidi and J.~Janquart and K.~Janssens and N.~N.~Janthalur and S.~Jaraba and P.~Jaranowski and R.~Jaume and W.~Javed and A.~Jennings and W.~Jia and J.~Jiang and J.~Kubisz and C.~Johanson and G.~R.~Johns and N.~A.~Johnson and M.~C.~Johnston and R.~Johnston and N.~Johny and D.~H.~Jones and D.~I.~Jones and R.~Jones and S.~Jose and P.~Joshi and L.~Ju and K.~Jung and J.~Junker and V.~Juste and T.~Kajita and I.~Kaku and C.~Kalaghatgi and V.~Kalogera and M.~Kamiizumi and N.~Kanda and S.~Kandhasamy and G.~Kang and J.~B.~Kanner and S.~J.~Kapadia and D.~P.~Kapasi and S.~Karat and C.~Karathanasis and R.~Kashyap and M.~Kasprzack and W.~Kastaun and T.~Kato and E.~Katsavounidis and W.~Katzman and R.~Kaushik and K.~Kawabe and R.~Kawamoto and A.~Kazemi and D.~Keitel and J.~Kelley-Derzon and J.~Kennington and R.~Kesharwani and J.~S.~Key and R.~Khadela and S.~Khadka and F.~Y.~Khalili and F.~Khan and I.~Khan and T.~Khanam and M.~Khursheed and N.~M.~Khusid and W.~Kiendrebeogo and N.~Kijbunchoo and C.~Kim and J.~C.~Kim and K.~Kim and M.~H.~Kim and S.~Kim and Y.-M.~Kim and C.~Kimball and M.~Kinley-Hanlon and M.~Kinnear and J.~S.~Kissel and S.~Klimenko and A.~M.~Knee and N.~Knust and K.~Kobayashi and P.~Koch and S.~M.~Koehlenbeck and G.~Koekoek and K.~Kohri and K.~Kokeyama and S.~Koley and P.~Kolitsidou and M.~Kolstein and K.~Komori and A.~K.~H.~Kong and A.~Kontos and M.~Korobko and R.~V.~Kossak and X.~Kou and A.~Koushik and N.~Kouvatsos and M.~Kovalam and D.~B.~Kozak and S.~L.~Kranzhoff and V.~Kringel and N.~V.~Krishnendu and A.~Królak and K.~Kruska and G.~Kuehn and P.~Kuijer and S.~Kulkarni and A.~Kulur Ramamohan and A.~Kumar and Praveen Kumar and Prayush Kumar and Rahul Kumar and Rakesh Kumar and J.~Kume and K.~Kuns and N.~Kuntimaddi and S.~Kuroyanagi and N.~J.~Kurth and S.~Kuwahara and K.~Kwak and K.~Kwan and J.~Kwok and G.~Lacaille and P.~Lagabbe and D.~Laghi and S.~Lai and A.~H.~Laity and M.~H.~Lakkis and E.~Lalande and M.~Lalleman and P.~C.~Lalremruati and M.~Landry and B.~B.~Lane and R.~N.~Lang and J.~Lange and B.~Lantz and A.~La Rana and I.~La Rosa and A.~Lartaux-Vollard and P.~D.~Lasky and J.~Lawrence and M.~N.~Lawrence and M.~Laxen and A.~Lazzarini and C.~Lazzaro and P.~Leaci and Y.~K.~Lecoeuche and H.~M.~Lee and H.~W.~Lee and K.~Lee and R.-K.~Lee and R.~Lee and S.~Lee and Y.~Lee and I.~N.~Legred and J.~Lehmann and L.~Lehner and M.~Le Jean and A.~Lemaître and M.~Lenti and M.~Leonardi and M.~Lequime and N.~Leroy and M.~Lesovsky and N.~Letendre and M.~Lethuillier and S.~E.~Levin and Y.~Levin and K.~Leyde and A.~K.~Y.~Li and K.~L.~Li and T.~G.~F.~Li and X.~Li and Z.~Li and A.~Lihos and C-Y.~Lin and C.-Y.~Lin and E.~T.~Lin and F.~Lin and H.~Lin and L.~C.-C.~Lin and Y.-C.~Lin and F.~Linde and S.~D.~Linker and T.~B.~Littenberg and A.~Liu and G.~C.~Liu and Jian Liu and F.~Llamas Villarreal and J.~Llobera-Querol and R.~K.~L.~Lo and J.-P.~Locquet and L.~T.~London and A.~Longo and D.~Lopez and M.~Lopez Portilla and M.~Lorenzini and A.~Lorenzo-Medina and V.~Loriette and M.~Lormand and G.~Losurdo and T.~P.~Lott IV and J.~D.~Lough and H.~A.~Loughlin and C.~O.~Lousto and M.~J.~Lowry and N.~Lu and H.~Lück and D.~Lumaca and A.~P.~Lundgren and A.~W.~Lussier and L.-T.~Ma and S.~Ma and M.~Ma'arif and R.~Macas and A.~Macedo and M.~MacInnis and R.~R.~Maciy and D.~M.~Macleod and I.~A.~O.~MacMillan and A.~Macquet and D.~Macri and K.~Maeda and S.~Maenaut and I.~Magaña Hernandez and S.~S.~Magare and C.~Magazzù and R.~M.~Magee and E.~Maggio and R.~Maggiore and M.~Magnozzi and M.~Mahesh and S.~Mahesh and M.~Maini and S.~Majhi and E.~Majorana and C.~N.~Makarem and E.~Makelele and J.~A.~Malaquias-Reis and U.~Mali and S.~Maliakal and A.~Malik and N.~Man and V.~Mandic and V.~Mangano and B.~Mannix and G.~L.~Mansell and G.~Mansingh and M.~Manske and M.~Mantovani and M.~Mapelli and F.~Marchesoni and D.~Marín Pina and F.~Marion and S.~Márka and Z.~Márka and A.~S.~Markosyan and A.~Markowitz and E.~Maros and S.~Marsat and F.~Martelli and I.~W.~Martin and R.~M.~Martin and B.~B.~Martinez and M.~Martinez and V.~Martinez and A.~Martini and K.~Martinovic and J.~C.~Martins and D.~V.~Martynov and E.~J.~Marx and L.~Massaro and A.~Masserot and M.~Masso-Reid and M.~Mastrodicasa and S.~Mastrogiovanni and T.~Matcovich and M.~Matiushechkina and M.~Matsuyama and N.~Mavalvala and N.~Maxwell and G.~McCarrol and R.~McCarthy and S.~McCormick and L.~McCuller and S.~McEachin and C.~McElhenny and G.~I.~McGhee and J.~McGinn and K.~B.~M.~McGowan and J.~McIver and A.~McLeod and T.~McRae and D.~Meacher and Q.~Meijer and A.~Melatos and S.~Mellaerts and A.~Menendez-Vazquez and C.~S.~Menoni and F.~Mera and R.~A.~Mercer and L.~Mereni and K.~Merfeld and E.~L.~Merilh and J.~R.~Mérou and J.~D.~Merritt and M.~Merzougui and C.~Messenger and C.~Messick and M.~Meyer-Conde and F.~Meylahn and A.~Mhaske and A.~Miani and H.~Miao and I.~Michaloliakos and C.~Michel and Y.~Michimura and H.~Middleton and A.~L.~Miller and S.~Miller and M.~Millhouse and E.~Milotti and V.~Milotti and Y.~Minenkov and N.~Mio and Ll.~M.~Mir and L.~Mirasola and M.~Miravet-Tenés and C.-A.~Miritescu and A.~K.~Mishra and A.~Mishra and C.~Mishra and T.~Mishra and A.~L.~Mitchell and J.~G.~Mitchell and S.~Mitra and V.~P.~Mitrofanov and R.~Mittleman and O.~Miyakawa and S.~Miyamoto and S.~Miyoki and G.~Mo and L.~Mobilia and S.~R.~P.~Mohapatra and S.~R.~Mohite and M.~Molina-Ruiz and C.~Mondal and M.~Mondin and M.~Montani and C.~J.~Moore and D.~Moraru and A.~More and S.~More and G.~Moreno and C.~Morgan and S.~Morisaki and Y.~Moriwaki and G.~Morras and A.~Moscatello and P.~Mourier and B.~Mours and C.~M.~Mow-Lowry and F.~Muciaccia and Arunava Mukherjee and D.~Mukherjee and Samanwaya Mukherjee and Soma Mukherjee and Subroto Mukherjee and Suvodip Mukherjee and N.~Mukund and A.~Mullavey and J.~Munch and J.~Mundi and C.~L.~Mungioli and W.~R.~Munn Oberg and Y.~Murakami and M.~Murakoshi and P.~G.~Murray and S.~Muusse and D.~Nabari and S.~L.~Nadji and A.~Nagar and N.~Nagarajan and K.~N.~Nagler and K.~Nakagaki and K.~Nakamura and H.~Nakano and M.~Nakano and D.~Nandi and V.~Napolano and P.~Narayan and I.~Nardecchia and H.~Narola and L.~Naticchioni and R.~K.~Nayak and J.~Neilson and A.~Nelson and T.~J.~N.~Nelson and M.~Nery and A.~Neunzert and S.~Ng and L.~Nguyen Quynh and S.~A.~Nichols and A.~B.~Nielsen and G.~Nieradka and A.~Niko and Y.~Nishino and A.~Nishizawa and S.~Nissanke and E.~Nitoglia and W.~Niu and F.~Nocera and M.~Norman and C.~North and J.~Novak and J.~F.~Nuño Siles and L.~K.~Nuttall and K.~Obayashi and J.~Oberling and J.~O'Dell and M.~Oertel and A.~Offermans and G.~Oganesyan and J.~J.~Oh and K.~Oh and T.~O'Hanlon and M.~Ohashi and M.~Ohkawa and F.~Ohme and A.~S.~Oliveira and R.~Oliveri and B.~O'Neal and K.~Oohara and B.~O'Reilly and N.~D.~Ormsby and M.~Orselli and R.~O'Shaughnessy and S.~O'Shea and Y.~Oshima and S.~Oshino and S.~Ossokine and C.~Osthelder and I.~Ota and D.~J.~Ottaway and A.~Ouzriat and H.~Overmier and B.~J.~Owen and A.~E.~Pace and R.~Pagano and M.~A.~Page and A.~Pai and A.~Pal and S.~Pal and M.~A.~Palaia and M.~Pálfi and P.~P.~Palma and C.~Palomba and P.~Palud and H.~Pan and J.~Pan and K.~C.~Pan and R.~Panai and P.~K.~Panda and S.~Pandey and L.~Panebianco and P.~T.~H.~Pang and F.~Pannarale and K.~A.~Pannone and B.~C.~Pant and F.~H.~Panther and F.~Paoletti and A.~Paolone and E.~E.~Papalexakis and L.~Papalini and G.~Papigkiotis and A.~Paquis and A.~Parisi and B.-J.~Park and J.~Park and W.~Parker and G.~Pascale and D.~Pascucci and A.~Pasqualetti and R.~Passaquieti and L.~Passenger and D.~Passuello and O.~Patane and D.~Pathak and M.~Pathak and A.~Patra and B.~Patricelli and A.~S.~Patron and K.~Paul and S.~Paul and E.~Payne and T.~Pearce and M.~Pedraza and R.~Pegna and A.~Pele and F.~E.~Peña Arellano and S.~Penn and M.~D.~Penuliar and A.~Perego and Z.~Pereira and J.~J.~Perez and C.~Périgois and G.~Perna and A.~Perreca and J.~Perret and S.~Perriès and J.~W.~Perry and D.~Pesios and S.~Petracca and C.~Petrillo and H.~P.~Pfeiffer and H.~Pham and K.~A.~Pham and K.~S.~Phukon and H.~Phurailatpam and M.~Piarulli and L.~Piccari and O.~J.~Piccinni and M.~Pichot and M.~Piendibene and F.~Piergiovanni and L.~Pierini and G.~Pierra and V.~Pierro and M.~Pietrzak and M.~Pillas and F.~Pilo and L.~Pinard and I.~M.~Pinto and M.~Pinto and B.~J.~Piotrzkowski and M.~Pirello and M.~D.~Pitkin and A.~Placidi and E.~Placidi and M.~L.~Planas and W.~Plastino and R.~Poggiani and E.~Polini and L.~Pompili and J.~Poon and E.~Porcelli and E.~K.~Porter and C.~Posnansky and R.~Poulton and J.~Powell and M.~Pracchia and B.~K.~Pradhan and T.~Pradier and A.~K.~Prajapati and K.~Prasai and R.~Prasanna and P.~Prasia and G.~Pratten and G.~Principe and M.~Principe and G.~A.~Prodi and L.~Prokhorov and P.~Prosposito and A.~Puecher and J.~Pullin and M.~Punturo and P.~Puppo and M.~Pürrer and H.~Qi and J.~Qin and G.~Quéméner and V.~Quetschke and C.~Quigley and P.~J.~Quinonez and R.~Quitzow-James and F.~J.~Raab and S.~S.~Raabith and G.~Raaijmakers and S.~Raja and C.~Rajan and B.~Rajbhandari and K.~E.~Ramirez and F.~A.~Ramis Vidal and A.~Ramos-Buades and D.~Rana and S.~Ranjan and K.~Ransom and P.~Rapagnani and B.~Ratto and S.~Rawat and A.~Ray and V.~Raymond and M.~Razzano and J.~Read and M.~Recaman Payo and T.~Regimbau and L.~Rei and S.~Reid and D.~H.~Reitze and P.~Relton and A.~I.~Renzini and P.~Rettegno and B.~Revenu and R.~Reyes and A.~S.~Rezaei and F.~Ricci and M.~Ricci and A.~Ricciardone and J.~W.~Richardson and M.~Richardson and A.~Rijal and K.~Riles and H.~K.~Riley and S.~Rinaldi and J.~Rittmeyer and C.~Robertson and F.~Robinet and M.~Robinson and A.~Rocchi and L.~Rolland and J.~G.~Rollins and A.~E.~Romano and R.~Romano and A.~Romero and I.~M.~Romero-Shaw and J.~H.~Romie and S.~Ronchini and T.~J.~Roocke and L.~Rosa and T.~J.~Rosauer and C.~A.~Rose and D.~Rosińska and M.~P.~Ross and M.~Rossello and S.~Rowan and S.~K.~Roy and S.~Roy and D.~Rozza and P.~Ruggi and N.~Ruhama and E.~Ruiz Morales and K.~Ruiz-Rocha and S.~Sachdev and T.~Sadecki and J.~Sadiq and P.~Saffarieh and M.~R.~Sah and S.~S.~Saha and S.~Saha and T.~Sainrat and S.~Sajith Menon and K.~Sakai and M.~Sakellariadou and S.~Sakon and O.~S.~Salafia and F.~Salces-Carcoba and L.~Salconi and M.~Saleem and F.~Salemi and M.~Sallé and S.~Salvador and A.~Sanchez and E.~J.~Sanchez and J.~H.~Sanchez and L.~E.~Sanchez and N.~Sanchis-Gual and J.~R.~Sanders and E.~M.~Sänger and F.~Santoliquido and T.~R.~Saravanan and N.~Sarin and S.~Sasaoka and A.~Sasli and P.~Sassi and B.~Sassolas and H.~Satari and R.~Sato and Y.~Sato and O.~Sauter and R.~L.~Savage and T.~Sawada and H.~L.~Sawant and S.~Sayah and V.~Scacco and D.~Schaetzl and M.~Scheel and A.~Schiebelbein and M.~G.~Schiworski and P.~Schmidt and S.~Schmidt and R.~Schnabel and M.~Schneewind and R.~M.~S.~Schofield and K.~Schouteden and B.~W.~Schulte and B.~F.~Schutz and E.~Schwartz and M.~Scialpi and J.~Scott and S.~M.~Scott and T.~C.~Seetharamu and M.~Seglar-Arroyo and Y.~Sekiguchi and D.~Sellers and A.~S.~Sengupta and D.~Sentenac and E.~G.~Seo and J.~W.~Seo and V.~Sequino and M.~Serra and G.~Servignat and A.~Sevrin and T.~Shaffer and U.~S.~Shah and M.~A.~Shaikh and L.~Shao and A.~K.~Sharma and P.~Sharma and S.~Sharma-Chaudhary and M.~R.~Shaw and P.~Shawhan and N.~S.~Shcheblanov and E.~Sheridan and Y.~Shikano and M.~Shikauchi and K.~Shimode and H.~Shinkai and J.~Shiota and D.~H.~Shoemaker and D.~M.~Shoemaker and R.~W.~Short and S.~ShyamSundar and A.~Sider and H.~Siegel and M.~Sieniawska and D.~Sigg and L.~Silenzi and M.~Simmonds and L.~P.~Singer and A.~Singh and D.~Singh and M.~K.~Singh and S.~Singh and A.~Singha and A.~M.~Sintes and V.~Sipala and V.~Skliris and B.~J.~J.~Slagmolen and T.~J.~Slaven-Blair and J.~Smetana and J.~R.~Smith and L.~Smith and R.~J.~E.~Smith and W.~J.~Smith and J.~Soldateschi and K.~Somiya and I.~Song and K.~Soni and S.~Soni and V.~Sordini and F.~Sorrentino and N.~Sorrentino and H.~Sotani and R.~Soulard and A.~Southgate and V.~Spagnuolo and A.~P.~Spencer and M.~Spera and P.~Spinicelli and J.~B.~Spoon and C.~A.~Sprague and A.~K.~Srivastava and F.~Stachurski and D.~A.~Steer and J.~Steinlechner and S.~Steinlechner and N.~Stergioulas and P.~Stevens and M.~StPierre and G.~Stratta and M.~D.~Strong and A.~Strunk and R.~Sturani and A.~L.~Stuver and M.~Suchenek and S.~Sudhagar and N.~Sueltmann and L.~Suleiman and K.~D.~Sullivan and L.~Sun and S.~Sunil and J.~Suresh and P.~J.~Sutton and T.~Suzuki and Y.~Suzuki and B.~L.~Swinkels and A.~Syx and M.~J.~Szczepańczyk and P.~Szewczyk and M.~Tacca and H.~Tagoshi and S.~C.~Tait and H.~Takahashi and R.~Takahashi and A.~Takamori and T.~Takase and K.~Takatani and H.~Takeda and K.~Takeshita and C.~Talbot and M.~Tamaki and N.~Tamanini and D.~Tanabe and K.~Tanaka and S.~J.~Tanaka and T.~Tanaka and D.~Tang and S.~Tanioka and D.~B.~Tanner and L.~Tao and R.~D.~Tapia and E.~N.~Tapia San Martín and R.~Tarafder and C.~Taranto and A.~Taruya and J.~D.~Tasson and M.~Teloi and R.~Tenorio and H.~Themann and A.~Theodoropoulos and M.~P.~Thirugnanasambandam and L.~M.~Thomas and M.~Thomas and P.~Thomas and J.~E.~Thompson and S.~R.~Thondapu and K.~A.~Thorne and E.~Thrane and J.~Tissino and A.~Tiwari and P.~Tiwari and S.~Tiwari and V.~Tiwari and M.~R.~Todd and A.~M.~Toivonen and K.~Toland and A.~E.~Tolley and T.~Tomaru and K.~Tomita and T.~Tomura and C.~Tong-Yu and A.~Toriyama and N.~Toropov and A.~Torres-Forné and C.~I.~Torrie and M.~Toscani and I.~Tosta e Melo and E.~Tournefier and A.~Trapananti and F.~Travasso and G.~Traylor and M.~Trevor and M.~C.~Tringali and A.~Tripathee and G.~Troian and L.~Troiano and A.~Trovato and L.~Trozzo and R.~J.~Trudeau and T.~T.~L.~Tsang and R.~Tso and S.~Tsuchida and L.~Tsukada and T.~Tsutsui and K.~Turbang and M.~Turconi and C.~Turski and H.~Ubach and T.~Uchiyama and R.~P.~Udall and T.~Uehara and M.~Uematsu and K.~Ueno and S.~Ueno and V.~Undheim and T.~Ushiba and M.~Vacatello and H.~Vahlbruch and N.~Vaidya and G.~Vajente and A.~Vajpeyi and G.~Valdes and J.~Valencia and M.~Valentini and S.~A.~Vallejo-Peña and S.~Vallero and V.~Valsan and N.~van Bakel and M.~van Beuzekom and M.~van Dael and J.~F.~J.~van den Brand and C.~Van Den Broeck and D.~C.~Vander-Hyde and M.~van der Sluys and A.~Van de Walle and J.~van Dongen and K.~Vandra and H.~van Haevermaet and J.~V.~van Heijningen and P.~Van Hove and M.~VanKeuren and J.~Vanosky and M.~H.~P.~M.~van Putten and Z.~van Ranst and N.~van Remortel and M.~Vardaro and A.~F.~Vargas and J.~J.~Varghese and V.~Varma and M.~Vasúth and A.~Vecchio and G.~Vedovato and J.~Veitch and P.~J.~Veitch and S.~Venikoudis and J.~Venneberg and P.~Verdier and D.~Verkindt and B.~Verma and P.~Verma and Y.~Verma and S.~M.~Vermeulen and F.~Vetrano and A.~Veutro and A.~M.~Vibhute and A.~Viceré and S.~Vidyant and A.~D.~Viets and A.~Vijaykumar and A.~Vilkha and V.~Villa-Ortega and E.~T.~Vincent and J.-Y.~Vinet and S.~Viret and A.~Virtuoso and S.~Vitale and A.~Vives and H.~Vocca and D.~Voigt and E.~R.~G.~von Reis and J.~S.~A.~von Wrangel and S.~P.~Vyatchanin and L.~E.~Wade and M.~Wade and K.~J.~Wagner and A.~Wajid and M.~Walker and G.~S.~Wallace and L.~Wallace and H.~Wang and J.~Z.~Wang and W.~H.~Wang and Z.~Wang and G.~Waratkar and J.~Warner and M.~Was and T.~Washimi and N.~Y.~Washington and D.~Watarai and K.~E.~Wayt and B.~R.~Weaver and B.~Weaver and C.~R.~Weaving and S.~A.~Webster and M.~Weinert and A.~J.~Weinstein and R.~Weiss and F.~Wellmann and L.~Wen and P.~Weßels and K.~Wette and J.~T.~Whelan and B.~F.~Whiting and C.~Whittle and J.~B.~Wildberger and O.~S.~Wilk and D.~Wilken and A.~T.~Wilkin and D.~J.~Willadsen and K.~Willetts and D.~Williams and M.~J.~Williams and N.~S.~Williams and J.~L.~Willis and B.~Willke and M.~Wils and J.~Winterflood and C.~C.~Wipf and G.~Woan and J.~Woehler and J.~K.~Wofford and N.~E.~Wolfe and H.~T.~Wong and H.~W.~Y.~Wong and I.~C.~F.~Wong and J.~L.~Wright and M.~Wright and C.~Wu and D.~S.~Wu and H.~Wu and E.~Wuchner and D.~M.~Wysocki and V.~A.~Xu and Y.~Xu and N.~Yadav and H.~Yamamoto and K.~Yamamoto and T.~S.~Yamamoto and T.~Yamamoto and S.~Yamamura and R.~Yamazaki and S.~Yan and T.~Yan and F.~W.~Yang and F.~Yang and K.~Z.~Yang and Y.~Yang and Z.~Yarbrough and H.~Yasui and S.-W.~Yeh and A.~B.~Yelikar and X.~Yin and J.~Yokoyama and T.~Yokozawa and J.~Yoo and H.~Yu and S.~Yuan and H.~Yuzurihara and A.~Zadrożny and M.~Zanolin and M.~Zeeshan and T.~Zelenova and J.-P.~Zendri and M.~Zeoli and M.~Zerrad and M.~Zevin and A.~C.~Zhang and L.~Zhang and R.~Zhang and T.~Zhang and Y.~Zhang and C.~Zhao and Yue Zhao and Yuhang Zhao and Y.~Zheng and H.~Zhong and R.~Zhou and X.-J.~Zhu and Z.-H.~Zhu and M.~E.~Zucker and J.~Zweizig}, title = {{A} search using {GEO}600 for gravitational waves coincident with fast radio bursts from {SGR} 1935+2154}, year = {2024}, eprint = {2410.09151}, note = {arXiv:2410.09151v1} }
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The magnetar SGR 1935+2154 is the only known Galactic source of fast radio bursts (FRBs). FRBs from SGR 1935+2154 were first detected by CHIME/FRB and STARE2 in 2020 April, after the conclusion of the LIGO, Virgo, and KAGRA Collaborations' O3 observing run. Here we analyze four periods of gravitational wave (GW) data from the GEO600 detector coincident with four periods of FRB activity detected by CHIME/FRB, as well as X-ray glitches and X-ray bursts detected by NICER and NuSTAR close to the time of one of the FRBs. We do not detect any significant GW emission from any of the events. Instead, using a short-duration GW search (for bursts $\leq$ 1 s) we derive 50\% (90\%) upper limits of $10^{48}$ ($10^{49}$) erg for GWs at 300 Hz and $10^{49}$ ($10^{50}$) erg at 2 kHz, and constrain the GW-to-radio energy ratio to $\leq 10^{14} - 10^{16}$. We also derive upper limits from a long-duration search for bursts with durations between 1 and 10 s. These represent the strictest upper limits on concurrent GW emission from FRBs.
The thermal emission in short GRBs with extended emission observed by Fermi/GBM
Xue-Zhao Chang, Hou-Jun Lü, Xing Yang, Jia-Ming Chen, En-Wei Liang
Oct 15 2024 astro-ph.HE arXiv:2410.09415v1

@misc{2410.09415, author = {Xue-Zhao Chang and Hou-Jun Lü and Xing Yang and Jia-Ming Chen and En-Wei Liang}, title = {{T}he thermal emission in short {GRB}s with extended emission observed by {F}ermi/{GBM}}, year = {2024}, eprint = {2410.09415}, note = {arXiv:2410.09415v1} }
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Short gamma-ray bursts (SGRBs) with extended emission (EE) are composed of initial main emission with a short-hard spike (ME) and followed by a long-lasting EE. Whether the ME and EE originated from the same origin or not, as well as the jet composition, remains an open question. In this paper, we present a systematic analysis to search for 36 GRBs in our sample, which are identified as the category of SGRBs with EE as observed by Fermi/GBM. By extracting time-integrated spectra of ME and EE with CPL or Band models for our sample, we find that 20 out of 36 SGRBs for which $\alpha$ values are exceeding the death line (e.g., -2/3) of synchrotron emission within either ME or EE phases, and suggest that the quasi-thermal component should exist in the prompt emission. Then, we extract the time-resolved spectra of our samples, but only four GRBs are bright enough to extract the time-resolved spectra. We find that both thermal and non-thermal emissions do exist in the prompt emission of those four bright GRBs, and it suggests that a hybrid jet (e.g., matter and Poynting-flux outflow) in GRB should exist. Moreover, strong positive correlations (e.g., $F_{\rm tot}-\Gamma$ and $F_{\rm tot}-kT$) in the time-resolved spectra of ME and EE for those four GRBs are discovered. It indicates that the spectral evolution of both ME and EE seem to share similar behavior, possibly from the same physical origin.
Dual-Mode Calorimetric Superconducting Nanowire Single Photon Detectors
Hsin-Yeh Wu, Marc Besançon, Jia-Wern Chen, Pisin Chen, Jean-François Glicenstein, Shu-Xiao Liu, Yu-Jung Lu Xavier-François Navick, Stathes Paganis, Boris Tuchming, Dimitra Tsionou, Feng-Yang Tsai
Oct 15 2024 physics.ins-det astro-ph.IM hep-ex quant-ph arXiv:2410.10280v1

@misc{2410.10280, author = {Hsin-Yeh Wu and Marc Besançon and Jia-Wern Chen and Pisin Chen and Jean-François Glicenstein and Shu-Xiao Liu and Yu-Jung Lu Xavier-François Navick and Stathes Paganis and Boris Tuchming and Dimitra Tsionou and Feng-Yang Tsai}, title = {{D}ual-{M}ode {C}alorimetric {S}uperconducting {N}anowire {S}ingle {P}hoton {D}etectors}, year = {2024}, eprint = {2410.10280}, note = {arXiv:2410.10280v1} }
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A dual-operation mode SNSPD is demonstrated. In the conventional Geiger SNSPD mode the sensor operates at temperatures well below the critical temperature, Tc, working as an event counter without sensitivity to the number of photons impinging the sensor. In the calorimetric mode, the detector is operated at temperatures just below Tc and displays photon-number sensitivity for wavelengths in the optical spectrum. In this energy sensitive mode, photon absorption causes Joule heating of the SNSPD that becomes partially resistive without the presence of latching. Depending on the application, by tuning the sample temperature and bias current using the same readout system, the SNSPD can readily switch between the two modes. In the calorimetric mode, SNSPD recovery times shorter than the ones in the Geiger mode are observed, reaching values as low as 580ps. Dual-mode SNSPD's may provide significant advancements in spectroscopy and calorimetry, where precise timing, photon counting and energy resolution are required.
Estimating Cosmological Parameters and Reconstructing Hubble Constant with Artificial Neural Networks: A Test with Reconstructed $H(z)$
Jiefeng Chen, Tingting Zhang, Tongjie Zhang, Ning Gai
Oct 14 2024 astro-ph.CO arXiv:2410.08369v1

@misc{2410.08369, author = {Jiefeng Chen and Tingting Zhang and Tongjie Zhang and Ning Gai}, title = {{E}stimating {C}osmological {P}arameters and {R}econstructing {H}ubble {C}onstant with {A}rtificial {N}eural {N}etworks: {A} {T}est with {R}econstructed ${H}(z)$}, year = {2024}, eprint = {2410.08369}, note = {arXiv:2410.08369v1} }
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In this work, we present a new approach to constrain the cosmological parameters and estimate Hubble constant. We reconstructed a function from observational Hubble data using an Artificial Neural Network (ANN). The training data we used are covariance matrix and mock $H(z)$. With the reconstructed $H(z)$, we can get the Hubble constant, and thus do the comparison with the CMB-based measurements. Furthermore, in order to constrain the cosmological parameters, we sampled data points from the reconstructed data and estimated the posterior distribution. The constraining result behaved well comparing to the ones from the mock observational Hubble data. We propose that the $H(z)$ reconstructed by our artificial neural network can represent the actual distribution of real observational data, and therefore can be used in further cosmological research.
Measuring the Diffuse Interstellar Bands at 5780, 5797, and 6614 Å in Low-Resolution Spectra of Cool Stars from LAMOST
Xiao-Xiao Ma, Jian-Jun Chen, A-Li Luo, He Zhao, Ji-Wei Shi, Jing Chen, Jun-Chao Liang, Shu-Guo Ma, Cai-Xia Qu, Bi-Wei Jiang
Oct 01 2024 astro-ph.GA astro-ph.SR physics.data-an arXiv:2409.19539v2

@misc{2409.19539, author = {Xiao-Xiao Ma and Jian-Jun Chen and A-Li Luo and He Zhao and Ji-Wei Shi and Jing Chen and Jun-Chao Liang and Shu-Guo Ma and Cai-Xia Qu and Bi-Wei Jiang}, title = {{M}easuring the {D}iffuse {I}nterstellar {B}ands at 5780, 5797, and 6614 Å in {L}ow-{R}esolution {S}pectra of {C}ool {S}tars from {LAMOST}}, year = {2024}, eprint = {2409.19539}, note = {arXiv:2409.19539v2} }
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We attempt to measure the DIBs $\lambda$5780, $\lambda$5797 and $\lambda$6614 in over two million low-resolution spectra of cool stars from LAMOST. Based on the DIB measurements, the correlation between DIBs and extinction, the kinematics of DIBs, and the Galactic distribution of DIBs are reviewed and investigated from the perspective of statistics. A pipeline is developed to measure the DIBs $\lambda$5780, $\lambda$5797 and $\lambda$6614 in the LAMOST low-resolution spectra. We obtain the DIB measurements of spectra of late-type stars from LAMOST, and screen out 176,831, 13,473 and 110,152 high-quality (HQ) measurements of the DIBs $\lambda$5780, $\lambda$5797 and $\lambda$6614, respectively, corresponding to 142,074, 11,480 and 85,301 unique sources. Utilizing these HQ measurements, we present the Galactic maps of the DIBs $\lambda$5780 and $\lambda$6614 in the northern sky for the first time. The central wavelengths of the DIBs $\lambda$5780, $\lambda$5797 and $\lambda$6614 in air are determined to be 5780.48 $\pm$ 0.01, 5796.94 $\pm$ 0.02 and 6613.64 $\pm$ 0.01 Å, respectively, based on their kinematics. The equivalent widths of these three DIBs per unit extinction are statistically fitted to be 0.565, 0.176 and 0.256 Å/mag. As a part of our work, three catalogs of the HQ measurements for the DIBs $\lambda$5780, $\lambda$5797 and $\lambda$6614 are provided online. To the best of our knowledge, this is the largest number of measurements of these three DIBs to date. It is also the first time that the Galactic maps of the DIBs $\lambda$5780 and $\lambda$6614 in the northern hemisphere are presented, and the central wavelengths of the DIBs $\lambda$5780, $\lambda$5797 and $\lambda$6614 are estimated from the kinematics.
Study of the relativistic charged particle beam propagation in Earth's magnetic field
Meihua Fang, Zheng liang, Yingkui Gong, Jianfei Chen, Guiping Zhu, Ting Liu, Yu Tian, Yu Zhou
Sep 12 2024 physics.space-ph astro-ph.IM hep-ph arXiv:2409.06713v1

@misc{2409.06713, author = {Meihua Fang and Zheng liang and Yingkui Gong and Jianfei Chen and Guiping Zhu and Ting Liu and Yu Tian and Yu Zhou}, title = {{S}tudy of the relativistic charged particle beam propagation in {E}arth's magnetic field}, year = {2024}, eprint = {2409.06713}, note = {arXiv:2409.06713v1} }
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Relativistic charged particle beam can be used as destructive beam weapons in space for debris removal tasks. The trajectories of charged particles are affected by both electric and magnetic forces in the Earth's magnetic field. In this paper, we firstly analyzed the correlation parameters of the charged particle beam as a weapon when it propagated in the geomagnetic field. Then the models were constructed based on COMSOL Multiphysics and the IGRF model was adopted in the simulation. The gyro-radius and the related uncertainty were analyzed by simulation of the charged particle transport in the geomagnetic field at different altitudes. The charged beam spot radius divergency was also simulated. The magnetic field pinch effect can be found and can limit the beam spreading.
ALMACAL XII. Data characterisation and products
Victoria Bollo, Martin Zwaan, Celine Peroux, Aleksandra Hamanowicz, Jianhang Chen, Simon Weng, Rob J. Ivison, Andrew Biggs
Sep 12 2024 astro-ph.GA astro-ph.HE astro-ph.IM arXiv:2409.07166v1

@misc{2409.07166, author = {Victoria Bollo and Martin Zwaan and Celine Peroux and Aleksandra Hamanowicz and Jianhang Chen and Simon Weng and Rob J.~Ivison and Andrew Biggs}, title = {{ALMACAL} {XII}. {D}ata characterisation and products}, year = {2024}, eprint = {2409.07166}, note = {arXiv:2409.07166v1} }
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The ALMACAL survey is based on a database of reprocessed ALMA calibration scans suitable for scientific analysis, observed as part of regular PI observations. We present all the data accumulated from the start of ALMA operations until May 2022 for 1047 calibrator fields across the southern sky spanning ALMA Bands 3 to 10 (~ 84 - 950 GHz), so-called ALMACAL-22. Encompassing over 1000 square arcmin and accumulating over 2000 hours of integration time, ALMACAL is not only one of the largest ALMA surveys to date, but it continues to grow with each new scientific observation. We outline the methods for processing and imaging a subset of the highest-quality data ('pruned sample'). Using deconvolution techniques within the visibility data (uv plane), we created data cubes as the final product for further scientific analysis. We describe the properties and shortcomings of ALMACAL and compare its area and sensitivity with other sub-millimetre surveys. Notably, ALMACAL overcomes limitations of previous sub-millimetre surveys, such as small sky coverage and the effects of cosmic variance. Moreover, we discuss the improvements introduced by the latest version of this dataset that will enhance our understanding of dusty star-forming galaxies, extragalactic absorption lines, active galactic nucleus physics, and ultimately the evolution of molecular gas.
Repeated partial disruptions in a WD-NS or WD-BH merger modulate the prompt emission of long-duration merger-type GRBs
Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Sep 04 2024 astro-ph.HE arXiv:2409.00472v2

@misc{2409.00472, author = {Junping Chen and Rong-Feng Shen and Wen-Jun Tan and Chen-Wei Wang and Shao-Lin Xiong and Run-Chao Chen and Bin-Bin Zhang}, title = {{R}epeated partial disruptions in a {WD}-{NS} or {WD}-{BH} merger modulate the prompt emission of long-duration merger-type {GRB}s}, year = {2024}, eprint = {2409.00472}, note = {arXiv:2409.00472v2} }
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The progenitors of gamma-ray bursts (GRBs) have long been an unresolved issue. GRB 230307A stands out as an exceptionally bright event, belonging to the long-duration GRBs but also exhibiting a late emission component reminiscent of a kilonova. Together with the similar events GRBs 060614 and 211211A, they make up a new sub-group of GRBs with intriguing progenitors. If such long-duration merger-type GRBs originated from the coalescence of a white dwarf (WD) with a neutron star (NS) or a black hole (BH), as proposed in the recent literature, then the larger tidal disruption radius of the WD, together with a non-negligible residual orbital eccentricity, would make repeated partial tidal disruptions inevitable. This may modulate the mass accretion and jet launching process at the NS or BH, resulting in a quasi-periodic modulation (QPM) in the light curve of the GRB, on the orbital period. The detection of potential QPMs during the early episode of prompt emission of these three GRBs supports this scenario, and the relatively slow QPM ($>$ 1 s) suggests that the lighter object can not be a NS. We propose that the progenitor system of GRBs 230307A, 060614, and 211211A consist of a WD of mass 1.3 $M_\odot$, 0.9 $M_\odot$ and 1.4 $M_\odot$, respectively, and a NS (or BH). After several cycles of modulations, the WD is completely destructed, and the accretion of the remaining debris dominates the extended emission episode.
Fate of the remnant in tidal stripping event: repeating and non-repeating
Jin-Hong Chen, Lixin Dai, Shang-Fei Liu, Jian-Wen Ou
Aug 21 2024 astro-ph.HE astro-ph.GA arXiv:2408.10925v1

@misc{2408.10925, author = {Jin-Hong Chen and Lixin Dai and Shang-Fei Liu and Jian-Wen Ou}, title = {{F}ate of the remnant in tidal stripping event: repeating and non-repeating}, year = {2024}, eprint = {2408.10925}, note = {arXiv:2408.10925v1} }
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Tidal disruption events (TDE) occur when a star ventures too close to a massive black hole. In a partial TDE (pTDE), the star only grazes the tidal radius, causing the outer envelope of the star to be stripped away while the stellar core survives. Previous research has shown that a star, once tidally stripped in a parabolic orbit, can acquire enough orbital energy for its remnant to become a high-velocity star potentially capable of escaping the galaxy. Conversely, some studies have reported that the remnant may lose orbital energy and undergo re-disruption, leading to a recurring pTDE. This study aims to uncover the physical mechanisms and determine the conditions that lead to these divergent outcomes. We find that the orbital energy change only depends on the impact factor and the stellar structure, and barely depends on the mass of the black hole or the exact mass or orbital eccentricity of the star. For a $\gamma=5/3$ (or $\gamma=4/3$) polytropic star, after a pTDE its remnant gains orbital energy when the impact factor $\beta \gtrsim 0.62$ (or $\gtrsim 1.1$) or loses energy vice versa. Additionally, we verify an analytical equation for orbital energy change that is applicable across various systems. Through hydrodynamic simulations, we also explore the structure of the stellar remnant post-tidal stripping. Our findings provide critical insights for interpreting observed pTDEs and advancing knowledge on the orbital evolution and event rate of these events.
Vector Dark Matter Halo: From Polarization Dynamics to Direct Detection
Jiajun Chen, Le Hoang Nguyen, David J. E. Marsh
Jul 25 2024 astro-ph.CO arXiv:2407.17315v3

@misc{2407.17315, author = {Jiajun Chen and Le Hoang Nguyen and David J.~E.~Marsh}, title = {{V}ector {D}ark {M}atter {H}alo: {F}rom {P}olarization {D}ynamics to {D}irect {D}etection}, year = {2024}, eprint = {2407.17315}, note = {arXiv:2407.17315v3} }
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This study investigates the characteristic polarization formation and evolution of vector dark matter (VDM) in the outer halo of galaxies. By employing numerical simulations, we analyze the behavior of VDM under different initial conditions -- homogeneous, isotropic, and partially polarized. The simulations solve the Schrödinger-Poisson equations, examining the spin density distribution and its evolution during gravitational collapse and halo formation. Our results reveal that VDM forms halos and central Proca stars from homogeneous and isotropic conditions, with the polarization density fluctuation amplitude mirroring VDM matter density. In scenarios with no initial polarization, spin density remains stable in the halo core but fluctuates in outer regions. Partially polarized initial conditions lead to a conservation of total polarization, with increased core polarization resulting in opposite polarization in the periphery. We examine the novel consequences of the partially polarized state for direct detection of dark photons, i.e., VDM kinetically mixed with ordinary photons.
A kiloparsec-scale ordered magnetic field in a galaxy at z=5.6
Jianhang Chen, Enrique Lopez-Rodriguez, R. J. Ivison, James E. Geach, Simon Dye, Xiaohui Liu, George Bendo
Jul 23 2024 astro-ph.GA astro-ph.HE physics.plasm-ph arXiv:2407.14596v2

@misc{2407.14596, author = {Jianhang Chen and Enrique Lopez-Rodriguez and R.~J.~Ivison and James E.~Geach and Simon Dye and Xiaohui Liu and George Bendo}, title = {{A} kiloparsec-scale ordered magnetic field in a galaxy at z=5.6}, year = {2024}, eprint = {2407.14596}, note = {arXiv:2407.14596v2} }
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Magnetic fields are prevalent on almost all astronomical scales, but their importance in different systems and over cosmic time is yet to be understood. Our current knowledge of the evolution of magnetic fields is limited by scarce observations in the distant Universe, where galaxies have recently been found to be more evolved than most model predictions. In this study, we conducted rest-frame 131 um full-polarisation observations of dust emission in a strongly lensed dusty star-forming galaxy, SPT0346-52, at z=5.6, when the Universe was only 1 Gyr old. Dust grains can become aligned with local magnetic fields, resulting in the emission of linearly polarised thermal infrared radiation. Our observations have revealed a median polarisation level of $0.9\pm0.2$ per cent with a variation of $\pm0.4$ per cent across the regions with polarisation detection, similar to that of local starburst galaxies. The polarised dust emission is patchy and mostly overlaps with the [C II] emission at a velocity of about -150 km/s, and extends over 3 kiloparsecs. The bimodal distribution of field orientations, their spatial distribution, and the connection with the cold gas kinematics further emphasise the complexity of the magnetic environment in this galaxy and the potential role of mergers in shaping its magnetic fields. Such early formation of ordered galactic magnetic fields also suggests that both small-scale and large-scale dynamos could be efficient in early galaxies. Continued observations of magnetic fields in early galaxies, as well as expanding surveys to a wider galaxy population, are essential for a comprehensive understanding of the prevalence and impact of magnetic fields in the evolving Universe.
Formation and desorption of sulfur chains (H$_2$S$_x$ and S$_x$) in cometary ice: effects of ice composition and temperature
H. Carrascosa, G. M. Muñoz Caro, R. Martín-Doménech, S. Cazaux, J. -Y. Chen, A. Fuente
Jul 22 2024 astro-ph.EP astro-ph.IM arXiv:2407.14135v1

@misc{2407.14135, author = {H.~Carrascosa and G.~M.~Muñoz Caro and R.~Martín-Doménech and S.~Cazaux and J.~-Y.~Chen and A.~Fuente}, title = {{F}ormation and desorption of sulfur chains ({H}$_2${S}$_x$ and {S}$_x$) in cometary ice: effects of ice composition and temperature}, year = {2024}, eprint = {2407.14135}, note = {arXiv:2407.14135v1} }
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The reservoir of sulfur accounting for sulfur depletion in the gas of dense clouds and circumstellar regions is still unclear. One possibility is the formation of sulfur chains, which would be difficult to detect by spectroscopic techniques. This work explores the formation of sulfur chains experimentally, both in pure H$_2$S ice samples and in H$_2$O:H$_2$S ice mixtures. An ultra-high vacuum chamber, ISAC, eqquipped with FTIR and QMS, was used for the experiments. Our results show that the formation of H$_2$S$_x$ species is efficient, not only in pure H$_2$S ice samples, but also in water-rich ice samples. Large sulfur chains are formed more efficiently at low temperatures ($\approx$10 K), while high temperatures ($\approx$50 K) favour the formation of short sulfur chains. Mass spectra of H$_2$S$_x$, x~=~2-6, species are presented for the first time. Their analysis suggests that H$_2$S$_x$ species are favoured in comparison with S$_x$ chains. Nevertheless, the detection of several S$_x^+$ fragments at high temperatures in H$_2$S:H$_2$O ice mixtures suggests the presence of S$_8$ in the irradiated ice samples, which could sublimate from 260~K. ROSINA instrument data from the cometary Rosetta mission detected mass-to-charge ratios 96 and 128. Comparing these detections with our experiments, we propose two alternatives: 1) H$_2$S$_4$ and H$_2$S$_5$ to be responsible of those S$_3^+$ and S$_4^+$ cations, respectively, or 2) S$_8$ species, sublimating and being fragmented in the mass spectrometer. If S$_8$ is the parent molecule, then S$_5^+$ and S$_6^+$ cations could be also detected in future missions by broadening the mass spectrometer range.
The FAST HI 21-cm absorption blind survey. II -- statistic exploration for associated and intervening systems
Wenkai Hu, Yougang Wang, Yichao Li, Ue-Li Pen, Jie Wang, Yingjie Jing, Ming Zhu, Xin Zhang, Wenxiu Yang, Yidong Xu, Xu Chen, Jingze Chen, Zheng Zheng, Di Li, Xuelei Chen
Jul 22 2024 astro-ph.GA arXiv:2407.14411v1

@misc{2407.14411, author = {Wenkai Hu and Yougang Wang and Yichao Li and Ue-Li Pen and Jie Wang and Yingjie Jing and Ming Zhu and Xin Zhang and Wenxiu Yang and Yidong Xu and Xu Chen and Jingze Chen and Zheng Zheng and Di Li and Xuelei Chen}, title = {{T}he {FAST} {HI} 21-cm absorption blind survey. {II} -- statistic exploration for associated and intervening systems}, year = {2024}, eprint = {2407.14411}, note = {arXiv:2407.14411v1} }
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We present an extragalactic HI 21-cm absorption lines catalog from a blind search at z $\leq$ 0.35, using drift-scan data collected in 1616.9 hours by the ongoing Commensal Radio Astronomy FasT Survey (CRAFTS) and FAST All Sky HI Survey (FASHI), which spans a sky area of 7456.8 deg$^{2}$ and covers 84,533 radio sources with a flux density greater than 12 mJy. 14 previously identified HI absorbers and 20 newly discovered HI absorbers were detected, comprising 14 associated systems, 11 intervening systems, and 9 systems with undetermined classifications. We fit HI profiles with multi-component Gaussian functions and calculate the redshift, width, flux density, optical depth, and HI column densities for each source. Through spectral stacking, the mean peak optical path, mean velocity-integrated optical path $\langle \tau\rangle$, mean FWHM and mean HI column density $\langle$ N$_{HI}\rangle$ are measured to be 0.46 and 0.34; 25.85 km/s and 4.62 km/s; 39.80 km/s and 8.95 km/s; 0.470 and 0.085 T$_{s} \times$ 10$^{20}$cm$^{-2}$K$^{-1}$, for the associated and intervening samples, respectively. Statistical analysis also reveals that associated systems tend to be hosted by red (g$-$r$>$0.7) galaxies at lower redshifts, whereas galaxies hosting intervening HI absorption are typically found at higher redshifts and are of a bluer (g$-$r$\leq$0.7) type. Additionally, it has been demonstrated that associated HI 21-cm absorptions connected to compact radio sources display higher N$_{HI}$ values compared to those linked with extended radio sources.
Asymmetric Hard X-ray Radiation of Two Ribbons in a Thermal-Dominated C-Class Flare
Guanglu Shi, Li Feng, Jun Chen, Beili Ying, Shuting Li, Qiao Li, Hui Li, Ying Li, Kaifan Ji, Yu Huang, Weiqun Gan, LST team
Jul 19 2024 astro-ph.SR physics.plasm-ph arXiv:2407.13099v1

@misc{2407.13099, author = {Guanglu Shi and Li Feng and Jun Chen and Beili Ying and Shuting Li and Qiao Li and Hui Li and Ying Li and Kaifan Ji and Yu Huang and Weiqun Gan and LST team}, title = {{A}symmetric {H}ard {X}-ray {R}adiation of {T}wo {R}ibbons in a {T}hermal-{D}ominated {C}-{C}lass {F}lare}, year = {2024}, eprint = {2407.13099}, note = {arXiv:2407.13099v1} }
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The asymmetry in hard X-ray (HXR) emission at the footpoints (FPs) of flare loops is a ubiquitous feature closely associated with nonthermal electron transport. We analyze the asymmetric HXR radiation at two flare ribbons which is thermal-dominated during a long-duration C4.4 flare that occurred on March 20, 2023, combining multi-view and multi-waveband observations from the ASO-S, SolO, and SDO spacecraft. We find that the H I Ly$\alpha$ emission captures similar features to the He II $\lambda$304 in both light curve and spatio-temporal evolution of a pair of conjugate flare ribbons. The spectra and imaging analysis of the HXR emission, detected by STIX in 4-18 keV, reveal that the two-ribbon flare radiation is thermal dominated by over 95%, and the radiation source mainly concentrates on the northern ribbon, leading to an asymmetric distribution. To understand the underlying reasons for the HXR radiation asymmetry, we extrapolate the magnetic field within the active region using the NLFFF model. For 78% of the magnetic field lines starting from the northern flare ribbon, their lengths from the loop-tops (LTs) to the northern FPs are shorter than those to the southern FPs. For 62% of the field lines, their magnetic field strengths at the southern FPs exceed those at the northern FPs. In addition, considering the larger density, $\approx1.0\times10^{10}$ cm$^{-3}$, of the low-lying flare loops (< 32 Mm), we find the shorter path from the LT to the northern FP enables more electrons to reach the northern FP more easily after collisions with the surrounding plasma. Therefore, in this thermal-dominated C-class flare, the asymmetric location of the flare LT relative to its two FPs plays a dominant role in the HXR radiation asymmetry, while such asymmetry is also slightly influenced by the magnetic mirror effect resulting in larger HXR radiation at the FPs with weaker magnetic strength.
Light Dark Matter Constraints from SuperCDMS HVeV Detectors Operated Underground with an Anticoincidence Event Selection
SuperCDMS Collaboration, M.F. Albakry, I. Alkhatib, D. Alonso-González, D.W.P. Amaral, J. Anczarski, T. Aralis, T. Aramaki, I.J. Arnquist, I. Ataee Langroudy, E. Azadbakht, C. Bathurst, R. Bhattacharyya, A.J. Biffl, P.L. Brink, M. Buchanan, R. Bunker, B. Cabrera, R. Calkins, R.A. Cameron, et al (122)
Jul 12 2024 hep-ex astro-ph.CO physics.ins-det arXiv:2407.08085v4

@misc{2407.08085, author = {SuperCDMS Collaboration and M.F.~Albakry and I.~Alkhatib and D.~Alonso-González and D.W.P.~Amaral and J.~Anczarski and T.~Aralis and T.~Aramaki and I.J.~Arnquist and I.~Ataee Langroudy and E.~Azadbakht and C.~Bathurst and R.~Bhattacharyya and A.J.~Biffl and P.L.~Brink and M.~Buchanan and R.~Bunker and B.~Cabrera and R.~Calkins and R.A.~Cameron and C.~Cartaro and D.G.~Cerdeño and Y.-Y.~Chang and M.~Chaudhuri and J.-H.~Chen and R.~Chen and N.~Chott and J.~Cooley and H.~Coombes and P.~Cushman and R.~Cyna and S.~Das and F.~De Brienne and S.~Dharani and M.L.~di Vacri and M.D.~Diamond and M.~Elwan and E.~Fascione and E.~Figueroa-Feliciano and K.~Fouts and M.~Fritts and R.~Germond and M.~Ghaith and S.R.~Golwala and J.~Hall and S.A.S.~Harms and K.~Harris and N.~Hassan and Z.~Hong and E.W.~Hoppe and L.~Hsu and M.E.~Huber and V.~Iyer and D.~Jardin and V.K.S.~Kashyap and S.T.D.~Keller and M.H.~Kelsey and K.T.~Kennard and A.~Kubik and N.A.~Kurinsky and M.~Lee and J.~Leyva and J.~Liu and Y.~Liu and B.~Loer and E.~Lopez Asamar and P.~Lukens and D.B.~MacFarlane and R.~Mahapatra and J.S.~Mammo and N.~Mast and A.J.~Mayer and H.~Meyer zu Theenhausen and É.~Michaud and E.~Michielin and N.~Mirabolfathi and M.~Mirzakhani and B.~Mohanty and D.~Monteiro and J.~Nelson and H.~Neog and V.~Novati and J.L.~Orrell and M.D.~Osborne and S.M.~Oser and L.~Pandey and S.~Pandey and R.~Partridge and D.S.~Pedreros and W.~Peng and L.~Perna and W.L.~Perry and R.~Podviianiuk and S.S.~Poudel and A.~Pradeep and M.~Pyle and W.~Rau and E.~Reid and R.~Ren and T.~Reynolds and M.~Rios and A.~Roberts and A.E.~Robinson and J.L.~Ryan and T.~Saab and D.~Sadek and B.~Sadoulet and S.P.~Sahoo and I.~Saikia and J.~Sander and A.~Sattari and B.~Schmidt and R.W.~Schnee and S.~Scorza and B.~Serfass and A.~Simchony and D.J.~Sincavage and P.~Sinervo and J.~Street and H.~Sun and E.~Tanner and G.D.~Terry and D.~Toback and S.~Verma and A.N.~Villano and B.~von Krosigk and S.L.~Watkins and O.~Wen and Z.~Williams and M.J.~Wilson and J.~Winchell and K.~Wykoff and S.~Yellin and B.A.~Young and T.C.~Yu and B.~Zatschler and S.~Zatschler and A.~Zaytsev and E.~Zhang and L.~Zheng and A.~Zuniga and M.J.~Zurowski}, title = {{L}ight {D}ark {M}atter {C}onstraints from {S}uper{CDMS} {HV}e{V} {D}etectors {O}perated {U}nderground with an {A}nticoincidence {E}vent {S}election}, year = {2024}, eprint = {2407.08085}, note = {arXiv:2407.08085v4} }
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This article presents constraints on dark-matter-electron interactions obtained from the first underground data-taking campaign with multiple SuperCDMS HVeV detectors operated in the same housing. An exposure of 7.63 g-days is used to set upper limits on the dark-matter-electron scattering cross section for dark matter masses between 0.5 and 1000 MeV/$c^2$, as well as upper limits on dark photon kinetic mixing and axion-like particle axioelectric coupling for masses between 1.2 and 23.3 eV/$c^2$. Compared to an earlier HVeV search, sensitivity was improved as a result of an increased overburden of 225 meters of water equivalent, an anticoincidence event selection, and better pile-up rejection. In the case of dark-matter-electron scattering via a heavy mediator, an improvement by up to a factor of 25 in cross-section sensitivity was achieved.
Association between a Failed Prominence Eruption and the Drainage of Mass from Another Prominence
Jianchao Xue, Li Feng, Hui Li, Ping Zhang, Jun Chen, Guanglu Shi, Kaifan Ji, Ye Qiu, Chuan Li, Lei Lu, Beili Ying, Ying Li, Yu Huang, Youping Li, Jingwei Li, Jie Zhao, Dechao Song, Shuting Li, Zhengyuan Tian, Yingna Su, et al (14)
Jun 18 2024 astro-ph.SR arXiv:2406.11602v2

@misc{2406.11602, author = {Jianchao Xue and Li Feng and Hui Li and Ping Zhang and Jun Chen and Guanglu Shi and Kaifan Ji and Ye Qiu and Chuan Li and Lei Lu and Beili Ying and Ying Li and Yu Huang and Youping Li and Jingwei Li and Jie Zhao and Dechao Song and Shuting Li and Zhengyuan Tian and Yingna Su and Qingmin Zhang and Yunyi Ge and Jiahui Shan and Qiao Li and Gen Li and Yue Zhou and Jun Tian and Xiaofeng Liu and Zhichen Jing and Bo Chen and Kefei Song and Lingping He and Shijun Lei and Weiqun Gan}, title = {{A}ssociation between a {F}ailed {P}rominence {E}ruption and the {D}rainage of {M}ass from {A}nother {P}rominence}, year = {2024}, eprint = {2406.11602}, note = {arXiv:2406.11602v2} }
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Sympathetic eruptions of solar prominences have been studied for decades, however, it is usually difficult to identify their causal links. Here we present two failed prominence eruptions on 26 October 2022 and explore their connections. Using stereoscopic observations, the south prominence (PRO-S) erupts with untwisting motions, flare ribbons occur underneath, and new connections are formed during the eruption. The north prominence (PRO-N) rises up along with PRO-S, and its upper part disappears due to catastrophic mass draining along an elongated structure after PRO-S failed eruption. We suggest that the eruption of PRO-S initiates due to a kink instability, further rises up, and fails to erupt due to reconnection with surrounding fields. The elongated structure connecting PRO-N overlies PRO-S, which causes the rising up of PRO-N along with PRO-S and mass drainage after PRO-S eruption. This study suggests that a prominence may end its life through mass drainage forced by an eruption underneath.
Interstellar Nitrogen Isotope Ratios: Measurements on tracers of C$^{14}$N and C$^{15}$N
J. L. Chen, J. S. Zhang, C. Henkel, Y. T. Yan, H. Z. Yu, Y. X. Wang, Y. P. Zou, J. Y. Zhao, X. Y. Wang
Jun 17 2024 astro-ph.GA arXiv:2406.09683v1

@misc{2406.09683, author = {J.~L.~Chen and J.~S.~Zhang and C.~Henkel and Y.~T.~Yan and H.~Z.~Yu and Y.~X.~Wang and Y.~P.~Zou and J.~Y.~Zhao and X.~Y.~Wang}, title = {{I}nterstellar {N}itrogen {I}sotope {R}atios: {M}easurements on tracers of {C}$^{14}${N} and {C}$^{15}${N}}, year = {2024}, eprint = {2406.09683}, howpublished = {The Astrophysical Journal (2004)}, note = {arXiv:2406.09683v1} }
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The nitrogen isotope ratio 14N/15N is a powerful tool to trace Galactic stellar nucleosynthesis and constraining Galactic chemical evolution. Previous observations have found lower 14N/15N ratios in the Galactic center and higher values in the Galactic disk. This is consistent with the inside-out formation scenario of our Milky Way. However, previous studies mostly utilized double isotope ratios also including 12C/13C, which introduces additional uncertainties. Here we therefore present observations of C14N and its rare isotopologue, C15N, toward a sample of star forming regions, measured by the IRAM 30 m and/or the ARO 12 m telescope at $\lambda$ ~3 mm wavelength. For those 35 sources detected in both isotopologues, physical parameters are determined. Furthermore we have obtained nitrogen isotope ratios using the strongest hyperfine components of CN and C15N. For those sources showing small deviations from Local Thermodynamical Equilibrium and/or self-absorption, the weakest hyperfine component, likely free of the latter effect, was used to obtain reliable 14N/15N values. Our measured 14N/15N isotope ratios from C14N and C15N measurements are compatible with those from our earlier measurements of NH3 and 15NH3 (Paper I), i.e., increasing ratios to a Galacticentric distance of ~9 kpc. The unweighted second order polynomial fit yields $\frac{{\rm C^{14}N}}{{\rm C^{15}N}} = (-4.85 \pm 1.89)\;{\rm kpc^{-2}} \times R_{\rm GC}^{2} + (82.11 \pm 31.93) \;{\rm kpc^{-1}} \times R_{\rm GC} - (28.12 \pm 126.62)$. Toward the outer galaxy, the isotope ratio tends to decrease, supporting an earlier finding by H13CN/HC15N. Galactic chemical evolution models are consistent with our measurements of the 14N/15N isotope ratio, i.e. a rising trend from the Galactic center region to approximately 9 kpc, followed by a decreasing trend with increasing $R_{\rm GC}$ toward the outer Galaxy.
GWnext 2024: Meeting Summary
Alejandro Torres-Orjuela, Veronica Vazquez-Aceves, Rui Xu, Jin-Hong Chen, Andrea Derdzinski, Matthias U. Kruckow, Stefano Rinaldi, Lorenzo Speri, Ziming Wang, Garvin Yim, Xue-Ting Zhang, Qian Hu, Miaoxin Liu, Xiangyu Lyu, Zheng Wu, Cong Zhou, Manuel Arca Sedda, Yan-Chen Bi, Hong-Yu Chen, Xian Chen, et al (2)
Jun 07 2024 astro-ph.HE gr-qc arXiv:2406.03498v1

@misc{2406.03498, author = {Alejandro Torres-Orjuela and Veronica Vazquez-Aceves and Rui Xu and Jin-Hong Chen and Andrea Derdzinski and Matthias U.~Kruckow and Stefano Rinaldi and Lorenzo Speri and Ziming Wang and Garvin Yim and Xue-Ting Zhang and Qian Hu and Miaoxin Liu and Xiangyu Lyu and Zheng Wu and Cong Zhou and Manuel Arca Sedda and Yan-Chen Bi and Hong-Yu Chen and Xian Chen and Jiageng Jiao and Yu-Mei Wu}, title = {{GW}next 2024: {M}eeting {S}ummary}, year = {2024}, eprint = {2406.03498}, note = {arXiv:2406.03498v1} }
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GWnext 2024 was a meeting held in the Kavli Institute for Astronomy and Astrophysics at Peking University in March $4^\text{th} - 8^\text{th}$, 2024. In the meeting researchers at different career stages -- with a particular focus on early career scientists -- working on the different aspects of gravitational wave (GW) astronomy gathered to discuss the current status as well as prospects of the field. The meeting was divided into three core sessions: Astrophysics, GW Theory, and Detection. Each session consisted of introductory talks and extended discussion sessions. Moreover, there was a poster session where students could present their results. In this paper, we summarize the results presented during the meeting and present the most important outcomes.
The formation rate and luminosity function of fast radio bursts
J. H. Chen, X. D. Jia, X. F. Dong, F. Y. Wang
Jun 07 2024 astro-ph.HE arXiv:2406.03672v1

@misc{2406.03672, author = {J.~H.~Chen and X.~D.~Jia and X.~F.~Dong and F.~Y.~Wang}, title = {{T}he formation rate and luminosity function of fast radio bursts}, year = {2024}, eprint = {2406.03672}, note = {arXiv:2406.03672v1} }
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Fast radio bursts (FRBs) are millisecond-duration flashes with unknown origins. Its formation rate is crucial for unveiling physical origins. However, the luminosity and formation rate are degenerated when directly fitting the redshift distribution of FRBs. In contrast to previous forward-fitting methods, we use the Lynden-Bell's $c^{-}$ method to derive luminosity function and formation rate of FRBs without any assumptions. Using the non-repeating FRBs from the first CHIME/FRB catalog, we find a relatively strong luminosity evolution, and luminosity function can be fitted by a broken power-law model with a break at $1.33\times10^{41}\ \mathrm{erg}\ \mathrm{s}^{-1}$. The formation rate declines rapidly as $(1+z)^{-4.9\pm0.3}$ with a local rate $1.13\times10^4\ \mathrm{Gpc}^{-3}\ \mathrm{yr}^{-1}$. This monotonic decrease is similar to the rate of short gamma-ray bursts. After comparing it with star formation rate and stellar mass density, we conclude that the old populations including neutron stars and black holes, are closely related to the origins of FRBs. Monte Carlo simulations are used to test our results. The distributions of mock sample are consistent with the observational data.
Correction for the Weakening Magnetic Field within the Sunspot Umbra Observed by ASO-S/FMG
Haiqing Xu, Jiangtao Su, Suo Liu, Yuanyong Deng, Xianyong Bai, Jie Chen, Xiaofan Wang, Xiao Yang, Yongliang Song
May 30 2024 astro-ph.SR arXiv:2405.18699v1

@misc{2405.18699, author = {Haiqing Xu and Jiangtao Su and Suo Liu and Yuanyong Deng and Xianyong Bai and Jie Chen and Xiaofan Wang and Xiao Yang and Yongliang Song}, title = {{C}orrection for the {W}eakening {M}agnetic {F}ield within the {S}unspot {U}mbra {O}bserved by {ASO}-{S}/{FMG}}, year = {2024}, eprint = {2405.18699}, note = {arXiv:2405.18699v1} }
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The magnetic field inside the sunspot umbra, as observed by the Full-disk MagnetoGraph (FMG) onboard the Advanced Space based Solar Observatory (ASO-S), was found to be experiencing a weakening. To address this issue, we employed a method developed by Xu et al. (2021) to correct the weakening in the data of 20 active regions observed by FMG during the period spanning December 29, 2022, to July 23, 2023. Research has revealed that the onset of magnetic field weakening occurs at a minimum magnetic field strength of 705 G, with the peak strength reaching up to 1931 G. We computed the change ratio (R1) of the unsigned magnetic flux within the sunspot umbra, considering measurements both before and after correction. The change ratio (R1) spans from 26% to 124%, indicating a significant increase in the unsigned magnetic flux within sunspot umbrae observed by FMG after correction. To illustrate this, we selected four active regions for comparison with data from the Helioseismic and Magnetic Imager (HMI). After correction, it is found that the unsigned magnetic flux in sunspot umbrae measured by FMG aligns more closely with that of HMI. This supports the effectiveness of the corrective method for FMG, despite imperfections, particularly at the umbra-penumbra boundary.
High-Resolution Observation and Magnetic Modeling of a Solar Minifilament: the Formation, Eruption and Failing Mechanisms
Weilin Teng, Yingna Su, Rui Liu, Jialin Chen, Yanjie Liu, Jun Dai, Wenda Cao, Jinhua Shen, Haisheng Ji
May 28 2024 astro-ph.SR arXiv:2405.17303v1

@misc{2405.17303, author = {Weilin Teng and Yingna Su and Rui Liu and Jialin Chen and Yanjie Liu and Jun Dai and Wenda Cao and Jinhua Shen and Haisheng Ji}, title = {{H}igh-{R}esolution {O}bservation and {M}agnetic {M}odeling of a {S}olar {M}inifilament: the {F}ormation, {E}ruption and {F}ailing {M}echanisms}, year = {2024}, eprint = {2405.17303}, note = {arXiv:2405.17303v1} }
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Minifilaments are widespread small-scale structures in the solar atmosphere. To better understand their formation and eruption mechanisms, we investigate the entire life of a sigmoidal minifilament located below a large quiescent filament observed by BBSO/GST on 2015 August 3. The H\alpha structure initially appears as a group of arched threads, then transforms into two J-shaped arcades, and finally forms a sigmoidal shape. SDO/AIA observations in 171Å show that two coronal jets occur around the southern footpoint of the minifilament before the minifilament eruption. The minifilament eruption starts from the southern footpoint, then interacts with the overlying filament and fails. The aforementioned observational changes correspond to three episodes of flux cancellations observed by SDO/HMI. Unlike previous studies, the flux cancellation occurs between the polarity where southern footpoint of the minifilament is rooted in and an external polarity. We construct two magnetic field models before the eruption using the flux rope insertion method, and find an hyperbolic flux tube (HFT) above the flux cancellation site. The observation and modeling results suggest that the eruption is triggered by the external magnetic reconnection between the core field of the minifilament and the external fields due to flux cancellations. This study reveals a new triggering mechanism for minifilament eruptions and a new relationship between minifilament eruptions and coronal jets.
A Study on Magnetic-sensitivity Wavelength Position of the Working Line Used by the Full-Disk Magnetograph onboard the Advanced Space based Solar Observatory (ASO-S/FMG)
S. Liu, J.T. Su, X.Y. Bai, Y.Y. Deng, J. Chen, Y.L. Song, X.F. Wang, H.Q. Xu, X. Yang, Shahid Idrees
May 28 2024 astro-ph.SR arXiv:2405.16741v1

@misc{2405.16741, author = {S.~Liu and J.T.~Su and X.Y.~Bai and Y.Y.~Deng and J.~Chen and Y.L.~Song and X.F.~Wang and H.Q.~Xu and X.~Yang and Shahid Idrees}, title = {{A} {S}tudy on {M}agnetic-sensitivity {W}avelength {P}osition of the {W}orking {L}ine {U}sed by the {F}ull-{D}isk {M}agnetograph onboard the {A}dvanced {S}pace based {S}olar {O}bservatory ({ASO}-{S}/{FMG})}, year = {2024}, eprint = {2405.16741}, howpublished = {Solar Physics, 2024,May}, doi = {10.1007/s11207-024-02311-0}, note = {arXiv:2405.16741v1} }
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Utilizing data from the $Solar$ $Magnetism$ and $Activity$ $Telescope$ (SMAT), analytical solutions of polarized radiative transfer equations, and in-orbit test data from the Full-disk Magnetograph (FMG) onboard the Advanced Space based Solar Observatory (ASO-S), this study reveals the magnetic-sensitivity spectral positions for the Fe \sc i $\lambda$5234.19 A, working line used by FMG. From the experimental data of SMAT, it is found that the most sensitivity position is located at the line center for linear polarization (Stokes-Q/U), while it is about -0.07 A away from the line center for circular polarization (Stokes-V). Moreover, both the theoretical analysis and the in-orbit test data analysis of FMG prove again the above results. Additionally, the theoretical analysis suggests the presence of distinct spectral pockets (centered at 0.08-0.15 A) from the line, harboring intense magnetic sensitivity across all three Stokes parameters. Striking a balance between high sensitivity for both linear and circular polarization while capturing additional valuable information, a spectral position of -0.08 A emerges as the champion for routine FMG magnetic-field observations.
A Study of the Spectral properties of Gamma-Ray Bursts with the Precursors and Main bursts
Hui-Ying Deng, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
May 24 2024 astro-ph.HE arXiv:2405.14588v2

@misc{2405.14588, author = {Hui-Ying Deng and Zhao-Yang Peng and Jia-Ming Chen and Yue Yin and Ting Li}, title = {{A} {S}tudy of the {S}pectral properties of {G}amma-{R}ay {B}ursts with the {P}recursors and {M}ain bursts}, year = {2024}, eprint = {2405.14588}, note = {arXiv:2405.14588v2} }
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There is no consensus yet on whether the precursor and the main burst of gamma-ray bursts (GRBs) have the same origin, and their jet composition is still unclear. In order to further investigate this issue, we systematically search 21 Fermi GRBs with both precursor and main burst for spectral analysis. We first perform Bayesian time-resolved spectral analysis and find that almost all the precursors and the main bursts (94.4$\%$) exhibit thermal components, and the vast majority of them have low-energy spectral index ($\alpha$) (72.2$\%$) that exceed the limit of synchrotron radiation. We then analyse the evolution and correlation of the spectral parameters and find that approximately half of the $\alpha$ (50$\%$) of the precursors and the main bursts evolve in a similar pattern, while peak energy ($E_{p}$) (55.6$\%$) behave similarly, and their evolution is mainly characterized by flux tracking; for the $\alpha-F$ (the flux) relation, more than half of the precursors and the main bursts (61.1$\%$) exhibit roughly similar patterns; the $E_{p}-F$ relation in both the precursor and main burst (100$\%$) exhibits a positive correlation of at least moderate strength. Next, we constrain the outflow properties of the precursors and the main bursts and find that most of them exhibit typical properties of photosphere radiation. Finally, we compare the time-integrated spectra of the precursors and the main bursts and find that nearly all of them are located in similar regions of the Amati relation and follow the Yonetoku relation. Therefore, we conclude that main bursts are continuations of precursors and they may share a common physical origin.
Observation of a large-scale filament eruption initiated by two small-scale erupting filaments pushing out from below
Yongliang Song, Jiangtao Su, Qingmin Zhang, Mei Zhang, Yuanyong Deng, Xianyong Bai, Suo Liu, Xiao Yang, Jie Chen, Haiqing Xu, Kaifan Ji, Ziyao Hu
May 24 2024 astro-ph.SR arXiv:2405.13311v1

@misc{2405.13311, author = {Yongliang Song and Jiangtao Su and Qingmin Zhang and Mei Zhang and Yuanyong Deng and Xianyong Bai and Suo Liu and Xiao Yang and Jie Chen and Haiqing Xu and Kaifan Ji and Ziyao Hu}, title = {{O}bservation of a large-scale filament eruption initiated by two small-scale erupting filaments pushing out from below}, year = {2024}, eprint = {2405.13311}, note = {arXiv:2405.13311v1} }
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Filament eruptions often result in flares and coronal mass ejections (CMEs). Most studies attribute the filament eruptions to their instabilities or magnetic reconnection. In this study, we report a unique observation of a filament eruption whose initiation process has not been reported before. This large-scale filament, with a length of about 360 Mm crossing an active region, is forced to erupted by two small-scale erupting filaments pushing out from below. This process of multi-filament eruption results in an M6.4 flare in the active region NOAA 13229 on 25th February 2023. The whole process can be divided into three stages: the eruptions of two active-region filaments F1 and F2; the interactions between the erupting F1, F2, and the large-scale filament F3; and the eruption of F3. Though this multi-filament eruption occurs near the northwest limb of the solar disk, it produces a strong halo CME that causes a significant geomagnetic disturbance. Our observations present a new filament eruption mechanism, in which the initial kinetic energy of the eruption is obtained from and transported to by other erupting structures. This event provides us a unique insight into the dynamics of multi-filament eruptions and their corresponding effects on the interplanetary space.
Solar fusion III: New data and theory for hydrogen-burning stars
B. Acharya, M. Aliotta, A. B. Balantekin, D. Bemmerer, C. A. Bertulani, A. Best, C. R. Brune, R. Buompane, F. Cavanna, J. W. Chen, J. Colgan, A. Czarnecki, B. Davids, R. J. deBoer, F. Delahaye, R. Depalo, A. García, M. Gatu Johnson, D. Gazit, L. Gialanella, et al (30)
May 13 2024 astro-ph.SR astro-ph.HE nucl-ex nucl-th arXiv:2405.06470v1

@misc{2405.06470, author = {B.~Acharya and M.~Aliotta and A.~B.~Balantekin and D.~Bemmerer and C.~A.~Bertulani and A.~Best and C.~R.~Brune and R.~Buompane and F.~Cavanna and J.~W.~Chen and J.~Colgan and A.~Czarnecki and B.~Davids and R.~J.~deBoer and F.~Delahaye and R.~Depalo and A.~García and M.~Gatu Johnson and D.~Gazit and L.~Gialanella and U.~Greife and D.~Guffanti and A.~Guglielmetti and K.~Hambleton and W.~C.~Haxton and Y.~Herrera and M.~Huang and C.~Iliadis and K.~Kravvaris and M.~La Cognata and K.~Langanke and L.~E.~Marcucci and T.~Nagayama and K.~M.~Nollett and D.~Odell and G.~D.~Orebi Gann and D.~Piatti and M.~Pinsonneault and L.~Platter and R.~G.~H.~Robertson and G.~Rupak and A.~Serenelli and M.~Sferrazza and T.~Szücs and X.~Tang and A.~Tumino and F.~L.~Villante and A.~Walker-Loud and X.~Zhang and K.~Zuber}, title = {{S}olar fusion {III}: {N}ew data and theory for hydrogen-burning stars}, year = {2024}, eprint = {2405.06470}, note = {arXiv:2405.06470v1} }
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In stars that lie on the main sequence in the Hertzsprung Russel diagram, like our sun, hydrogen is fused to helium in a number of nuclear reaction chains and series, such as the proton-proton chain and the carbon-nitrogen-oxygen cycles. Precisely determined thermonuclear rates of these reactions lie at the foundation of the standard solar model. This review, the third decadal evaluation of the nuclear physics of hydrogen-burning stars, is motivated by the great advances made in recent years by solar neutrino observatories, putting experimental knowledge of the proton-proton chain neutrino fluxes in the few-percent precision range. The basis of the review is a one-week community meeting held in July 2022 in Berkeley, California, and many subsequent digital meetings and exchanges. Each of the relevant reactions of solar and quiescent stellar hydrogen burning is reviewed here, from both theoretical and experimental perspectives. Recommendations for the state of the art of the astrophysical S-factor and its uncertainty are formulated for each of them. Several other topics of paramount importance for the solar model are reviewed, as well: recent and future neutrino experiments, electron screening, radiative opacities, and current and upcoming experimental facilities. In addition to reaction-specific recommendations, also general recommendations are formed.
A comparative analysis of two peculiar long Gamma-ray bursts: GRB 230307A and GRB 211211A
Zhao-Yang Peng, Jia-Ming Chen, Jirong Mao
Apr 30 2024 astro-ph.HE arXiv:2404.17913v1

@misc{2404.17913, author = {Zhao-Yang Peng and Jia-Ming Chen and Jirong Mao}, title = {{A} comparative analysis of two peculiar long {G}amma-ray bursts: {GRB} 230307{A} and {GRB} 211211{A}}, year = {2024}, eprint = {2404.17913}, note = {arXiv:2404.17913v1} }
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GRB 211211A is a peculiar long Gamma-ray burst (GRB) with very high brightness and short burst properties. It's full lightcurve consists of three emission episodes, i.e. a precursor, a main burst and a extended emission. We find a recently detected long-duration GRB 230307A also includes the three consistent emission episodes. Furthermore, the two bursts have similar redshift 0.076 and 0.065, respectively. We perform a detail temporal and spectral analysis of the two GRBs to compare their temporal and spectral properties. Our analysis shows that the two bursts share great similarities for both the whole emission and the three corresponding emission phases, which are listed as follows: (1) they have near zero spectral lag, (2) they have very short minimum variability timescale (MVT), (3) they lie in the same region of in the MVT-$T_{90}$, Amati relation, and hardness-$T_{90}$ planes, (4) the three phases are quasi-thermal spectra, (5) both the peak energy and the low-energy index track the flux, (6) the time-resolved spectra are much wider than those of the blackbody prediced by theory model, (7) there are strong correlations between thermal flux and total flux and the correlation coefficients as well as the slopes for the corresponding stages are very consistent, (8) the photosphere emission properties are very consistent. Other investigations and observations suggest the two GRBs indeed belong to short burst with a compact star merger origin. Therefore, we think that GRB 230307A and GRB 211211A are the rare and similar GRBs and the photospheric radiation can interpret their radiation mechanisms.
A Comparative Study of the Ground State Transitions of CO and [C I] as Molecular Gas Tracers at High Redshift
Marta Frias Castillo, Matus Rybak, Jacqueline A. Hodge, Paul Van der Werk, Ian Smail, Joshua Butterworth, Jasper Jansen, Theodoros Topkaras, Chian-Chou Chen, Scott C. Chapman, Axel Weiss, Hiddo Algera, Jack E. Birkin, Elisabete da Cunha, Jianhang Chen, Helmut Dannerbauer, E.F. Jiménez-Andrade, Soh Ikarashi, Cheng-Lin Liao, Eric J. Murphy, et al (5)
Apr 09 2024 astro-ph.GA arXiv:2404.05596v1

@misc{2404.05596, author = {Marta Frias Castillo and Matus Rybak and Jacqueline A.~Hodge and Paul Van der Werk and Ian Smail and Joshua Butterworth and Jasper Jansen and Theodoros Topkaras and Chian-Chou Chen and Scott C.~Chapman and Axel Weiss and Hiddo Algera and Jack E.~Birkin and Elisabete da Cunha and Jianhang Chen and Helmut Dannerbauer and E.F.~Jiménez-Andrade and Soh Ikarashi and Cheng-Lin Liao and Eric J.~Murphy and A.M.~Swinbank and Fabian Walter and Gabriela Calistro Rivera and R.~J.~Ivison and Claudia del P.~Lagos}, title = {{A} {C}omparative {S}tudy of the {G}round {S}tate {T}ransitions of {CO} and [{C} {I}] as {M}olecular {G}as {T}racers at {H}igh {R}edshift}, year = {2024}, eprint = {2404.05596}, note = {arXiv:2404.05596v1} }
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The CO(1--0) and [\ionC1](1--0) emission lines are well-established tracers of cold molecular gas mass in local galaxies. At high redshift, where the interstellar medium (ISM) is likely to be denser, there have been limited direct comparisons of both ground state transitions. Here we present a study of CO(1--0) and [\ionC1](1--0) emission in a sample of 20 unlensed dusty, star-forming galaxies at $z=2-5$. The CO(1--0)/[\ionC1](1--0) ratio is constant up to at least $z=5$, supporting the use of [CI](1-0) as a gas mass tracer. PDR modelling of the available data indicates a median H$_2$ density of log$(n~[$cm$^{-3}])=4.7\pm0.2$, and UV radiation field log$(G_{\mathrm{UV}} [G$_0$])=3.2\pm0.2$. We use the CO(1--0), [\ionC1](1--0) and 3mm dust continuum measurements to cross--calibrate the respective gas mass conversion factors, finding no dependence of these factors on either redshift or infrared luminosity. Assuming a variable CO conversion factor then implies [\ionC1] and dust conversion factors that differ from canonically assumed values but are consistent with the solar/super-solar metallicities expected for our sources. Radiative transfer modelling shows that the warmer CMB at high redshift can significantly affect the [\ionC1] as well as CO emission, which can change the derived molecular gas masses by up to 70\% for the coldest kinetic gas temperatures expected. Nevertheless, we show that the magnitude of the effect on the ratio of the tracers is within the known scatter of the $L'_\mathrm{CO}-L'_\mathrm{[CI]}$ relation. Further determining the absolute decrease of individual line intensities will require well-sampled spectral line energy distributions (SLEDs) to model the gas excitation conditions in more detail.
Observation of Gravitational Waves from the Coalescence of a $2.5\text{-}4.5~M_\odot$ Compact Object and a Neutron Star
LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, A. G. Abac, R. Abbott, I. Abouelfettouh, F. Acernese, K. Ackley, S. Adhicary, N. Adhikari, R. X. Adhikari, V. K. Adkins, D. Agarwal, M. Agathos, M. Aghaei Abchouyeh, O. D. Aguiar, I. Aguilar, L. Aiello, A. Ain, P. Ajith, et al (1776)
Apr 08 2024 astro-ph.HE gr-qc arXiv:2404.04248v3

@misc{2404.04248, author = {LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration and A.~G.~Abac and R.~Abbott and I.~Abouelfettouh and F.~Acernese and K.~Ackley and S.~Adhicary and N.~Adhikari and R.~X.~Adhikari and V.~K.~Adkins and D.~Agarwal and M.~Agathos and M.~Aghaei Abchouyeh and O.~D.~Aguiar and I.~Aguilar and L.~Aiello and A.~Ain and P.~Ajith and S.~Akçay and T.~Akutsu and S.~Albanesi and R.~A.~Alfaidi and A.~Al-Jodah and C.~Alléné and A.~Allocca and S.~Al-Shammari and P.~A.~Altin and S.~Alvarez-Lopez and A.~Amato and L.~Amez-Droz and A.~Amorosi and C.~Amra and A.~Ananyeva and S.~B.~Anderson and W.~G.~Anderson and M.~Andia and M.~Ando and T.~Andrade and N.~Andres and M.~Andrés-Carcasona and T.~Andrić and J.~Anglin and S.~Ansoldi and J.~M.~Antelis and S.~Antier and M.~Aoumi and E.~Z.~Appavuravther and S.~Appert and S.~K.~Apple and K.~Arai and A.~Araya and M.~C.~Araya and J.~S.~Areeda and L.~Argianas and N.~Aritomi and F.~Armato and N.~Arnaud and M.~Arogeti and S.~M.~Aronson and K.~G.~Arun and G.~Ashton and Y.~Aso and M.~Assiduo and S.~Assis de Souza Melo and S.~M.~Aston and P.~Astone and F.~Attadio and F.~Aubin and K.~AultONeal and G.~Avallone and D.~Azrad and S.~Babak and F.~Badaracco and C.~Badger and S.~Bae and S.~Bagnasco and E.~Bagui and J.~G.~Baier and L.~Baiotti and R.~Bajpai and T.~Baka and M.~Ball and G.~Ballardin and S.~W.~Ballmer and S.~Banagiri and B.~Banerjee and D.~Bankar and P.~Baral and J.~C.~Barayoga and B.~C.~Barish and D.~Barker and P.~Barneo and F.~Barone and B.~Barr and L.~Barsotti and M.~Barsuglia and D.~Barta and A.~M.~Bartoletti and M.~A.~Barton and I.~Bartos and S.~Basak and A.~Basalaev and R.~Bassiri and A.~Basti and D.~E.~Bates and M.~Bawaj and P.~Baxi and J.~C.~Bayley and A.~C.~Baylor and P.~A.~Baynard II and M.~Bazzan and V.~M.~Bedakihale and F.~Beirnaert and M.~Bejger and D.~Belardinelli and A.~S.~Bell and V.~Benedetto and W.~Benoit and I.~Bentara and J.~D.~Bentley and M.~Ben Yaala and S.~Bera and M.~Berbel and F.~Bergamin and B.~K.~Berger and S.~Bernuzzi and M.~Beroiz and C.~P.~L.~Berry and D.~Bersanetti and A.~Bertolini and J.~Betzwieser and D.~Beveridge and N.~Bevins and R.~Bhandare and U.~Bhardwaj and R.~Bhatt and D.~Bhattacharjee and S.~Bhaumik and S.~Bhowmick and A.~Bianchi and I.~A.~Bilenko and G.~Billingsley and A.~Binetti and S.~Bini and O.~Birnholtz and S.~Biscoveanu and A.~Bisht and M.~Bitossi and M.-A.~Bizouard and J.~K.~Blackburn and L.~A.~Blagg and C.~D.~Blair and D.~G.~Blair and F.~Bobba and N.~Bode and G.~Boileau and M.~Boldrini and G.~N.~Bolingbroke and A.~Bolliand and L.~D.~Bonavena and R.~Bondarescu and F.~Bondu and E.~Bonilla and M.~S.~Bonilla and A.~Bonino and R.~Bonnand and P.~Booker and A.~Borchers and V.~Boschi and S.~Bose and V.~Bossilkov and V.~Boudart and A.~Boudon and A.~Bozzi and C.~Bradaschia and P.~R.~Brady and M.~Braglia and A.~Branch and M.~Branchesi and J.~Brandt and I.~Braun and M.~Breschi and T.~Briant and A.~Brillet and M.~Brinkmann and P.~Brockill and E.~Brockmueller and A.~F.~Brooks and B.~C.~Brown and D.~D.~Brown and M.~L.~Brozzetti and S.~Brunett and G.~Bruno and R.~Bruntz and J.~Bryant and F.~Bucci and J.~Buchanan and O.~Bulashenko and T.~Bulik and H.~J.~Bulten and A.~Buonanno and K.~Burtnyk and R.~Buscicchio and D.~Buskulic and C.~Buy and R.~L.~Byer and G.~S.~Cabourn Davies and G.~Cabras and R.~Cabrita and V.~Cáceres-Barbosa and L.~Cadonati and G.~Cagnoli and C.~Cahillane and J.~Calderón Bustillo and T.~A.~Callister and E.~Calloni and J.~B.~Camp and M.~Canepa and G.~Caneva Santoro and K.~C.~Cannon and H.~Cao and L.~A.~Capistran and E.~Capocasa and E.~Capote and G.~Carapella and F.~Carbognani and M.~Carlassara and J.~B.~Carlin and M.~Carpinelli and G.~Carrillo and J.~J.~Carter and G.~Carullo and J.~Casanueva Diaz and C.~Casentini and S.~Y.~Castro-Lucas and S.~Caudill and M.~Cavaglià and R.~Cavalieri and G.~Cella and P.~Cerdá-Durán and E.~Cesarini and W.~Chaibi and P.~Chakraborty and S.~Chalathadka Subrahmanya and J.~C.~L.~Chan and M.~Chan and K.~Chandra and R.-J.~Chang and S.~Chao and P.~Char and E.~L.~Charlton and P.~Charlton and E.~Chassande-Mottin and C.~Chatterjee and Debarati Chatterjee and Deep Chatterjee and D.~Chattopadhyay and M.~Chaturvedi and S.~Chaty and K.~Chatziioannou and A.~Chen and A.~H.-Y.~Chen and D.~Chen and H.~Chen and H.~Y.~Chen and J.~Chen and K.~H.~Chen and Y.~Chen and Yanbei Chen and Yitian Chen and H.~P.~Cheng and P.~Chessa and H.~T.~Cheung and S.~Y.~Cheung and F.~Chiadini and G.~Chiarini and R.~Chierici and A.~Chincarini and M.~L.~Chiofalo and A.~Chiummo and C.~Chou and S.~Choudhary and N.~Christensen and S.~S.~Y.~Chua and P.~Chugh and G.~Ciani and P.~Ciecielag and M.~Cieślar and M.~Cifaldi and R.~Ciolfi and F.~Clara and J.~A.~Clark and J.~Clarke and T.~A.~Clarke and P.~Clearwater and S.~Clesse and E.~Coccia and E.~Codazzo and P.-F.~Cohadon and S.~Colace and M.~Colleoni and C.~G.~Collette and J.~Collins and S.~Colloms and A.~Colombo and M.~Colpi and C.~M.~Compton and G.~Connolly and L.~Conti and T.~R.~Corbitt and I.~Cordero-Carrión and S.~Corezzi and N.~J.~Cornish and A.~Corsi and S.~Cortese and C.~A.~Costa and R.~Cottingham and M.~W.~Coughlin and A.~Couineaux and J.-P.~Coulon and S.~T.~Countryman and J.-F.~Coupechoux and P.~Couvares and D.~M.~Coward and M.~J.~Cowart and R.~Coyne and K.~Craig and R.~Creed and J.~D.~E.~Creighton and T.~D.~Creighton and P.~Cremonese and A.~W.~Criswell and J.~C.~G.~Crockett-Gray and S.~Crook and R.~Crouch and J.~Csizmazia and J.~R.~Cudell and T.~J.~Cullen and A.~Cumming and E.~Cuoco and M.~Cusinato and P.~Dabadie and T.~Dal Canton and S.~Dall'Osso and S.~Dal Pra and G.~Dálya and B.~D'Angelo and S.~Danilishin and S.~D'Antonio and K.~Danzmann and K.~E.~Darroch and L.~P.~Dartez and A.~Dasgupta and S.~Datta and V.~Dattilo and A.~Daumas and N.~Davari and I.~Dave and A.~Davenport and M.~Davier and T.~F.~Davies and D.~Davis and L.~Davis and M.~C.~Davis and P.~J.~Davis and M.~Dax and J.~De Bolle and M.~Deenadayalan and J.~Degallaix and M.~De Laurentis and S.~Deléglise and F.~De Lillo and D.~Dell'Aquila and W.~Del Pozzo and F.~De Marco and F.~De Matteis and V.~D'Emilio and N.~Demos and T.~Dent and A.~Depasse and N.~DePergola and R.~De Pietri and R.~De Rosa and C.~De Rossi and R.~DeSalvo and R.~De Simone and A.~Dhani and R.~Diab and M.~C.~Díaz and M.~Di Cesare and G.~Dideron and N.~A.~Didio and T.~Dietrich and L.~Di Fiore and C.~Di Fronzo and M.~Di Giovanni and T.~Di Girolamo and D.~Diksha and A.~Di Michele and J.~Ding and S.~Di Pace and I.~Di Palma and F.~Di Renzo and Divyajyoti and A.~Dmitriev and Z.~Doctor and E.~Dohmen and P.~P.~Doleva and D.~Dominguez and L.~D'Onofrio and F.~Donovan and K.~L.~Dooley and T.~Dooney and S.~Doravari and O.~Dorosh and M.~Drago and J.~C.~Driggers and J.-G.~Ducoin and L.~Dunn and U.~Dupletsa and D.~D'Urso and H.~Duval and P.-A.~Duverne and S.~E.~Dwyer and C.~Eassa and M.~Ebersold and T.~Eckhardt and G.~Eddolls and B.~Edelman and T.~B.~Edo and O.~Edy and A.~Effler and J.~Eichholz and H.~Einsle and M.~Eisenmann and R.~A.~Eisenstein and A.~Ejlli and R.~M.~Eleveld and M.~Emma and K.~Endo and A.~J.~Engl and E.~Enloe and L.~Errico and R.~C.~Essick and H.~Estellés and D.~Estevez and T.~Etzel and M.~Evans and T.~Evstafyeva and B.~E.~Ewing and J.~M.~Ezquiaga and F.~Fabrizi and F.~Faedi and V.~Fafone and S.~Fairhurst and A.~M.~Farah and B.~Farr and W.~M.~Farr and G.~Favaro and M.~Favata and M.~Fays and M.~Fazio and J.~Feicht and M.~M.~Fejer and R.~Felicetti and E.~Fenyvesi and D.~L.~Ferguson and S.~Ferraiuolo and I.~Ferrante and T.~A.~Ferreira and F.~Fidecaro and P.~Figura and A.~Fiori and I.~Fiori and M.~Fishbach and R.~P.~Fisher and R.~Fittipaldi and V.~Fiumara and R.~Flaminio and S.~M.~Fleischer and L.~S.~Fleming and E.~Floden and E.~M.~Foley and H.~Fong and J.~A.~Font and B.~Fornal and P.~W.~F.~Forsyth and K.~Franceschetti and N.~Franchini and S.~Frasca and F.~Frasconi and A.~Frattale Mascioli and Z.~Frei and A.~Freise and O.~Freitas and R.~Frey and W.~Frischhertz and P.~Fritschel and V.~V.~Frolov and G.~G.~Fronzé and M.~Fuentes-Garcia and S.~Fujii and T.~Fujimori and P.~Fulda and M.~Fyffe and B.~Gadre and J.~R.~Gair and S.~Galaudage and V.~Galdi and H.~Gallagher and S.~Gallardo and B.~Gallego and R.~Gamba and A.~Gamboa and D.~Ganapathy and A.~Ganguly and B.~Garaventa and J.~García-Bellido and C.~García Núñez and C.~García-Quirós and J.~W.~Gardner and K.~A.~Gardner and J.~Gargiulo and A.~Garron and F.~Garufi and C.~Gasbarra and B.~Gateley and V.~Gayathri and G.~Gemme and A.~Gennai and V.~Gennari and J.~George and R.~George and O.~Gerberding and L.~Gergely and S.~Ghonge and Archisman Ghosh and Sayantan Ghosh and Shaon Ghosh and Shrobana Ghosh and Suprovo Ghosh and Tathagata Ghosh and L.~Giacoppo and J.~A.~Giaime and K.~D.~Giardina and D.~R.~Gibson and D.~T.~Gibson and C.~Gier and P.~Giri and F.~Gissi and S.~Gkaitatzis and J.~Glanzer and F.~Glotin and J.~Godfrey and P.~Godwin and N.~L.~Goebbels and E.~Goetz and J.~Golomb and S.~Gomez Lopez and B.~Goncharov and Y.~Gong and G.~González and P.~Goodarzi and S.~Goode and A.~W.~Goodwin-Jones and M.~Gosselin and A.~S.~Göttel and R.~Gouaty and D.~W.~Gould and K.~Govorkova and S.~Goyal and B.~Grace and A.~Grado and V.~Graham and A.~E.~Granados and M.~Granata and V.~Granata and S.~Gras and P.~Grassia and A.~Gray and C.~Gray and R.~Gray and G.~Greco and A.~C.~Green and S.~M.~Green and S.~R.~Green and A.~M.~Gretarsson and E.~M.~Gretarsson and D.~Griffith and W.~L.~Griffiths and H.~L.~Griggs and G.~Grignani and A.~Grimaldi and C.~Grimaud and H.~Grote and D.~Guerra and D.~Guetta and G.~M.~Guidi and A.~R.~Guimaraes and H.~K.~Gulati and F.~Gulminelli and A.~M.~Gunny and H.~Guo and W.~Guo and Y.~Guo and Anchal Gupta and Anuradha Gupta and Ish Gupta and N.~C.~Gupta and P.~Gupta and S.~K.~Gupta and T.~Gupta and N.~Gupte and J.~Gurs and N.~Gutierrez and F.~Guzman and H.-Y.~H and D.~Haba and M.~Haberland and S.~Haino and E.~D.~Hall and E.~Z.~Hamilton and G.~Hammond and W.-B.~Han and M.~Haney and J.~Hanks and C.~Hanna and M.~D.~Hannam and O.~A.~Hannuksela and A.~G.~Hanselman and H.~Hansen and J.~Hanson and R.~Harada and A.~R.~Hardison and K.~Haris and T.~Harmark and J.~Harms and G.~M.~Harry and I.~W.~Harry and J.~Hart and B.~Haskell and C.-J.~Haster and J.~S.~Hathaway and K.~Haughian and H.~Hayakawa and K.~Hayama and R.~Hayes and A.~Heffernan and A.~Heidmann and M.~C.~Heintze and J.~Heinze and J.~Heinzel and H.~Heitmann and F.~Hellman and P.~Hello and A.~F.~Helmling-Cornell and G.~Hemming and O.~Henderson-Sapir and M.~Hendry and I.~S.~Heng and E.~Hennes and C.~Henshaw and T.~Hertog and M.~Heurs and A.~L.~Hewitt and J.~Heyns and S.~Higginbotham and S.~Hild and S.~Hill and Y.~Himemoto and N.~Hirata and C.~Hirose and S.~Hoang and S.~Hochheim and D.~Hofman and N.~A.~Holland and K.~Holley-Bockelmann and Z.~J.~Holmes and D.~E.~Holz and L.~Honet and C.~Hong and J.~Hornung and S.~Hoshino and J.~Hough and S.~Hourihane and E.~J.~Howell and C.~G.~Hoy and C.~A.~Hrishikesh and H.-F.~Hsieh and C.~Hsiung and H.~C.~Hsu and W.-F.~Hsu and P.~Hu and Q.~Hu and H.~Y.~Huang and Y.-J.~Huang and A.~D.~Huddart and B.~Hughey and D.~C.~Y.~Hui and V.~Hui and S.~Husa and R.~Huxford and T.~Huynh-Dinh and L.~Iampieri and G.~A.~Iandolo and M.~Ianni and A.~Iess and H.~Imafuku and K.~Inayoshi and Y.~Inoue and G.~Iorio and M.~H.~Iqbal and J.~Irwin and R.~Ishikawa and M.~Isi and M.~A.~Ismail and Y.~Itoh and H.~Iwanaga and M.~Iwaya and B.~R.~Iyer and V.~JaberianHamedan and C.~Jacquet and P.-E.~Jacquet and S.~J.~Jadhav and S.~P.~Jadhav and T.~Jain and A.~L.~James and P.~A.~James and R.~Jamshidi and J.~Janquart and K.~Janssens and N.~N.~Janthalur and S.~Jaraba and P.~Jaranowski and R.~Jaume and W.~Javed and A.~Jennings and W.~Jia and J.~Jiang and J.~Kubisz and C.~Johanson and G.~R.~Johns and N.~A.~Johnson and N.~K.~Johnson-McDaniel and M.~C.~Johnston and R.~Johnston and N.~Johny and D.~H.~Jones and D.~I.~Jones and R.~Jones and S.~Jose and P.~Joshi and L.~Ju and K.~Jung and J.~Junker and V.~Juste and T.~Kajita and I.~Kaku and C.~Kalaghatgi and V.~Kalogera and M.~Kamiizumi and N.~Kanda and S.~Kandhasamy and G.~Kang and J.~B.~Kanner and S.~J.~Kapadia and D.~P.~Kapasi and S.~Karat and C.~Karathanasis and R.~Kashyap and M.~Kasprzack and W.~Kastaun and T.~Kato and E.~Katsavounidis and W.~Katzman and R.~Kaushik and K.~Kawabe and R.~Kawamoto and A.~Kazemi and A.~Kedia and D.~Keitel and J.~Kelley-Derzon and J.~Kennington and R.~Kesharwani and J.~S.~Key and R.~Khadela and S.~Khadka and F.~Y.~Khalili and F.~Khan and I.~Khan and T.~Khanam and M.~Khursheed and N.~M.~Khusid and W.~Kiendrebeogo and N.~Kijbunchoo and C.~Kim and J.~C.~Kim and K.~Kim and M.~H.~Kim and S.~Kim and Y.-M.~Kim and C.~Kimball and M.~Kinley-Hanlon and M.~Kinnear and J.~S.~Kissel and S.~Klimenko and A.~M.~Knee and N.~Knust and K.~Kobayashi and P.~Koch and S.~M.~Koehlenbeck and G.~Koekoek and K.~Kohri and K.~Kokeyama and S.~Koley and P.~Kolitsidou and M.~Kolstein and K.~Komori and A.~K.~H.~Kong and A.~Kontos and M.~Korobko and R.~V.~Kossak and X.~Kou and A.~Koushik and N.~Kouvatsos and M.~Kovalam and D.~B.~Kozak and S.~L.~Kranzhoff and V.~Kringel and N.~V.~Krishnendu and A.~Królak and K.~Kruska and G.~Kuehn and P.~Kuijer and S.~Kulkarni and A.~Kulur Ramamohan and A.~Kumar and Praveen Kumar and Prayush Kumar and Rahul Kumar and Rakesh Kumar and J.~Kume and K.~Kuns and N.~Kuntimaddi and S.~Kuroyanagi and N.~J.~Kurth and S.~Kuwahara and K.~Kwak and K.~Kwan and J.~Kwok and G.~Lacaille and P.~Lagabbe and D.~Laghi and S.~Lai and A.~H.~Laity and M.~H.~Lakkis and E.~Lalande and M.~Lalleman and P.~C.~Lalremruati and M.~Landry and P.~Landry and B.~B.~Lane and R.~N.~Lang and J.~Lange and B.~Lantz and A.~La Rana and I.~La Rosa and A.~Lartaux-Vollard and P.~D.~Lasky and J.~Lawrence and M.~N.~Lawrence and M.~Laxen and A.~Lazzarini and C.~Lazzaro and P.~Leaci and Y.~K.~Lecoeuche and H.~M.~Lee and H.~W.~Lee and K.~Lee and R.-K.~Lee and R.~Lee and S.~Lee and Y.~Lee and I.~N.~Legred and J.~Lehmann and L.~Lehner and M.~Le Jean and A.~Lemaître and M.~Lenti and M.~Leonardi and M.~Lequime and N.~Leroy and M.~Lesovsky and N.~Letendre and M.~Lethuillier and S.~E.~Levin and Y.~Levin and K.~Leyde and A.~K.~Y.~Li and K.~L.~Li and T.~G.~F.~Li and X.~Li and Z.~Li and A.~Lihos and C-Y.~Lin and C.-Y.~Lin and E.~T.~Lin and F.~Lin and H.~Lin and L.~C.-C.~Lin and Y.-C.~Lin and F.~Linde and S.~D.~Linker and T.~B.~Littenberg and A.~Liu and G.~C.~Liu and Jian Liu and F.~Llamas Villarreal and J.~Llobera-Querol and R.~K.~L.~Lo and J.-P.~Locquet and L.~T.~London and A.~Longo and D.~Lopez and M.~Lopez Portilla and M.~Lorenzini and A.~Lorenzo-Medina and V.~Loriette and M.~Lormand and G.~Losurdo and T.~P.~Lott IV and J.~D.~Lough and H.~A.~Loughlin and C.~O.~Lousto and M.~J.~Lowry and N.~Lu and H.~Lück and D.~Lumaca and A.~P.~Lundgren and A.~W.~Lussier and L.-T.~Ma and S.~Ma and M.~Ma'arif and R.~Macas and A.~Macedo and M.~MacInnis and R.~R.~Maciy and D.~M.~Macleod and I.~A.~O.~MacMillan and A.~Macquet and D.~Macri and K.~Maeda and S.~Maenaut and I.~Magaña Hernandez and S.~S.~Magare and C.~Magazzù and R.~M.~Magee and E.~Maggio and R.~Maggiore and M.~Magnozzi and M.~Mahesh and S.~Mahesh and M.~Maini and S.~Majhi and E.~Majorana and C.~N.~Makarem and E.~Makelele and J.~A.~Malaquias-Reis and U.~Mali and S.~Maliakal and A.~Malik and N.~Man and V.~Mandic and V.~Mangano and B.~Mannix and G.~L.~Mansell and G.~Mansingh and M.~Manske and M.~Mantovani and M.~Mapelli and F.~Marchesoni and D.~Marín Pina and F.~Marion and S.~Márka and Z.~Márka and A.~S.~Markosyan and A.~Markowitz and E.~Maros and S.~Marsat and F.~Martelli and I.~W.~Martin and R.~M.~Martin and B.~B.~Martinez and M.~Martinez and V.~Martinez and A.~Martini and K.~Martinovic and J.~C.~Martins and D.~V.~Martynov and E.~J.~Marx and L.~Massaro and A.~Masserot and M.~Masso-Reid and M.~Mastrodicasa and S.~Mastrogiovanni and T.~Matcovich and M.~Matiushechkina and M.~Matsuyama and N.~Mavalvala and N.~Maxwell and G.~McCarrol and R.~McCarthy and D.~E.~McClelland and S.~McCormick and L.~McCuller and S.~McEachin and C.~McElhenny and G.~I.~McGhee and J.~McGinn and K.~B.~M.~McGowan and J.~McIver and A.~McLeod and T.~McRae and D.~Meacher and Q.~Meijer and A.~Melatos and S.~Mellaerts and A.~Menendez-Vazquez and C.~S.~Menoni and F.~Mera and R.~A.~Mercer and L.~Mereni and K.~Merfeld and E.~L.~Merilh and J.~R.~Mérou and J.~D.~Merritt and M.~Merzougui and C.~Messenger and C.~Messick and M.~Meyer-Conde and F.~Meylahn and A.~Mhaske and A.~Miani and H.~Miao and I.~Michaloliakos and C.~Michel and Y.~Michimura and H.~Middleton and A.~L.~Miller and S.~Miller and M.~Millhouse and E.~Milotti and V.~Milotti and Y.~Minenkov and N.~Mio and Ll.~M.~Mir and L.~Mirasola and M.~Miravet-Tenés and C.-A.~Miritescu and A.~K.~Mishra and A.~Mishra and C.~Mishra and T.~Mishra and A.~L.~Mitchell and J.~G.~Mitchell and S.~Mitra and V.~P.~Mitrofanov and R.~Mittleman and O.~Miyakawa and S.~Miyamoto and S.~Miyoki and G.~Mo and L.~Mobilia and S.~R.~P.~Mohapatra and S.~R.~Mohite and M.~Molina-Ruiz and C.~Mondal and M.~Mondin and M.~Montani and C.~J.~Moore and D.~Moraru and A.~More and S.~More and G.~Moreno and C.~Morgan and S.~Morisaki and Y.~Moriwaki and G.~Morras and A.~Moscatello and P.~Mourier and B.~Mours and C.~M.~Mow-Lowry and F.~Muciaccia and Arunava Mukherjee and D.~Mukherjee and Samanwaya Mukherjee and Soma Mukherjee and Subroto Mukherjee and Suvodip Mukherjee and N.~Mukund and A.~Mullavey and J.~Munch and J.~Mundi and C.~L.~Mungioli and W.~R.~Munn Oberg and Y.~Murakami and M.~Murakoshi and P.~G.~Murray and S.~Muusse and D.~Nabari and S.~L.~Nadji and A.~Nagar and N.~Nagarajan and K.~N.~Nagler and K.~Nakagaki and K.~Nakamura and H.~Nakano and M.~Nakano and D.~Nandi and V.~Napolano and P.~Narayan and I.~Nardecchia and T.~Narikawa and H.~Narola and L.~Naticchioni and R.~K.~Nayak and J.~Neilson and A.~Nelson and T.~J.~N.~Nelson and M.~Nery and A.~Neunzert and S.~Ng and L.~Nguyen Quynh and S.~A.~Nichols and A.~B.~Nielsen and G.~Nieradka and A.~Niko and Y.~Nishino and A.~Nishizawa and S.~Nissanke and E.~Nitoglia and W.~Niu and F.~Nocera and M.~Norman and C.~North and J.~Novak and J.~F.~Nuño Siles and L.~K.~Nuttall and K.~Obayashi and J.~Oberling and J.~O'Dell and M.~Oertel and A.~Offermans and G.~Oganesyan and J.~J.~Oh and K.~Oh and T.~O'Hanlon and M.~Ohashi and M.~Ohkawa and F.~Ohme and A.~S.~Oliveira and R.~Oliveri and B.~O'Neal and K.~Oohara and B.~O'Reilly and N.~D.~Ormsby and M.~Orselli and R.~O'Shaughnessy and S.~O'Shea and Y.~Oshima and S.~Oshino and S.~Ossokine and C.~Osthelder and I.~Ota and D.~J.~Ottaway and A.~Ouzriat and H.~Overmier and B.~J.~Owen and A.~E.~Pace and R.~Pagano and M.~A.~Page and A.~Pai and A.~Pal and S.~Pal and M.~A.~Palaia and M.~Pálfi and P.~P.~Palma and C.~Palomba and P.~Palud and H.~Pan and J.~Pan and K.~C.~Pan and R.~Panai and P.~K.~Panda and S.~Pandey and L.~Panebianco and P.~T.~H.~Pang and F.~Pannarale and K.~A.~Pannone and B.~C.~Pant and F.~H.~Panther and F.~Paoletti and A.~Paolone and E.~E.~Papalexakis and L.~Papalini and G.~Papigkiotis and A.~Paquis and A.~Parisi and B.-J.~Park and J.~Park and W.~Parker and G.~Pascale and D.~Pascucci and A.~Pasqualetti and R.~Passaquieti and L.~Passenger and D.~Passuello and O.~Patane and D.~Pathak and M.~Pathak and A.~Patra and B.~Patricelli and A.~S.~Patron and K.~Paul and S.~Paul and E.~Payne and T.~Pearce and M.~Pedraza and R.~Pegna and A.~Pele and F.~E.~Peña Arellano and S.~Penn and M.~D.~Penuliar and A.~Perego and Z.~Pereira and J.~J.~Perez and C.~Périgois and G.~Perna and A.~Perreca and J.~Perret and S.~Perriès and J.~W.~Perry and D.~Pesios and S.~Petracca and C.~Petrillo and H.~P.~Pfeiffer and H.~Pham and K.~A.~Pham and K.~S.~Phukon and H.~Phurailatpam and M.~Piarulli and L.~Piccari and O.~J.~Piccinni and M.~Pichot and M.~Piendibene and F.~Piergiovanni and L.~Pierini and G.~Pierra and V.~Pierro and M.~Pietrzak and M.~Pillas and F.~Pilo and L.~Pinard and I.~M.~Pinto and M.~Pinto and B.~J.~Piotrzkowski and M.~Pirello and M.~D.~Pitkin and A.~Placidi and E.~Placidi and M.~L.~Planas and W.~Plastino and R.~Poggiani and E.~Polini and L.~Pompili and J.~Poon and E.~Porcelli and E.~K.~Porter and C.~Posnansky and R.~Poulton and J.~Powell and M.~Pracchia and B.~K.~Pradhan and T.~Pradier and A.~K.~Prajapati and K.~Prasai and R.~Prasanna and P.~Prasia and G.~Pratten and G.~Principe and M.~Principe and G.~A.~Prodi and L.~Prokhorov and P.~Prosposito and A.~Puecher and J.~Pullin and M.~Punturo and P.~Puppo and M.~Pürrer and H.~Qi and J.~Qin and G.~Quéméner and V.~Quetschke and C.~Quigley and P.~J.~Quinonez and F.~J.~Raab and S.~S.~Raabith and G.~Raaijmakers and S.~Raja and C.~Rajan and B.~Rajbhandari and K.~E.~Ramirez and F.~A.~Ramis Vidal and A.~Ramos-Buades and D.~Rana and S.~Ranjan and K.~Ransom and P.~Rapagnani and B.~Ratto and S.~Rawat and A.~Ray and V.~Raymond and M.~Razzano and J.~Read and M.~Recaman Payo and T.~Regimbau and L.~Rei and S.~Reid and D.~H.~Reitze and P.~Relton and A.~I.~Renzini and P.~Rettegno and B.~Revenu and R.~Reyes and A.~S.~Rezaei and F.~Ricci and M.~Ricci and A.~Ricciardone and J.~W.~Richardson and M.~Richardson and A.~Rijal and K.~Riles and H.~K.~Riley and S.~Rinaldi and J.~Rittmeyer and C.~Robertson and F.~Robinet and M.~Robinson and A.~Rocchi and L.~Rolland and J.~G.~Rollins and A.~E.~Romano and R.~Romano and A.~Romero and I.~M.~Romero-Shaw and J.~H.~Romie and S.~Ronchini and T.~J.~Roocke and L.~Rosa and T.~J.~Rosauer and C.~A.~Rose and D.~Rosińska and M.~P.~Ross and M.~Rossello and S.~Rowan and S.~K.~Roy and S.~Roy and D.~Rozza and P.~Ruggi and N.~Ruhama and E.~Ruiz Morales and K.~Ruiz-Rocha and S.~Sachdev and T.~Sadecki and J.~Sadiq and P.~Saffarieh and M.~R.~Sah and S.~S.~Saha and S.~Saha and T.~Sainrat and S.~Sajith Menon and K.~Sakai and M.~Sakellariadou and S.~Sakon and O.~S.~Salafia and F.~Salces-Carcoba and L.~Salconi and M.~Saleem and F.~Salemi and M.~Sallé and S.~Salvador and A.~Sanchez and E.~J.~Sanchez and J.~H.~Sanchez and L.~E.~Sanchez and N.~Sanchis-Gual and J.~R.~Sanders and E.~M.~Sänger and F.~Santoliquido and T.~R.~Saravanan and N.~Sarin and S.~Sasaoka and A.~Sasli and P.~Sassi and B.~Sassolas and H.~Satari and B.~S.~Sathyaprakash and R.~Sato and Y.~Sato and O.~Sauter and R.~L.~Savage and T.~Sawada and H.~L.~Sawant and S.~Sayah and V.~Scacco and D.~Schaetzl and M.~Scheel and A.~Schiebelbein and M.~G.~Schiworski and P.~Schmidt and S.~Schmidt and R.~Schnabel and M.~Schneewind and R.~M.~S.~Schofield and K.~Schouteden and B.~W.~Schulte and B.~F.~Schutz and E.~Schwartz and M.~Scialpi and J.~Scott and S.~M.~Scott and T.~C.~Seetharamu and M.~Seglar-Arroyo and Y.~Sekiguchi and D.~Sellers and A.~S.~Sengupta and D.~Sentenac and E.~G.~Seo and J.~W.~Seo and V.~Sequino and M.~Serra and G.~Servignat and A.~Sevrin and T.~Shaffer and U.~S.~Shah and M.~A.~Shaikh and L.~Shao and A.~K.~Sharma and P.~Sharma and S.~Sharma-Chaudhary and M.~R.~Shaw and P.~Shawhan and N.~S.~Shcheblanov and E.~Sheridan and Y.~Shikano and M.~Shikauchi and K.~Shimode and H.~Shinkai and J.~Shiota and D.~H.~Shoemaker and D.~M.~Shoemaker and R.~W.~Short and S.~ShyamSundar and A.~Sider and H.~Siegel and M.~Sieniawska and D.~Sigg and L.~Silenzi and M.~Simmonds and L.~P.~Singer and A.~Singh and D.~Singh and M.~K.~Singh and S.~Singh and A.~Singha and A.~M.~Sintes and V.~Sipala and V.~Skliris and B.~J.~J.~Slagmolen and T.~J.~Slaven-Blair and J.~Smetana and J.~R.~Smith and L.~Smith and R.~J.~E.~Smith and W.~J.~Smith and J.~Soldateschi and K.~Somiya and I.~Song and K.~Soni and S.~Soni and V.~Sordini and F.~Sorrentino and N.~Sorrentino and H.~Sotani and R.~Soulard and A.~Southgate and V.~Spagnuolo and A.~P.~Spencer and M.~Spera and P.~Spinicelli and J.~B.~Spoon and C.~A.~Sprague and A.~K.~Srivastava and F.~Stachurski and D.~A.~Steer and J.~Steinlechner and S.~Steinlechner and N.~Stergioulas and P.~Stevens and S.~Stevenson and M.~StPierre and G.~Stratta and M.~D.~Strong and A.~Strunk and R.~Sturani and A.~L.~Stuver and M.~Suchenek and S.~Sudhagar and N.~Sueltmann and L.~Suleiman and K.~D.~Sullivan and L.~Sun and S.~Sunil and J.~Suresh and P.~J.~Sutton and T.~Suzuki and Y.~Suzuki and B.~L.~Swinkels and A.~Syx and M.~J.~Szczepańczyk and P.~Szewczyk and M.~Tacca and H.~Tagoshi and S.~C.~Tait and H.~Takahashi and R.~Takahashi and A.~Takamori and T.~Takase and K.~Takatani and H.~Takeda and K.~Takeshita and C.~Talbot and M.~Tamaki and N.~Tamanini and D.~Tanabe and K.~Tanaka and S.~J.~Tanaka and T.~Tanaka and D.~Tang and S.~Tanioka and D.~B.~Tanner and L.~Tao and R.~D.~Tapia and E.~N.~Tapia San Martín and R.~Tarafder and C.~Taranto and A.~Taruya and J.~D.~Tasson and M.~Teloi and R.~Tenorio and H.~Themann and A.~Theodoropoulos and M.~P.~Thirugnanasambandam and L.~M.~Thomas and M.~Thomas and P.~Thomas and J.~E.~Thompson and S.~R.~Thondapu and K.~A.~Thorne and E.~Thrane and J.~Tissino and A.~Tiwari and P.~Tiwari and S.~Tiwari and V.~Tiwari and M.~R.~Todd and A.~M.~Toivonen and K.~Toland and A.~E.~Tolley and T.~Tomaru and K.~Tomita and T.~Tomura and H.~Tong and C.~Tong-Yu and A.~Toriyama and N.~Toropov and A.~Torres-Forné and C.~I.~Torrie and M.~Toscani and I.~Tosta e Melo and E.~Tournefier and A.~Trapananti and F.~Travasso and G.~Traylor and M.~Trevor and M.~C.~Tringali and A.~Tripathee and G.~Troian and L.~Troiano and A.~Trovato and L.~Trozzo and R.~J.~Trudeau and T.~T.~L.~Tsang and S.~Tsuchida and L.~Tsukada and T.~Tsutsui and K.~Turbang and M.~Turconi and C.~Turski and H.~Ubach and N.~Uchikata and T.~Uchiyama and R.~P.~Udall and T.~Uehara and M.~Uematsu and K.~Ueno and S.~Ueno and V.~Undheim and T.~Ushiba and M.~Vacatello and H.~Vahlbruch and N.~Vaidya and G.~Vajente and A.~Vajpeyi and G.~Valdes and J.~Valencia and M.~Valentini and S.~A.~Vallejo-Peña and S.~Vallero and V.~Valsan and N.~van Bakel and M.~van Beuzekom and M.~van Dael and J.~F.~J.~van den Brand and C.~Van Den Broeck and D.~C.~Vander-Hyde and M.~van der Sluys and A.~Van de Walle and J.~van Dongen and K.~Vandra and H.~van Haevermaet and J.~V.~van Heijningen and P.~Van Hove and M.~VanKeuren and J.~Vanosky and M.~H.~P.~M.~van Putten and Z.~van Ranst and N.~van Remortel and M.~Vardaro and A.~F.~Vargas and J.~J.~Varghese and V.~Varma and A.~Vecchio and G.~Vedovato and J.~Veitch and P.~J.~Veitch and S.~Venikoudis and J.~Venneberg and P.~Verdier and D.~Verkindt and B.~Verma and P.~Verma and Y.~Verma and S.~M.~Vermeulen and F.~Vetrano and A.~Veutro and A.~M.~Vibhute and A.~Viceré and S.~Vidyant and A.~D.~Viets and A.~Vijaykumar and A.~Vilkha and V.~Villa-Ortega and E.~T.~Vincent and J.-Y.~Vinet and S.~Viret and A.~Virtuoso and S.~Vitale and A.~Vives and H.~Vocca and D.~Voigt and E.~R.~G.~von Reis and J.~S.~A.~von Wrangel and S.~P.~Vyatchanin and L.~E.~Wade and M.~Wade and K.~J.~Wagner and A.~Wajid and M.~Walker and G.~S.~Wallace and L.~Wallace and H.~Wang and J.~Z.~Wang and W.~H.~Wang and Z.~Wang and G.~Waratkar and J.~Warner and M.~Was and T.~Washimi and N.~Y.~Washington and D.~Watarai and K.~E.~Wayt and B.~R.~Weaver and B.~Weaver and C.~R.~Weaving and S.~A.~Webster and M.~Weinert and A.~J.~Weinstein and R.~Weiss and F.~Wellmann and L.~Wen and P.~Weßels and K.~Wette and J.~T.~Whelan and B.~F.~Whiting and C.~Whittle and J.~B.~Wildberger and O.~S.~Wilk and D.~Wilken and A.~T.~Wilkin and D.~J.~Willadsen and K.~Willetts and D.~Williams and M.~J.~Williams and N.~S.~Williams and J.~L.~Willis and B.~Willke and M.~Wils and J.~Winterflood and C.~C.~Wipf and G.~Woan and J.~Woehler and J.~K.~Wofford and N.~E.~Wolfe and H.~T.~Wong and H.~W.~Y.~Wong and I.~C.~F.~Wong and J.~L.~Wright and M.~Wright and C.~Wu and D.~S.~Wu and H.~Wu and E.~Wuchner and D.~M.~Wysocki and V.~A.~Xu and Y.~Xu and N.~Yadav and H.~Yamamoto and K.~Yamamoto and T.~S.~Yamamoto and T.~Yamamoto and S.~Yamamura and R.~Yamazaki and S.~Yan and T.~Yan and F.~W.~Yang and F.~Yang and K.~Z.~Yang and Y.~Yang and Z.~Yarbrough and H.~Yasui and S.-W.~Yeh and A.~B.~Yelikar and X.~Yin and J.~Yokoyama and T.~Yokozawa and J.~Yoo and H.~Yu and S.~Yuan and H.~Yuzurihara and A.~Zadrożny and M.~Zanolin and M.~Zeeshan and T.~Zelenova and J.-P.~Zendri and M.~Zeoli and M.~Zerrad and M.~Zevin and A.~C.~Zhang and L.~Zhang and R.~Zhang and T.~Zhang and Y.~Zhang and C.~Zhao and Yue Zhao and Yuhang Zhao and Y.~Zheng and H.~Zhong and R.~Zhou and X.-J.~Zhu and Z.-H.~Zhu and A.~B.~Zimmerman and M.~E.~Zucker and J.~Zweizig}, title = {{O}bservation of {G}ravitational {W}aves from the {C}oalescence of a $2.5\text{-}4.5~{M}_\odot$ {C}ompact {O}bject and a {N}eutron {S}tar}, year = {2024}, eprint = {2404.04248}, howpublished = {ApJL 970, L34 (2024)}, doi = {10.3847/2041-8213/ad5beb}, note = {arXiv:2404.04248v3} }
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We report the observation of a coalescing compact binary with component masses $2.5\text{-}4.5~M_\odot$ and $1.2\text{-}2.0~M_\odot$ (all measurements quoted at the 90% credible level). The gravitational-wave signal GW230529_181500 was observed during the fourth observing run of the LIGO-Virgo-KAGRA detector network on 2023 May 29 by the LIGO Livingston Observatory. The primary component of the source has a mass less than $5~M_\odot$ at 99% credibility. We cannot definitively determine from gravitational-wave data alone whether either component of the source is a neutron star or a black hole. However, given existing estimates of the maximum neutron star mass, we find the most probable interpretation of the source to be the coalescence of a neutron star with a black hole that has a mass between the most massive neutron stars and the least massive black holes observed in the Galaxy. We provisionally estimate a merger rate density of $55^{+127}_{-47}~\text{Gpc}^{-3}\,\text{yr}^{-1}$ for compact binary coalescences with properties similar to the source of GW230529_181500; assuming that the source is a neutron star-black hole merger, GW230529_181500-like sources constitute about 60% of the total merger rate inferred for neutron star-black hole coalescences. The discovery of this system implies an increase in the expected rate of neutron star-black hole mergers with electromagnetic counterparts and provides further evidence for compact objects existing within the purported lower mass gap.
Licking the plate: dusty star-forming galaxies buried in the ALMA calibration data
Jianhang Chen, R. J. Ivison, M. Zwaan, Celine Peroux, A. D. Biggs
Apr 04 2024 astro-ph.GA astro-ph.CO arXiv:2404.02293v1

@misc{2404.02293, author = {Jianhang Chen and R.~J.~Ivison and M.~Zwaan and Celine Peroux and A.~D.~Biggs}, title = {{L}icking the plate: dusty star-forming galaxies buried in the {ALMA} calibration data}, year = {2024}, eprint = {2404.02293}, howpublished = {https://www.epj-conferences.org/articles/epjconf/abs/2024/03/epjconf_mmUniverse2023_00011/epjconf_mmUniverse2023_00011.html}, doi = {10.1051/epjconf/202429300011}, note = {arXiv:2404.02293v1} }
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Deep, unbiased surveys are essential to decipher the cosmic evolution of galaxies. The submillimetre (submm) and millimetre (mm) windows complement the UV/optical waveband and are key to revealing the cold and dusty Universe. Traditional ways of conducting deep surveys resort to either lensed fields or target small areas for ultra-long integrations. These surveys have greatly advanced our understanding of dusty star-forming galaxies (DSFGs), but are susceptible to lensing uncertainties and cosmic variance and will be expensive to expand. Here, we summarise our recent multi-wavelength survey of DSFGs in the vicinity of ALMA's calibrators: the ALMACAL survey. These fields have accumulated many hundreds of hours of on-source time, reaching depths and effective areas that are competitive with bespoke cosmological surveys. We summarise the multi-wavelength number counts from ALMACAL and the resolved fraction of the Cosmic Infrared Background (CIB) from submm to mm wavelengths. Meanwhile, combining all available ALMA observations in each field results in impressive frequency coverage, which often yields the redshifts of these DSFGs. The ALMACAL survey has demonstrated the scientific value of calibration scans for all submm/mm and radio telescopes, existing and planned.
On the Connection between the Repeated X-ray Quasi-periodic Oscillation and Warm Absorber in the Active Galaxy RE~J1034+396
Zheng Zhou, Junjie Mao, Taotao Fang, Yijun Wang, Fabrizio Nicastro, Jiayi Chen
Apr 03 2024 astro-ph.HE arXiv:2404.01377v1

@misc{2404.01377, author = {Zheng Zhou and Junjie Mao and Taotao Fang and Yijun Wang and Fabrizio Nicastro and Jiayi Chen}, title = {{O}n the {C}onnection between the {R}epeated {X}-ray {Q}uasi-periodic {O}scillation and {W}arm {A}bsorber in the {A}ctive {G}alaxy {RE}~{J}1034+396}, year = {2024}, eprint = {2404.01377}, note = {arXiv:2404.01377v1} }
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We conduct an in-depth spectral analysis of $\sim1{\rm ~Ms}$ XMM-Newton data of the narrow line Seyfert 1 galaxy RE J1034+396. The long exposure ensures high spectral quality and provides us with a detailed look at the intrinsic absorption and emission features toward this target. Two warm-absorber (WA) components with different ionization states ($\log (\xi/{\rm erg~cm~s}^{-1}) \sim 4$ and $\log (\xi/{\rm erg~cm~s}^{-1}) \sim 2.5-3$) are required to explain the intrinsic absorption features in the RGS spectra. The estimated outflow velocities are around $-1400{\rm ~km~s}^{-1}$ and $-(100-300){\rm ~km~s}^{-1}$ for the high- and low-ionization WA components, respectively. Both absorbers are located beyond the broad-line region and cannot significantly affect the host environment. We analyze the warm absorbers in different flux states. We also examine the May-2007 observation in the low and high phases of quasi-periodic oscillation (QPO). In contrast to previous analyses showing a negative correlation between the high-ionization WA and the QPO phase, we have found no such variation in this WA component. We discover a broad emission bump in the spectral range of $\sim12-18$ Angstrom, covering the primary features of the high-ionization WA. This emission bump shows a dramatic change in different source states, and its intensity may positively correlate with the QPO phase. The absence of this emission bump in previous work may contribute to the suggested WA-QPO connection.
New constraints on Triton's atmosphere from the 6 October 2022 stellar occultation
Ye Yuan, Chen Zhang, Fan Li, Jian Chen, Yanning Fu, Chunhai Bai, Xing Gao, Yong Wang, Tuhong Zhong, Yixing Gao, Liang Wang, Donghua Chen, Yixing Zhang, Yang Zhang, Wenpeng Xie, Shupi Zhang, Ding Liu, Jun Cao, Xiangdong Yin, Xiaojun Mo, et al (30)
Mar 15 2024 astro-ph.EP arXiv:2403.09464v2

@misc{2403.09464, author = {Ye Yuan and Chen Zhang and Fan Li and Jian Chen and Yanning Fu and Chunhai Bai and Xing Gao and Yong Wang and Tuhong Zhong and Yixing Gao and Liang Wang and Donghua Chen and Yixing Zhang and Yang Zhang and Wenpeng Xie and Shupi Zhang and Ding Liu and Jun Cao and Xiangdong Yin and Xiaojun Mo and Jing Liu and Xinru Han and Tong Liu and Yuqiang Chen and Zhendong Gao and Xiang Zeng and Guihua Niu and Xiansheng Zheng and Yuchen Lin and Peiyu Ye and Weitang Liang and Chengcheng Zhu and Zhiqiang Hu and Jianguo He and Wei Zhang and Yue Chen and Zhuo Cheng and Yang Zhang and Tianrui Sun and Chenyang Guo and Yue Lu and Jiajun Lin and Wei Tan and Jia Zhou and Jun Xu and Jun He and Jiahui Ye and Delai Li and Shuai Zhang and Qingyue Qu}, title = {{N}ew constraints on {T}riton's atmosphere from the 6 {O}ctober 2022 stellar occultation}, year = {2024}, eprint = {2403.09464}, doi = {10.1051/0004-6361/202348460}, note = {arXiv:2403.09464v2} }
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The atmosphere of Triton was probed directly by observing a ground-based stellar occultation on 6 October 2022. This rare event yielded 23 positive light curves collected from 13 separate observation stations contributing to our campaign. The significance of this event lies in its potential to directly validate the modest pressure fluctuation on Triton, a phenomenon not definitively verified by previous observations, including only five stellar occultations, and the Voyager 2 radio occultation in 1989. Using an approach consistent with a comparable study, we precisely determined a surface pressure of $14.07_{-0.13}^{+0.21}~\mathrm{\mu bar}$ in 2022. This new pressure rules out any significant monotonic variation in pressure between 2017 and 2022 through direct observations, as it is in alignment with the 2017 value. Additionally, both the pressures in 2017 and 2022 align with the 1989 value. This provides further support for the conclusion drawn from the previous volatile transport model simulation, which is consistent with the observed alignment between the pressures in 1989 and 2017; that is to say, the pressure fluctuation is modest. Moreover, this conclusion suggests the existence of a northern polar cap extended down to at least $45^\circ$N$-60^\circ$N and the presence of nitrogen between $30^\circ$S and $0^\circ$.
Distribution Properties of the 6.7 GHz Methanol Masers and Their Surrounding Gases in the Milky Way
Tian Yang, Xi Chen, Yan-Kun Zhang, Xu-Jia Ouyang, Shi-Min Song, Jia-Liang Chen, Ying Lu
Mar 01 2024 astro-ph.GA arXiv:2402.19206v1

@misc{2402.19206, author = {Tian Yang and Xi Chen and Yan-Kun Zhang and Xu-Jia Ouyang and Shi-Min Song and Jia-Liang Chen and Ying Lu}, title = {{D}istribution {P}roperties of the 6.7 {GH}z {M}ethanol {M}asers and {T}heir {S}urrounding {G}ases in the {M}ilky {W}ay}, year = {2024}, eprint = {2402.19206}, note = {arXiv:2402.19206v1} }
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An updated catalog consisting of 1092 6.7-GHz methanol maser sources was reported in this work. Additionally, the NH3 (1, 1), NH3 (2, 2), and NH3 (3, 3) transitions were observed towards 214 star forming regions using the Shanghai Tianma radio telescope (TMRT) in order to examine the differences in physical environments, such as excitation temperature and column density of molecular clouds associated with methanol masers on the Galactic scale. Statistical results reveal that the number of 6.7 GHz methanol masers in the Perseus arm is significantly lower than that in the other three main spiral arms. In addition, the Perseus arm also has the lowest gas column density among the main spiral arms traced by the NH3 observations. Both of these findings suggest that the Perseus arm has the lowest rate of high-mass star formation compared to the other three main spiral arms. We also observed a trend in which both the luminosity of 6.7 GHz methanol masers and the ammonia gas column density decreased as the galactocentric distances. This finding indicates that the density of material in the inner Milky Way is generally higher than that in the outer Milky Way. It further suggests that high-mass stars are more easily formed at the head of spiral arms. Furthermore, we found that the column density of ammonia gas is higher in the regions on the arms than that in the inter-arm regions, supporting that the former is more likely to be the birthplace of high-mass stars.
Constructing Wavefunctions for One-Body and Two-Body Gravitational Orbits in Classical Mechanics
Jixin Chen
Feb 12 2024 astro-ph.EP physics.class-ph physics.space-ph arXiv:2402.06109v2

@misc{2402.06109, author = {Jixin Chen}, title = {{C}onstructing {W}avefunctions for {O}ne-{B}ody and {T}wo-{B}ody {G}ravitational {O}rbits in {C}lassical {M}echanics}, year = {2024}, eprint = {2402.06109}, note = {arXiv:2402.06109v2} }
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The circular orbits and elliptical orbits of moving objects in a gravitational field are essential information in astronomy. There have been many methods developed in the literature and textbooks to describe these orbits. In this report, I propose to use the vis-viva equation to construct a complex function to store the state of a moving object in elliptical orbits such that one can calculate its near future numerically. This state function is constructed by splitting its momentum into real and imaginary parts with one perpendicular to the radius of the mass center and the other parallel. The wavefunctions of electrons of hydrogen atoms in quantum mechanics inspire this idea. The equations are derived for one-body problems. Two-body problems can be constructed with subsets of one-body problems with the same center of mass, but different effective mass pinned there, significantly different from existing methods and providing the same results.
Forecast of foreground cleaning strategies for AliCPT-1
Junzhou Zhang, Shamik Ghosh, Jiazheng Dou, Yang Liu, Siyu Li, Jiming Chen, Jiaxin Wang, Zhaoxuan Zhang, Jacques Delabrouille, Mathieu Remazeilles, Chang Feng, Bin Hu, Hao Liu, Larissa Santos, Pengjie Zhang, Wen Zhao, Le Zhang, Zhi-Qi Huang, Hong Li, Chao-Lin Kuo, et al (1)
Feb 05 2024 astro-ph.CO arXiv:2402.01233v2

@misc{2402.01233, author = {Junzhou Zhang and Shamik Ghosh and Jiazheng Dou and Yang Liu and Siyu Li and Jiming Chen and Jiaxin Wang and Zhaoxuan Zhang and Jacques Delabrouille and Mathieu Remazeilles and Chang Feng and Bin Hu and Hao Liu and Larissa Santos and Pengjie Zhang and Wen Zhao and Le Zhang and Zhi-Qi Huang and Hong Li and Chao-Lin Kuo and Xinmin Zhang}, title = {{F}orecast of foreground cleaning strategies for {A}li{CPT}-1}, year = {2024}, eprint = {2402.01233}, note = {arXiv:2402.01233v2} }
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We report the test results of several independent foreground-cleaning pipelines used in the Ali CMB Polarization Telescope experiment (AliCPT-1), a high-altitude CMB imager in the Northern hemisphere with thousands of detectors dedicated to the search for a primordial CMB polarization $B$-mode signature. Based on simulated data from 4 detector modules and a single season of observation, which we refer to as Data Challenge 1 (DC1), we employ different and independent pipelines to examine the robustness and effectiveness of the estimates on foreground parameters and the primordial $B$-mode detection. The foreground-cleaning strategies used in the pipelines include the parametric method of template fitting (TF) and the non-parametric methods of the constrained internal linear combination (cILC), the analytical blind separation (ABS), and the generalized least squares (GLS). We examine the impact of possible foreground residuals on the estimate of the CMB tensor-to-scalar ratio ($r$) for each pipeline by changing the contamination components in the simulated maps and varying the foreground models and sky patches for various tests. According to the DC1 data with the simulation input value $r_{\rm true}=0.023$, the foreground residual contamination levels in the TF/ABS/cILC/GLS pipelines are well within the corresponding statistical errors at the $2\sigma$ level. Furthermore, by utilizing the tension estimator, which helps identify significant residual foreground contamination in the detection of the primordial $B$-mode signal by quantifying the discrepancy between various $r$ measurements, we conclude that the presence of small foreground residuals does not lead to any significant inconsistency in the estimation of $r$.
Inferring binary parameters with dual-line gravitational wave detection from tight inspiraling double neutron stars
Wen-Fan Feng, Jie-Wen Chen, Tan Liu, Yan Wang, Soumya D. Mohanty
Jan 23 2024 astro-ph.HE gr-qc arXiv:2401.11241v1

@misc{2401.11241, author = {Wen-Fan Feng and Jie-Wen Chen and Tan Liu and Yan Wang and Soumya D.~Mohanty}, title = {{I}nferring binary parameters with dual-line gravitational wave detection from tight inspiraling double neutron stars}, year = {2024}, eprint = {2401.11241}, note = {arXiv:2401.11241v1} }
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Neutron star (NS) binaries can be potentially intriguing gravitational wave (GW) sources, with both high- and low-frequency radiations from the possibly aspherical individual stars and the binary orbit, respectively. The successful detection of such a dual-line source could provide fresh insights into binary geometry and NS physics. In the absence of electromagnetic observations, we develop a strategy for inferring the spin-orbit misalignment angle using the tight dual-line double NS system under the spin-orbit coupling. Based on the four-year joint detection of a typical dual-line system with LISA and Cosmic Explorer, we find that the misalignment angle and the NS moment of inertia can be measured with sub-percentage and 5% accuracy, respectively.
Transient quasi-periodic oscillations in the gamma-ray light curves of bright blazars
Junping Chen, Jinjie Yu, Weitian Huang, Nan Ding
Jan 22 2024 astro-ph.HE arXiv:2401.10658v1

@misc{2401.10658, author = {Junping Chen and Jinjie Yu and Weitian Huang and Nan Ding}, title = {{T}ransient quasi-periodic oscillations in the gamma-ray light curves of bright blazars}, year = {2024}, eprint = {2401.10658}, note = {arXiv:2401.10658v1} }
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Transient quasi-periodic oscillations (QPOs) are extremely interesting observational phenomena. However, the precise physical mechanisms leading to their generation are still hotly debated. We performed a systematic search for transient QPO signals using Weighted Wavelet Z-transforms on the gamma-ray light curves of 134 bright blazars with peak flux exceeding $1\times10^{-6}$~ph~cm$^{-2}$~s$^{-1}$ as monitored by Fermi-LAT. Artificial light curves were generated from the power spectral density and probability distribution functions of the original light curves to assess the significance level of transient QPO. We discuss several physical mechanisms that produce transient QPOs, with the helical jet model providing the best explanation. This study identified four new transient QPO events. Interestingly, repetitive transient QPOs are observed in PKS 0537-441, and nested transient QPOs are detected in PKS 1424-41. Additionally, we find that transient QPOs tend to occur in the flare state of the blazar. Finally, we estimate the incidence of transient QPO events to be only about 3\%.
A spectral data release for 104 Type II Supernovae from the Tsinghua Supernova Group
Han Lin, Xiaofeng Wang, Jujia Zhang, Danfeng Xiang, Tianmeng Zhang, Xulin Zhao, Xinghan Zhang, Hanna Sai, Liming Rui, Jun Mo, Gaobo Xi, Fang Huang, Xue Li, Yongzhi Cai, Weili Lin, Jie Lin, Chengyuan Wu, Jicheng Zhang, Zhihao Chen, Zhitong Li, et al (16)
Jan 12 2024 astro-ph.HE arXiv:2401.05889v1

@misc{2401.05889, author = {Han Lin and Xiaofeng Wang and Jujia Zhang and Danfeng Xiang and Tianmeng Zhang and Xulin Zhao and Xinghan Zhang and Hanna Sai and Liming Rui and Jun Mo and Gaobo Xi and Fang Huang and Xue Li and Yongzhi Cai and Weili Lin and Jie Lin and Chengyuan Wu and Jicheng Zhang and Zhihao Chen and Zhitong Li and Wenxiong Li and Linyi Li and Kaicheng Zhang and Cheng Miao and Juncheng Chen and Zhou Fan and Jianning Fu and Shengbang Qian and Hong Wu and Xue-Bing Wu and Jingzhi Yan and Huawei Zhang and Junbo Zhang and Liyun Zhang and Jie Zheng and Qian Zhai}, title = {{A} spectral data release for 104 {T}ype {II} {S}upernovae from the {T}singhua {S}upernova {G}roup}, year = {2024}, eprint = {2401.05889}, note = {arXiv:2401.05889v1} }
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We present 206 unpublished optical spectra of 104 type II supernovae obtained by the Xinglong 2.16m telescope and Lijiang 2.4m telescope during the period from 2011 to 2018, spanning the phases from about 1 to 200 days after the SN explosion. The spectral line identifications, evolution of line velocities and pseudo equivalent widths, as well as correlations between some important spectral parameters are presented. Our sample displays a large range in expansion velocities. For instance, the Fe~\sc ii $5169$ velocities measured from spectra at $t\sim 50$ days after the explosion vary from ${\rm 2000\ km\ s^{-1}}$ to ${\rm 5500\ km\ s^{-1}}$, with an average value of ${\rm 3872 \pm 949\ km\ s^{-1}}$. Power-law functions can be used to fit the velocity evolution, with the power-law exponent quantifying the velocity decline rate. We found an anticorrelation existing between H$\beta$ velocity at mid-plateau phase and its velocity decay exponent, SNe II with higher velocities tending to have smaller velocity decay rate. Moreover, we noticed that the velocity decay rate inferred from the Balmer lines (i.e., H$\alpha$ and H$\beta$) have moderate correlations with the ratio of absorption to emission for H$\alpha$ (a/e). In our sample, two objects show possibly flash-ionized features at early phases. Besides, we noticed that multiple high-velocity components may exist on the blue side of hydrogen lines of SN 2013ab, possibly suggesting that these features arise from complex line forming region. All our spectra can be found in WISeREP and Zenodo.
Towards Systematic Evaluation of de Sitter Correlators via Generalized Integration-By-Parts Relations
Jiaqi Chen, Bo Feng
Jan 02 2024 hep-th astro-ph.CO gr-qc hep-ph arXiv:2401.00129v4

@misc{2401.00129, author = {Jiaqi Chen and Bo Feng}, title = {{T}owards {S}ystematic {E}valuation of de {S}itter {C}orrelators via {G}eneralized {I}ntegration-{B}y-{P}arts {R}elations}, year = {2024}, eprint = {2401.00129}, howpublished = {JHEP06(2024)199}, doi = {10.1007/JHEP06(2024)199}, note = {arXiv:2401.00129v4} }
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We generalize Integration-By-Parts (IBP) and differential equations methods to de Sitter correlators related to inflation. While massive correlators in de Sitter spacetime are usually regarded as highly intricate, we find they have remarkably hidden concise structures from the perspective of IBP. We find the factorization of the IBP relations of each vertex integral family corresponding to $\mathrm{d} \tau_i$ integration. Furthermore, with a smart construction of master integrals, the universal formulas for iterative reduction and $\mathrm{d} \log$-form differential equations of arbitrary vertex integral family are presented and proved. These formulas dominate all tree-level de Sitter correlators and play a kernel role at the loop-level as well.
Corona-heated Accretion-disk Reprocessing: Frequency-Resolved Lag Predictions for UV/Optical Reverberation Mapping of Active Galactic Nuclei
Jie Chen, Mouyuan Sun, Zhi-Xiang Zhang
Dec 18 2023 astro-ph.HE astro-ph.GA arXiv:2312.09590v1

@misc{2312.09590, author = {Jie Chen and Mouyuan Sun and Zhi-Xiang Zhang}, title = {{C}orona-heated {A}ccretion-disk {R}eprocessing: {F}requency-{R}esolved {L}ag {P}redictions for {UV}/{O}ptical {R}everberation {M}apping of {A}ctive {G}alactic {N}uclei}, year = {2023}, eprint = {2312.09590}, note = {arXiv:2312.09590v1} }
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Continuum reverberation mapping with high-cadence, long-term UV/optical monitoring of Active Galactic Nuclei (AGNs) enables us to resolve the AGN central engine sizes on different timescales. The frequency-resolved time lags of NGC 5548 (the target for the AGN STORM I campaign) are inconsistent with the X-ray reprocessing of the classical Shakura $\&$ Sunyaev disk model. Here we show that the frequency-resolved time lags in NGC 5548 can be well produced by the Corona-Heated Accretion-disk Reprocessing (CHAR) model. Moreover, we make the CHAR model predictions of the frequency-resolved time lags for Mrk 817, the source of the AGN STORM II campaign. We also obtain the frequency-resolved time lags as a function of the black-hole mass and Eddington ratio, which is valid for black-hole masses from $10^{6.5}$ to $10^9\ M_{\odot}$, and Eddington ratios from 0.01 to 1. Moreover, we demonstrate that, with the time spans of current continuum reverberation-mapping campaigns, the lag-luminosity relation of the CHAR model can be $\tau_{\mathrm{gz}}\propto L_{\mathrm{5100}}^{0.55\pm0.04}$, which is consistent with observations. Future observations can test our results and shed new light on resolving the AGN central engine.
Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 (NGC 5904) with FAST and Arecibo
Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gugercinoglu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, et al (12)
Dec 12 2023 astro-ph.HE arXiv:2312.05835v1

@misc{2312.05835, author = {Lei Zhang and Paulo C.~C.~Freire and Alessandro Ridolfi and Zhichen Pan and Jiaqi Zhao and Craig O.~Heinke and Jianxing Chen and Mario Cadelano and Cristina Pallanca and Xian Hou and Xiaoting Fu and Shi Dai and Erbil Gugercinoglu and Meng Guo and Jason Hessels and Jiale Hu and Guodong Li and Mengmeng Ni and Jingshan Pan and Scott M.~Ransom and Qitong Ruan and Ingrid Stairs and Chao-Wei Tsai and Pei Wang and Long Wang and Na Wang and Qingdong Wu and Jianping Yuan and Jie Zhang and Weiwei Zhu and Yongkun Zhang and Di Li}, title = {{D}iscovery and {T}iming of {M}illisecond {P}ulsars in the {G}lobular {C}luster {M}5 ({NGC} 5904) with {FAST} and {A}recibo}, year = {2023}, eprint = {2312.05835}, howpublished = {ApJS, 2013, 269:56}, doi = {10.3847/1538-4365/acfb03}, note = {arXiv:2312.05835v1} }
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We report on a comprehensive multi-wavelength study of the pulsars in the globular cluster (GC) M5, including the discovery of M5G, a new compact non-eclipsing "black widow" pulsar. Thanks to the analysis of 34 years of radio data taken with the FAST and Arecibo telescopes, we obtained new phase-connected timing solutions for four pulsars in the clusters and improved those of the other three known pulsars. These have resulted in, among other things: a) much improved proper motions for five pulsars, with transverse velocities that are smaller than their respective escape velocities; b) 3-sigma and 1.5-sigma detections of Shapiro delays in M5F and M5D, respectively; c) greatly improved measurement of the periastron advance in M5B, whose value of 0.01361(6) implies that M5B is still likely to be a heavy neutron star. The binary pulsars M5D, E and F are confirmed to be in low-eccentricity binary systems, the low-mass companions of which are newly identified to be He white dwarfs using Hubble Space Telescope data. Four pulsars are also found to be associated with X-ray sources. Similarly to the eclipsing pulsar M5C, M5G shows little or no non-thermal X-ray emission, indicative of weak synchrotron radiation produced by intra-binary shocks. All the seven pulsars known in M5 have short spin periods and five are in binary systems with low orbital eccentricities. These characteristics differ from the overall GC pulsar population, but confirm the expectations for the pulsar population in a cluster with a small rate of stellar encounters per binary system.
The Magnetic Field Calibration of the Full-Disk Magnetograph onboard the Advanced Space based Solar Observatory (ASO-S/FMG)
S. Liu, J.T. Su, X.Y. Bai, Y.Y. Deng, J. Chen, Y.L. Song, X.F. Wang, H.Q. Xu, X. Yang
Dec 04 2023 astro-ph.SR physics.space-ph arXiv:2312.00319v1

@misc{2312.00319, author = {S.~Liu and J.T.~Su and X.Y.~Bai and Y.Y.~Deng and J.~Chen and Y.L.~Song and X.F.~Wang and H.Q.~Xu and X.~Yang}, title = {{T}he {M}agnetic {F}ield {C}alibration of the {F}ull-{D}isk {M}agnetograph onboard the {A}dvanced {S}pace based {S}olar {O}bservatory ({ASO}-{S}/{FMG})}, year = {2023}, eprint = {2312.00319}, howpublished = {solphys 2023}, note = {arXiv:2312.00319v1} }
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The Full-disk magnetograph is a main scientific payload onboard the Advanced Space based Solar Observatory (ASO-S/FMG) that through Stokes parameter observation to measures the vector magnetic field. The accuracy of magnetic-field values is an important aspect of checking the quality of the FMG magnetic-field measurement. According to the design of the FMG, the linear calibration method under the weak-field approximation is the preferred scheme for magnetic-field calibration. However, the spacecraft orbital velocity can affect the position of observed spectral lines, then result in a change of the polarization-signal strength. Thus, the magnetic field is modulated by the orbit velocity of the spacecraft. In this article, through cross calibration between FMG and HMI (Helioseismic and Magnetic Imager onboard the Solar Dynamic Observatory), the effects of spacecraft orbital velocity on the coefficient of magnetic-field calibration are investigated. By comparing the magnetic field of FMG and HMI with spacecraft orbital velocity as an auxiliary reference, the revised linear-calibration coefficients that depend on spacecraft orbital velocity are obtained. Magnetic field of FMG corrected by the revised calibration coefficients removing the effect of spacecraft orbital velocity will be more accurate and suitable for scientific research.
Observations of a Failed Solar Filament Eruption Involving External Reconnection
Yuehong Chen, Xin Cheng, Jun Chen, Yu Dai, Mingde Ding
Nov 30 2023 astro-ph.SR arXiv:2311.17637v1

@misc{2311.17637, author = {Yuehong Chen and Xin Cheng and Jun Chen and Yu Dai and Mingde Ding}, title = {{O}bservations of a {F}ailed {S}olar {F}ilament {E}ruption {I}nvolving {E}xternal {R}econnection}, year = {2023}, eprint = {2311.17637}, note = {arXiv:2311.17637v1} }
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We report a failed solar filament eruption that involves external magnetic reconnection in a quadrupolar magnetic configuration. The evolution exhibits three kinematic evolution phases: a slow-rise phase, an acceleration phase, and a deceleration phase. In the early slow rise, extreme-ultraviolet (EUV) brightenings appear at the expected null point above the filament and are connected to the outer polarities by the hot loops, indicating the occurrence of a breakout reconnection. Subsequently, the filament is accelerated outward, accompanied by the formation of low-lying high-temperature post-flare loops ($>$ 15 MK), complying with the standard flare model. However, after 2--3 minutes, the erupting filament starts to decelerate and is finally confined in the corona. The important finding is that the confinement is closely related to an external reconnection as evidenced by the formation of high-lying large-scale hot loops ($>$ 10 MK) with their brightened footpoints at the outer polarities, the filament fragmentation and subsequent falling along the newly formed large-scale loops, as well as a hard X-ray source close to one of the outer footpoint brightenings. We propose that, even though the initial breakout reconnection and subsequent flare reconnection commence and accelerate the filament eruption, the following external reconnection between the erupting flux rope and overlying field, as driven by the upward filament eruption, makes the eruption finally failed, as validated by the numerical simulation of a failed flux rope eruption.
A Shock Flash Breaking Out of a Dusty Red Supergiant
Gaici Li, Maokai Hu, Wenxiong Li, Yi Yang, Xiaofeng Wang, Shengyu Yan, Lei Hu, Jujia Zhang, Yiming Mao, Henrik Riise, Xing Gao, Tianrui Sun, Jialian Liu, Dingrong Xiong, Lifan Wang, Jun Mo, Abdusamatjan Iskandar, Gaobo Xi, Danfeng Xiang, Lingzhi Wang, et al (24)
Nov 27 2023 astro-ph.HE astro-ph.SR arXiv:2311.14409v3

@misc{2311.14409, author = {Gaici Li and Maokai Hu and Wenxiong Li and Yi Yang and Xiaofeng Wang and Shengyu Yan and Lei Hu and Jujia Zhang and Yiming Mao and Henrik Riise and Xing Gao and Tianrui Sun and Jialian Liu and Dingrong Xiong and Lifan Wang and Jun Mo and Abdusamatjan Iskandar and Gaobo Xi and Danfeng Xiang and Lingzhi Wang and Guoyou Sun and Keming Zhang and Jian Chen and Weili Lin and Fangzhou Guo and Qichun Liu and Guangyao Cai and Wenjie Zhou and Jingyuan Zhao and Jin Chen and Xin Zheng and Keying Li and Mi Zhang and Shijun Xu and Xiaodong Lyu and A.J.Castro-Tirado and Vasilii Chufarin and Nikolay Potapov and Ivan Ionov and Stanislav Korotkiy and Sergey Nazarov and Kirill Sokolovsky and Norman Hamann and Eliot Herman}, title = {{A} {S}hock {F}lash {B}reaking {O}ut of a {D}usty {R}ed {S}upergiant}, year = {2023}, eprint = {2311.14409}, howpublished = {Nature volume 627, pages 754-758 (2024)}, doi = {10.1038/s41586-023-06843-6}, note = {arXiv:2311.14409v3} }
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Shock breakout emission is light that arises when a shockwave, generated by core-collapse explosion of a massive star, passes through its outer envelope. Hitherto, the earliest detection of such a signal was at several hours after the explosion, though a few others had been reported. The temporal evolution of early light curves should reveal insights into the shock propagation, including explosion asymmetry and environment in the vicinity, but this has been hampered by the lack of multiwavelength observations. Here we report the instant multiband observations of a type II supernova (SN 2023ixf) in the galaxy M101 (at a distance of 6.85+/-0.15 Mpc), beginning at about 1.4 hours after the explosion. The exploding star was a red supergiant with a radius of about 440 solar radii. The light curves evolved rapidly, on timescales of 1-2 hours, and appeared unusually fainter and redder than predicted by models within the first few hours, which we attribute to an optically thick dust shell before it was disrupted by the shockwave. We infer that the breakout and perhaps the distribution of the surrounding dust were not spherically symmetric.
Observations of Magnetic Helicity Proxies in Solar Photosphere: Helicity with Solar Cycles
Hongqi Zhang, Shangbin Yang, Haiqing Xu, Xiao Yang, Jie Chen, Jihong Liu
Nov 14 2023 astro-ph.SR arXiv:2311.07131v1

@misc{2311.07131, author = {Hongqi Zhang and Shangbin Yang and Haiqing Xu and Xiao Yang and Jie Chen and Jihong Liu}, title = {{O}bservations of {M}agnetic {H}elicity {P}roxies in {S}olar {P}hotosphere: {H}elicity with {S}olar {C}ycles}, year = {2023}, eprint = {2311.07131}, note = {arXiv:2311.07131v1} }
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Observations of magnetic helicity transportation through the solar photosphere reflect the interaction of turbulent plasma movements and magnetic fields in the solar dynamo process. In this chapter, we have reviewed the research process of magnetic helicity inferred from the observed solar magnetic fields in the photosphere and also the solar morphological configurations with solar cycles. After introducing some achievements in the study of magnetic helicity, some key points would like to be summarized. The magnetic (current) helicity in the solar surface layer presents a statistical distribution similar to that of the sunspot butterfly diagram, but its maximum value is delayed from the extreme value of the sunspot butterfly diagram and corresponds in the phase with the statistical eruption of solar flares. During the spatial transport of magnetic (current) helicity from the interior of the sun into the interplanetary space at the time-space scale of the solar cycle, it shows the statistical distribution and the fluctuation with the hemispheric sign rule. These show that the current helicity and magnetic helicity transport calculation methods are complementary to each other. We also notice that the study of the inherent relationship between magnetic helicity and the solar cycle still depends on the observed accuracy of the solar magnetic field.
Classifications of Fermi-LAT unassociated sources in multiple machine learning methods
K.R. Zhu, J.M. Chen, Y.G. Zheng, L.Zhang
Nov 08 2023 astro-ph.HE astro-ph.IM arXiv:2311.03678v1

@misc{2311.03678, author = {K.R.~Zhu and J.M.~Chen and Y.G.~Zheng and L.Zhang}, title = {{C}lassifications of {F}ermi-{LAT} unassociated sources in multiple machine learning methods}, year = {2023}, eprint = {2311.03678}, doi = {10.1093/mnras/stad2813}, note = {arXiv:2311.03678v1} }
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The classifications of Fermi-LAT unassociated sources are studied using multiple machine learning (ML) methods. The update data from 4FGL-DR3 are divided into high Galactic latitude (HGL, Galactic latitude $|b|>10^\circ$) and low Galactic latitude (LGL, $|b|\le10^\circ$) regions. In the HGL region, a voting ensemble of four binary ML classifiers achieves a 91$\%$ balanced accuracy. In the LGL region, an additional Bayesian-Gaussian (BG) model with three parameters is introduced to eliminate abnormal soft spectrum AGNs from the training set and ML-identified AGN candidates, a voting ensemble of four ternary ML algorithms reach an 81$\%$ balanced accuracy. And then, a catalog of Fermi-LAT all-sky unassociated sources is constructed. Our classification results show that (i) there are 1037 AGN candidates and 88 pulsar candidates with a balanced accuracy of $0.918 \pm 0.029$ in HGL region, which are consistent with those given in previous all-sky ML approaches; and (ii) there are 290 AGN-like candidates, 135 pulsar-like candidates, and 742 other-like candidates with a balanced accuracy of $0.815 \pm 0.027$ in the LGL region, which are different from those in previous all-sky ML approaches. Additionally, different training sets and class weights were tested for their impact on classifier accuracy and predicted results. The findings suggest that while different training approaches can yield similar model accuracy, the predicted numbers across different categories can vary significantly. Thus, reliable evaluation of the predicted results is deemed crucial in the ML approach for Fermi-LAT unassociated sources.
A Systematic Observational Study on Galactic Interstellar Ratio 18O/17O. II. C18O and C17O J=2-1 Data Analysis
Y. P. Zou, J. S. Zhang, C. Henkel, D. Romano, W. Liu, Y. H. Zheng, Y. T. Yan, J. L. Chen, Y. X. Wang, J. Y. Zhao
Nov 02 2023 astro-ph.GA arXiv:2311.00547v1

@misc{2311.00547, author = {Y.~P.~Zou and J.~S.~Zhang and C.~Henkel and D.~Romano and W.~Liu and Y.~H.~Zheng and Y.~T.~Yan and J.~L.~Chen and Y.~X.~Wang and J.~Y.~Zhao}, title = {{A} {S}ystematic {O}bservational {S}tudy on {G}alactic {I}nterstellar {R}atio 18{O}/17{O}. {II}. {C}18{O} and {C}17{O} {J}=2-1 {D}ata {A}nalysis}, year = {2023}, eprint = {2311.00547}, doi = {10.3847/1538-4365/acee6b}, note = {arXiv:2311.00547v1} }
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To investigate the relative amount of ejecta from high-mass versus intermediate-mass stars and to trace the chemical evolution of the Galaxy, we have performed with the IRAM 30m and the SMT 10m telescopes a systematic study of Galactic interstellar 18O/17O ratios toward a sample of 421 molecular clouds, covering a galactocentric distance range of 1-22 kpc. The results presented in this paper are based on the J=2-1 transition and encompass 364 sources showing both C18O and C17O detections. The previously suggested 18O/17O gradient is confirmed. For the 41 sources detected with both facilities, good agreement is obtained. A correlation of 18O/17O ratios with heliocentric distance is not found, indicating that beam dilution and linear beam sizes are not relevant. For the subsample of IRAM 30 m high-mass star-forming regions with accurate parallax distances, an unweighted fit gives 18O/17O = (0.12+-0.02)R_GC+(2.38+-0.13) with a correlation coefficient of R = 0.67. While the slope is consistent with our J=1-0 measurement, ratios are systematically lower. This should be caused by larger optical depths of C18O 2-1 lines, w.r.t the corresponding 1-0 transitions, which is supported by RADEX calculations and the fact that C18O/C17O is positively correlated with 13CO/C18O. After considering optical depth effects with C18O J=2-1 reaching typically an optical depth of 0.5, corrected 18O/17O ratios from the J=1-0 and J=2-1 lines become consistent. A good numerical fit to the data is provided by the MWG-12 model, including both rotating stars and novae.
The spin of a stellar black hole 4U 1543-47 determined by Insight-HXMT
Jiashi Chen, Wei Wang
Oct 11 2023 astro-ph.HE astro-ph.SR arXiv:2310.06634v1

@misc{2310.06634, author = {Jiashi Chen and Wei Wang}, title = {{T}he spin of a stellar black hole 4{U} 1543-47 determined by {I}nsight-{HXMT}}, year = {2023}, eprint = {2310.06634}, note = {arXiv:2310.06634v1} }
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We present a spectral analysis of \textitInsight-HXMT observations of the low-mass X-ray binary 4U 1543-47 which locates in our Milky Way galaxy during the 2021 outburst. We focus on the observations in its soft state, and attempt to determine the spin of the black hole candidate through Thermal-Continuum Fitting (CF) method. The spin derived from CF method is highly dependent on black hole mass, distance and inclination angle of inner disk. In this article, we have adopted the preferred range of parameters: $M=9.4\pm 1 M_{\odot}$, D=$7.5{\pm}0.5$ kpc and $i=36.3^{+5.3}_{-3.4}$ degrees. We attain a moderate spin, $a=0.46\pm0.12$, which is consistent with previous results measured in the 2002 outburst. Besides, we notice the spectra show a wide blue shifted absorption feature between 8-10 keV which would originate from the highly ionized iron line. We try to fit the feature with \em xstar model and suggest that this feature may come from relativistic disk wind with a velocity of $v_{\rm wind}\sim 0.2c$. We attribute this relativistic disk wind to the super-Eddington accretion during the black hole outburst.
Calibrating the effective magnitudes of type Ia supernovae with a model-independent method
Jian Hu, Jian-Ping Hu, Zhongmu Li, Wenchang Zhao, Jing Chen
Oct 02 2023 astro-ph.CO arXiv:2309.17163v1

@misc{2309.17163, author = {Jian Hu and Jian-Ping Hu and Zhongmu Li and Wenchang Zhao and Jing Chen}, title = {{C}alibrating the effective magnitudes of type {I}a supernovae with a model-independent method}, year = {2023}, eprint = {2309.17163}, note = {arXiv:2309.17163v1} }
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This research explores the correlation between the absolute magnitude and the redshift of Type Ia supernovae (SNe Ia) with a model-independent approach. The Pantheon sample of SNe Ia and strong gravitational lensing systems (SGLS) are used. With the cosmic distance-duality relation (CDDR), the evolution parameter of the magnitude, the light curve parameters of SNe Ia, and the parameters of the SGLS geometric model are constrained simultaneously. Considering the consistency of the redshifts, we selected a subsample of SNe Ia in which the redshift of each SNe Ia is close to the corresponding redshift of the SGLS sample. Two parametric models are used to describe this evolution, which can be written as $\delta_M=\varepsilon z$ and $\delta_M=\varepsilon\log(1+z)$, respectively. Our analysis reveals that $\varepsilon=-0.036^{+0.357}_{-0.339}$ in the first parametric model and $\varepsilon=-0.014^{+0.588}_{-0.630}$ in the second model, indicating that no significant evolution ($\varepsilon=0$) is supported at the 1$\sigma$ confidence level in this study. These results represent a significant advancement in our understanding of the intrinsic properties of SNe Ia and provide important constraints for future SNe Ia study.
Reconciling results of 2019 and 2020 stellar occultations on Pluto's atmosphere. New constraints from both the 5 September 2019 event and consistency analysis
Ye Yuan, Fan Li, Yanning Fu, Jian Chen, Wei Tan, Shuai Zhang, Wei Zhang, Chen Zhang, Qiang Zhang, Jiahui Ye, Delai Li, Yijing Zhu, Zhensen Fu, Ansheng Zhu, Yue Chen, Jun Xu, Yang Zhang
Sep 27 2023 astro-ph.EP arXiv:2309.14724v2

@misc{2309.14724, author = {Ye Yuan and Fan Li and Yanning Fu and Jian Chen and Wei Tan and Shuai Zhang and Wei Zhang and Chen Zhang and Qiang Zhang and Jiahui Ye and Delai Li and Yijing Zhu and Zhensen Fu and Ansheng Zhu and Yue Chen and Jun Xu and Yang Zhang}, title = {{R}econciling results of 2019 and 2020 stellar occultations on {P}luto's atmosphere. {N}ew constraints from both the 5 {S}eptember 2019 event and consistency analysis}, year = {2023}, eprint = {2309.14724}, note = {arXiv:2309.14724v2} }
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A stellar occultation by Pluto on 5 September 2019 yielded positive detections at two separate stations. Using an approach consistent with comparable studies, we derived a surface pressure of $11.478 \pm 0.55~\mathrm{\mu bar}$ for Pluto's atmosphere from the observations of this event. In addition, to avoid potential method inconsistancies highlighted by Sicardy et al. when comparing with historical pressure measurements, we reanalyzed the data by 15 August 2018 and 17 July 2019 events, respectively. All the new measurements provide a bridge between the two different perspectives on the pressure variation since 2015: a rapid pressure drop from previous studies of the 15 August 2018 and 17 July 2019 events and a plateau phase from that of the 6 June 2020 event. The pressure measurement from the 5 September 2019 event aligns with those from 2016, 2018, and 2020, supporting the latter perspective. While the measurements from the 4 June 2011 and 17 July 2019 events suggest probable V-shaped pressure variations unaccounted for by the volatile transport model (VTM) from Meza et al., the VTM remains applicable on average. And, the validity of the V-shaped variations is debatable due to the stellar faintness of the 4 June 2011 event and the grazing single-chord geometry of the 17 July 2019 event. To reveal and understand all significant pressure variations of Pluto's atmosphere, it is essential to provide constraints on both short-term and long-term evolutions of the interacting atmosphere and surface by continuous pressure monitoring through occultation observations, whenever possible, complemented by frequent spectroscopy and photometry of the surface.
Polarized thermal emission from dust in a galaxy at redshift 2.6
J. E. Geach, E. Lopez-Rodriguez, M. J. Doherty, Jianhang Chen, R. J. Ivison, G. J. Bendo, S. Dye, K. E. K. Coppin
Sep 06 2023 astro-ph.GA astro-ph.CO arXiv:2309.02034v1

@misc{2309.02034, author = {J.~E.~Geach and E.~Lopez-Rodriguez and M.~J.~Doherty and Jianhang Chen and R.~J.~Ivison and G.~J.~Bendo and S.~Dye and K.~E.~K.~Coppin}, title = {{P}olarized thermal emission from dust in a galaxy at redshift 2.6}, year = {2023}, eprint = {2309.02034}, doi = {10.1038/s41586-023-06346-4}, note = {arXiv:2309.02034v1} }
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Magnetic fields are fundamental to the evolution of galaxies, playing a key role in the astrophysics of the interstellar medium and star formation. Large-scale ordered magnetic fields have been mapped in the Milky Way and nearby galaxies, but it is not known how early in the Universe such structures form. Here we report the detection of linearly polarized thermal emission from dust grains in a strongly lensed, intrinsically luminous galaxy that is forming stars at a rate more than a thousand times that of the Milky Way at redshift 2.6, within 2.5 Gyr of the Big Bang. The polarized emission arises from the alignment of dust grains with the local magnetic field. The median polarization fraction is of order one per cent, similar to nearby spiral galaxies. Our observations support the presence of a 5 kiloparsec-scale ordered magnetic field with a strength of around 500uG or lower, orientated parallel to the molecular gas disk. This confirms that such structures can be rapidly formed in galaxies, early in cosmic history.
A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-Wave Candidates from the Third Gravitational-wave Observing Run
C. Fletcher, J. Wood, R. Hamburg, P. Veres, C. M. Hui, E. Bissaldi, M. S. Briggs, E. Burns, W. H. Cleveland, M. M. Giles, A. Goldstein, B. A. Hristov, D. Kocevski, S. Lesage, B. Mailyan, C. Malacaria, S. Poolakkil, A. von Kienlin, C. A. Wilson-Hodge, Fermi Gamma-ray Burst Monitor Team, et al (1679)
Aug 29 2023 astro-ph.HE arXiv:2308.13666v1

@misc{2308.13666, author = {C.~Fletcher and J.~Wood and R.~Hamburg and P.~Veres and C.~M.~Hui and E.~Bissaldi and M.~S.~Briggs and E.~Burns and W.~H.~Cleveland and M.~M.~Giles and A.~Goldstein and B.~A.~Hristov and D.~Kocevski and S.~Lesage and B.~Mailyan and C.~Malacaria and S.~Poolakkil and A.~von Kienlin and C.~A.~Wilson-Hodge and Fermi Gamma-ray Burst Monitor Team and M.~Crnogorčević and J.~DeLaunay and A.~Tohuvavohu and R.~Caputo and S.~B.~Cenko and S.~Laha and T.~Parsotan and R.~Abbott and H.~Abe and F.~Acernese and K.~Ackley and N.~Adhikari and R.~X.~Adhikari and V.~K.~Adkins and V.~B.~Adya and C.~Affeldt and D.~Agarwal and M.~Agathos and K.~Agatsuma and N.~Aggarwal and O.~D.~Aguiar and L.~Aiello and A.~Ain and P.~Ajith and T.~Akutsu and S.~Albanesi and R.~A.~Alfaidi and A.~Allocca and P.~A.~Altin and A.~Amato and C.~Anand and S.~Anand and A.~Ananyeva and S.~B.~Anderson and W.~G.~Anderson and M.~Ando and T.~Andrade and N.~Andres and M.~Andrés-Carcasona and T.~Andríc and S.~V.~Angelova and S.~Ansoldi and J.~M.~Antelis and S.~Antier and T.~Apostolatos and E.~Z.~Appavuravther and S.~Appert and S.~K.~Apple and K.~Arai and A.~Araya and M.~C.~Araya and J.~S.~Areeda and M.~Arène and N.~Aritomi and N.~Arnaud and M.~Arogeti and S.~M.~Aronson and K.~G.~Arun and H.~Asada and Y.~Asali and G.~Ashton and Y.~Aso and M.~Assiduo and S.~Assis de Souza Melo and S.~M.~Aston and P.~Astone and F.~Aubin and K.~AultONeal and C.~Austin and S.~Babak and F.~Badaracco and M.~K.~M.~Bader and C.~Badger and S.~Bae and Y.~Bae and A.~M.~Baer and S.~Bagnasco and Y.~Bai and J.~Baird and R.~Bajpai and T.~Baka and M.~Ball and G.~Ballardin and S.~W.~Ballmer and A.~Balsamo and G.~Baltus and S.~Banagiri and B.~Banerjee and D.~Bankar and J.~C.~Barayoga and C.~Barbieri and B.~C.~Barish and D.~Barker and P.~Barneo and F.~Barone and B.~Barr and L.~Barsotti and M.~Barsuglia and D.~Barta and J.~Bartlett and M.~A.~Barton and I.~Bartos and S.~Basak and R.~Bassiri and A.~Basti and M.~Bawaj and J.~C.~Bayley and M.~Bazzan and B.~R.~Becher and B.~Becsy and V.~M.~Bedakihale and F.~Beirnaert and M.~Bejger and I.~Belahcene and V.~Benedetto and D.~Beniwal and M.~G.~Benjamin and T.~F.~Bennett and J.~D.~Bentley and M.~BenYaala and S.~Bera and M.~Berbel and F.~Bergamin and B.~K.~Berger and S.~Bernuzzi and C.~P.~L.~Berry and D.~Bersanetti and A.~Bertolini and J.~Betzwieser and D.~Beveridge and R.~Bhandare and A.~V.~Bhandari and U.~Bhardwaj and R.~Bhatt and D.~Bhattacharjee and S.~Bhaumik and A.~Bianchi and I.~A.~Bilenko and G.~Billingsley and S.~Bini and R.~Birney and O.~Birnholtz and S.~Biscans and M.~Bischi and S.~Biscoveanu and A.~Bisht and B.~Biswas and M.~Bitossi and M.~A.~Bizouard and J.~K.~Blackburn and C.~D.~Blair and D.~G.~Blair and R.~M.~Blair and F.~Bobba and N.~Bode and M.~Boër and G.~Bogaert and M.~Boldrini and G.~N.~Bolingbroke and L.~D.~Bonavena and F.~Bondu and E.~Bonilla and R.~Bonnand and P.~Booker and B.~A.~Boom and R.~Bork and V.~Boschi and N.~Bose and S.~Bose and V.~Bossilkov and V.~Boudart and Y.~Bouffanais and A.~Bozzi and C.~Bradaschia and P.~R.~Brady and A.~Bramley and A.~Branch and M.~Branchesi and J.~E.~Brau and M.~Breschi and T.~Briant and J.~H.~Briggs and A.~Brillet and M.~Brinkmann and P.~Brockill and A.~F.~Brooks and J.~Brooks and D.~D.~Brown and S.~Brunett and G.~Bruno and R.~Bruntz and J.~Bryant and F.~Bucci and T.~Bulik and H.~J.~Bulten and A.~Buonanno and K.~Burtnyk and R.~Buscicchio and D.~Buskulic and C.~Buy and R.~L.~Byer and G.~S.~Cabourn Davies and G.~Cabras and R.~Cabrita and L.~Cadonati and M.~Caesar and G.~Cagnoli and C.~Cahillane and J.~Calderòn Bustillo and J.~D.~Callaghan and T.~A.~Callister and E.~Calloni and J.~Cameron and J.~B.~Camp and M.~Canepa and S.~Canevarolo and M.~Cannavacciuolo and K.~C.~Cannon and H.~Cao and Z.~Cao and E.~Capocasa and E.~Capote and G.~Carapella and F.~Carbognani and M.~Carlassara and J.~B.~Carlin and M.~F.~Carney and M.~Carpinelli and G.~Carrillo and G.~Carullo and T.~L.~Carver and J.~Casanueva Díaz and C.~Casentini and G.~Castaldi and S.~Caudill and M.~Cavaglià and F.~Cavalier and R.~Cavalieri and G.~Cella and P.~Cerdá-Durán and E.~Cesarini and W.~Chaibi and S.~Chalathadka Subrahmanya and E.~Champion and C.~H.~Chan and C.~Chan and C.~L.~Chan and K.~Chan and M.~Chan and K.~Chandra and I.~P.~Chang and P.~Chanial and S.~Chao and C.~Chapman-Bird and P.~Charlton and E.~A.~Chase and E.~Chassande-Mottin and C.~Chatterjee and Debarati Chatterjee and Deep Chatterjee and M.~Chaturvedi and S.~Chaty and C.~Chen and D.~Chen and H.~Y.~Chen and J.~Chen and K.~Chen and X.~Chen and Y.~B.~Chen and Y.~R.~Chen and Z.~Chen and H.~Cheng and C.~K.~Cheong and H.~Y.~Cheung and H.~Y.~Chia and F.~Chiadini and C.~Y.~Chiang and G.~Chiarini and R.~Chierici and A.~Chincarini and M.~L.~Chiofalo and A.~Chiummo and R.~K.~Choudhary and S.~Choudhary and N.~Christensen and Q.~Chu and Y.~K.~Chu and S.~S.~Y.~Chua and K.~W.~Chung and G.~Ciani and P.~Ciecielag and M.~Cieślar and M.~Cifaldi and A.~A.~Ciobanu and R.~Ciolfi and F.~Cipriano and F.~Clara and J.~A.~Clark and P.~Clearwater and S.~Clesse and F.~Cleva and E.~Coccia and E.~Codazzo and P.~F.~Cohadon and D.~E.~Cohen and M.~Colleoni and C.~G.~Collette and A.~Colombo and M.~Colpi and C.~M.~Compton and M.~Constancio Jr.~and L.~Conti and S.~J.~Cooper and P.~Corban and T.~R.~Corbitt and I.~Cordero-Carrión and S.~Corezzi and K.~R.~Corley and N.~J.~Cornish and D.~Corre and A.~Corsi and S.~Cortese and C.~A.~Costa and R.~Cotesta and R.~Cottingham and M.~W.~Coughlin and J.~P.~Coulon and S.~T.~Countryman and B.~Cousins and P.~Couvares and D.~M.~Coward and M.~J.~Cowart and D.~C.~Coyne and R.~Coyne and J.~D.~E.~Creighton and T.~D.~Creighton and A.~W.~Criswell and M.~Croquette and S.~G.~Crowder and J.~R.~Cudell and T.~J.~Cullen and A.~Cumming and R.~Cummings and L.~Cunningham and E.~Cuoco and M.~Cury lo and P.~Dabadie and T.~Dal Canton and S.~Dall'Osso and G.~Dálya and A.~Dana and B.~D'Angelo and S.~Danilishin and S.~D'Antonio and K.~Danzmann and C.~Darsow-Fromm and A.~Dasgupta and L.~E.~H.~Datrier and Sayak Datta and Sayantani Datta and V.~Dattilo and I.~Dave and M.~Davier and D.~Davis and M.~C.~Davis and E.~J.~Daw and R.~Dean and D.~DeBra and M.~Deenadayalan and J.~Degallaix and M.~De Laurentis and S.~Deléglise and V.~Del Favero and F.~De Lillo and N.~De Lillo and D.~Dell'Aquila and W.~Del Pozzo and L.~M.~DeMarchi and F.~De Matteis and V.~D'Emilio and N.~Demos and T.~Dent and A.~Depasse and R.~De Pietri and R.~De Rosa and C.~De Rossi and R.~DeSalvo and R.~De Simone and S.~Dhurandhar and M.~C.~D'iaz and N.~A.~Didio and T.~Dietrich and L.~Di Fiore and C.~Di Fronzo and C.~Di Giorgio and F.~Di Giovanni and M.~Di Giovanni and T.~Di Girolamo and A.~Di Lieto and A.~Di Michele and B.~Ding and S.~Di Pace and I.~Di Palma and F.~Di Renzo and A.~K.~Divakarla and A.~Dmitriev and Z.~Doctor and L.~Donahue and L.~D'Onofrio and F.~Donovan and K.~L.~Dooley and S.~Doravari and M.~Drago and J.~C.~Driggers and Y.~Drori and J.~G.~Ducoin and P.~Dupej and U.~Dupletsa and O.~Durante and D.~D'Urso and P.~A.~Duverne and S.~E.~Dwyer and C.~Eassa and P.~J.~Easter and M.~Ebersold and T.~Eckhardt and G.~Eddolls and B.~Edelman and T.~B.~Edo and O.~Edy and A.~Effler and S.~Eguchi and J.~Eichholz and S.~S.~Eikenberry and M.~Eisenmann and R.~A.~Eisenstein and A.~Ejlli and E.~Engelby and Y.~Enomoto and L.~Errico and R.~C.~Essick and H.~Estellés and D.~Estevez and Z.~Etienne and T.~Etzel and M.~Evans and T.~M.~Evans and T.~Evstafyeva and B.~E.~Ewing and F.~Fabrizi and F.~Faedi and V.~Fafone and H.~Fair and S.~Fairhurst and P.~C.~Fan and A.~M.~Farah and S.~Farinon and B.~Farr and W.~M.~Farr and E.~J.~Fauchon-Jones and G.~Favaro and M.~Favata and M.~Fays and M.~Fazio and J.~Feicht and M.~M.~Fejer and E.~Fenyvesi and D.~L.~Ferguson and A.~Fernandez-Galiana and I.~Ferrante and T.~A.~Ferreira and F.~Fidecaro and P.~Figura and A.~Fiori and I.~Fiori and M.~Fishbach and R.~P.~Fisher and R.~Fittipaldi and V.~Fiumara and R.~Flaminio and E.~Floden and H.~K.~Fong and J.~A.~Font and B.~Fornal and P.~W.~F.~Forsyth and A.~Franke and S.~Frasca and F.~Frasconi and J.~P.~Freed and Z.~Frei and A.~Freise and O.~Freitas and R.~Frey and P.~Fritschel and V.~V.~Frolov and G.~G.~Fronzé and Y.~Fujii and Y.~Fujikawa and Y.~Fujimoto and P.~Fulda and M.~Fyffe and H.~A.~Gabbard and W.~E.~Gabella and B.~U.~Gadre and J.~R.~Gair and J.~Gais and S.~Galaudage and R.~Gamba and D.~Ganapathy and A.~Ganguly and D.~Gao and S.~G.~Gaonkar and B.~Garaventa and C.~García Núñez and C.~García-Quirós and F.~Garufi and B.~Gateley and V.~Gayathri and G.~G.~Ge and G.~Gemme and A.~Gennai and J.~George and O.~Gerberding and L.~Gergely and P.~Gewecke and S.~Ghonge and Abhirup Ghosh and Archisman Ghosh and Shaon Ghosh and Shrobana Ghosh and Tathagata Ghosh and B.~Giacomazzo and L.~Giacoppo and J.~A.~Giaime and K.~D.~Giardina and D.~R.~Gibson and C.~Gier and M.~Giesler and P.~Giri and F.~Gissi and S.~Gkaitatzis and J.~Glanzer and A.~E.~Gleckl and P.~Godwin and E.~Goetz and R.~Goetz and N.~Gohlke and J.~Golomb and B.~Goncharov and G.~Gonzalez and M.~Gosselin and R.~Gouaty and D.~W.~Gould and S.~Goyal and B.~Grace and A.~Grado and V.~Graham and M.~Granata and V.~Granata and A.~Grant and S.~Gras and P.~Grassia and C.~Gray and R.~Gray and G.~Greco and A.~C.~Green and R.~Green and A.~M.~Gretarsson and E.~M.~Gretarsson and D.~Griffith and W.~L.~Griffiths and H.~L.~Griggs and G.~Grignani and A.~Grimaldi and E.~Grimes and S.~J.~Grimm and H.~Grote and S.~Grunewald and P.~Gruning and A.~S.~Gruson and D.~Guerra and G.~M.~Guidi and A.~R.~Guimaraes and G.~Guixe and H.~K.~Gulati and A.~M.~Gunny and H.~K.~Guo and Y.~Guo and Anchal Gupta and Anuradha Gupta and I.~M.~Gupta and P.~Gupta and S.~K.~Gupta and R.~Gustafson and F.~Guzman and S.~Ha and I.~P.~W.~Hadiputrawan and L.~Haegel and S.~Haino and O.~Halim and E.~D.~Hall and E.~Z.~Hamilton and G.~Hammond and W.~B.~Han and M.~Haney and J.~Hanks and C.~Hanna and M.~D.~Hannam and O.~Hannuksela and H.~Hansen and T.~J.~Hansen and J.~Hanson and T.~Harder and K.~Haris and J.~Harms and G.~M.~Harry and I.~W.~Harry and D.~Hartwig and K.~Hasegawa and B.~Haskell and C.~J.~Haster and J.~S.~Hathaway and K.~Hattori and K.~Haughian and H.~Hayakawa and K.~Hayama and F.~J.~Hayes and J.~Healy and A.~Heidmann and A.~Heidt and M.~C.~Heintze and J.~Heinze and J.~Heinzel and H.~Heitmann and F.~Hellman and P.~Hello and A.~F.~Helmling-Cornell and G.~Hemming and M.~Hendry and I.~S.~Heng and E.~Hennes and J.~Hennig and M.~H.~Hennig and C.~Henshaw and A.~G.~Hernandez and F.~Hernandez Vivanco and M.~Heurs and A.~L.~Hewitt and S.~Higginbotham and S.~Hild and P.~Hill and Y.~Himemoto and A.~S.~Hines and N.~Hirata and C.~Hirose and T.~C.~Ho and S.~Hochheim and D.~Hofman and J.~N.~Hohmann and D.~G.~Holcomb and N.~A.~Holland and I.~J.~Hollows and Z.~J.~Holmes and K.~Holt and D.~E.~Holz and Q.~Hong and J.~Hough and S.~Hourihane and E.~J.~Howell and C.~G.~Hoy and D.~Hoyland and A.~Hreibi and B.~H.~Hsieh and H.~F.~Hsieh and C.~Hsiung and Y.~Hsu and H.~Y.~Huang and P.~Huang and Y.~C.~Huang and Y.~J.~Huang and Yiting Huang and Yiwen Huang and M.~T.~Hübner and A.~D.~Huddart and B.~Hughey and D.~C.~Y.~Hui and V.~Hui and S.~Husa and S.~H.~Huttner and R.~Huxford and T.~Huynh-Dinh and S.~Ide and B.~Idzkowski and A.~Iess and K.~Inayoshi and Y.~Inoue and P.~Iosif and M.~Isi and K.~Isleif and K.~Ito and Y.~Itoh and B.~R.~Iyer and V.~JaberianHamedan and T.~Jacqmin and P.~E.~Jacquet and S.~J.~Jadhav and S.~P.~Jadhav and T.~Jain and A.~L.~James and A.~Z.~Jan and K.~Jani and J.~Janquart and K.~Janssens and N.~N.~Janthalur and P.~Jaranowski and D.~Jariwala and R.~Jaume and A.~C.~Jenkins and K.~Jenner and C.~Jeon and W.~Jia and J.~Jiang and H.~B.~Jin and G.~R.~Johns and R.~Johnston and A.~W.~Jones and D.~I.~Jones and P.~Jones and R.~Jones and P.~Joshi and L.~Ju and A.~Jue and P.~Jung and K.~Jung and J.~Junker and V.~Juste and K.~Kaihotsu and T.~Kajita and M.~Kakizaki and C.~V.~Kalaghatgi and V.~Kalogera and B.~Kamai and M.~Kamiizumi and N.~Kanda and S.~Kandhasamy and G.~Kang and J.~B.~Kanner and Y.~Kao and S.~J.~Kapadia and D.~P.~Kapasi and C.~Karathanasis and S.~Karki and R.~Kashyap and M.~Kasprzack and W.~Kastaun and T.~Kato and S.~Katsanevas and E.~Katsavounidis and W.~Katzman and T.~Kaur and K.~Kawabe and K.~Kawaguchi and F.~Kéfélian and D.~Keitel and J.~S.~Key and S.~Khadka and F.~Y.~Khalili and S.~Khan and T.~Khanam and E.~A.~Khazanov and N.~Khetan and M.~Khursheed and N.~Kijbunchoo and A.~Kim and C.~Kim and J.~C.~Kim and J.~Kim and K.~Kim and W.~S.~Kim and Y.~M.~Kim and C.~Kimball and N.~Kimura and M.~Kinley-Hanlon and R.~Kirchhoff and J.~S.~Kissel and S.~Klimenko and T.~Klinger and A.~M.~Knee and T.~D.~Knowles and N.~Knust and E.~Knyazev and Y.~Kobayashi and P.~Koch and G.~Koekoek and K.~Kohri and K.~Kokeyama and S.~Koley and P.~Kolitsidou and M.~Kolstein and K.~Komori and V.~Kondrashov and A.~K.~H.~Kong and A.~Kontos and N.~Koper and M.~Korobko and M.~Kovalam and N.~Koyama and D.~B.~Kozak and C.~Kozakai and V.~Kringel and N.~V.~Krishnendu and A.~Królak and G.~Kuehn and F.~Kuei and P.~Kuijer and S.~Kulkarni and A.~Kumar and Prayush Kumar and Rahul Kumar and Rakesh Kumar and J.~Kume and K.~Kuns and Y.~Kuromiya and S.~Kuroyanagi and K.~Kwak and G.~Lacaille and P.~Lagabbe and D.~Laghi and E.~Lalande and M.~Lalleman and T.~L.~Lam and A.~Lamberts and M.~Landry and B.~B.~Lane and R.~N.~Lang and J.~Lange and B.~Lantz and I.~La Rosa and A.~Lartaux-Vollard and P.~D.~Lasky and M.~Laxen and A.~Lazzarini and C.~Lazzaro and P.~Leaci and S.~Leavey and S.~LeBohec and Y.~K.~Lecoeuche and E.~Lee and H.~M.~Lee and H.~W.~Lee and K.~Lee and R.~Lee and I.~N.~Legred and J.~Lehmann and A.~Lemaitre and M.~Lenti and M.~Leonardi and E.~Leonova and N.~Leroy and N.~Letendre and C.~Levesque and Y.~Levin and J.~N.~Leviton and K.~Leyde and A.~K.~Y.~Li and B.~Li and J.~Li and K.~L.~Li and P.~Li and T.~G.~F.~Li and X.~Li and C.~Y.~Lin and E.~T.~Lin and F.~K.~Lin and F.~L.~Lin and H.~L.~Lin and L.~C.~C.~Lin and F.~Linde and S.~D.~Linker and J.~N.~Linley and T.~B.~Littenberg and G.~C.~Liu and J.~Liu and K.~Liu and X.~Liu and F.~Llamas and R.~K.~L.~Lo and T.~Lo and L.~T.~London and A.~Longo and D.~Lopez and M.~Lopez Portilla and M.~Lorenzini and V.~Loriette and M.~Lormand and G.~Losurdo and T.~P.~Lott and J.~D.~Lough and C.~O.~Lousto and G.~Lovelace and J.~F.~Lucaccioni and H.~Lück and D.~Lumaca and A.~P.~Lundgren and L.~W.~Luo and J.~E.~Lynam and M.~Maarif and R.~Macas and J.~B.~Machtinger and M.~MacInnis and D.~M.~Macleod and I.~A.~O.~MacMillan and A.~Macquet and I.~Magaña Hernandez and C.~Magazzù and R.~M.~Magee and R.~Maggiore and M.~Magnozzi and S.~Mahesh and E.~Majorana and I.~Maksimovic and S.~Maliakal and A.~Malik and N.~Man and V.~Mandic and V.~Mangano and G.~L.~Mansell and M.~Manske and M.~Mantovani and M.~Mapelli and F.~Marchesoni and D.~Marín Pina and F.~Marion and Z.~Mark and S.~Márka and Z.~Márka and C.~Markakis and A.~S.~Markosyan and A.~Markowitz and E.~Maros and A.~Marquina and S.~Marsat and F.~Martelli and I.~W.~Martin and R.~M.~Martin and M.~Martinez and V.~A.~Martinez and V.~Martinez and K.~Martinovic and D.~V.~Martynov and E.~J.~Marx and H.~Masalehdan and K.~Mason and E.~Massera and A.~Masserot and M.~Masso-Reid and S.~Mastrogiovanni and A.~Matas and M.~Mateu-Lucena and F.~Matichard and M.~Matiushechkina and N.~Mavalvala and J.~J.~McCann and R.~McCarthy and D.~E.~McClelland and P.~K.~McClincy and S.~McCormick and L.~McCuller and G.~I.~McGhee and S.~C.~McGuire and C.~McIsaac and J.~McIver and T.~McRae and S.~T.~McWilliams and D.~Meacher and M.~Mehmet and A.~K.~Mehta and Q.~Meijer and A.~Melatos and D.~A.~Melchor and G.~Mendell and A.~Menendez-Vazquez and C.~S.~Menoni and R.~A.~Mercer and L.~Mereni and K.~Merfeld and E.~L.~Merilh and J.~D.~Merritt and M.~Merzougui and S.~Meshkov and C.~Messenger and C.~Messick and P.~M.~Meyers and F.~Meylahn and A.~Mhaske and A.~Miani and H.~Miao and I.~Michaloliakos and C.~Michel and Y.~Michimura and H.~Middleton and D.~P.~Mihaylov and L.~Milano and A.~L.~Miller and A.~Miller and B.~Miller and M.~Millhouse and J.~C.~Mills and E.~Milotti and Y.~Minenkov and N.~Mio and Ll.~M.~Mir and M.~Miravet-Tenés and A.~Mishkin and C.~Mishra and T.~Mishra and T.~Mistry and S.~Mitra and V.~P.~Mitrofanov and G.~Mitselmakher and R.~Mittleman and O.~Miyakawa and K.~Miyo and S.~Miyoki and Geoffrey Mo and L.~M.~Modafferi and E.~Moguel and K.~Mogushi and S.~R.~P.~Mohapatra and S.~R.~Mohite and I.~Molina and M.~Molina-Ruiz and M.~Mondin and M.~Montani and C.~J.~Moore and J.~Moragues and D.~Moraru and F.~Morawski and A.~More and C.~Moreno and G.~Moreno and Y.~Mori and S.~Morisaki and N.~Morisue and Y.~Moriwaki and B.~Mours and C.~M.~Mow-Lowry and S.~Mozzon and F.~Muciaccia and 130 and Arunava Mukherjee and D.~Mukherjee and Soma Mukherjee and Subroto Mukherjee and Suvodip Mukherjee and N.~Mukund and A.~Mullavey and J.~Munch and E.~A.~Muniz and P.~G.~Murray and R.~Musenich and S.~Muusse and S.~L.~Nadji and K.~Nagano and A.~Nagar and K.~Nakamura and H.~Nakano and M.~Nakano and Y.~Nakayama and V.~Napolano and I.~Nardecchia and H.~Narola and L.~Naticchioni and B.~Nayak and R.~K.~Nayak and B.~F.~Neil and J.~Neilson and A.~Nelson and T.~J.~N.~Nelson and M.~Nery and P.~Neubauer and A.~Neunzert and K.~Y.~Ng and S.~W.~S.~Ng and C.~Nguyen and P.~Nguyen and T.~Nguyen and L.~Nguyen Quynh and J.~Ni and W.~T.~Ni and S.~A.~Nichols and T.~Nishimoto and A.~Nishizawa and S.~Nissanke and E.~Nitoglia and F.~Nocera and M.~Norman and C.~North and S.~Nozaki and G.~Nurbek and L.~K.~Nuttall and Y.~Obayashi and J.~Oberling and B.~D.~O'Brien and J.~O'Dell and E.~Oelker and W.~Ogaki and G.~Oganesyan and J.~J.~Oh and K.~Oh and S.~H.~Oh and M.~Ohashi and T.~Ohashi and M.~Ohkawa and F.~Ohme and H.~Ohta and M.~A.~Okada and Y.~Okutani and C.~Olivetto and K.~Oohara and R.~Oram and B.~O'Reilly and R.~G.~Ormiston and N.~D.~Ormsby and R.~O'Shaughnessy and E.~O'Shea and S.~Oshino and S.~Ossokine and C.~Osthelder and S.~Otabe and D.~J.~Ottaway and H.~Overmier and A.~E.~Pace and G.~Pagano and R.~Pagano and M.~A.~Page and G.~Pagliaroli and A.~Pai and S.~A.~Pai and S.~Pal and J.~R.~Palamos and O.~Palashov and C.~Palomba and H.~Pan and K.~C.~Pan and P.~K.~Panda and P.~T.~H.~Pang and C.~Pankow and F.~Pannarale and B.~C.~Pant and F.~H.~Panther and F.~Paoletti and A.~Paoli and A.~Paolone and G.~Pappas and A.~Parisi and H.~Park and J.~Park and W.~Parker and D.~Pascucci and A.~Pasqualetti and R.~Passaquieti and D.~Passuello and M.~Patel and M.~Pathak and B.~Patricelli and A.~S.~Patron and S.~Paul and E.~Payne and M.~Pedraza and R.~Pedurand and M.~Pegoraro and A.~Pele and F.~E.~Pena Arellano and S.~Penano and S.~Penn and A.~Perego and A.~Pereira and T.~Pereira and C.~J.~Perez and C.~Pèrigois and C.~C.~Perkins and A.~Perreca and S.~Perriés and D.~Pesios and J.~Petermann and D.~Petterson and H.~P.~Pfeiffer and H.~Pham and K.~A.~Pham and K.~S.~Phukon and H.~Phurailatpam and O.~J.~Piccinni and 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L.~Troiano and A.~Trovato and L.~Trozzo and R.~J.~Trudeau and D.~Tsai and K.~W.~Tsang and T.~Tsang and J.~S.~Tsao and M.~Tse and R.~Tso and S.~Tsuchida and L.~Tsukada and D.~Tsuna and T.~Tsutsui and K.~Turbang and M.~Turconi and D.~Tuyenbayev and A.~S.~Ubhi and T.~Uchiyama and R.~P.~Udall and A.~Ueda and T.~Uehara and K.~Ueno and G.~Ueshima and C.~S.~Unnikrishnan and A.~L.~Urban and T.~Ushiba and A.~Utina and G.~Vajente and A.~Vajpeyi and G.~Valdes and M.~Valentini and V.~Valsan and N.~van Bakel and M.~van Beuzekom and M.~van Dael and J.~F.~J.~van den Brand and C.~Van Den Broeck and D.~C.~Vander-Hyde and H.~van Haevermaet and J.~V.~van Heijningen and M.~H.~P.~M.~van Putten and N.~van Remortel and M.~Vardaro and A.~F.~Vargas and V.~Varma and M.~Vasuth and A.~Vecchio and G.~Vedovato and J.~Veitch and P.~J.~Veitch and J.~Venneberg and G.~Venugopalan and D.~Verkindt and P.~Verma and Y.~Verma and S.~M.~Vermeulen and D.~Veske and F.~Vetrano and A.~Vicere and S.~Vidyant and A.~D.~Viets and 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H.~Yamamoto and K.~Yamamoto and T.~Yamamoto and K.~Yamashita and R.~Yamazaki and F.~W.~Yang and K.~Z.~Yang and L.~Yang and Y.~C.~Yang and Y.~Yang and Yang Yang and M.~J.~Yap and D.~W.~Yeeles and S.~W.~Yeh and A.~B.~Yelikar and M.~Ying and J.~Yokoyama and T.~Yokozawa and J.~Yoo and T.~Yoshioka and Hang Yu and Haocun Yu and H.~Yuzurihara and A.~Zadrozny and M.~Zanolin and S.~Zeidler and T.~Zelenova and J.P.~Zendri and M.~Zevin and M.~Zhan and H.~Zhang and J.~Zhang and L.~Zhang and R.~Zhang and T.~Zhang and Y.~Zhang and C.~Zhao and G.~Zhao and Y.~Zhao and Yue Zhao and R.~Zhou and Z.~Zhou and X.~J.~Zhu and Z.~H.~Zhu and A.~B.~Zimmerman and M.~E.~Zucker and J.~Zweizig and LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration}, title = {{A} {J}oint {F}ermi-{GBM} and {S}wift-{BAT} {A}nalysis of {G}ravitational-{W}ave {C}andidates from the {T}hird {G}ravitational-wave {O}bserving {R}un}, year = {2023}, eprint = {2308.13666}, note = {arXiv:2308.13666v1} }
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We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM on-board triggers and sub-threshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift-BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma-rays from binary black hole mergers.
Search for Eccentric Black Hole Coalescences during the Third Observing Run of LIGO and Virgo
LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, A. G. Abac, R. Abbott, H. Abe, F. Acernese, K. Ackley, C. Adamcewicz, S. Adhicary, N. Adhikari, R. X. Adhikari, V. K. Adkins, V. B. Adya, C. Affeldt, D. Agarwal, M. Agathos, O. D. Aguiar, I. Aguilar, L. Aiello, et al (1755)
Aug 09 2023 astro-ph.HE arXiv:2308.03822v1

@misc{2308.03822, author = {LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration and A.~G.~Abac and R.~Abbott and H.~Abe and F.~Acernese and K.~Ackley and C.~Adamcewicz and S.~Adhicary and N.~Adhikari and R.~X.~Adhikari and V.~K.~Adkins and V.~B.~Adya and C.~Affeldt and D.~Agarwal and M.~Agathos and O.~D.~Aguiar and I.~Aguilar and L.~Aiello and A.~Ain and P.~Ajith and T.~Akutsu and S.~Albanesi and R.~A.~Alfaidi and A.~Al-Jodah and C.~Alléné and A.~Allocca and M.~Almualla and P.~A.~Altin and S.~Álvarez-López and A.~Amato and L.~Amez-Droz and A.~Amorosi and S.~Anand and A.~Ananyeva and R.~Andersen and S.~B.~Anderson and W.~G.~Anderson and M.~Andia and M.~Ando and T.~Andrade and N.~Andres and M.~Andrés-Carcasona and T.~Andrić and S.~Ansoldi and J.~M.~Antelis and S.~Antier and M.~Aoumi and T.~Apostolatos and E.~Z.~Appavuravther and S.~Appert and S.~K.~Apple and K.~Arai and A.~Araya and M.~C.~Araya and J.~S.~Areeda and N.~Aritomi and F.~Armato and N.~Arnaud and M.~Arogeti and S.~M.~Aronson and K.~G.~Arun and G.~Ashton and Y.~Aso and M.~Assiduo and S.~Assis de Souza Melo and S.~M.~Aston and P.~Astone and F.~Aubin and K.~AultONeal and S.~Babak and A.~Badalyan and F.~Badaracco and C.~Badger and S.~Bae and S.~Bagnasco and Y.~Bai and J.~G.~Baier and R.~Bajpai and T.~Baka and M.~Ball and G.~Ballardin and S.~W.~Ballmer and G.~Baltus and S.~Banagiri and B.~Banerjee and D.~Bankar and P.~Baral and J.~C.~Barayoga and J.~Barber and B.~C.~Barish and D.~Barker and P.~Barneo and F.~Barone and B.~Barr and L.~Barsotti and M.~Barsuglia and D.~Barta and S.~D.~Barthelmy and M.~A.~Barton and I.~Bartos and S.~Basak and A.~Basalaev and R.~Bassiri and A.~Basti and M.~Bawaj and P.~Baxi and J.~C.~Bayley and A.~C.~Baylor and M.~Bazzan and B.~Bécsy and V.~M.~Bedakihale and F.~Beirnaert and M.~Bejger and A.~S.~Bell and V.~Benedetto and D.~Beniwal and W.~Benoit and J.~D.~Bentley and M.~Ben Yaala and S.~Bera and M.~Berbel and F.~Bergamin and B.~K.~Berger and S.~Bernuzzi and M.~Beroiz and C.~P.~L.~Berry and D.~Bersanetti and A.~Bertolini and J.~Betzwieser and D.~Beveridge and N.~Bevins and R.~Bhandare and A.~V.~Bhandari and U.~Bhardwaj and R.~Bhatt and D.~Bhattacharjee and S.~Bhaumik and A.~Bianchi and I.~A.~Bilenko and M.~Bilicki and G.~Billingsley and A.~Binetti and S.~Bini and O.~Birnholtz and S.~Biscans and M.~Bischi and S.~Biscoveanu and A.~Bisht and M.~Bitossi and M.-A.~Bizouard and J.~K.~Blackburn and C.~D.~Blair and D.~G.~Blair and F.~Bobba and N.~Bode and M.~Boër and G.~Bogaert and G.~Boileau and M.~Boldrini and G.~N.~Bolingbroke and L.~D.~Bonavena and R.~Bondarescu and F.~Bondu and E.~Bonilla and M.~S.~Bonilla and R.~Bonnand and P.~Booker and V.~Boschi and S.~Bose and V.~Bossilkov and V.~Boudart and A.~Bozzi and C.~Bradaschia and P.~R.~Brady and M.~Braglia and A.~Branch and M.~Branchesi and M.~Breschi and T.~Briant and A.~Brillet and M.~Brinkmann and P.~Brockill and A.~F.~Brooks and D.~D.~Brown and M.~L.~Brozzetti and S.~Brunett and G.~Bruno and R.~Bruntz and J.~Bryant and F.~Bucci and J.~Buchanan and O.~Bulashenko and T.~Bulik and H.~J.~Bulten and A.~Buonanno and K.~Burtnyk and R.~Buscicchio and D.~Buskulic and C.~Buy and G.~S.~Cabourn Davies and G.~Cabras and R.~Cabrita and L.~Cadonati and G.~Cagnoli and C.~Cahillane and H.~W.~Cain III and J.~Calderón Bustillo and J.~D.~Callaghan and T.~A.~Callister and E.~Calloni and J.~B.~Camp and M.~Canepa and G.~Caneva Santoro and M.~Cannavacciuolo and K.~C.~Cannon and H.~Cao and Z.~Cao and L.~A.~Capistran and E.~Capocasa and E.~Capote and G.~Carapella and F.~Carbognani and M.~Carlassara and J.~B.~Carlin and M.~Carpinelli and J.~J.~Carter and G.~Carullo and J.~Casanueva Diaz and C.~Casentini and G.~Castaldi and S.~Y.~Castro-Lucas and S.~Caudill and M.~Cavaglià and R.~Cavalieri and G.~Cella and P.~Cerdá-Durán and E.~Cesarini and W.~Chaibi and S.~Chalathadka-Subrahmanya and C.~Chan and J.~C.~L.~Chan and K.~H.~M.~Chan and M.~Chan and W.~L.~Chan and K.~Chandra and I.~P.~Chang and R.-J.~Chang and W.~Chang and P.~Chanial and S.~Chao and C.~Chapman-Bird and E.~L.~Charlton and P.~Charlton and E.~Chassande-Mottin and L.~Chastain and C.~Chatterjee and Debarati Chatterjee and Deep Chatterjee and M.~Chaturvedi and S.~Chaty and K.~Chatziioannou and A.~Chen and A.~H.-Y.~Chen and D.~Chen and H.~Chen and H.~Y.~Chen and J.~Chen and K.~H.~Chen and X.~Chen and Y.-R.~Chen and Y.~Chen and H.~Cheng and P.~Chessa and H.~Y.~Chia and F.~Chiadini and C.~Chiang and G.~Chiarini and A.~Chiba and R.~Chiba and R.~Chierici and A.~Chincarini and M.~L.~Chiofalo and A.~Chiummo and C.~Chou and S.~Choudhary and N.~Christensen and S.~S.~Y.~Chua and K.~W.~Chung and G.~Ciani and P.~Ciecielag and M.~Cieślar and M.~Cifaldi and A.~A.~Ciobanu and R.~Ciolfi and F.~Clara and J.~A.~Clark and T.~A.~Clarke and P.~Clearwater and S.~Clesse and F.~Cleva and E.~Coccia and E.~Codazzo and P.-F.~Cohadon and M.~Colleoni and C.~G.~Collette and J.~Collins and A.~Colombo and M.~Colpi and C.~M.~Compton and L.~Conti and S.~J.~Cooper and T.~R.~Corbitt and I.~Cordero-Carrión and S.~Corezzi and N.~J.~Cornish and A.~Corsi and S.~Cortese and C.~A.~Costa and R.~Cottingham and M.~W.~Coughlin and A.~Couineaux and J.-P.~Coulon and S.~T.~Countryman and J.-F.~Coupechoux and B.~Cousins and P.~Couvares and D.~M.~Coward and M.~J.~Cowart and B.~D.~Cowburn and D.~C.~Coyne and R.~Coyne and K.~Craig and J.~D.~E.~Creighton and T.~D.~Creighton and A.~W.~Criswell and J.~C.~G.~Crockett-Gray and M.~Croquette and R.~Crouch and S.~G.~Crowder and J.~R.~Cudell and T.~J.~Cullen and A.~Cumming and E.~Cuoco and M.~Curyło and M.~Cusinato and P.~Dabadie and T.~Dal Canton and S.~Dall'Osso and G.~Dálya and B.~D'Angelo and S.~Danilishin and S.~D'Antonio and K.~Danzmann and K.~E.~Darroch and C.~Darsow-Fromm and L.~P.~Dartez and A.~Dasgupta and S.~Datta and V.~Dattilo and A.~Daumas and I.~Dave and A.~Davenport and M.~Davier and D.~Davis and M.~C.~Davis and E.~J.~Daw and M.~Dax and M.~Deenadayalan and J.~Degallaix and M.~De Laurentis and S.~Deléglise and V.~Del Favero and F.~De Lillo and D.~Dell'Aquila and W.~Del Pozzo and F.~De Marco and F.~De Matteis and V.~D'Emilio and N.~Demos and T.~Dent and A.~Depasse and R.~De Pietri and R.~De Rosa and C.~De Rossi and R.~De Simone and S.~Dhurandhar and R.~Diab and P.~Z.~Diamond and M.~C.~Díaz and N.~A.~Didio and T.~Dietrich and L.~Di Fiore and C.~Di Fronzo and F.~Di Giovanni and M.~Di Giovanni and T.~Di Girolamo and D.~Diksha and A.~Di Lieto and A.~Di Michele and J.~Ding and S.~Di Pace and I.~Di Palma and F.~Di Renzo and Divyajyoti and A.~Dmitriev and Z.~Doctor and E.~Dohmen and P.~P.~Doleva and L.~Donahue and L.~D'Onofrio and F.~Donovan and K.~L.~Dooley and T.~Dooney and S.~Doravari and O.~Dorosh and M.~Drago and J.~C.~Driggers and Y.~Drori and H.~Du and J.-G.~Ducoin and L.~Dunn and U.~Dupletsa and D.~D'Urso and H.~Duval and P.-A.~Duverne and S.~E.~Dwyer and C.~Eassa and M.~Ebersold and T.~Eckhardt and G.~Eddolls and B.~Edelman and T.~B.~Edo and O.~Edy and A.~Effler and J.~Eichholz and H.~Einsle and M.~Eisenmann and R.~A.~Eisenstein and A.~Ejlli and E.~Engelby and A.~J.~Engl and L.~Errico and R.~C.~Essick and H.~Estellés and D.~Estevez and T.~Etzel and C.~R.~Evans and M.~Evans and T.~M.~Evans and T.~Evstafyeva and B.~E.~Ewing and J.~M.~Ezquiaga and F.~Fabrizi and F.~Faedi and V.~Fafone and H.~Fair and S.~Fairhurst and P.~C.~Fan and A.~M.~Farah and B.~Farr and W.~M.~Farr and E.~J.~Fauchon-Jones and G.~Favaro and M.~Favata and M.~Fays and J.~Feicht and M.~M.~Fejer and E.~Fenyvesi and D.~L.~Ferguson and I.~Ferrante and T.~A.~Ferreira and F.~Fidecaro and A.~Fiori and I.~Fiori and M.~Fishbach and R.~P.~Fisher and R.~Fittipaldi and V.~Fiumara and R.~Flaminio and S.~M.~Fleischer and L.~S.~Fleming and E.~Floden and H.~Fong and J.~A.~Font and B.~Fornal and P.~W.~F.~Forsyth and K.~Franceschetti and A.~Franke and S.~Frasca and F.~Frasconi and A.~Frattale Mascioli and Z.~Frei and A.~Freise and O.~Freitas and R.~Frey and W.~Frischhertz and P.~Fritschel and V.~V.~Frolov and G.~G.~Fronzé and S.~Fujii and I.~Fukunaga and P.~Fulda and M.~Fyffe and W.~E.~Gabella and B.~Gadre and J.~R.~Gair and J.~Gais and S.~Galaudage and S.~Gallardo and R.~Gamba and D.~Ganapathy and A.~Ganguly and S.~G.~Gaonkar and B.~Garaventa and J.~Garcia-Bellido and C.~García-Núñez and C.~García-Quirós and J.~W.~Gardner and K.~A.~Gardner and J.~Gargiulo and F.~Garufi and C.~Gasbarra and B.~Gateley and V.~Gayathri and G.~Gemme and A.~Gennai and J.~George and O.~Gerberding and L.~Gergely and N.~Ghadiri and Abhirup Ghosh and Archisman Ghosh and Shaon Ghosh and Shrobana Ghosh and Suprovo Ghosh and Tathagata Ghosh and L.~Giacoppo and J.~A.~Giaime and K.~D.~Giardina and D.~R.~Gibson and C.~Gier and P.~Giri and F.~Gissi and S.~Gkaitatzis and J.~Glanzer and A.~E.~Gleckl and F.~Glotin and J.~Godfrey and P.~Godwin and E.~Goetz and R.~Goetz and J.~Golomb and S.~Gomez Lopez and B.~Goncharov and G.~González and A.~W.~Goodwin-Jones and M.~Gosselin and R.~Gouaty and D.~W.~Gould and S.~Goyal and B.~Grace and A.~Grado and V.~Graham and A.~E.~Granados and M.~Granata and V.~Granata and S.~Gras and P.~Grassia and C.~Gray and R.~Gray and G.~Greco and A.~C.~Green and S.~M.~Green and S.~R.~Green and A.~M.~Gretarsson and E.~M.~Gretarsson and D.~Griffith and W.~L.~Griffiths and H.~L.~Griggs and G.~Grignani and A.~Grimaldi and C.~Grimaud and H.~Grote and A.~S.~Gruson and D.~Guerra and D.~Guetta and G.~M.~Guidi and A.~R.~Guimaraes and H.~K.~Gulati and F.~Gulminelli and A.~M.~Gunny and H.~Guo and Y.~Guo and Anchal Gupta and Anuradha Gupta and Ish Gupta and N.~C.~Gupta and P.~Gupta and S.~K.~Gupta and N.~Gupte and R.~Gurav and J.~Gurs and E.~K.~Gustafson and N.~Gutierrez and F.~Guzman and D.~Haba and L.~Haegel and G.~Hain and S.~Haino and O.~Halim and E.~D.~Hall and E.~Z.~Hamilton and G.~Hammond and W.-B.~Han and M.~Haney and J.~Hanks and C.~Hanna and M.~D.~Hannam and O.~A.~Hannuksela and A.~G.~Hanselman and H.~Hansen and J.~Hanson and R.~Harada and T.~Harder and K.~Haris and T.~Harmark and J.~Harms and G.~M.~Harry and I.~W.~Harry and D.~Hartwig and B.~Haskell and C.-J.~Haster and J.~S.~Hathaway and K.~Haughian and H.~Hayakawa and K.~Hayama and F.~J.~Hayes and J.~Healy and A.~Heffernan and A.~Heidmann and M.~C.~Heintze and J.~Heinze and J.~Heinzel and H.~Heitmann and F.~Hellman and P.~Hello and A.~F.~Helmling-Cornell and G.~Hemming and M.~Hendry and I.~S.~Heng and E.~Hennes and J.-S.~Hennig and M.~Hennig and C.~Henshaw and A.~Hernandez and T.~Hertog and M.~Heurs and A.~L.~Hewitt and S.~Higginbotham and S.~Hild and P.~Hill and Y.~Himemoto and A.~S.~Hines and N.~Hirata and C.~Hirose and J.~Ho and S.~Hoang and S.~Hochheim and D.~Hofman and J.~N.~Hohmann and N.~A.~Holland and K.~Holley-Bockelmann and I.~J.~Hollows and Z.~J.~Holmes and D.~E.~Holz and C.~Hong and Q.~Hong and J.~Hornung and S.~Hoshino and J.~Hough and S.~Hourihane and E.~J.~Howell and C.~G.~Hoy and D.~Hoyland and H.-F.~Hsieh and C.~Hsiung and H.~C.~Hsu and S.-C.~Hsu and W.-F.~Hsu and P.~Hu and Q.~Hu and H.~Y.~Huang and Y.-J.~Huang and Y.~Huang and Y.~T.~Huang and M.~T.~Hübner and A.~D.~Huddart and B.~Hughey and D.~C.~Y.~Hui and V.~Hui and R.~Hur and S.~Husa and R.~Huxford and T.~Huynh-Dinh and J.~Hyland and A.~Iakovlev and G.~A.~Iandolo and A.~Iess and K.~Inayoshi and Y.~Inoue and G.~Iorio and P.~Iosif and J.~Irwin and M.~Isi and M.~A.~Ismail and Y.~Itoh and M.~Iwaya and B.~R.~Iyer and V.~JaberianHamedan and T.~Jacqmin and P.-E.~Jacquet and S.~J.~Jadhav and S.~P.~Jadhav and D.~Jain and T.~Jain and A.~L.~James and P.~A.~James and R.~Jamshidi and A.~Z.~Jan and K.~Jani and L.~Janiurek and J.~Janquart and K.~Janssens and N.~N.~Janthalur and S.~Jaraba and P.~Jaranowski and S.~Jarov and P.~Jasal and R.~Jaume and W.~Javed and K.~Jenner and A.~Jennings and W.~Jia and J.~Jiang and H.-B.~Jin and K.~Johansmeyer and G.~R.~Johns and N.~A.~Johnson and R.~Johnston and N.~Johny and D.~H.~Jones and D.~I.~Jones and R.~Jones and P.~Joshi and L.~Ju and K.~Jung and J.~Junker and V.~Juste and T.~Kajita and C.~Kalaghatgi and V.~Kalogera and M.~Kamiizumi and N.~Kanda and S.~Kandhasamy and G.~Kang and J.~B.~Kanner and S.~J.~Kapadia and D.~P.~Kapasi and S.~Karat and C.~Karathanasis and S.~Karki and T.~Karydas and Y.~A.~Kas-danouche and R.~Kashyap and M.~Kasprzack and W.~Kastaun and J.~Kato and T.~Kato and S.~Katsanevas and E.~Katsavounidis and J.~K.~Katsuren and W.~Katzman and T.~Kaur and K.~Kawabe and F.~Kéfélian and D.~Keitel and J.~Kelley-Derzon and S.~A.~Kemper and J.~Kennington and R.~Kesharwani and J.~S.~Key and S.~Khadka and F.~Y.~Khalili and T.~Khanam and E.~A.~Khazanov and M.~Khursheed and N.~Kijbunchoo and C.~Kim and J.~C.~Kim and K.~Kim and M.~H.~Kim and P.~Kim and S.~Kim and W.~S.~Kim and Y.-M.~Kim and C.~Kimball and N.~Kimura and M.~Kinley-Hanlon and R.~Kirchhoff and J.~S.~Kissel and T.~Kiyota and S.~Klimenko and T.~Klinger and A.~M.~Knee and N.~Knust and P.~Koch and S.~M.~Koehlenbeck and G.~Koekoek and K.~Kohri and K.~Kokeyama and S.~Koley and N.~D.~Koliadko and P.~Kolitsidou and M.~Kolstein and K.~Komori and V.~Kondrashov and A.~K.~H.~Kong and A.~Kontos and M.~Korobko and R.~V.~Kossak and N.~Kouvatsos and M.~Kovalam and N.~Koyama and D.~B.~Kozak and S.~L.~Kranzhoff and V.~Kringel and N.~V.~Krishnendu and A.~Królak and G.~Kuehn and P.~Kuijer and S.~Kulkarni and A.~Kulur Ramamohan and A.~Kumar and Praveen Kumar and Prayush Kumar and Rahul Kumar and Rakesh Kumar and J.~Kume and K.~Kuns and S.~Kuroyanagi and S.~Kuwahara and K.~Kwak and K.~Kwan and G.~Lacaille and P.~Lagabbe and D.~Laghi and S.~Lai and M.~H.~Lakkis and E.~Lalande and M.~Lalleman and A.~Lamberts and M.~Landry and B.~B.~Lane and R.~N.~Lang and J.~Lange and B.~Lantz and A.~La Rana and I.~La Rosa and A.~Lartaux-Vollard and P.~D.~Lasky and J.~Lawrence and M.~Laxen and A.~Lazzarini and C.~Lazzaro and P.~Leaci and S.~Leavey and S.~LeBohec and Y.~K.~Lecoeuche and H.~M.~Lee and H.~W.~Lee and K.~Lee and R.-K.~Lee and R.~Lee and S.~Lee and Y.~Lee and I.~N.~Legred and J.~Lehmann and L.~Lehner and A.~Lemaître and M.~Lenti and M.~Leonardi and E.~Leonova and N.~Leroy and M.~Lesovsky and N.~Letendre and M.~Lethuillier and C.~Levesque and Y.~Levin and K.~Leyde and A.~K.~Y.~Li and K.~L.~Li and T.~G.~F.~Li and X.~Li and Chien-Yu Lin and Chun-Yu Lin and E.~T.~Lin and F.~Lin and H.~Lin and L.~C.-C.~Lin and Y.~Lin and F.~Linde and S.~D.~Linker and T.~B.~Littenberg and A.~Liu and G.~C.~Liu and Jian Liu and F.~Llamas and R.~K.~L.~Lo and T.~Lo and J.-P.~Locquet and L.~London and A.~Longo and D.~Lopez and M.~Lopez Portilla and M.~Lorenzini and V.~Loriette and M.~Lormand and G.~Losurdo and T.~P.~Lott and J.~D.~Lough and H.~A.~Loughlin and C.~O.~Lousto and G.~Lovelace and M.~J.~Lowry and H.~Lück and D.~Lumaca and A.~P.~Lundgren and A.~W.~Lussier and J.~E.~Lynam and L.-T.~Ma and S.~Ma and M.~Ma'arif and R.~Macas and M.~MacInnis and D.~M.~Macleod and I.~A.~O.~MacMillan and A.~Macquet and K.~Maeda and S.~Maenaut and I.~Magaña Hernandez and C.~Magazzù and R.~M.~Magee and R.~Maggiore and M.~Magnozzi and M.~Mahesh and S.~Mahesh and M.~Maini and S.~Majhi and E.~Majorana and C.~N.~Makarem and S.~Maliakal and A.~Malik and N.~Man and V.~Mandic and V.~Mangano and B.~Mannix and G.~L.~Mansell and G.~Mansingh and M.~Manske and M.~Mantovani and M.~Mapelli and F.~Marchesoni and D.~Marín Pina and F.~Marion and S.~Márka and Z.~Márka and C.~Markakis and A.~S.~Markosyan and A.~Markowitz and E.~Maros and A.~Marquina and S.~Marsat and F.~Martelli and I.~W.~Martin and R.~M.~Martin and B.~B.~Martinez and M.~Martinez and V.~A.~Martinez and V.~Martinez and A.~Martini and K.~Martinovic and D.~V.~Martynov and E.~J.~Marx and H.~Masalehdan and A.~Masserot and M.~Masso-Reid and M.~Mastrodicasa and S.~Mastrogiovanni and M.~Mateu-Lucena and M.~Matiushechkina and M.~Matsuyama and N.~Mavalvala and N.~Maxwell and G.~McCarrol and R.~McCarthy and D.~E.~McClelland and S.~McCormick and L.~McCuller and G.~I.~McGhee and J.~McGinn and M.~Mchedlidze and C.~McIsaac and J.~McIver and K.~McKinney and A.~McLeod and T.~McRae and S.~T.~McWilliams and D.~Meacher and M.~Mehmet and A.~K.~Mehta and Q.~Meijer and A.~Melatos and S.~Mellaerts and A.~Menendez-Vazquez and C.~S.~Menoni and R.~A.~Mercer and L.~Mereni and K.~Merfeld and E.~L.~Merilh and J.~D.~Merritt and M.~Merzougui and C.~Messenger and C.~Messick and M.~Meyer-Conde and F.~Meylahn and A.~Mhaske and A.~Miani and H.~Miao and I.~Michaloliakos and C.~Michel and Y.~Michimura and H.~Middleton and D.~P.~Mihaylov and A.~L.~Miller and A.~Miller and B.~Miller and S.~Miller and M.~Millhouse and E.~Milotti and Y.~Minenkov and N.~Mio and Ll.~M.~Mir and L.~Mirasola and M.~Miravet-Tenés and C.~.~Miritescu and A.~Mishkin and A.~Mishra and C.~Mishra and T.~Mishra and T.~Mistry and A.~L.~Mitchell and S.~Mitra and V.~P.~Mitrofanov and G.~Mitselmakher and R.~Mittleman and O.~Miyakawa and S.~Miyamoto and S.~Miyoki and G.~Mo and L.~Mobilia and L.~M.~Modafferi and S.~R.~P.~Mohapatra and S.~R.~Mohite and M.~Molina-Ruiz and C.~Mondal and M.~Mondin and M.~Montani and C.~J.~Moore and M.~Morales and D.~Moraru and F.~Morawski and A.~More and S.~More and C.~Moreno and G.~Moreno and S.~Morisaki and Y.~Moriwaki and G.~Morras and A.~Moscatello and B.~Mours and C.~M.~Mow-Lowry and S.~Mozzon and F.~Muciaccia and Arunava Mukherjee and D.~Mukherjee and Soma Mukherjee and Subroto Mukherjee and Suvodip Mukherjee and N.~Mukund and A.~Mullavey and J.~Munch and E.~A.~Muñiz and M.~Murakoshi and P.~G.~Murray and S.~Muusse and S.~L.~Nadji and A.~Nagar and T.~Nagar and N.~Nagarajan and K.~Nakamura and H.~Nakano and M.~Nakano and V.~Napolano and I.~Nardecchia and T.~Narikawa and H.~Narola and L.~Naticchioni and R.~K.~Nayak and B.~F.~Neil and J.~Neilson and A.~Nelson and T.~J.~N.~Nelson and M.~Nery and S.~Nesseris and A.~Neunzert and K.~Y.~Ng and S.~W.~S.~Ng and C.~Nguyen and P.~Nguyen and L.~Nguyen Quynh and S.~A.~Nichols and G.~Nieradka and A.~Niko and Y.~Nishino and A.~Nishizawa and S.~Nissanke and E.~Nitoglia and W.~Niu and F.~Nocera and M.~Norman and C.~North and J.~Novak and J.~F.~Nuño Siles and G.~Nurbek and L.~K.~Nuttall and K.~Obayashi and J.~Oberling and J.~O'Dell and E.~Oelker and M.~Oertel and A.~Offermans and G.~Oganesyan and J.~J.~Oh and K.~Oh and S.~H.~Oh and T.~O'Hanlon and M.~Ohashi and M.~Ohkawa and F.~Ohme and H.~Ohta and A.~S.~Oliveira and R.~Oliveri and V.~Oloworaran and B.~O'Neal and K.~Oohara and B.~O'Reilly and R.~G.~Ormiston and N.~D.~Ormsby and M.~Orselli and R.~O'Shaughnessy and Y.~Oshima and S.~Oshino and S.~Ossokine and C.~Osthelder and D.~J.~Ottaway and A.~Ouzriat and H.~Overmier and A.~E.~Pace and R.~Pagano and M.~A.~Page and A.~Pai and S.~A.~Pai and A.~Pal and S.~Pal and O.~Palashov and M.~Pálfi and C.~Palomba and K.-C.~Pan and P.~K.~Panda and L.~Panebianco and P.~T.~H.~Pang and F.~Pannarale and B.~C.~Pant and F.~H.~Panther and C.~D.~Panzer and F.~Paoletti and A.~Paoli and A.~Paolone and E.~E.~Papalexakis and L.~Papalini and G.~Pappas and A.~Parisi and J.~Park and W.~Parker and D.~Pascucci and A.~Pasqualetti and R.~Passaquieti and D.~Passuello and M.~Patel and D.~Pathak and M.~Pathak and A.~Patra and B.~Patricelli and A.~S.~Patron and S.~Paul and E.~Payne and T.~Pearce and M.~Pedraza and R.~Pegna and M.~Pegoraro and A.~Pele and F.~E.~Peña Arellano and S.~Penn and A.~Perego and A.~Pereira and C.~J.~Perez and J.~J.~Perez and L.~H.~Perez and C.~Périgois and C.~C.~Perkins and A.~Perreca and J.~Perret and S.~Perriès and J.~W.~Perry and D.~Pesios and J.~Petermann and C.~Petrillo and H.~P.~Pfeiffer and H.~Pham and K.~A.~Pham and K.~S.~Phukon and H.~Phurailatpam and O.~J.~Piccinni and M.~Pichot and M.~Piendibene and F.~Piergiovanni and L.~Pierini and G.~Pierra and V.~Pierro and M.~.~Pietrzak and G.~Pillant and M.~Pillas and F.~Pilo and L.~Pinard and C.~Pineda-Bosque and I.~M.~Pinto and M.~Pinto and B.~J.~Piotrzkowski and M.~Pirello and M.~D.~Pitkin and A.~Placidi and E.~Placidi and M.~L.~Planas and W.~Plastino and R.~Poggiani and E.~Polini and L.~Pompili and S.~Ponrathnam and J.~Poon and E.~Porcelli and J.~Portell and E.~K.~Porter and C.~Posnansky and R.~Poulton and J.~Powell and M.~Pracchia and B.~K.~Pradhan and T.~Pradier and A.~K.~Prajapati and K.~Prasai and R.~Prasanna and P.~Prasia and G.~Pratten and M.~Principe and G.~A.~Prodi and L.~Prokhorov and P.~Prosposito and L.~Prudenzi and A.~Puecher and J.~Pullin and M.~Punturo and F.~Puosi and P.~Puppo and M.~Pürrer and H.~Qi and J.~Qin and V.~Quetschke and P.~J.~Quinonez and R.~Quitzow-James and F.~J.~Raab and G.~Raaijmakers and N.~Radulesco and P.~Raffai and S.~X.~Rail and S.~Raja and C.~Rajan and K.~E.~Ramirez and A.~Ramos-Buades and D.~Rana and E.~Randel and P.~R.~Rangnekar and P.~Rapagnani and A.~Ray and V.~Raymond and M.~Razzano and J.~Read and M.~Recaman Payo and T.~Regimbau and L.~Rei and S.~Reid and S.~W.~Reid and D.~H.~Reitze and P.~Relton and A.~Renzini and P.~Rettegno and B.~Revenu and A.~Reza and M.~Rezac and A.~S.~Rezaei and F.~Ricci and M.~Ricci and D.~Richards and J.~W.~Richardson and A.~Rijal and K.~Riles and H.~K.~Riley and S.~Rinaldi and C.~Robertson and N.~A.~Robertson and F.~Robinet and M.~Robinson and A.~Rocchi and L.~Rolland and J.~G.~Rollins and M.~Romanelli and A.~E.~Romano and R.~Romano and A.~Romero and I.~M.~Romero-Shaw and J.~H.~Romie and S.~Ronchini and T.~J.~Roocke and L.~Rosa and T.~J.~Rosauer and C.~A.~Rose and D.~Rosińska and M.~P.~Ross and M.~Rossello and S.~Rowan and S.~Roy and A.~Royzman and D.~Rozza and P.~Ruggi and E.~Ruiz Morales and K.~Ruiz-Rocha and S.~Sachdev and T.~Sadecki and J.~Sadiq and P.~Saffarieh and S.~S.~Saha and T.~Sainrat and S.~Sajith Menon and K.~Sakai and M.~Sakellariadou and T.~Sako and S.~Sakon and O.~S.~Salafia and F.~Salces-Carcoba and L.~Salconi and M.~Saleem and F.~Salemi and M.~Sallé and S.~Salvador and A.~Sanchez and E.~J.~Sanchez and J.~H.~Sanchez and L.~E.~Sanchez and N.~Sanchis-Gual and J.~R.~Sanders and E.~M.~Sänger and T.~R.~Saravanan and N.~Sarin and A.~Sasli and P.~Sassi and B.~Sassolas and H.~Satari and R.~Sato and S.~Sato and Y.~Sato and O.~Sauter and R.~L.~Savage and V.~Savant and T.~Sawada and H.~L.~Sawant and S.~Sayah and D.~Schaetzl and M.~Scheel and S.~J.~Scherf and J.~Scheuer and M.~G.~Schiworski and P.~Schmidt and S.~Schmidt and S.~J.~Schmitz and R.~Schnabel and M.~Schneewind and R.~M.~S.~Schofield and A.~Schönbeck and K.~Schouteden and H.~Schuler and B.~W.~Schulte and B.~F.~Schutz and E.~Schwartz and J.~Scott and S.~M.~Scott and T.~C.~Seetharamu and M.~Seglar-Arroyo and Y.~Sekiguchi and D.~Sellers and A.~S.~Sengupta and D.~Sentenac and E.~G.~Seo and J.~W.~Seo and V.~Sequino and G.~Servignat and Y.~Setyawati and T.~Shaffer and M.~S.~Shahriar and M.~A.~Shaikh and B.~Shams and L.~Shao and P.~Sharma and S.~Sharma-Chaudhary and P.~Shawhan and N.~S.~Shcheblanov and A.~Sheela and B.~Shen and K.~G.~Shepard and Y.~Shikano and M.~Shikauchi and K.~Shimode and H.~Shinkai and J.~Shiota and D.~H.~Shoemaker and D.~M.~Shoemaker and R.~W.~Short and S.~ShyamSundar and A.~Sider and H.~Siegel and M.~Sieniawska and D.~Sigg and L.~Silenzi and M.~Simmonds and L.~P.~Singer and A.~Singh and D.~Singh and M.~K.~Singh and A.~Singha and A.~M.~Sintes and V.~Sipala and V.~Skliris and B.~J.~J.~Slagmolen and T.~J.~Slaven-Blair and J.~Smetana and J.~R.~Smith and L.~Smith and R.~J.~E.~Smith and J.~Soldateschi and S.~N.~Somala and K.~Somiya and K.~Soni and S.~Soni and V.~Sordini and F.~Sorrentino and N.~Sorrentino and R.~Soulard and T.~Souradeep and E.~Sowell and V.~Spagnuolo and A.~P.~Spencer and M.~Spera and P.~Spinicelli and A.~K.~Srivastava and V.~Srivastava and C.~Stachie and F.~Stachurski and D.~A.~Steer and J.~Steinlechner and S.~Steinlechner and N.~Stergioulas and P.~Stevens and M.~StPierre and L.~C.~Strang and G.~Stratta and M.~D.~Strong and A.~Strunk and R.~Sturani and A.~L.~Stuver and M.~Suchenek and S.~Sudhagar and N.~Sueltmann and H.~G.~Suh and A.~G.~Sullivan and T.~Z.~Summerscales and L.~Sun and S.~Sunil and A.~Sur and J.~Suresh and P.~J.~Sutton and Takamasa Suzuki and Takanori Suzuki and B.~L.~Swinkels and A.~Syx and M.~J.~Szczepańczyk and P.~Szewczyk and M.~Tacca and H.~Tagoshi and S.~C.~Tait and H.~Takahashi and R.~Takahashi and A.~Takamori and K.~Takatani and H.~Takeda and M.~Takeda and C.~J.~Talbot and C.~Talbot and M.~Tamaki and N.~Tamanini and D.~Tanabe and K.~Tanaka and S.~J.~Tanaka and T.~Tanaka and A.~J.~Tanasijczuk and S.~Tanioka and D.~B.~Tanner and D.~Tao and L.~Tao and R.~D.~Tapia and E.~N.~Tapia San Martín and R.~Tarafder and C.~Taranto and A.~Taruya and J.~D.~Tasson and M.~Teloi and R.~Tenorio and L.~Terkowski and H.~Themann and M.~P.~Thirugnanasambandam and L.~M.~Thomas and M.~Thomas and P.~Thomas and J.~E.~Thompson and S.~R.~Thondapu and K.~A.~Thorne and E.~Thrane and J.~Tissino and Shubhanshu Tiwari and Srishti Tiwari and V.~Tiwari and A.~M.~Toivonen and A.~E.~Tolley and T.~Tomaru and K.~Tomita and T.~Tomura and M.~Tonelli and A.~Toriyama and A.~Torres-Forné and C.~I.~Torrie and M.~Toscani and I.~Tosta e Melo and E.~Tournefier and A.~A.~Trani and A.~Trapananti and F.~Travasso and G.~Traylor and J.~Trenado and M.~Trevor and M.~C.~Tringali and A.~Tripathee and L.~Troiano and A.~Trovato and L.~Trozzo and R.~J.~Trudeau and M.~Tse and R.~Tso and S.~Tsuchida and L.~Tsukada and T.~Tsutsui and K.~Turbang and M.~Turconi and C.~Turski and H.~Ubach and A.~S.~Ubhi and N.~Uchikata and T.~Uchiyama and R.~P.~Udall and T.~Uehara and K.~Ueno and C.~S.~Unnikrishnan and T.~Ushiba and A.~Utina and H.~Vahlbruch and N.~Vaidya and G.~Vajente and A.~Vajpeyi and G.~Valdes and M.~Valentini and S.~A.~Vallejo-Peña and S.~Vallero and V.~Valsan and N.~van Bakel and M.~van Beuzekom and M.~van Dael and J.~F.~J.~van den Brand and C.~Van Den Broeck and D.~C.~Vander-Hyde and M.~van der Sluys and A.~Van de Walle and J.~van Dongen and H.~van Haevermaet and J.~V.~van Heijningen and J.~Vanosky and M.~H.~P.~M.~van Putten and Z.~van Ranst and N.~van Remortel and M.~Vardaro and A.~F.~Vargas and V.~Varma and M.~Vasúth and A.~Vecchio and G.~Vedovato and J.~Veitch and P.~J.~Veitch and J.~Venneberg and P.~Verdier and D.~Verkindt and P.~Verma and Y.~Verma and S.~M.~Vermeulen and D.~Veske and F.~Vetrano and A.~Veutro and A.~Viceré and S.~Vidyant and A.~D.~Viets and A.~Vijaykumar and V.~Villa-Ortega and E.~T.~Vincent and J.-Y.~Vinet and S.~Viret and A.~Virtuoso and S.~Vitale and H.~Vocca and D.~Voigt and E.~R.~G.~von Reis and J.~S.~A.~von Wrangel and S.~P.~Vyatchanin and L.~E.~Wade and M.~Wade and K.~J.~Wagner and R.~C.~Walet and M.~Walker and G.~S.~Wallace and L.~Wallace and H.~Wang and J.~Z.~Wang and W.~H.~Wang and R.~L.~Ward and J.~Warner and M.~Was and T.~Washimi and N.~Y.~Washington and K.~Watada and D.~Watarai and K.~E.~Wayt and B.~Weaver and C.~R.~Weaving and S.~A.~Webster and M.~Weinert and A.~J.~Weinstein and R.~Weiss and C.~M.~Weller and R.~A.~Weller and F.~Wellmann and L.~Wen and P.~Weßels and K.~Wette and J.~T.~Whelan and D.~D.~White and B.~F.~Whiting and C.~Whittle and J.~B.~Wildberger and O.~S.~Wilk and D.~Wilken and K.~Willetts and D.~Williams and M.~J.~Williams and A.~R.~Williamson and J.~L.~Willis and B.~Willke and M.~Wils and C.~C.~Wipf and G.~Woan and J.~Woehler and J.~K.~Wofford and D.~Wong and H.~T.~Wong and I.~C.~F.~Wong and M.~Wright and C.~Wu and D.~S.~Wu and H.~Wu and D.~M.~Wysocki and L.~Xiao and V.~A.~Xu and N.~Yadav and H.~Yamamoto and K.~Yamamoto and M.~Yamamoto and T.~S.~Yamamoto and T.~Yamamoto and S.~Yamamura and R.~Yamazaki and S.~Yan and F.~W.~Yang and K.~Z.~Yang and L.-C.~Yang and Y.-C.~Yang and Yang Yang and Yi Yang and M.~J.~Yap and Z.~Yarbrough and S.-W.~Yeh and A.~B.~Yelikar and S.~M.~C.~Yeung and T.~Y.~Yeung and J.~Yokoyama and T.~Yokozawa and J.~Yoo and H.~Yu and H.~Yuzurihara and A.~Zadrożny and A.~J.~Zannelli and M.~Zanolin and M.~Zeeshan and T.~Zelenova and J.-P.~Zendri and M.~Zevin and J.~Zhang and L.~Zhang and R.~Zhang and T.~Zhang and Yanqi Zhang and Ya Zhang and C.~Zhao and Yue Zhao and Yuhang Zhao and Y.~Zheng and H.~Zhong and R.~Zhou and Z.-H.~Zhu and A.~B.~Zimmerman and M.~E.~Zucker and J.~Zweizig}, title = {{S}earch for {E}ccentric {B}lack {H}ole {C}oalescences during the {T}hird {O}bserving {R}un of {LIGO} and {V}irgo}, year = {2023}, eprint = {2308.03822}, note = {arXiv:2308.03822v1} }
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Despite the growing number of confident binary black hole coalescences observed through gravitational waves so far, the astrophysical origin of these binaries remains uncertain. Orbital eccentricity is one of the clearest tracers of binary formation channels. Identifying binary eccentricity, however, remains challenging due to the limited availability of gravitational waveforms that include effects of eccentricity. Here, we present observational results for a waveform-independent search sensitive to eccentric black hole coalescences, covering the third observing run (O3) of the LIGO and Virgo detectors. We identified no new high-significance candidates beyond those that were already identified with searches focusing on quasi-circular binaries. We determine the sensitivity of our search to high-mass (total mass $M>70$ $M_\odot$) binaries covering eccentricities up to 0.3 at 15 Hz orbital frequency, and use this to compare model predictions to search results. Assuming all detections are indeed quasi-circular, for our fiducial population model, we place an upper limit for the merger rate density of high-mass binaries with eccentricities $0 < e \leq 0.3$ at $0.33$ Gpc$^{-3}$ yr$^{-1}$ at 90\% confidence level.
A Search for Technosignatures Around 11,680 Stars with the Green Bank Telescope at 1.15-1.73 GHz
Jean-Luc Margot, Megan G. Li, Pavlo Pinchuk, Nathan Myhrvold, Larry Lesyna, Lea E. Alcantara, Megan T. Andrakin, Jeth Arunseangroj, Damien S. Baclet, Madison H. Belk, Zerxes R. Bhadha, Nicholas W. Brandis, Robert E. Carey, Harrison P. Cassar, Sai S. Chava, Calvin Chen, James Chen, Kellen T. Cheng, Alessia Cimbri, Benjamin Cloutier, et al (59)
Aug 08 2023 astro-ph.IM astro-ph.EP arXiv:2308.02712v4

@misc{2308.02712, author = {Jean-Luc Margot and Megan G.~Li and Pavlo Pinchuk and Nathan Myhrvold and Larry Lesyna and Lea E.~Alcantara and Megan T.~Andrakin and Jeth Arunseangroj and Damien S.~Baclet and Madison H.~Belk and Zerxes R.~Bhadha and Nicholas W.~Brandis and Robert E.~Carey and Harrison P.~Cassar and Sai S.~Chava and Calvin Chen and James Chen and Kellen T.~Cheng and Alessia Cimbri and Benjamin Cloutier and Jordan A.~Combitsis and Kelly L.~Couvrette and Brandon P.~Coy and Kyle W.~Davis and Antoine F.~Delcayre and Michelle R.~Du and Sarah E.~Feil and Danning Fu and Travis J.~Gilmore and Emery Grahill-Bland and Laura M.~Iglesias and Zoe Juneau and Anthony G.~Karapetian and George Karfakis and Christopher T.~Lambert and Eric A.~Lazbin and Jian H.~Li and Zhuofu Li and Nicholas M.~Liskij and Anthony V.~Lopilato and Darren J.~Lu and Detao Ma and Vedant Mathur and Mary H.~Minasyan and Maxwell K.~Muller and Mark T.~Nasielski and Janice T.~Nguyen and Lorraine M.~Nicholson and Samantha Niemoeller and Divij Ohri and Atharva U.~Padhye and Supreethi V.~Penmetcha and Yugantar Prakash and Xinyi Qi and Liam Rindt and Vedant Sahu and Joshua A.~Scally and Zefyr Scott and Trevor J.~Seddon and Lara-Lynn V.~Shohet and Anchal Sinha and Anthony E.~Sinigiani and Jiuxu Song and Spencer M.~Stice and Andria Uplisashvili and Krishna Vanga and Amaury G.~Vazquez and George Vetushko and Valeria Villa and Maria Vincent and Ian J.~Waasdorp and Ian B.~Wagaman and Amanda Wang and Jade C.~Wight and Ella Wong and Natsuko Yamaguchi and Zijin Zhang and Junyang Zhao and Ryan S.~Lynch}, title = {{A} {S}earch for {T}echnosignatures {A}round 11,680 {S}tars with the {G}reen {B}ank {T}elescope at 1.15-1.73 {GH}z}, year = {2023}, eprint = {2308.02712}, note = {arXiv:2308.02712v4} }
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We conducted a search for narrowband radio signals over four observing sessions in 2020-2023 with the L-band receiver (1.15-1.73 GHz) of the 100 m diameter Green Bank Telescope. We pointed the telescope in the directions of 62 TESS Objects of Interest, capturing radio emissions from a total of ~11,680 stars and planetary systems in the ~9 arcminute beam of the telescope. All detections were either automatically rejected or visually inspected and confirmed to be of anthropogenic nature. In this work, we also quantified the end-to-end efficiency of radio SETI pipelines with a signal injection and recovery analysis. The UCLA SETI pipeline recovers 94.0% of the injected signals over the usable frequency range of the receiver and 98.7% of the injections when regions of dense RFI are excluded. In another pipeline that uses incoherent sums of 51 consecutive spectra, the recovery rate is ~15 times smaller at ~6%. The pipeline efficiency affects calculations of transmitter prevalence and SETI search volume. Accordingly, we developed an improved Drake Figure of Merit and a formalism to place upper limits on transmitter prevalence that take the pipeline efficiency and transmitter duty cycle into account. Based on our observations, we can state at the 95% confidence level that fewer than 6.6% of stars within 100 pc host a transmitter that is detectable in our search (EIRP > 1e13 W). For stars within 20,000 ly, the fraction of stars with detectable transmitters (EIRP > 5e16 W) is at most 3e-4. Finally, we showed that the UCLA SETI pipeline natively detects the signals detected with AI techniques by Ma et al. (2023).
Sub-second periodic radio oscillations in a microquasar
Pengfu Tian, Ping Zhang, Wei Wang, Pei Wang, Xiaohui Sun, Jifeng Liu, Bing Zhang, Zigao Dai, Feng Yuan, Shuangnan Zhang, Qingzhong Liu, Peng Jiang, Xuefeng Wu, Zheng Zheng, Jiashi Chen, Di Li, Zonghong Zhu, Zhichen Pan, Hengqian Gan, Xiao Chen, et al (1)
Jul 27 2023 astro-ph.HE astro-ph.SR arXiv:2307.14015v1

@misc{2307.14015, author = {Pengfu Tian and Ping Zhang and Wei Wang and Pei Wang and Xiaohui Sun and Jifeng Liu and Bing Zhang and Zigao Dai and Feng Yuan and Shuangnan Zhang and Qingzhong Liu and Peng Jiang and Xuefeng Wu and Zheng Zheng and Jiashi Chen and Di Li and Zonghong Zhu and Zhichen Pan and Hengqian Gan and Xiao Chen and Na Sai}, title = {{S}ub-second periodic radio oscillations in a microquasar}, year = {2023}, eprint = {2307.14015}, doi = {10.1038/s41586-023-06336-6}, note = {arXiv:2307.14015v1} }
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Powerful relativistic jets are one of the ubiquitous features of accreting black holes in all scales. GRS 1915+105 is a well-known fast-spinning black-hole X-ray binary with a relativistic jet, termed as a ``microquasar'', as indicated by its superluminal motion of radio emission. It exhibits persistent x-ray activity over the last 30 years, with quasi-periodic oscillations of $\sim 1-10$ Hz and 34 and 67 Hz in the x-ray band. These oscillations likely originate in the inner accretion disk, but other origins have been considered. Radio observations found variable light curves with quasi-periodic flares or oscillations with periods of $\sim 20-50$ minutes. Here we report two instances of $\sim$5 Hz transient periodic oscillation features from the source detected in the 1.05-1.45 GHz radio band that occurred in January 2021 and June 2022, respectively. Circular polarization was also observed during the oscillation phase.
Observing white dwarf tidal stripping with TianQin gravitational wave observatory
Chang-Qing Ye, Jin-Hong Chen, Jian-dong Zhang, Hui-Min Fan, Yi-Ming Hu
Jul 18 2023 astro-ph.HE gr-qc arXiv:2307.08231v2

@misc{2307.08231, author = {Chang-Qing Ye and Jin-Hong Chen and Jian-dong Zhang and Hui-Min Fan and Yi-Ming Hu}, title = {{O}bserving white dwarf tidal stripping with {T}ian{Q}in gravitational wave observatory}, year = {2023}, eprint = {2307.08231}, howpublished = {MNRAS,stad3296,2023}, doi = {10.1093/mnras/stad3296}, note = {arXiv:2307.08231v2} }
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Recently discovered regular X-ray bursts known as quasi-periodic eruptions have a proposed model that suggests a tidal stripping white dwarf inspiralling into the galaxy's central black hole on an eccentric orbit. According to this model, the interaction of the stripping white dwarf with the central black hole would emit gravitational wave signals as well, their detection can help explore the formation mechanism of quasi-periodic eruptions and facilitate multi-messenger observations. In this paper, we aim to perform a preliminary study of the gravitation wave observation of TianQin on this stripping white dwarf model. We investigated the horizon distance of TianQin on this type of gravitation wave signal and found it can be set to 200Mpc. We also find that those stripping white dwarf model sources with central black hole mass within $10^4\sim10^{5.5}M_\odot$ are more likely to be detected by TianQin. We assessed the parameter estimation precision of TianQin on those stripping white dwarf model sources. Our result shows that, even in the worst case, TianQin can determine the central black hole mass, the white dwarf mass, the central black hole spin, and the orbital initial eccentricity with a precision of $10^{-2}$. In the optimistic case, TianQin can determine the central black hole mass and the white dwarf mass with a precision of $10^{-7}$, determine the central black hole spin with a precision of $10^{-5}$, and determine the orbital initial eccentricity with a precision of $10^{-8}$. Moreover, TianQin can determine the luminosity distance with a precision of $10^{-1}$ and determine the sky localization with a precision of $10^{-2}\sim10$ $\rm deg^2$.
Effects of spin-orbit coupling on gravitational waveforms from a triaxial non-aligned neutron star in a binary system
Wen-Fan Feng, Tan Liu, Jie-Wen Chen, Yan Wang, Soumya D. Mohanty
Jul 04 2023 gr-qc astro-ph.HE arXiv:2307.01055v2

@misc{2307.01055, author = {Wen-Fan Feng and Tan Liu and Jie-Wen Chen and Yan Wang and Soumya D.~Mohanty}, title = {{E}ffects of spin-orbit coupling on gravitational waveforms from a triaxial non-aligned neutron star in a binary system}, year = {2023}, eprint = {2307.01055}, note = {arXiv:2307.01055v2} }
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Spinning neutron stars (NSs) can emit continuous gravitational waves (GWs) that carry a wealth of information about the compact object. If such a signal is detected, it will provide us with new insight into the physical properties of matter under extreme conditions. Future space-based GW detectors, such as LISA and TianQin, can potentially detect some double NSs in tight binaries with orbital periods shorter than 10 minutes. The possibility of a successful directed search for continuous GWs from the spinning NS in such a binary system identified by LISA/TianQin will be significantly increased with the proposed next-generation ground-based GW observatories, such as Cosmic Explorer and Einstein Telescope. Searching for continuous GWs from such a tight binary system requires highly accurate waveform templates that account for the interaction of the NS with its companion. In this spirit, we derive analytic approximations that describe the GWs emitted by a triaxial non-aligned NS in a binary system in which the effects of spin-orbit coupling have been incorporated. The difference with the widely used waveform for the isolated NS is estimated and the parameter estimation accuracy of an example signal using Cosmic Explorer is calculated. For a typical tight double NS system with a 6~min orbital period, the angular frequency correction of the spinning NS in this binary due to spin precession is $\sim 10^{-6}~{\rm Hz}$, which is in the same order of magnitude as the angular frequency of orbital precession. The fitting factor between the waveforms with and without spin precession will drop to less than 0.97 after a few days ($\sim 10^5~{\rm s}$). We find that spin-orbit coupling has the potential to improve the accuracy of parameter estimation, especially for the binary inclination angle and spin precession cone opening angle, by up to 3 orders of magnitude. (Abridged)
ALMACAL. XI. Over-densities as signposts to proto-clusters? A cautionary tale
Jianhang Chen, R. J. Ivison, Martin A. Zwaan, Anne Klitsch, Celine Peroux, Christopher C. Lovell, Claudia del P. Lagos, Andrew D. Biggs, Victoria Bollo
Jul 03 2023 astro-ph.GA arXiv:2306.17313v3

@misc{2306.17313, author = {Jianhang Chen and R.~J.~Ivison and Martin A.~Zwaan and Anne Klitsch and Celine Peroux and Christopher C.~Lovell and Claudia del P.~Lagos and Andrew D.~Biggs and Victoria Bollo}, title = {{ALMACAL}. {XI}. {O}ver-densities as signposts to proto-clusters? {A} cautionary tale}, year = {2023}, eprint = {2306.17313}, howpublished = {A&A 675, L10 (2023)}, doi = {10.1051/0004-6361/202347107}, note = {arXiv:2306.17313v3} }
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It may be unsurprising that the most common approach to finding proto-clusters is to search for over-densities of galaxies. Upgrades to submillimetre (submm) interferometers and the advent of the James Webb Space Telescope will soon offer the opportunity to find more distant candidate proto-clusters in deep sky surveys without any spectroscopic confirmation. In this letter, we report the serendipitous discovery of an extremely dense region centred on the blazar, J0217-0820, at z=0.6 in the ALMACAL sky survey. Its density is eight times higher than that predicted by blind submm surveys. Among the seven submm-bright galaxies, three are as bright as conventional single-dish submm galaxies, with S_870um > 3mJy. The over-density is thus comparable to the densest known and confirmed proto-cluster cores. However, their spectra betray a wide range of redshifts. We investigate the likelihood of line-of-sight projection effects using light cones from cosmological simulations, finding that the deeper we search, the higher the chance that we will suffer from such projection effects. The extreme over-density around J0217-0820 demonstrates the strong cosmic variance we may encounter in the deep submm surveys. Thus, we should also question the fidelity of galaxy proto-cluster candidates selected via over-densities of galaxies, where the negative K correction eases the detection of dusty galaxies along an extraordinarily extended line of sight.
Sequential Remote Brightenings and Co-spatial Fast Downflows during Two Successive Flares
B. T. Wang, X. Cheng, C. Li, J. Chen, M. D. Ding
Jun 29 2023 astro-ph.SR arXiv:2306.15991v1

@misc{2306.15991, author = {B.~T.~Wang and X.~Cheng and C.~Li and J.~Chen and M.~D.~Ding}, title = {{S}equential {R}emote {B}rightenings and {C}o-spatial {F}ast {D}ownflows during {T}wo {S}uccessive {F}lares}, year = {2023}, eprint = {2306.15991}, note = {arXiv:2306.15991v1} }
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Remote brightenings often appear at outskirts of source active regions of solar eruptive events, nevertheless, their origin remains to be ascertained. In this study, we report imaging and spectroscopic observations of sequential remote brightenings with a combination of H$\alpha$ Imaging Spectrograph (HIS) onboard the Chinese H$\alpha$ Solar Explorer (CHASE), which is the first space-based solar telescope of China, and the Solar Dynamics Observatory. It is found that, during two successive M-class flares occurring on 2022 August 17, multiple ribbon-like brightenings appeared in sequence away from the flaring active region. Meanwhile, abundant cool filament materials moved downward to the sequential remote brightenings as visible at the H$\alpha$ red wing with a line-of-sight speed up to 70 km s$^{-1}$. The extrapolated three-dimensional magnetic field configuration shows that the sequential remote brightenings correspond to the footpoints of closed ambient field lines whose conjugate footpoints are rooted in the main flare site. We suggest that the sequential remote brightenings are most likely caused by the heating of interchange reconnection between the erupting flux rope and closed ambient field, during which the rope-hosting filament materials are transferred to the periphery of flaring active region along the closed ambient field rather than to the interplanetary space like in the scenario of the slow solar wind formation.
A Model for Confined Solar Eruptions Including External Reconnection
Jun Chen, Xin Cheng, Bernhard Kliem, Mingde Ding
Jun 09 2023 astro-ph.SR physics.space-ph arXiv:2306.04993v1

@misc{2306.04993, author = {Jun Chen and Xin Cheng and Bernhard Kliem and Mingde Ding}, title = {{A} {M}odel for {C}onfined {S}olar {E}ruptions {I}ncluding {E}xternal {R}econnection}, year = {2023}, eprint = {2306.04993}, note = {arXiv:2306.04993v1} }
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The violent disruption of the coronal magnetic field is often observed to be restricted to the low corona, appearing as a confined eruption. The possible causes of the confinement remain elusive. Here, we model the eruption of a magnetic flux rope in a quadrupolar active region, with the parameters set such that magnetic X-lines exist both below and above the rope. This facilitates the onset of magnetic reconnection in either place but with partly opposing effects on the eruption. The lower reconnection initially adds poloidal flux to the rope, increasing the upward hoop force and supporting the rise of the rope. However, when the flux of the magnetic side lobes enters the lower reconnection, the flux rope is found to separate from the reconnection site and the flux accumulation ceases. At the same time, the upper reconnection begins to reduce the poloidal flux of the rope, decreasing its hoop force; eventually this cuts the rope completely. The relative weight of the two reconnection processes is varied in the model, and it is found that their combined effect and the tension force of the overlying field confine the eruption if the flux ratio of the outer to the inner polarities exceeds a threshold, which is about 1.3 for our Cartesian box and chosen parameters. We hence propose that external reconnection between an erupting flux rope and overlying flux can play a vital role in confining eruptions.
An Escaping Outflow in a Galaxy with an Intermediate-mass Black Hole
Zhiyuan Zheng, Yong Shi, Fuyan Bian, Xiaoling Yu, Junfeng Wang, Jianhang Chen, Xin Li, Qiusheng Gu
Jun 07 2023 astro-ph.GA arXiv:2306.03404v1

@misc{2306.03404, author = {Zhiyuan Zheng and Yong Shi and Fuyan Bian and Xiaoling Yu and Junfeng Wang and Jianhang Chen and Xin Li and Qiusheng Gu}, title = {{A}n {E}scaping {O}utflow in a {G}alaxy with an {I}ntermediate-mass {B}lack {H}ole}, year = {2023}, eprint = {2306.03404}, doi = {10.1093/mnras/stad1642}, note = {arXiv:2306.03404v1} }
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While in massive galaxies active galactic nuclei (AGN) feedback plays an important role, the role of AGN feedback is still under debate in dwarf galaxies. With well spatially resolved data obtained from the Multi-Unit Spectroscopic Explorer (MUSE), we identify a spatially extended ($\rm \sim 3\; kpc$) and fast ($V_{80} \sim 471\; \rm km\;s^{-1}$) AGN-driven outflow in a dwarf galaxy: SDSS J022849.51-090153.8 with $M_{*} \sim 10^{9.6}\;{\rm M_{\odot}}$ that host an intermediate-mass black hole of $M_{\rm BH} \sim 10^5\;{\rm M_{\odot}}$ and $L_{\rm AGN}/L_{\rm Edd} \sim 0.15$. Through the measurement of the rotation curve, we estimate the escape velocity of the halo and the ratio of the outflow velocity to the halo escape velocity to be $1.09\pm0.04$, indicating that the outflow is capable of escaping not only the galaxy disk but the halo. The outflow size of our AGN is found to be larger than AGN in massive galaxies at the given AGN [O III] luminosity, while the size of the photo-ionized narrow-line region is comparable. These results suggest the important role of AGN feedback through outflows in dwarf galaxies when their central intermediate-mass black holes accrete at high-Eddington ratios.
Centralised Design and Production of the Ultra-High Vacuum and Laser-Stabilisation Systems for the AION Ultra-Cold Strontium Laboratories
B. Stray, O. Ennis, S. Hedges, S. Dey, M. Langlois, K. Bongs, S. Lellouch, M. Holynski, B. Bostwick, J. Chen, Z. Eyler, V. Gibson, T. L. Harte, M. Hsu, M. Karzazi, J. Mitchell, N. Mouelle, U. Schneider, Y. Tang, K. Tkalcec, et al (52)
Jun 01 2023 physics.atom-ph astro-ph.IM hep-ex physics.ins-det quant-ph arXiv:2305.20060v1

@misc{2305.20060, author = {B.~Stray and O.~Ennis and S.~Hedges and S.~Dey and M.~Langlois and K.~Bongs and S.~Lellouch and M.~Holynski and B.~Bostwick and J.~Chen and Z.~Eyler and V.~Gibson and T.~L.~Harte and M.~Hsu and M.~Karzazi and J.~Mitchell and N.~Mouelle and U.~Schneider and Y.~Tang and K.~Tkalcec and Y.~Zhi and K.~Clarke and A.~Vick and K.~Bridges and J.~Coleman and G.~Elertas and L.~Hawkins and S.~Hindley and K.~Hussain and C.~Metelko and H.~Throssell and C.~F.~A.~Baynham and O.~Buchmuller and D.~Evans and R.~Hobson and L.~Iannizzotto-Venezze and A.~Josset and E.~Pasatembou and B.~E.~Sauer and M.~R.~Tarbutt and L Badurina and A.~Beniwal and D.~Blas and J.~Carlton and J.~Ellis and C.~McCabe and E.~Bentine and M.~Booth and D.~Bortoletto and C.~Foot and C.~Gomez and T.~Hird and K.~Hughes and A.~James and A.~Lowe and J.~March-Russell and J.~Schelfhout and I.~Shipsey and D.~Weatherill and D.~Wood and S.~Balashov and M.~G.~Bason and J.~Boehm and M.~Courthold and M.~van der Grinten and P.~Majewski and A.~L.~Marchant and D.~Newbold and Z.~Pan and Z.~Tam and T.~Valenzuela and I.~Wilmut}, title = {{C}entralised {D}esign and {P}roduction of the {U}ltra-{H}igh {V}acuum and {L}aser-{S}tabilisation {S}ystems for the {AION} {U}ltra-{C}old {S}trontium {L}aboratories}, year = {2023}, eprint = {2305.20060}, note = {arXiv:2305.20060v1} }
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This paper outlines the centralised design and production of the Ultra-High-Vacuum sidearm and Laser-Stabilisation systems for the AION Ultra-Cold Strontium Laboratories. Commissioning data on the residual gas and steady-state pressures in the sidearm chambers, on magnetic field quality, on laser stabilisation, and on the loading rate for the 3D Magneto-Optical Trap are presented. Streamlining the design and production of the sidearm and laser stabilisation systems enabled the AION Collaboration to build and equip in parallel five state-of-the-art Ultra-Cold Strontium Laboratories within 24 months by leveraging key expertise in the collaboration. This approach could serve as a model for the development and construction of other cold atom experiments, such as atomic clock experiments and neutral atom quantum computing systems, by establishing dedicated design and production units at national laboratories.
Asteroseismic investigation on KIC 10526294 to probe convective core overshoot mixing
Qian-Sheng Zhang, Li Yan, Wu Tao, Jiang Chen
May 29 2023 astro-ph.SR arXiv:2305.16721v1

@misc{2305.16721, author = {Qian-Sheng Zhang and Li Yan and Wu Tao and Jiang Chen}, title = {{A}steroseismic investigation on {KIC} 10526294 to probe convective core overshoot mixing}, year = {2023}, eprint = {2305.16721}, note = {arXiv:2305.16721v1} }
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In the overshoot mixing model with an exponentially decreasing diffusion coefficient, the initial value of the diffusion coefficient plays a crucial role. According to the turbulent convective mixing model, the characteristic length of convection in the convection zone differs from that in the overshoot region, resulting in a rapid decrease of the diffusion coefficient near the convective boundary. To investigate this quick decrease, we conducted an asteroseismic study on the intermediate-mass SPB star KIC 10526294. We generated stellar models with varied input parameters, including the overshoot parameters, and compared the resulting stellar oscillation periods with observations. To mitigate the potential issue arising from large steps in the stellar parameters and stellar age, we employed a comprehensive interpolation scheme for the stellar oscillatory frequencies, considering all stellar parameters and stellar age. Our analysis revealed that the quick decreasing of the diffusion coefficient has discernible effects on the stellar oscillations and a quick decrease with 4 magnitude orders shows the best oscillatory frequencies compared with the observations. This provides weak evidence in support of the prediction made by the turbulent convective mixing model. Furthermore, we examined the residuals of the oscillation periods and discovered a potential association between abundance anomalies in the buoyancy frequency profile and the oscillation-like patterns observed in the residuals.
S-type stars from LAMOST DR10: classification of intrinsic and extrinsic stars
Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
May 17 2023 astro-ph.SR astro-ph.GA arXiv:2305.09294v1

@misc{2305.09294, author = {Jing Chen and Yin-Bi Li and A-Li Luo and Xiao-Xiao Ma and Shuo Li}, title = {{S}-type stars from {LAMOST} {DR}10: classification of intrinsic and extrinsic stars}, year = {2023}, eprint = {2305.09294}, note = {arXiv:2305.09294v1} }
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In this paper, we found 2939 S-type stars from LAMOST Data Release 10 using two machine-learning methods, and 2306 of them were reported for the first time. The main purpose of this work is to study how to divide S-type stars into intrinsic and extrinsic stars with photometric data and LAMOST spectra. Using infrared photometric data, we adopted two methods to distinguish S-type stars, i.e., XGBoost algorithm and color-color diagrams. We trained XGBoost model with 15 input features consisting of colors and absolute magnitudes of Two Micron All Sky Survey (2MASS), AllWISE, AKARI, and IRAS, and found that the model trained by input features with 2MASS, AKARI, and IRAS data has the highest accuracy of 95.52%. Furthermore, using this XGBoost model, we found four color-color diagrams with six infrared color criteria to divide S-type stars, which has an accuracy of about 90%. Applying the two methods to the 2939 S-type stars, 381 (XGBoost)/336 (color-color diagrams) intrinsic and 495 (XGBoost)/82 (color-color diagrams) extrinsic stars were classified, respectively. Using these photometrically classified intrinsic and extrinsic stars, we retrained XGBoost model with their blue and red medium-resolution spectra, and the 2939 stars were divided into 855 intrinsic and 2056 extrinsic stars from spectra with an accuracy of 94.82%. In addition, we also found four spectral regions of Zr I (6451.6A), Ne II (6539.6A), H\alpha (6564.5A), and Fe I (6609.1A) and C I (6611.4A) are the most important features, which can reach an accuracy of 92.1% when using them to classify S-type stars.
SN 2016ije: An SN 2002es-like Type Ia Supernova Exploded in a Metal-poor and Low-surface Brightness Galaxy
Zhitong Li, Tianmeng Zhang, Xiaofeng Wang, Jujia Zhang, Lluís Galbany, Alexei V. Filippenko, Thomas G. Brink, Chris Ashall, WeiKang Zheng, Thomas de Jaeger, Fabio Ragosta, Maxime Deckers, Mariusz Gromadzki, D. R. Young, Gaobo Xi, Juncheng Chen, Xulin Zhao, Hanna Sai, Shengyu Yan, Danfeng Xiang, et al (11)
May 17 2023 astro-ph.HE astro-ph.SR arXiv:2305.09417v2

@misc{2305.09417, author = {Zhitong Li and Tianmeng Zhang and Xiaofeng Wang and Jujia Zhang and Lluís Galbany and Alexei V.~Filippenko and Thomas G.~Brink and Chris Ashall and WeiKang Zheng and Thomas de Jaeger and Fabio Ragosta and Maxime Deckers and Mariusz Gromadzki and D.~R.~Young and Gaobo Xi and Juncheng Chen and Xulin Zhao and Hanna Sai and Shengyu Yan and Danfeng Xiang and Zhihao Chen and Wenxiong Li and Bo Wang and Hu Zou and Jipeng Sui and Jiali Wang and Jun Ma and Jundan Nie and Suijian Xue and Xu Zhou and Zhimin Zhou}, title = {{SN} 2016ije: {A}n {SN} 2002es-like {T}ype {I}a {S}upernova {E}xploded in a {M}etal-poor and {L}ow-surface {B}rightness {G}alaxy}, year = {2023}, eprint = {2305.09417}, note = {arXiv:2305.09417v2} }
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We have conducted photometric and spectroscopic observations of the peculiar Type Ia supernova (SN Ia) 2016ije that was discovered through the Tsinghua-NAOC Transient Survey. This peculiar object exploded in the outskirts of a metal-poor, low-surface brightness galaxy (i.e., $M_{g}$ = $-$14.5 mag). Our photometric analysis reveals that SN 2016ije is subluminous ($M_{B,\rm{max}}$ = $-$17.65$\pm$0.06 mag) but exhibits relatively broad light curves (${\Delta}m_{15}(B)$ = 1.35$\pm$0.14 mag), similar to the behavior of SN 2002es. Our analysis of the bolometric light curve indicates that only 0.14$\pm$0.04 $M_{\odot}$ of $^{56}$Ni was synthesized in the explosion of SN 2016ije, which suggests a less energetic thermonuclear explosion when compared to normal SNe Ia, and this left a considerable amount of unburned materials in the ejecta. Spectroscopically, SN 2016ije resembles other SN 2002es-like SNe Ia, except that the ejecta velocity inferred from its carbon absorption line ($\sim$ 4500 km s$^{-1}$) is much lower than that from silicon lines ($\sim$ 8300 km s$^{-1}$) at around the maximum light. Additionally, most of the absorption lines are broader than other 02es-like SNe Ia. These peculiarities suggest the presence of significant unburned carbon in the inner region and a wide line-forming region along the line of sight. These characteristics suggest that SN 2016ije might originate from the violent merger of a white dwarf binary system, when viewed near an orientation along the iron-group-element cavity caused by the companion star.
Coronal Heating as Determined by the Solar Flare Frequency Distribution Obtained by Aggregating Case Studies
James Paul Mason, Alexandra Werth, Colin G. West, Allison A. Youngblood, Donald L. Woodraska, Courtney Peck, Kevin Lacjak, Florian G. Frick, Moutamen Gabir, Reema A. Alsinan, Thomas Jacobsen, Mohammad Alrubaie, Kayla M. Chizmar, Benjamin P. Lau, Lizbeth Montoya Dominguez, David Price, Dylan R. Butler, Connor J. Biron, Nikita Feoktistov, Kai Dewey, et al (982)
May 11 2023 astro-ph.SR arXiv:2305.05687v1

@misc{2305.05687, author = {James Paul Mason and Alexandra Werth and Colin G.~West and Allison A.~Youngblood and Donald L.~Woodraska and Courtney Peck and Kevin Lacjak and Florian G.~Frick and Moutamen Gabir and Reema A.~Alsinan and Thomas Jacobsen and Mohammad Alrubaie and Kayla M.~Chizmar and Benjamin P.~Lau and Lizbeth Montoya Dominguez and David Price and Dylan R.~Butler and Connor J.~Biron and Nikita Feoktistov and Kai Dewey and N.~E.~Loomis and Michal Bodzianowski and Connor Kuybus and Henry Dietrick and Aubrey M.~Wolfe and Matt Guerrero and Jessica Vinson and Peter Starbuck and Shelby D Litton and M.~G.~Beck and Jean-Paul Fisch and Ayana West and Alexis A.~Muniz and Luis Chavez and Zachary T.~Upthegrove and Brenton M.~Runyon and J.~Salazar and Jake E.~Kritzberg and Tyler Murrel and Ella Ho and Quintin Y.~LaFemina and Sara I.~Elbashir and Ethan C.~Chang and Zachary A.~Hudson and Rosemary O.~Nussbaum and Kellen Kennedy and Kevin Kim and Camila Villamil Arango and Mohammed A.~Albakr and Michael Rotter and A.~J.~Garscadden and Antonio Salcido-Alcontar JR and Harrison M.~Pearl and Tyler Stepaniak and Josie A.~Marquez and Lauren Marsh and Jesse C Andringa and Austin Osogwin and Amanda M.~Shields and Sarah Brookins and Grace K.~Hach and Alexis R.~Clausi and Emily B.~Millican and Alan A Jaimes and Alaina S.~Graham and John J.~Burritt and J.~S.~Perez and Nathaniel Ramirez and Rohan Suri and Michael S.~Myer and Zoe M.~Kresek and C.~A.~Goldsberry and Genevieve K.~Payne and Tara Jourabchi and J.~Hu and Jeffrey Lucca and Zitian Feng and Connor B.~Gilpatrick and Ibraheem A.~Khan and Keenan Warble and Joshua D.~Sweeney and Philip Dorricott and Ethan Meyer and Yash S.~Kothamdi and Arman S.~Sohail and Kristyn Grell and Aidan Floyd and Titus Bard and Randi M.~Mathieson and Joseph Reed and Alexis Cisneros and Matthew P.~Payne and J.~R.~Jarriel and Jacqueline Rodriguez Mora and M.~E.~Sundell and Kajal Patel and Mohammad Alesmail and Yousef A Alnasrallah and Jumana T.~Abdullah and Luis Molina-Saenz and K.~E.~Tayman and Gabriel T.~Brown and Liana Kerr-Layton and Zachary D.~Berriman-Rozen and Quinn Hiatt and Etash Kalra and Jason Ong and Shreenija Vadayar and Callie D.~Shannahan and Evan Benke and Jinhua zhang and Jane Geisman and Cara Martyr and Federico Ameijenda and Ushmi H.~Akruwala and Molly Nehring and Natalie Kissner and Ian C.~Rule and Tyler Learned and Alexandra N.~Smith and Liam Mazzotta and Tyndall Rounsefell and Elizabeth A.~Eyeson and Arlee K.~Shelby and Tyler S Moll and Riley Menke and Hannan Shahba and Tony A.~House Jr.~and David B.~Clark and Annemarie C.~Burns and Tristan de La Beaujardiere and Emily D.~Trautwein and Will Plantz and Justin Reeves and Ian Faber and B.~W.~Buxton and Nigel Highhouse and Kalin Landrey and Connor M Hansen and Kevin Chen and Ryder Buchanan Hales and Luke R.~Borgerding and Mutian Guo and Christian J.~Crow and Lloyd C.~Whittall and Conor Simmons and Adeduni Folarin and Evan J.~Parkinson and Anna L.~Rahn and Olivia Blevins and Annalise M.~Morelock and Nicholas Kelly and Nathan L.~Parker and Kelly Smith and Audrey E.~Plzak and David Saeb and Cameron T.~Hares and Sasha R.~Parker and Andrew McCoy and Alexander V.~Pham and Megan Lauzon and Cayla J.~Kennedy and Andrea B.~Reyna and Daniela M.~Meza Acosta and Destiny J.~Cool and Sheen L.~Steinbarth and Patricia Mendoza-Anselmi and Kaitlyn E.~Plutt and Isabel M Kipp and M.~Rakhmonova and Cameron L.~Brown and Gabreece Van Anne and Alexander P.~Moss and Olivia Golden and Hunter B.~Kirkpatrick and Jake R.~Colleran and Brandon J Sullivan and Kevin Tran and Michael Andrew Carpender and Aria T.~Mundy and Greta Koenig and Jessica Oudakker and Rasce Engelhardt and Nolan Ales and Ethan Benjamin Wexler and Quinn I Beato and Lily Chen and Brooke Cochran and Paula Hill and Sean R.~Hamilton and Kyle Hashiro and Usman Khan and Alexa M.~Martinez and Jennifer L.~Brockman and Macguire Mallory and Charlie Reed and Richard Terrile and Savi Singh and James Adam Watson and Joshua B.~Creany and Nicholas K.~Price and Aya M.~Miften and Bryn Tran and Margaret Kamenetskiy and Jose R.~Martinez and Elena N.~Opp and Jianyang Huang and Avery M.~Fails and Brennan J.~Belei and Ryan Slocum and Justin Astalos and Andrew East and Lena P.~Nguyen and Callie C Pherigo and Andrew N.~East and David Y.~Li and Maya LI Nelson and Nicole Taylor and Anand Odbayar and Anna Linnea Rives and Kabir P.~Mathur and Jacob Billingsley and Hyden Polikoff and Michael Driscoll and Orion K.~Wilson and Kyle Lahmers and Nathaniel J.~Toon and Sam Lippincott and Andrew J.~Musgrave and Alannah H.~Gregory and Sedique Pitsuean-Meier and Trevor Jesse and Corey Smith and Ethan J.~Miles and Sabrina J.~H.~T.~Kainz and Soo Yeun Ji and Lena Nguyen and Maryam Aryan and Alexis M.~Dinser and Jadon Shortman and Catalina S Bastias and Thomas D Umbricht and Breonna Cage and Parker Randolph and Matthew Pollard and Dylan M.~Simone and Andrew Aramians and Ariana E.~Brecl and Amanda M.~Robert and Thomas Zenner and Maxwell Saldi and Gavin Morales and Citlali Mendez and Konner Syed and Connor Maklain Vogel and Rebecca A.~Cone and Naomi Berhanu and Emily Carpenter and Cecilia Leoni and Samuel Bryan and Nidhi Ramachandra and Timothy Shaw and E.~C.~Lee and Eli Monyek and Aidan B.~Wegner and Shajesh Sharma and Barrett Lister and Jamison R.~White and John S.~Willard and S.~A Sulaiman and Guillermo Blandon and Anoothi Narayan and Ryan Ruger and Morgan A.~Kelley and Angel J.~Moreno and Leo M Balcer and N.~R.~D.~Ward-Chene and Emma Shelby and Brian D.~Reagan and Toni Marsh and Sucheta Sarkar and Michael P.~Kelley and Kevin Fell and Sahana Balaji and Annalise K.~Hildebrand and Dominick Shoha and Kshmya Nandu and Julia Tucker and Alejandro R.~Cancio and Jiawei Wang and Sarah Grace Rapaport and Aimee S.~Maravi and Victoria A.~Mayer and Andrew Miller and Caden Bence and Emily Koke and John T Fauntleroy and Timothy Doermer and Adel Al-Ghazwi and Remy Morgan and Mohammed S.~Alahmed and Adam Izz Khan Mohd Reduan Mathavan and H.~K.~Silvester and Amanda M.~Weiner and Nianzi Liu and Taro Iovan and Alexander V.~Jensen and Yazeed A.~AlHarbi and Yufan Jiang and Jiaqi Zhang and Olivia M.~Jones and Chenqi Huang and Eileen N.~Reh and Dania Alhamli and Joshua Pettine and Chongrui Zhou and Dylan Kriegman and Jianing Yang and Kevin Ash and Carl Savage and Emily Kaiser and Dakota N.~Augenstein and Jacqueline Padilla and Ethan K.~Stark and Joshua A.~Hansen and Thomas Kokes and Leslie Huynh and Gustavo Sanchez-Sanchez and Luke A.~Jeseritz and Emma L.~Carillion and Aditya V.~Vepa and Sapriya Khanal and Braden Behr and Logan S.~Martin and Jesse J.~McMullan and Tianwei Zhao and Abigail K.~Williams and Emeen Alqabani and Gale H.~Prinster and Linda Horne and Kendall Ruggles-Delgado and Grant Otto and Angel R.~Gomez and Leonardo Nguyen and Preston J.~Brumley and Nancy Ortiz Venegas and Ilian Varela and Jordi Brownlow and Avril Cruz and Linzhi Leiker and Jasleen Batra and Abigail P.~Hutabarat and Dario Nunes-Valdes and Connor Jameson and Abdulaziz Naqi and Dante Q.~Adams and Blaine B.~Biediger and William T Borelli and Nicholas A.~Cisne and Nathaniel A.~Collins and Tyler L.~Curnow and Sean Gopalakrishnan and Nicholas F.~Griffin and Emanuel Herrera and Meaghan V.~McGarvey and Sarah Mellett and Igor Overchuk and Nathan Shaver and Cooper N.~Stratmeyer and Marcus T.~Vess and Parker Juels and Saleh A.~Alyami and Skylar Gale and Steven P.~Wallace and Samuel C Hunter and Mia C.~Lonergan and Trey Stewart and Tiffany E.~Maksimuk and Antonia Lam and Judah Tressler and Elena R.~Napoletano and Joshua B.~Miller and Marc G.~Roy and Jasey Chanders and Emmalee Fischer and A.~J.~Croteau and Nicolas A.~Kuiper and Alex Hoffman and Elyse DeBarros and Riley T.~Curry and A.~Brzostowicz and Jonas Courtney and Tiannie Zhao and Emi Szabo and Bandar Abu Ghaith and Colin Slyne and Lily Beck and Oliver Quinonez and Sarah Collins and Claire A.~Madonna and Cora Morency and Mallory Palizzi and Tim Herwig and Jacob N.~Beauprez and Dorsa Ghiassi and Caroline R.~Doran and Zhanchao Yang and Hannah M.~Padgette and Cyrus A.~Dicken and Bryce W.~Austin and Ethan J.~Phalen and Catherine Xiao and Adler Palos and Phillip Gerhardstein and Ava L.~Altenbern and Dan Orbidan and Jackson A.~Dorr and Guillermo A.~Rivas and Calvin A Ewing and B.~C.~Giebner and Kelleen McEntee and Emily R.~Kite and K.~A.~Crocker and Mark S.~Haley and Adrienne R.~Lezak and Ella McQuaid and Jacob Jeong and Jonathan Albaum and E.~M.~Hrudka and Owen T.~Mulcahy and Nolan C.~Tanguma and Sean Oishi-Holder and Zachary White and Ryan W.~Coe and Christine Boyer and Mitchell G.~Chapman and Elise Fortino and Jose A.~Salgado and Tim Hellweg and Hazelia K.~Martinez and Alexander J.~Mitchell and Stephanie H.~Schubert and Grace K Schumacher and Corey D Tesdahl and C.~H.~Uphoff and Alexandr Vassilyev and Briahn Witkoff and Jackson R.~Wolle and Kenzie A.~Dice and Timothy A.~Behrer and Troy Bowen and Andrew J Campbell and Peter C Clarkson and Tien Q.~Duong and Elijah Hawat and Christian Lopez and Nathaniel P.~Olson and Matthew Osborn and Munisettha E.~Peou and Nicholas J.~Vaver and Troy Husted and Nicolas Ian Kallemeyn and Ava A Spangler and Kyle Mccurry and Courtney Schultze and Thomas Troisi and Daniel Thomas and Althea E.~Ort and Maya A.~Singh and Caitlin Soon and Catherine Patton and Jayce A.~Billman and Sam Jarvis and Travis Hitt and Mirna Masri and Yusef J.~Albalushi and Matthew J Schofer and Katherine B.~Linnane and Philip Whiting Knott and Whitney Valencia and Brian A.~Arias-Robles and Diana Ryder and Anna Simone and Jonathan M.~Abrams and Annelene L.~Belknap and Charlotte Rouse and Alexander Reynolds and Romeo S.L.~Petric and Angel A.~Gomez and Jonah B.~Meiselman-Ashen and Luke Carey and John S.~Dias and Jules Fischer-White and Aidan E.~Forbes and Gabriela Galarraga and Forrest Kennedy and Rian Lawlor and Maxwell J.~Murphy and Cooper Norris and Josh Quarderer and Caroline Waller and Robert J.~Weber and Nicole Gunderson and Tom Boyne and Joshua A.~Gregory and Henry Austin Propper and Charles B.~Beck von Peccoz and Donovan Branch and Evelyn Clarke and Libby Cutler and Frederick M.~Dabberdt and Swagatam Das and John Alfred D.~Figueirinhas and Benjamin L.~Fougere and Zoe A.~Roy and Noah Y.~Zhao and Corben L.~Cox and Logan D.~W.~Barnhart and Wilmsen B.~Craig and Hayden Moll and Kyle Pohle and Alexander Mueller and Elena K.~Smith and Benjamin C.~Spicer and Matthew C.~Aycock and Batchimeg Bat-Ulzii and Madalyn C.~Murphy and Abdullah Altokhais and Noah R.~Thornally and Olivia R.~Kleinhaus and Darian Sarfaraz and Grant M.~Barnes and Sara Beard and David J Banda and Emma A.~B.~Davis and Tyler J.~Huebsch and Michaela Wagoner and Justus Griego and Jack J.~Mc Hale and Trevor J.~Porter and Riley Abrashoff and Denise M.~Phan and Samantha M.~Smith and Ashish Srivastava and Jared A.~W.~Schlenker and Kasey O.~Madsen and Anna E.~Hirschmann and Frederick C Rankin and Zainab A.~Akbar and Ethan Blouin and Aislinn Coleman-Plante and Evan Hintsa and Emily Lookhoff and Hamzi Amer and Tianyue Deng and Peter Dvorak and Josh Minimo and William C.~Plummer and Kelly Ton and Lincoln Solt and Batool H.~AlAbbas and Areej A.~AlAwadhi and Nicholas M.~Cooper and Jessica S Corbitt and Christian Dunlap and Owen Johnson and Ryan A.~Malone and Yesica Tellez and Logan Wallace and Michael-Tan D.~Ta and Nicola H.~Wheeler and Ariana C.~Ramirez and Shancheng Huang and Amar Mehidic and Katherine E Christiansen and Om Desai and Emerson N.~Domke and Noah H.~Howell and Martin Allsbrook and Teeb Alnaji and Colin England and Nathan Siles and Nicholas David Burton and Zoe Cruse and Dalton Gilmartin and Brian T.~Kim and Elsie Hattendorf and Maryam Buhamad and Lily Gayou and Kasper Seglem and Tameem Alkhezzi and Imari R.~Hicks and Ryann Fife and Lily M.~Pelster and Alexander Fix and Sohan N.~Sur and Joshua K.~Truong and Bartlomiej Kubiak and Matthew Bondar and Kyle Z.~Shi and Julia Johnston and Andres B.~Acevedo and Junwon Lee and William J.~Solorio and Braedon Y.~Johnston and Tyler McCormick and Nicholas Olguin and Paige J.~Pastor and Evan M.~Wilson and Benjamin L.~Trunko and Chris Sjoroos and Kalvyn N Adams and Aislyn Bell and Grant Brumage-Heller and Braden P.~Canales and Bradyn Chiles and Kailer H.~Driscoll and Hallie Hill and Samuel A.~Isert and Marilyn Ketterer and Matthew M.~Kim and William J.~Mewhirter and Lance Phillips and Krista Phommatha and Megan S.~Quinn and Brooklyn J.~Reddy and Matthew Rippel and Bowman Russell and Sajan Williams and Andrew M.~Pixley and Keala C.~Gapin and B.~Peterson and Collin Ruprecht and Isabelle Hardie and Isaac Li and Abbey Erickson and Clint Gersabeck and Mariam Gopalani and Nasser Allanqawi and Taylor Burton and Jackson R.~Cahn and Reese Conti and Oliver S.~White and Stewart Rojec and Blake A.~Hogen and Jason R.~Swartz and R.~Dick and Lexi Battist and Gabrielle M.~Dunn and Rachel Gasser and Timothy W.~Logan and Madeline Sinkovic and Marcus T.~Schaller and Danielle A.~Heintz and Andrew Enrich and Ethan S.~Sanchez and Freddy Perez and Fernando Flores and Shaun D.~Kapla and Michael C.~Shockley and Justin Phillips and Madigan Rumley and Johnston Daboub and Brennan J.~Karsh and Bridget Linders and Sam Chen and Helen C.~Do and Abhinav Avula and James M.~French and Chrisanna Bertuccio and Tyler Hand and Adrianna J.~Lee and Brenna K Neeland and Violeta Salazar and Carter Andrew and Abby Barmore and Thomas Beatty and Nicholas Alonzi and Ryan Brown and Olivia M.~Chandler and Curran Collier and Hayden Current and Megan E.~Delasantos and Alberto Espinosa de los Monteros Bonilla and Alexandra A.~Fowler and Julianne R.~Geneser and Eleanor Gentry and E.~R.~Gustavsson and Jonathan Hansson and Tony Yunfei Hao and Robert N.~Herrington and James Kelly and Teagan Kelly and Abigail Kennedy and Mathew J.~Marquez and Stella Meillon and Madeleine L.~Palmgren and Anneliese Pesce and Anurag Ranjan and Samuel M.~Robertson and Percy Smith and Trevor J Smith and Daniel A.~Soby and Grant L.~Stratton and Quinn N.~Thielmann and Malena C.Toups and Jenna S.~Veta and Trenton J.~Young and Blake Maly and Xander R.~Manzanares and Joshua Beijer and Jacob D.~George and Dylan P.~Mills and Josh J Ziebold and Paige Chambers and Michael Montoya and Nathan M.Cheang and Hunter J.~Anderson and Sheridan J.~Duncan and Lauren Ehrlich and Nathan C.~Hudson and Jack L.~Kiechlin and Will Koch and Justin Lee and Dominic Menassa and S.~H.~Oakes and Audrey J.~Petersen and J.~R.~Ramirez Bunsow and Joshua Bay and Sacha Ramirez and Logan D.~Fenwick and Aidan P.~Boyle and Lea Pearl Hibbard and Calder Haubrich and Daniel P.~Sherry and Josh Jenkins and Sebastian Furney and Anjali A.~Velamala and Davis J.~Krueger and William N.~Thompson and Jenisha Chhetri and Alexis Ying-Shan Lee and Mia G.~V.~Ray and John C.~Recchia and Dylan Lengerich and Kyle Taulman and Andres C.~Romero and Ellie N.~Steward and Sloan Russell and Dillon F.~Hardwick and Katelynn Wootten and Valerie A.~Nguyen and Devon Quispe and Cameron Ragsdale and Isabel Young and N.~S.~Atchley-Rivers and Jordin L.~Stribling and Julia G Gentile and Taylor A.~Boeyink and Daniel Kwiatkowski and Tomi Oshima Dupeyron and Anastasia Crews and Mitchell Shuttleworth and Danielle C.~Dresdner and Lydia Flackett and Nicholas Haratsaris and Morgan I Linger and Jay H.~Misener and Samuel Patti and Tawanchai P.~Pine and Nasreen Marikar and Giorgio Matessi and Allie C.~Routledge and Suhail Alkaabi and Jessica L.~Bartman and Gabrielle E.~Bisacca and Celeste Busch and Bree Edwards and Caitlyn Staudenmier and Travis Starling and Caden McVey and Maximus Montano and Charles J.~Contizano and Eleanor Taylor and James K.~McIntyre and Andrew Victory and Glen S.~McCammon and Aspen Kimlicko and Tucker Sheldrake and Grace Shelchuk and Ferin J.~Von Reich and Andrew J.~Hicks and Ian O'neill and Beth Rossman and Liam C.~Taylor and William MacDonald and Simone E.~Becker and Soonhee Han and Cian O'Sullivan and Isaac Wilcove and David J.~Brennan and Luke C.~Hanley and Owen Hull and Timothy R.~Wilson and Madison H.~Kalmus and Owen A.~Berv and Logan Swous Harris and Chris H Doan and Nathan Londres and Anish Parulekar and Megan M.~Adam and Abigail Angwin and Carter C.~Cabbage and Zachary Colleran and Alex Pietras and Octave Seux and Ryan Oros and Blake C.~Wilkinson and Khoa D Nguyen and Maedee Trank-Greene and Kevin M.~Barone and G.~L.~Snyder and Samuel J Biehle and Brennen Billig and Justin Thomas Almquist and Alyssa M.~Dixon and Benjamin Erickson and Nathan Evans and SL Genne and Christopher M Kelly and Serafima M.~Marcus and Caleb Ogle and Akhil Patel and Evan Vendetti and Olivia Courtney and Sean Deel and Leonardo Del Foco and Michael Gjini and Jessica Haines and Isabelle J.~Hoff and M.~R.~Jones and Dominic Killian and Kirsten Kuehl and Chrisanne Kuester and Maxwell B.~Lantz and Christian J Lee and Graham Mauer and Finbar K.~McKemey and Sarah J.~Millican and Ryan Rosasco and T.~C.~Stewart and Eleanor VanEtten and Zachary Derwin and Lauren Serio and Molly G.~Sickler and Cassidy A.~Blake and Neil S.~Patel and Margaret Fox and Michael J Gray and Lucas J.~Ziegler and Aman Priyadarshi Kumar and Madelyn Polly and Sarah Mesgina and Zane McMorris and Kyle J.~Griffin and L.~N.~Haile and Claire Bassel and Thomas J.~Dixon and Ryan Beattie and Timothy J Houck and Maeve Rodgers and Tyson R.~Trofino and Dax Lukianow and Korben Smart and Jacqueline L.~Hall and Lauren Bone and James O.~Baldwin and Connor Doane and Yousef A.~Almohsen and Emily Stamos and Iker Acha and Jake Kim and Antonio E.~Samour II and S.~Chavali and Jeerakit Kanokthippayakun and Nicholas Gotlib and Ryan C.~Murphy and Jack.~W.~Archibald and Alexander J Brimhall and Aidan Boyer and Logan T.~Chapman and Shivank Chadda and Lisa Sibrell and Mia M.~Vallery and Thomas C.~Conroy and Luke J.~Pan and Brian Balajonda and Bethany E.~S.~Fuhrman and Mohamed Alkubaisi and Jacob Engelstad and Joshua Dodrill and Calvin R.~Fuchs and Gigi Bullard-Connor and Isehaq Alhuseini and James C.~Zygmunt and Leo Sipowicz and Griffin A.~Hayrynen and Riley M.~McGill and Caden J.~Keating and Omer Hart and Aidan St.~Cyr and Christopher H.~Steinsberger and Gerig Thoman and Travis M.~Wood and Julia A.~Ingram and J.~Dominguez and Nathaniel James Georgiades and Matthew Johnson and Sawyer Johnson and Alexander J.~Pedersen and Anoush K Ralapanawe and Jeffrey J.~Thomas and Ginn A.~Sato and Hope Reynolds and Liebe Nasser and Alexander Z.~Mizzi and Olivia Damgaard and Abdulrahman A.~Baflah and Steven Y.~Liu and Adam D.~Salindeho and Kelso Norden and Emily E.~Gearhart and Zack Krajnak and Philip Szeremeta and Meggan Amos and Kyungeun Shin and Brandon A.~Muckenthaler and Melissa Medialdea and Simone Beach and Connor B.~Wilson and Elena R Adams and Ahmed Aldhamen and Coyle M.~Harris and Troy M.~Hesse and Nathan T.~Golding and Zachary Larter and Angel Hernandez and Genaro Morales and Robert B.~Traxler and Meshal Alosaimi and Aidan F.~Fitton and James Holland Aaron and Nathaniel F.~Lee and Ryan Z.~Liao and Judy Chen and Katherine V.~French and Justin Loring and Aurora Colter and Rowan McConvey and Michael Colozzi and John D.~Vann and Benjamin T.~Scheck and Anthony A Weigand and Abdulelah Alhabeeb and Yolande Idoine and Aiden L.~Woodard and Mateo M.~Medellin and Nicholas O Ratajczyk and Darien P.~Tobin and Jack C.~Collins and Thomas M.~Horning and Nick Pellatz and John Pitten and Noah Lordi and Alyx Patterson and Thi D Hoang and Ingrid H Zimmermann and Hongda Wang and Daniel Steckhahn and Arvind J.~Aradhya and Kristin A.~Oliver and Yijian Cai and Chaoran Wang and Nikolay Yegovtsev and Mengyu Wu and Koushik Ganesan and Andrew Osborne and Evan Wickenden and Josephine C.~Meyer and David Chaparro and Aseem Visal and Haixin Liu and Thanmay S.~Menon and Yan Jin and John Wilson and James W.~Erikson and Zheng Luo and Nanako Shitara and Emma E Nelson and T.~R.~Geerdts and Jorge L Ramirez Ortiz and H.~J.~Lewandowski}, title = {{C}oronal {H}eating as {D}etermined by the {S}olar {F}lare {F}requency {D}istribution {O}btained by {A}ggregating {C}ase {S}tudies}, year = {2023}, eprint = {2305.05687}, doi = {10.3847/1538-4357/accc89}, note = {arXiv:2305.05687v1} }
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Flare frequency distributions represent a key approach to addressing one of the largest problems in solar and stellar physics: determining the mechanism that counter-intuitively heats coronae to temperatures that are orders of magnitude hotter than the corresponding photospheres. It is widely accepted that the magnetic field is responsible for the heating, but there are two competing mechanisms that could explain it: nanoflares or Alfvén waves. To date, neither can be directly observed. Nanoflares are, by definition, extremely small, but their aggregate energy release could represent a substantial heating mechanism, presuming they are sufficiently abundant. One way to test this presumption is via the flare frequency distribution, which describes how often flares of various energies occur. If the slope of the power law fitting the flare frequency distribution is above a critical threshold, $\alpha=2$ as established in prior literature, then there should be a sufficient abundance of nanoflares to explain coronal heating. We performed $>$600 case studies of solar flares, made possible by an unprecedented number of data analysts via three semesters of an undergraduate physics laboratory course. This allowed us to include two crucial, but nontrivial, analysis methods: pre-flare baseline subtraction and computation of the flare energy, which requires determining flare start and stop times. We aggregated the results of these analyses into a statistical study to determine that $\alpha = 1.63 \pm 0.03$. This is below the critical threshold, suggesting that Alfvén waves are an important driver of coronal heating.