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The EXTRA-BL4S experiment for the measurement of the energy and angular distributions of transition radiation X-rays
M. N. Mazziotta, F. Loparco, A. Anelli, M. M. Belviso, A. Buquicchio, E. V. Cassano, M. De Cosmo, P. Ginefra, M. L. Martulli, C. Picci, D. Picicci, R. D. Soriano, A. P. Tatulli, G. Tripaldella, V. M. Zupo, M. F. Muscarella, S. Turbacci, M. Boselli, C. B. da Cruz E Silva, M. Joos, et al (1)
Jan 27 2023 hep-ex physics.ins-det arXiv:2301.11247v2

@misc{2301.11247, author = {M.~N.~Mazziotta and F.~Loparco and A.~Anelli and M.~M.~Belviso and A.~Buquicchio and E.~V.~Cassano and M.~De Cosmo and P.~Ginefra and M.~L.~Martulli and C.~Picci and D.~Picicci and R.~D.~Soriano and A.~P.~Tatulli and G.~Tripaldella and V.~M.~Zupo and M.~F.~Muscarella and S.~Turbacci and M.~Boselli and C.~B.~da Cruz E Silva and M.~Joos and P.~Schütze}, title = {{T}he {EXTRA}-{BL}4{S} experiment for the measurement of the energy and angular distributions of transition radiation {X}-rays}, year = {2023}, eprint = {2301.11247}, note = {arXiv:2301.11247v2} }
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We have designed and implemented an experiment to measure the angular distributions and the energy spectra of the transition radiation X-rays emitted by fast electrons and positrons crossing different radiators. Our experiment was selected among the proposals of the 2021 Beamline for Schools contest, a competition for high-school students organized every year by CERN and DESY, and was performed at the DESY II Test Beam facility area TB21, using a high-purity beam of electrons or positrons with momenta in the range from 1 to 6 GeV/c. The measurements were performed using a 100 um thick silicon pixel detector, with a pitch of 55 um. Our results are consistent with the expectations from the theoretical models describing the production of transition radiation in multilayer regular radiators.
Search for relativistic fractionally charged particles in space
DAMPE Collaboration, F. Alemanno, C. Altomare, Q. An, P. Azzarello, F. C. T. Barbato, P. Bernardini, X. J. Bi, M. S. Cai, E. Casilli, E. Catanzani, J. Chang, D. Y. Chen, J. L. Chen, Z. F. Chen, M. Y. Cui, T. S. Cui, Y. X. Cui, H. T. Dai, A. De-Benedittis, et al (131)
Sep 12 2022 astro-ph.HE hep-ex hep-ph physics.space-ph arXiv:2209.04260v1

@misc{2209.04260, author = {DAMPE Collaboration and F.~Alemanno and C.~Altomare and Q.~An and P.~Azzarello and F.~C.~T.~Barbato and P.~Bernardini and X.~J.~Bi and M.~S.~Cai and E.~Casilli and E.~Catanzani and J.~Chang and D.~Y.~Chen and J.~L.~Chen and Z.~F.~Chen and M.~Y.~Cui and T.~S.~Cui and Y.~X.~Cui and H.~T.~Dai and A.~De-Benedittis and I.~De Mitri and F.~de Palma and M.~Deliyergiyev and A.~Di Giovanni and M.~Di Santo and Q.~Ding and T.~K.~Dong and Z.~X.~Dong and G.~Donvito and D.~Droz and J.~L.~Duan and K.~K.~Duan and D.~D'Urso and R.~R.~Fan and Y.~Z.~Fan and F.~Fang and K.~Fang and C.~Q.~Feng and L.~Feng and M.~F.~Alonso and J.~M.~Frieden and P.~Fusco and M.~Gao and F.~Gargano and K.~Gong and Y.~Z.~Gong and D.~Y.~Guo and J.~H.~Guo and S.~X.~Han and Y.~M.~Hu and G.~S.~Huang and X.~Y.~Huang and Y.~Y.~Huang and M.~Ionica and L.~Y.~Jiang and W.~Jiang and J.~Kong and A.~Kotenko and D.~Kyratzis and S.~J.~Lei and W.~L.~Li and W.~H.~Li and X.~Li and X.~Q.~Li and Y.~M.~Liang and C.~M.~Liu and H.~Liu and J.~Liu and S.~B.~Liu and Y.~Liu and F.~Loparco and C.~N.~Luo and M.~Ma and P.~X.~Ma and T.~Ma and X.~Y.~Ma and G.~Marsella and M.~N.~Mazziotta and D.~Mo and M.~M.~Salinas and X.~Y.~Niu and X.~Pan and A.~Parenti and W.~X.~Peng and X.~Y.~Peng and C.~Perrina and R.~Qiao and J.~N.~Rao and A.~Ruina and Z.~Shangguan and W.~H.~Shen and Z.~Q.~Shen and Z.~T.~Shen and L.~Silveri and J.~X.~Song and M.~Stolpovskiy and H.~Su and M.~Su and H.~R.~Sun and Z.~Y.~Sun and A.~Surdo and X.~J.~Teng and A.~Tykhonov and J.~Z.~Wang and L.~G.~Wang and S.~Wang and S.~X.~Wang and X.~L.~Wang and Y.~Wang and Y.~F.~Wang and Y.~Z.~Wang and D.~M.~Wei and J.~J.~Wei and Y.~F.~Wei and D.~Wu and J.~Wu and L.~B.~Wu and S.~S.~Wu and X.~Wu and Z.~Q.~Xia and E.~H.~Xu and H.~T.~Xu and J.~Xu and Z.~H.~Xu and Z.~L.~Xu and Z.~Z.~Xu and G.~F.~Xue and H.~B.~Yang and P.~Yang and Y.~Q.~Yang and H.~J.~Yao and Y.~H.~Yu and G.~W.~Yuan and Q.~Yuan and C.~Yue and J.~J.~Zang and S.~X.~Zhang and W.~Z.~Zhang and Yan Zhang and Yi.~Zhang and Y.~J.~Zhang and Y.~L.~Zhang and Y.~P.~Zhang and Y.~Q.~Zhang and Z.~Zhang and Z.~Y.~Zhang and C.~Zhao and H.~Y.~Zhao and X.~F.~Zhao and C.~Y.~Zhou and Y.~Zhu}, title = {{S}earch for relativistic fractionally charged particles in space}, year = {2022}, eprint = {2209.04260}, note = {arXiv:2209.04260v1} }
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More than a century after the performance of the oil drop experiment, the possible existence of fractionally charged particles FCP still remains unsettled. The search for FCPs is crucial for some extensions of the Standard Model in particle physics. Most of the previously conducted searches for FCPs in cosmic rays were based on experiments underground or at high altitudes. However, there have been few searches for FCPs in cosmic rays carried out in orbit other than AMS-01 flown by a space shuttle and BESS by a balloon at the top of the atmosphere. In this study, we conduct an FCP search in space based on on-orbit data obtained using the DArk Matter Particle Explorer (DAMPE) satellite over a period of five years. Unlike underground experiments, which require an FCP energy of the order of hundreds of GeV, our FCP search starts at only a few GeV. An upper limit of $6.2\times 10^{-10}~~\mathrm{cm^{-2}sr^{-1} s^{-1}}$ is obtained for the flux. Our results demonstrate that DAMPE exhibits higher sensitivity than experiments of similar types by three orders of magnitude that more stringently restricts the conditions for the existence of FCP in primary cosmic rays.
Measurement of the angular correlation between the two gamma rays emitted in the radioactive decays of a $^{60}$Co source with two NaI(Tl) scintillator
E. C. Amato, A. Anelli, M. Barbieri, D. Cataldi, V. Cellamare, D. Cerasole, F. Conserva, S. De Gaetano, D. Depalo, A. Digennaro, E. Fiorente, F. Gargano, D. Gatti, P. Loizzo, F. Loparco, O. Mele, N. Nicassio, G. Perfetto, R. Pillera, R. Pirlo, et al (2)
Jan 14 2022 physics.ed-ph physics.ins-det arXiv:2201.04867v1

@misc{2201.04867, author = {E.~C.~Amato and A.~Anelli and M.~Barbieri and D.~Cataldi and V.~Cellamare and D.~Cerasole and F.~Conserva and S.~De Gaetano and D.~Depalo and A.~Digennaro and E.~Fiorente and F.~Gargano and D.~Gatti and P.~Loizzo and F.~Loparco and O.~Mele and N.~Nicassio and G.~Perfetto and R.~Pillera and R.~Pirlo and E.~Schygulla and D.~Troiano}, title = {{M}easurement of the angular correlation between the two gamma rays emitted in the radioactive decays of a $^{60}${C}o source with two {N}a{I}({T}l) scintillator}, year = {2022}, eprint = {2201.04867}, note = {arXiv:2201.04867v1} }
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We implemented a didactic experiment to study the angular correlation between the two gamma rays emitted in typical $^{60}$Co radioactive decays. We used two NaI(Tl) scintillators, already available in our laboratory, and a low-activity $^{60}$Co source. The detectors were mounted on two rails, with the source at their center. The first rail was fixed, while the second could be rotated around the source. We performed several measurements by changing the angle between the two scintillators in the range from $90^\circ$ to $180^\circ$. Dedicated background runs were also performed, removing the source from the experimental setup. We found that the signal rate increases with the angular separation between the two scintillators, with small discrepancies from the theoretical expectations.
Comparison of proton shower developments in the BGO calorimeter of the Dark Matter Particle Explorer between GEANT4 and FLUKA simulations
Wei Jiang, Chuan Yue, Ming-Yang Cui, Xiang Li, Qiang Yuan, Francesca Alemanno, Paolo Bernardini, Giovanni Catanzani, Zhan-Fang Chen, Ivan De Mitri, Tie-Kuang Dong, Giacinto Donvito, David Francois Droz, Piergiorgio Fusco, Fabio Gargano, Dong-Ya Guo, Dimitrios Kyratzis, Shi-Jun Lei, Yang Liu, Francesco Loparco, et al (13)
Sep 29 2020 physics.ins-det astro-ph.IM arXiv:2009.13036v1

@misc{2009.13036, author = {Wei Jiang and Chuan Yue and Ming-Yang Cui and Xiang Li and Qiang Yuan and Francesca Alemanno and Paolo Bernardini and Giovanni Catanzani and Zhan-Fang Chen and Ivan De Mitri and Tie-Kuang Dong and Giacinto Donvito and David Francois Droz and Piergiorgio Fusco and Fabio Gargano and Dong-Ya Guo and Dimitrios Kyratzis and Shi-Jun Lei and Yang Liu and Francesco Loparco and Peng-Xiong Ma and Giovanni Marsella and Mario Nicola Mazziotta and Xu Pan and Wen-Xi Peng and Antonio Surdo and Andrii Tykhonov and Yi-Yeng Wei and Yu-Hong Yu and Jing-Jing Zang and Ya-Peng Zhang and Yong-Jie Zhang and Yun-Long Zhang}, title = {{C}omparison of proton shower developments in the {BGO} calorimeter of the {D}ark {M}atter {P}article {E}xplorer between {GEANT}4 and {FLUKA} simulations}, year = {2020}, eprint = {2009.13036}, note = {arXiv:2009.13036v1} }
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The DArk Matter Particle Explorer (DAMPE) is a satellite-borne detector for high-energy cosmic rays and $\gamma$-rays. To fully understand the detector performance and obtain reliable physical results, extensive simulations of the detector are necessary. The simulations are particularly important for the data analysis of cosmic ray nuclei, which relies closely on the hadronic and nuclear interactions of particles in the detector material. Widely adopted simulation softwares include the GEANT4 and FLUKA, both of which have been implemented for the DAMPE simulation tool. Here we describe the simulation tool of DAMPE and compare the results of proton shower properties in the calorimeter from the two simulation softwares. Such a comparison gives an estimate of the most significant uncertainties of our proton spectral analysis.
Identification of particles with Lorentz factor up to $10^{4}$ with Transition Radiation Detectors based on micro-strip silicon detectors
J. Alozy, N. Belyaev, M. Campbell, M. Cherry, F. Dachs, S. Doronin, K. Filippov, P. Fusco, F. Gargano, E. Heijne, S. Konovalov, D. Krasnopevtsev, X. Llopart, F. Loparco, V. Mascagna, M. N. Mazziotta, H. Pernegger, D. Ponomarenko, M. Prest, D. Pyatiizbyantseva, et al (22)
Feb 01 2019 physics.ins-det arXiv:1901.11265v2

@misc{1901.11265, author = {J.~Alozy and N.~Belyaev and M.~Campbell and M.~Cherry and F.~Dachs and S.~Doronin and K.~Filippov and P.~Fusco and F.~Gargano and E.~Heijne and S.~Konovalov and D.~Krasnopevtsev and X.~Llopart and F.~Loparco and V.~Mascagna and M.~N.~Mazziotta and H.~Pernegger and D.~Ponomarenko and M.~Prest and D.~Pyatiizbyantseva and R.~Radomskii and C.~Rembser and A.~Romaniouk and A.~A.~Savchenko and D.~Schaefer and E.~J.~Schioppa and D.~Shchukin and D.~Yu Sergeeva and E.~Shulga and S.~Smirnov and Y.~Smirnov and M.~Soldani and P.~Spinelli and M.~Strikhanov and P.~Teterin and V.~Tikhomirov and A.~A.~Tishchenko and E.~Vallazza and M.~van Beuzekom and B.~van der Heijden and K.~Vorobev and K.~Zhukov}, title = {{I}dentification of particles with {L}orentz factor up to $10^{4}$ with {T}ransition {R}adiation {D}etectors based on micro-strip silicon detectors}, year = {2019}, eprint = {1901.11265}, howpublished = {Nuclear Instruments & Methods A, volume 927 (2019), pages 1-13}, doi = {10.1016/j.nima.2019.02.032}, note = {arXiv:1901.11265v2} }
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This work is dedicated to the study of a technique for hadron identification in the TeV momentum range, based on the simultaneous measurement of the energies and of the emission angles of the Transition Radiation (TR) X-rays with respect to the radiating particles. A detector setup has been built and tested with particles in a wide range of Lorentz factors (from about $10^3$ to about $4 \times 10^4$ crossing different types of radiators. The measured double-differential (in energy and angle) spectra of the TR photons are in a reasonably good agreement with TR simulation predictions.
In-flight performance of the DAMPE silicon tracker
A. Tykhonov, G. Ambrosi, R. Asfandiyarov, P. Azzarello, P. Bernardini, B. Bertucci, A. Bolognini, F. Cadoux, A. D'Amone, A. De Benedittis, I. De Mitri, M. Di Santo, Y. F. Dong, M. Duranti, D. D'Urso, R. R. Fan, P. Fusco, V. Gallo, M. Gao, F. Gargano, et al (22)
Jun 28 2018 astro-ph.IM physics.ins-det arXiv:1806.10355v1

@misc{1806.10355, author = {A.~Tykhonov and G.~Ambrosi and R.~Asfandiyarov and P.~Azzarello and P.~Bernardini and B.~Bertucci and A.~Bolognini and F.~Cadoux and A.~D'Amone and A.~De Benedittis and I.~De Mitri and M.~Di Santo and Y.~F.~Dong and M.~Duranti and D.~D'Urso and R.~R.~Fan and P.~Fusco and V.~Gallo and M.~Gao and F.~Gargano and S.~Garrappa and K.~Gong and M.~Ionica and D.~La Marra and F.~Loparco and G.~Marsella and M.N.~Mazziotta and W.~X.~Peng and R.~Qiao and M.~M.~Salinas and A.~Surdo and V.~Vagelli and S.~Vitillo and H.~Y.~Wang and J.~Z.~Wang and Z.~M.~Wang and D.~Wu and X.~Wu and F.~Zhang and J.~Y.~Zhang and H.~Zhao and S.~Zimmer}, title = {{I}n-flight performance of the {DAMPE} silicon tracker}, year = {2018}, eprint = {1806.10355}, doi = {10.1016/j.nima.2018.06.036}, note = {arXiv:1806.10355v1} }
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DAMPE (DArk Matter Particle Explorer) is a spaceborne high-energy cosmic ray and gamma-ray detector, successfully launched in December 2015. It is designed to probe astroparticle physics in the broad energy range from few GeV to 100 TeV. The scientific goals of DAMPE include the identification of possible signatures of Dark Matter annihilation or decay, the study of the origin and propagation mechanisms of cosmic-ray particles, and gamma-ray astronomy. DAMPE consists of four sub-detectors: a plastic scintillator strip detector, a Silicon-Tungsten tracKer-converter (STK), a BGO calorimeter and a neutron detector. The STK is composed of six double layers of single-sided silicon micro-strip detectors interleaved with three layers of tungsten for photon conversions into electron-positron pairs. The STK is a crucial component of DAMPE, allowing to determine the direction of incoming photons, to reconstruct tracks of cosmic rays and to estimate their absolute charge (Z). We present the in-flight performance of the STK based on two years of in-flight DAMPE data, which includes the noise behavior, signal response, thermal and mechanical stability, alignment and position resolution.
Internal alignment and position resolution of the silicon tracker of DAMPE determined with orbit data
A. Tykhonov, G. Ambrosi, R. Asfandiyarov, P. Azzarello, P. Bernardini, B. Bertucci, A. Bolognini, F. Cadoux, A. D'Amone, A. De Benedittis, I. De Mitri, M. Di Santo, Y. F. Dong, M. Duranti, D. D'Urso, R. R. Fan, P. Fusco, V. Gallo, M. Gao, F. Gargano, et al (23)
Dec 08 2017 physics.ins-det arXiv:1712.02739v2

@misc{1712.02739, author = {A.~Tykhonov and G.~Ambrosi and R.~Asfandiyarov and P.~Azzarello and P.~Bernardini and B.~Bertucci and A.~Bolognini and F.~Cadoux and A.~D'Amone and A.~De Benedittis and I.~De Mitri and M.~Di Santo and Y.~F.~Dong and M.~Duranti and D.~D'Urso and R.~R.~Fan and P.~Fusco and V.~Gallo and M.~Gao and F.~Gargano and S.~Garrappa and K.~Gong and M.~Ionica and D.~La Marra and S.~J.~Lei and X.~Li and F.~Loparco and G.~Marsella and M.N.~Mazziotta and W.~X.~Peng and R.~Qiao and M.~M.~Salinas and A.~Surdo and V.~Vagelli and S.~Vitillo and H.~Y.~Wang and J.~Z.~Wang and D.~Wu and X.~Wu and F.~Zhang and J.~Y.~Zhang and H.~Zhao and S.~Zimmer}, title = {{I}nternal alignment and position resolution of the silicon tracker of {DAMPE} determined with orbit data}, year = {2017}, eprint = {1712.02739}, howpublished = {Nucl. Instrum. Methods Phys. Res. A 893 (2018) 43-56}, doi = {10.1016/j.nima.2018.02.105}, note = {arXiv:1712.02739v2} }
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The DArk Matter Particle Explorer (DAMPE) is a space-borne particle detector designed to probe electrons and gamma-rays in the few GeV to 10 TeV energy range, as well as cosmic-ray proton and nuclei components between 10 GeV and 100 TeV. The silicon-tungsten tracker-converter is a crucial component of DAMPE. It allows the direction of incoming photons converting into electron-positron pairs to be estimated, and the trajectory and charge (Z) of cosmic-ray particles to be identified. It consists of 768 silicon micro-strip sensors assembled in 6 double layers with a total active area of 6.6 m$^2$. Silicon planes are interleaved with three layers of tungsten plates, resulting in about one radiation length of material in the tracker. Internal alignment parameters of the tracker have been determined on orbit, with non-showering protons and helium nuclei. We describe the alignment procedure and present the position resolution and alignment stability measurements.
The DArk Matter Particle Explorer mission
J. Chang, G. Ambrosi, Q. An, R. Asfandiyarov, P. Azzarello, P. Bernardini, B. Bertucci, M. S. Cai, M. Caragiulo, D. Y. Chen, H. F. Chen, J. L. Chen, W. Chen, M. Y. Cui, T. S. Cui, A. D'Amone, A. De Benedittis, I. De Mitri, M. Di Santo, J. N. Dong, et al (144)
Jun 27 2017 astro-ph.IM astro-ph.HE hep-ex physics.ins-det arXiv:1706.08453v2

@misc{1706.08453, author = {J.~Chang and G.~Ambrosi and Q.~An and R.~Asfandiyarov and P.~Azzarello and P.~Bernardini and B.~Bertucci and M.~S.~Cai and M.~Caragiulo and D.~Y.~Chen and H.~F.~Chen and J.~L.~Chen and W.~Chen and M.~Y.~Cui and T.~S.~Cui and A.~D'Amone and A.~De Benedittis and I.~De Mitri and M.~Di Santo and J.~N.~Dong and T.~K.~Dong and Y.~F.~Dong and Z.~X.~Dong and G.~Donvito and D.~Droz and K.~K.~Duan and J.~L.~Duan and M.~Duranti and D.~D'Urso and R.~R.~Fan and Y.~Z.~Fan and F.~Fang and C.~Q.~Feng and L.~Feng and P.~Fusco and V.~Gallo and F.~J.~Gan and W.~Q.~Gan and M.~Gao and S.~S.~Gao and F.~Gargano and K.~Gong and Y.~Z.~Gong and J.~H.~Guo and Y.~M.~Hu and G.~S.~Huang and Y.~Y.~Huang and M.~Ionica and D.~Jiang and W.~Jiang and X.~Jin and J.~Kong and S.~J.~Lei and S.~Li and X.~Li and W.~L.~Li and Y.~Li and Y.~F.~Liang and Y.~M.~Liang and N.~H.~Liao and Q.~Z.~Liu and H.~Liu and J.~Liu and S.~B.~Liu and Q.~Z.~Liu and W.~Q.~Liu and Y.~Liu and F.~Loparco and J.~Lü and M.~Ma and P.~X.~Ma and S.~Y.~Ma and T.~Ma and X.~Q.~Ma and X.~Y.~Ma and G.~Marsella and M.N.~Mazziotta and D.~Mo and T.~T.~Miao and X.~Y.~Niu and M.~Pohl and X.~Y.~Peng and W.~X.~Peng and R.~Qiao and J.~N.~Rao and M.~M.~Salinas and G.~Z.~Shang and W.~H.~Shen and Z.~Q.~Shen and Z.~T.~Shen and J.~X.~Song and H.~Su and M.~Su and Z.~Y.~Sun and A.~Surdo and X.~J.~Teng and X.~B.~Tian and A.~Tykhonov and V.~Vagelli and S.~Vitillo and C.~Wang and Chi Wang and H.~Wang and H.~Y.~Wang and J.~Z.~Wang and L.~G.~Wang and Q.~Wang and S.~Wang and X.~H.~Wang and X.~L.~Wang and Y.~F.~Wang and Y.~P.~Wang and Y.~Z.~Wang and S.~C.~Wen and Z.~M.~Wang and D.~M.~Wei and J.~J.~Wei and Y.~F.~Wei and D.~Wu and J.~Wu and S.~S.~Wu and X.~Wu and K.~Xi and Z.~Q.~Xia and Y.~L.~Xin and H.~T.~Xu and Z.~L.~Xu and Z.~Z.~Xu and G.~F.~Xue and H.~B.~Yang and J.~Yang and P.~Yang and Y.~Q.~Yang and Z.~L.~Yang and H.~J.~Yao and Y.~H.~Yu and Q.~Yuan and C.~Yue and J.~J.~Zang and C.~Zhang and D.~L.~Zhang and F.~Zhang and J.~B.~Zhang and J.~Y.~Zhang and J.~Z.~Zhang and L.~Zhang and P.~F.~Zhang and S.~X.~Zhang and W.~Z.~Zhang and Y.~Zhang and Y.~J.~Zhang and Y.~Q.~Zhang and Y.~L.~Zhang and Y.~P.~Zhang and Z.~Zhang and Z.~Y.~Zhang and H.~Zhao and H.~Y.~Zhao and X.~F.~Zhao and C.~Y.~Zhou and Y.~Zhou and X.~Zhu and Y.~Zhu and S.~Zimmer}, title = {{T}he {DA}rk {M}atter {P}article {E}xplorer mission}, year = {2017}, eprint = {1706.08453}, howpublished = {Astropart. Phys. 95 (2017) 6-24}, doi = {10.1016/j.astropartphys.2017.08.005}, note = {arXiv:1706.08453v2} }
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The DArk Matter Particle Explorer (DAMPE), one of the four scientific space science missions within the framework of the Strategic Pioneer Program on Space Science of the Chinese Academy of Sciences, is a general purpose high energy cosmic-ray and gamma-ray observatory, which was successfully launched on December 17th, 2015 from the Jiuquan Satellite Launch Center. The DAMPE scientific objectives include the study of galactic cosmic rays up to $\sim 10$ TeV and hundreds of TeV for electrons/gammas and nuclei respectively, and the search for dark matter signatures in their spectra. In this paper we illustrate the layout of the DAMPE instrument, and discuss the results of beam tests and calibrations performed on ground. Finally we present the expected performance in space and give an overview of the mission key scientific goals.
Measurement of the ratio h/e with a photomultiplier tube and a set of LEDs
F. Loparco, M. S. Malagoli, S. Rainò, P. Spinelli
Nov 15 2016 physics.ed-ph arXiv:1611.04310v1

@misc{1611.04310, author = {F.~Loparco and M.~S.~Malagoli and S.~Rainò and P.~Spinelli}, title = {{M}easurement of the ratio h/e with a photomultiplier tube and a set of {LED}s}, year = {2016}, eprint = {1611.04310}, note = {arXiv:1611.04310v1} }
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We propose a laboratory experience aimed at undergraduate physics students to understand the main features of the photoelectric effect and to perform a measurement of the ratio h/e, where h is the Planck's constant and e is the electron charge. The experience is based on the method developed by Millikan for his measurements on the photoelectric effect in the years from 1912 to 1915. The experimental setup consists of a photomultiplier tube (PMT) equipped with a voltage divider properly modified to set variable retarding potentials between the photocathode and the first dynode, and a set of LEDs emitting at different wavelengths. The photocathode is illuminated with the various LEDs and, for each wavelength of the incident light, the output anode current is measured as a function of the retarding potential applied between the cathode and the first dynode. From each measurement, a value of the stopping potential for the anode current is derived. Finally, the stopping potentials are plotted as a function of the frequency of the incident light, and a linear fit is performed. The slope and the intercept of the line allow respectively to evaluate the ratio h/e and the ratio W/e, where W is the work function of the photocathode.
SuperB Technical Design Report
SuperB Collaboration, M. Baszczyk, P. Dorosz, J. Kolodziej, W. Kucewicz, M. Sapor, A. Jeremie, E. Grauges Pous, G. E. Bruno, G. De Robertis, D. Diacono, G. Donvito, P. Fusco, F. Gargano, F. Giordano, F. Loddo, F. Loparco, G. P. Maggi, V. Manzari, M. N. Mazziotta, et al (389)
Jun 25 2013 physics.ins-det hep-ex arXiv:1306.5655v1

@misc{1306.5655, author = {SuperB Collaboration and M.~Baszczyk and P.~Dorosz and J.~Kolodziej and W.~Kucewicz and M.~Sapor and A.~Jeremie and E.~Grauges Pous and G.~E.~Bruno and G.~De Robertis and D.~Diacono and G.~Donvito and P.~Fusco and F.~Gargano and F.~Giordano and F.~Loddo and F.~Loparco and G.~P.~Maggi and V.~Manzari and M.~N.~Mazziotta and E.~Nappi and A.~Palano and B.~Santeramo and I.~Sgura and L.~Silvestris and V.~Spinoso and G.~Eigen and J.~Zalieckas and Z.~Zhuo and L.~Jenkovszky and G.~Balbi and M.~Boldini and D.~Bonacorsi and V.~Cafaro and I.~D'Antone and G.~M.~Dallavalle and R.~Di Sipio and F.~Fabbri and L.~Fabbri and A.~Gabrielli and D.~Galli and P.~Giacomelli and V.~Giordano and F.~M.~Giorgi and C.~Grandi and I.~Lax and S.~Lo Meo and U.~Marconi and A.~Montanari and G.~Pellegrini and M.~Piccinini and T.~Rovelli and N.~Semprini Cesari and G.~Torromeo and N.~Tosi and R.~Travaglini and V.~M.~Vagnoni and S.~Valentinetti and M.~Villa and A.~Zoccoli and J.-F.~Caron and C.~Hearty and P.~F.-T.~Lu and T.~S.~Mattison and J.~A.~McKenna and R.~Y.-C.~So and M.~Yu.~Barnyakov and V.~E.~Blinov and A.~A.~Botov and V.~P.~Druzhinin and V.~B.~Golubev and S.~A.~Kononov and E.~A.~Kravchenko and E.~B.~Levichev and A.~P.~Onuchin and S.~I.~Serednyakov and D.~A.~Shtol and Y.~I.~Skovpen and E.~P.~Solodov and A.~Cardini and M.~Carpinelli and D.~S.-T.~Chao and C.~H.~Cheng and D.~A.~Doll and B.~Echenard and K.~Flood and J.~Hanson and D.~G.~Hitlin and P.~Ongmongkolkul and F.~C.~Porter and R.~Y.~Zhu and N.~Randazzo and E.~De La Cruz Burelo and Y.~Zheng and P.~Campos and M.~De Silva and A.~Kathirgamaraju and B.~Meadows and B.~Pushpawela and Y.~Shi and M.~Sokoloff and G.~Lopez Castro and V.~Ciaschini and P.~Franchini and F.~Giacomini and A.~Paolini and G.~A.~Calderon Polania and S.~Laczek and P.~Romanowicz and B.~Szybinski and M.~Czuchry and L.~Flis and D.~Harezlak and J.~Kocot and M.~Radecki and M.~Sterzel and T.~Szepieniec and T.~Szymocha and P.~Wójcik and M.~Andreotti and W.~Baldini and R.~Calabrese and V.~Carassiti and G.~Cibinetto and A.~Cotta Ramusino and F.~Evangelisti and A.~Gianoli and E.~Luppi and R.~Malaguti and M.~Manzali and M.~Melchiorri and M.~Munerato and C.~Padoan and V.~Santoro and L.~Tomassetti and M.~M.~Beretta and M.~Biagini and M.~Boscolo and E.~Capitolo and R.~de Sangro and M.~Esposito and G.~Felici and G.~Finocchiaro and M.~Gatta and C.~Gatti and S.~Guiducci and S.~Lauciani and P.~Patteri and I.~Peruzzi and M.~Piccolo and P.~Raimondi and M.~Rama and C.~Sanelli and S.~Tomassini and P.~Fabbricatore and D.~Delepine and M.~A.~Reyes Santos and M.~Chrzaszcz and R.~Grzymkowski and P.~Knap and J.~Kotula and T.~Lesiak and J.~Ludwin and J.~Michalowski and B.~Pawlik and B.~Rachwal and M.~Stodulski and J.~Wiechczynski and M.~Witek and L.~Zawiejski and M.~Zdybal and V.~Y.~Aushev and A.~Ustynov and N.~Arnaud and P.~Bambade and C.~Beigbeder and F.~Bogard and M.~Borsato and D.~Breton and J.~Brossard and L.~Burmistrov and D.~Charlet and V.~Chaumat and O.~Dadoun and M.~El Berni and J.~Maalmi and V.~Puill and C.~Rimbault and A.~Stocchi and V.~Tocut and A.~Variola and S.~Wallon and G.~Wormser and F.~Grancagnolo and E.~Ben-Haim and S.~Sitt and M.~Baylac and O.~Bourrion and J.-M.~Deconto and Y.~Gomez Martinez and N.~Monseu and J.-F.~Muraz and J.-S.~Real and C.~Vescovi and R.~Cenci and A.~Jawahery and D.~Roberts and E.~W.~Twedt and R.~Cheaib and D.~Lindemann and S.~Nderitu and P.~Patel and S.~H.~Robertson and D.~Swersky and A.~Warburton and E.~Cuautle Flores and G.~Toledo Sanchez and P.~Biassoni and L.~Bombelli and M.~Citterio and S.~Coelli and C.~Fiorini and V.~Liberali and M.~Monti and B.~Nasri and N.~Neri and F.~Palombo and F.~Sabatini and A.~Stabile and A.~Berra and A.~Giachero and C.~Gotti and D.~Lietti and M.~Maino and G.~Pessina and M.~Prest and J.-P.~Martin and M.~Simard and N.~Starinski and P.~Taras and A.~Drutskoy and S.~Makarychev and A.~V.~Nefediev and A.~Aloisio and S.~Cavaliere and G.~De Nardo and M.~Della Pietra and A.~Doria and R.~Giordano and A.~Ordine and S.~Pardi and G.~Russo and C.~Sciacca and I.~I.~Bigi and C.~P.~Jessop and W.~Wang and M.~Bellato and M.~Benettoni and M.~Corvo and A.~Crescente and F.~Dal Corso and U.~Dosselli and C.~Fanin and A.~Gianelle and S.~Longo and M.~Michelotto and F.~Montecassiano and M.~Morandin and R.~Pengo and M.~Posocco and M.~Rotondo and G.~Simi and R.~Stroili and L.~Gaioni and A.~Manazza and M.~Manghisoni and L.~Ratti and V.~Re and G.~Traversi and S.~Zucca and S.~Bizzaglia and M.~Bizzarri and C.~Cecchi and S.~Germani and M.~Lebeau and P.~Lubrano and E.~Manoni and A.~Papi and A.~Rossi and G.~Scolieri and G.~Batignani and S.~Bettarini and G.~Casarosa and A.~Cervelli and A.~Fella and F.~Forti and M.~Giorgi and L.~Lilli and A.~Lusiani and B.~Oberhof and A.~Paladino and F.~Pantaleo and E.~Paoloni and A.~L.~Perez Perez and G.~Rizzo and J.~Walsh and A.~Fernández Téllez and G.~Beck and M.~Berman and A.~Bevan and F.~Gannaway and G.~Inguglia and A.~J.~Martin and J.~Morris and V.~Bocci and M.~Capodiferro and G.~Chiodi and I.~Dafinei and N.~V.~Drenska and R.~Faccini and F.~Ferroni and C.~Gargiulo and P.~Gauzzi and C.~Luci and R.~Lunadei and G.~Martellotti and F.~Pellegrino and V.~Pettinacci and D.~Pinci and L.~Recchia and D.~Ruggeri and A.~Zullo and P.~Camarri and R.~Cardarelli and C.~De Santis and A.~Di Ciaccio and V.~Di Felice and F.~Di Palma and A.~Di Simone and L.~Marcelli and R.~Messi and D.~Moricciani and R.~Sparvoli and S.~Tammaro and P.~Branchini and A.~Budano and S.~Bussino and M.~Ciuchini and F.~Nguyen and A.~Passeri and F.~Ruggieri and E.~Spiriti and F.~Wilson and I.~Leon Monzon and J.~R.~Millan-Almaraz and P.~L.~M.~Podesta-Lerma and D.~Aston and B.~Dey and A.~Fisher and P.~D.~Jackson and D.~W.~G.~S.~Leith and S.~Luitz and D.~MacFarlane and M.~McCulloch and S.~Metcalfe and A.~Novokhatski and S.~Osier and R.~Prepost and B.~Ratcliff and J.~Seeman and M.~Sullivan and J.~Va'vra and U.~Wienands and W.~Wisniewski and B.~D.~Altschul and M.~V.~Purohit and J.~Baudot and I.~Ripp-Baudot and G.~A.~P.~Cirrone and G.~Cuttone and O.~Bezshyyko and G.~Dolinska and A.~Soffer and F.~Bianchi and F.~De Mori and A.~Filippi and D.~Gamba and S.~Marcello and M.~Bomben and L.~Bosisio and P.~Cristaudo and L.~Lanceri and B.~Liberti and I.~Rashevskaya and C.~Stella and E.~S.~Vallazza and L.~Vitale and G.~Auriemma and C.~Satriano and F.~Martinez Vidal and J.~Mazorra de Cos and A.~Oyanguren and P.~Ruiz Valls and A.~Beaulieu and S.~Dejong and J.~Franta and M.~J.~Lewczuk and M.~Roney and R.~Sobie}, title = {{S}uper{B} {T}echnical {D}esign {R}eport}, year = {2013}, eprint = {1306.5655}, note = {arXiv:1306.5655v1} }
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In this Technical Design Report (TDR) we describe the SuperB detector that was to be installed on the SuperB e+e- high luminosity collider. The SuperB asymmetric collider, which was to be constructed on the Tor Vergata campus near the INFN Frascati National Laboratory, was designed to operate both at the Upsilon(4S) center-of-mass energy with a luminosity of 10^36 cm^-2s^-1 and at the tau/charm production threshold with a luminosity of 10^35 cm^-2s^-1. This high luminosity, producing a data sample about a factor 100 larger than present B Factories, would allow investigation of new physics effects in rare decays, CP Violation and Lepton Flavour Violation. This document details the detector design presented in the Conceptual Design Report (CDR) in 2007. The R&D and engineering studies performed to arrive at the full detector design are described, and an updated cost estimate is presented. A combination of a more realistic cost estimates and the unavailability of funds due of the global economic climate led to a formal cancelation of the project on Nov 27, 2012.
A Bayesian approach to evaluate confidence intervals in counting experiments with background
F. Loparco, M. N. Mazziotta
May 17 2011 physics.data-an hep-ex arXiv:1105.3041v1

@misc{1105.3041, author = {F.~Loparco and M.~N.~Mazziotta}, title = {{A} {B}ayesian approach to evaluate confidence intervals in counting experiments with background}, year = {2011}, eprint = {1105.3041}, howpublished = {Nucl.Instrum.Meth.A646:167-173,2011}, doi = {10.1016/j.nima.2011.05.023}, note = {arXiv:1105.3041v1} }
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In this paper we propose a procedure to evaluate Bayesian confidence intervals in counting experiments where both signal and background fluctuations are described by the Poisson statistics. The results obtained when the method is applied to the calculation of upper limits will also be illustrated.
Science with the new generation high energy gamma- ray experiments
M. Alvarez, D. D'Armiento, G. Agnetta, A. Alberdi, A. Antonelli, A. Argan, P. Assis, E. A. Baltz, C. Bambi, G. Barbiellini, H. Bartko, M. Basset, D. Bastieri, P. Belli, G. Benford, L. Bergstrom, R. Bernabei, G. Bertone, A. Biland, B. Biondo, et al (180)
Dec 05 2007 astro-ph gr-qc hep-ph physics.space-ph arXiv:0712.1548v1

@misc{0712.1548, author = {M.~Alvarez and D.~D'Armiento and G.~Agnetta and A.~Alberdi and A.~Antonelli and A.~Argan and P.~Assis and E.~A.~Baltz and C.~Bambi and G.~Barbiellini and H.~Bartko and M.~Basset and D.~Bastieri and P.~Belli and G.~Benford and L.~Bergstrom and R.~Bernabei and G.~Bertone and A.~Biland and B.~Biondo and F.~Bocchino and E.~Branchini and M.~Brigida and T.~Bringmann and P.~Brogueira and A.~Bulgarelli and J.~A.~Caballero and G.~A.~Caliandro and P.~Camarri and F.~Cappella and P.~Caraveo and R.~Carbone and M.~Carvajal and S.~Casanova and A.~J.~Castro-Tirado and O.~Catalano and R.~Catena and F.~Celi and A.~Celotti and R.~Cerulli and A.~Chen and R.~Clay and V.~Cocco and J.~Conrad and E.~Costa and A.~Cuoco and G.~Cusumano and C.~J.~Dai and B.~Dawson and B.~De Lotto and G.~De Paris and A.~de Ugarte Postigo and E.~Del Monte and C.~Delgado and A.~Di Ciaccio and G.~Di Cocco and S.~Di Falco and G.~Di Persio and B.~L.~Dingus and A.~Dominguez and F.~Donato and I.~Donnarumma and M.~Doro and J.~Edsjo and J.~M.~Espino Navas and M.~C.~Espirito Santo and Y.~Evangelista and C.~Evoli and D.~Fargion and C.~Favuzzi and M.~Feroci and M.~Fiorini and L.~Foggetta and N.~Fornengo and T.~Froysland and M.~Frutti and F.~Fuschino and J.~L.~Gomez and M.~Gomez and D.~Gaggero and N.~Galante and M.~I.~Gallardo and M.~Galli and J.~E.~Garcia and M.~Garczarczyk and F.~Gargano and M.~Gaug and F.~Gianotti and S.~Giarrusso and B.~Giebels and N.~Giglietto and P.~Giommi and F.~Giordano and A.~Giuliani and J.~Glicenstein and P.~Goncalves and D.~Grasso and M.~Guerriero and H.~L.~He and A.~Incicchitti and J.~Kirk and H.~H.~Kuang and A.~La Barbera and G.~La Rosa and C.~Labanti and G.~Lamanna and I.~Lapshov and F.~Lazzarotto and S.~Liberati and F.~Liello and P.~Lipari and F.~Longo and F.~Loparco and M.~Lozano and P.~G.~Lucentini De Sanctis and J.~M.~Ma and M.~C.~Maccarone and L.~Maccione and V.~Malvezzi and A.~Mangano and M.~Mariotti and M.~Marisaldi and I.~Martel and A.~Masiero and E.~Massaro and M.~Mastropietro and E.~Mattaini and F.~Mauri and M.~N.~Mazziotta and S.~Mereghetti and T.~Mineo and S.~Mizobuchi and A.~Moiseev and M.~Moles and C.~Monte and F.~Montecchia and E.~Morelli and A.~Morselli and I.~Moskalenko and F.~Nozzoli and J.~F.~Ormes and M.~A.~Peres-Torres and L.~Pacciani and A.~Pellizzoni and F.~Perez-Bernal and F.~Perotti and P.~Picozza and L.~Pieri and M.~Pietroni and M.~Pimenta and A.~Pina and C.~Pittori and C.~Pontoni and G.~Porrovecchio and F.~Prada and M.~Prest and D.~Prosperi and R.~Protheroe and G.~Pucella and J.~M.~Quesada and J.~M.~Quintana and J.~R.~Quintero and S.~Raino and M.~Rapisarda and M.~Rissi and J.~Rodriguez and E.~Rossi and G.~Rowell and A.~Rubini and F.~Russo and M.~Sanchez-Conde and B.~Sacco and V.~Scapin and M.~Schelke and A.~Segreto and A.~Sellerholm and X.~D.~Sheng and A.~Smith and P.~Soffitta and R.~Sparvoli and P.~Spinelli and V.~Stamatescu and L.~S.~Stark and M.~Tavani and G.~Thornton and L.~G.~Titarchuk and B.~Tome and A.~Traci and M.~Trifoglio and A.~Trois and P.~Vallania and E.~Vallazza and S.~Vercellone and S.~Vernetto and V.~Vitale and N.~Wild and Z.~P.~Ye and A.~Zambra and F.~Zandanel and D.~Zanello}, title = {{S}cience with the new generation high energy gamma- ray experiments}, year = {2007}, eprint = {0712.1548}, howpublished = {Frascati Physics Series vol.45 (2007) A.Lionetto, A.Morselli editors ISBN 978-88-86409-54-0}, note = {arXiv:0712.1548v1} }
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This Conference is the fifth of a series of Workshops on High Energy Gamma- ray Experiments, following the Conferences held in Perugia 2003, Bari 2004, Cividale del Friuli 2005, Elba Island 2006. This year the focus was on the use of gamma-ray to study the Dark Matter component of the Universe, the origin and propagation of Cosmic Rays, Extra Large Spatial Dimensions and Tests of Lorentz Invariance.