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SPLASH: The Southern Parkes Large-Area Survey in Hydroxyl -- Data Description & Release
J. R. Dawson, P. A. Jones, C. Purcell, A. J. Walsh, S. L. Breen, C. Brown, E. Carretti, M. R. Cunningham, J. M. Dickey, S. P. Ellingsen, S. J. Gibson, J. F. Gomez, J. A. Green, H. Imai, V. Krishnan, N. Lo, V. Lowe, M. Marquarding, N. M. McClure-Griffiths .
Mar 11 2022 astro-ph.GA arXiv:2203.05131v1

@misc{2203.05131, author = {J.~R.~Dawson and P.~A.~Jones and C.~Purcell and A.~J.~Walsh and S.~L.~Breen and C.~Brown and E.~Carretti and M.~R.~Cunningham and J.~M.~Dickey and S.~P.~Ellingsen and S.~J.~Gibson and J.~F.~Gomez and J.~A.~Green and H.~Imai and V.~Krishnan and N.~Lo and V.~Lowe and M.~Marquarding and N.~M.~McClure-Griffiths .}, title = {{SPLASH}: {T}he {S}outhern {P}arkes {L}arge-{A}rea {S}urvey in {H}ydroxyl -- {D}ata {D}escription & {R}elease}, year = {2022}, eprint = {2203.05131}, note = {arXiv:2203.05131v1} }
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We present the full data release for the Southern Parkes Large-Area Survey in Hydroxyl (SPLASH), a sensitive, unbiased single-dish survey of the Southern Galactic Plane in all four ground-state transitions of the OH radical at 1612, 1665, 1667 and 1720 MHz. The survey covers the inner Galactic Plane, Central Molecular Zone and Galactic Centre over the range $|b|<$ 2$^{\circ}$, 332$^{\circ}$ $< l <$ 10$^{\circ}$, with a small extension between 2$^{\circ}$ $< b <$ 6$^{\circ}$, 358$^{\circ}$ $< l <$ 4$^{\circ}$. SPLASH is the most sensitive large-scale survey of OH to-date, reaching a characteristic root-mean-square sensitivity of $\sim15$ mK for an effective velocity resolution of $\sim0.9$ km/s. The spectral line datacubes are optimised for the analysis of extended, quasi-thermal OH, but also contain numerous maser sources, which have been confirmed interferometrically and published elsewhere. We also present radio continuum images at 1612, 1666 and 1720 MHz. Based on initial comparisons with $^{12}$CO(J=1-0), we find that OH rarely extends outside CO cloud boundaries in our data, but suggest that large variations in CO-to-OH brightness temperature ratios may reflect differences in the total gas column density traced by each. Column density estimation in the complex, continuum-bright Inner Galaxy is a challenge, and we demonstrate how failure to appropriately model sub-beam structure and the line-of-sight source distribution can lead to order-of-magnitude errors. Anomalous excitation of the 1612 and 1720 MHz satellite lines is ubiquitous in the inner Galaxy, but is disabled by line overlap in and around the Central Molecular Zone.
An ultra-wide bandwidth (704 to 4032 MHz) receiver for the Parkes radio telescope
G. Hobbs, R. N. Manchester, A. Dunning, A. Jameson, P. Roberts, D. George, J. A. Green, J. Tuthill, L. Toomey, J. F. Kaczmarek, S. Mader, M. Marquarding, A. Ahmed, S. W. Amy, M. Bailes, R. Beresford, N. D. R. Bhat, D. C.-J. Bock, M. Bourne, M. Bowen, et al (52)
Nov 05 2019 astro-ph.IM arXiv:1911.00656v1

@misc{1911.00656, author = {G.~Hobbs and R.~N.~Manchester and A.~Dunning and A.~Jameson and P.~Roberts and D.~George and J.~A.~Green and J.~Tuthill and L.~Toomey and J.~F.~Kaczmarek and S.~Mader and M.~Marquarding and A.~Ahmed and S.~W.~Amy and M.~Bailes and R.~Beresford and N.~D.~R.~Bhat and D.~C.-J.~Bock and M.~Bourne and M.~Bowen and M.~Brothers and A.~D.~Cameron and E.~Carretti and N.~Carter and S.~Castillo and R.~Chekkala and W.~Cheng and Y.~Chung and D.~A.~Craig and S.~Dai and J.~R.~Dawson and J.~Dempsey and P.~Doherty and B.~Dong and P.~G.~Edwards and T.~Ergesh and X.~Y.~Gao and J.~L.~Han and D.~B.~Hayman and B.~T.~Indermuehle and K.~Jeganathan and S.~Johnston and H.~Kanoniuk and M.~Kesteven and M.~Kramer and M.~Leach and V.~J.~Mcintyre and V.~A.~Moss and S.~Oslowski and C.~J.~Phillips and N.~C.~Pope and B.~Preisig and D.~C.~Price and K.~Reeves and L.~Reilly and J.~E.~Reynolds and T.~Robishaw and P.~Roush and T.~Ruckley and E.~M.~Sadler and J.~Sarkissian and S.~Severs and R.~M.~Shannon and K.~W.~Smart and M.~Smith and S.~L.~Smith.~C.~Sobey and L.~Staveley-Smith and A.~K.~Tzioumis and W.~van Straten and N.~Wang and L.~Wen and M.~T.~Whiting}, title = {{A}n ultra-wide bandwidth (704 to 4032 {MH}z) receiver for the {P}arkes radio telescope}, year = {2019}, eprint = {1911.00656}, note = {arXiv:1911.00656v1} }
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We describe an ultra-wide-bandwidth, low-frequency receiver ("UWL") recently installed on the Parkes radio telescope. The receiver system provides continuous frequency coverage from 704 to 4032 MHz. For much of the band (~60%) the system temperature is approximately 22K and the receiver system remains in a linear regime even in the presence of strong mobile phone transmissions. We discuss the scientific and technical aspects of the new receiver including its astronomical objectives, as well as the feed, receiver, digitiser and signal-processor design. We describe the pipeline routines that form the archive-ready data products and how those data files can be accessed from the archives. The system performance is quantified including the system noise and linearity, beam shape, antenna efficiency, polarisation calibration and timing stability.
The Australian Square Kilometre Array Pathfinder: Performance of the Boolardy Engineering Test Array
D. McConnell, J.R. Allison, K. Bannister, M.E. Bell, H.E. Bignall, A.P. Chippendale, P.G. Edwards, L. Harvey-Smith, S. Hegarty, I. Heywood, A.W. Hotan, B.T. Indermuehle, E. Lenc, J. Marvil, A. Popping, W. Raja, J.E. Reynolds, R.J. Sault, P. Serra, M.A. Voronkov, et al (54)
Aug 03 2016 astro-ph.IM arXiv:1608.00750v1

@misc{1608.00750, author = {D.~McConnell and J.R.~Allison and K.~Bannister and M.E.~Bell and H.E.~Bignall and A.P.~Chippendale and P.G.~Edwards and L.~Harvey-Smith and S.~Hegarty and I.~Heywood and A.W.~Hotan and B.T.~Indermuehle and E.~Lenc and J.~Marvil and A.~Popping and W.~Raja and J.E.~Reynolds and R.J.~Sault and P.~Serra and M.A.~Voronkov and M.~Whiting and S.W.~Amy and P.~Axtens and L.~Ball and T.J.~Bateman and D.C.-J.~Bock and R.~Bolton and D.~Brodrick and M.~Brothers and A.J.~Brown and J.D.~Bunton and W.~Cheng and T.~Cornwell and D.~DeBoer and I.~Feain and R.~Gough and N.~Gupta and J.C.~Guzman and G.A.~Hampson and S.~Hay and D.B.~Hayman and S.~Hoyle and B.~Humphreys and C.~Jacka and C.A.~Jackson and S.~Jackson and K.~Jeganathan and J.~Joseph and B.S.~Koribalski and M.~Leach and E.S.~Lensson and A.~MacLeod and S.~Mackay and M.~Marquarding and N.M.~McClure-Griffiths and P.~Mirtschin and D.~Mitchell and S.~Neuhold and A.~Ng and R.~Norris and S.~Pearce and R.Y.~Qiao and A.E.T.~Schinckel and M.~Shields and T.W.~Shimwell and M.~Storey and E.~Troup and B.~Turner and J.~Tuthill and A.~Tzioumis and R.M.~Wark and T.~Westmeier and C.~Wilson and T.~Wilson}, title = {{T}he {A}ustralian {S}quare {K}ilometre {A}rray {P}athfinder: {P}erformance of the {B}oolardy {E}ngineering {T}est {A}rray}, year = {2016}, eprint = {1608.00750}, note = {arXiv:1608.00750v1} }
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We describe the performance of the Boolardy Engineering Test Array (BETA), the prototype for the Australian Square Kilometre Array Pathfinder telescope ASKAP. BETA is the first aperture synthesis radio telescope to use phased array feed technology, giving it the ability to electronically form up to nine dual-polarization beams. We report the methods developed for forming and measuring the beams, and the adaptations that have been made to the traditional calibration and imaging procedures in order to allow BETA to function as a multi-beam aperture synthesis telescope. We describe the commissioning of the instrument and present details of BETA's performance: sensitivity, beam characteristics, polarimetric properties and image quality. We summarise the astronomical science that it has produced and draw lessons from operating BETA that will be relevant to the commissioning and operation of the final ASKAP telescope.
A pilot ASKAP survey of radio transient events in the region around the intermittent pulsar PSR J1107-5907
G. Hobbs, I. Heywood, M. E. Bell, M. Kerr, A. Rowlinson, S. Johnston, R. M. Shannon, M. A. Voronkov, C. Ward, J. Banyer, P. J. Hancock, Tara Murphy, J. R. Allison, S. W. Amy, L. Ball, K. Bannister, D. C.-J. Bock, D. Brodrick, M. Brothers, A. J. Brown, et al (58)
Dec 10 2015 astro-ph.SR astro-ph.IM arXiv:1512.02702v1

@misc{1512.02702, author = {G.~Hobbs and I.~Heywood and M.~E.~Bell and M.~Kerr and A.~Rowlinson and S.~Johnston and R.~M.~Shannon and M.~A.~Voronkov and C.~Ward and J.~Banyer and P.~J.~Hancock and Tara Murphy and J.~R.~Allison and S.~W.~Amy and L.~Ball and K.~Bannister and D.~C.-J.~Bock and D.~Brodrick and M.~Brothers and A.~J.~Brown and J.~D.~Bunton and J.~Chapman and A.~P.~Chippendale and Y.~Chung and D.~DeBoer and P.~Diamond and P.~G.~Edwards and R.~Ekers and R.~H.~Ferris and R.~Forsyth and R.~Gough and A.~Grancea and N.~Gupta and L.~Harvey-Smith and S.~Hay and D.~B.~Hayman and A.~W.~Hotan and S.~Hoyle and B.~Humphreys and B.~Indermuehle and C.~E.~Jacka and C.~A.~Jackson and S.~Jackson and K.~Jeganathan and J Joseph and R.~Kendall and D.~Kiraly and B.~Koribalski and M.~Leach and E.~Lenc and A.~MacLeod and S.~Mader and M.~Marquarding and J.~Marvil and N.~McClure-Griffiths and D.~McConnell and P.~Mirtschin and S.~Neuhold and A.~Ng and R.~P.~Norris and J.~O'Sullivan and S.~Pearce and C.~J.~Phillips and A.~Popping and R.~Y.~Qiao and J.~E.~Reynolds and P.~Roberts and R.~J.~Sault and A.~E.~T.~Schinckel and P.~Serra and R.~Shaw and T.~W.~Shimwell and M.~Storey and A.~W.~Sweetnam and A.~Tzioumis and T.~Westmeier and M.~Whiting and C.~D.~Wilson}, title = {{A} pilot {ASKAP} survey of radio transient events in the region around the intermittent pulsar {PSR} {J}1107-5907}, year = {2015}, eprint = {1512.02702}, note = {arXiv:1512.02702v1} }
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We use observations from the Boolardy Engineering Test Array (BETA) of the Australian Square Kilometre Array Pathfinder (ASKAP) telescope to search for transient radio sources in the field around the intermittent pulsar PSR J1107-5907. The pulsar is thought to switch between an "off" state in which no emission is detectable, a weak state and a strong state. We ran three independent transient detection pipelines on two-minute snapshot images from a 13 hour BETA observation in order to 1) study the emission from the pulsar, 2) search for other transient emission from elsewhere in the image and 3) to compare the results from the different transient detection pipelines. The pulsar was easily detected as a transient source and, over the course of the observations, it switched into the strong state three times giving a typical timescale between the strong emission states of 3.7 hours. After the first switch it remained in the strong state for almost 40 minutes. The other strong states lasted less than 4 minutes. The second state change was confirmed using observations with the Parkes radio telescope. No other transient events were found and we place constraints on the surface density of such events on these timescales. The high sensitivity Parkes observations enabled us to detect individual bright pulses during the weak state and to study the strong state over a wide observing band. We conclude by showing that future transient surveys with ASKAP will have the potential to probe the intermittent pulsar population.
ASKAP HI imaging of the galaxy group IC 1459
P. Serra, B. Koribalski, V. Kilborn, J. R. Allison, S. W. Amy, L. Ball, K. Bannister, M. E. Bell, D. C.-J. Bock, R. Bolton, M. Bowen, B. Boyle, S. Broadhurst, D. Brodrick, M. Brothers, J. D. Bunton, J. Chapman, W. Cheng, A. P. Chippendale, Y. Chung, et al (59)
Jun 16 2015 astro-ph.GA arXiv:1506.04399v1

@misc{1506.04399, author = {P.~Serra and B.~Koribalski and V.~Kilborn and J.~R.~Allison and S.~W.~Amy and L.~Ball and K.~Bannister and M.~E.~Bell and D.~C.-J.~Bock and R.~Bolton and M.~Bowen and B.~Boyle and S.~Broadhurst and D.~Brodrick and M.~Brothers and J.~D.~Bunton and J.~Chapman and W.~Cheng and A.~P.~Chippendale and Y.~Chung and F.~Cooray and T.~Cornwell and D.~DeBoer and P.~Diamond and R.~Forsyth and R.~Gough and N.~Gupta and G.~A.~Hampson and L.~Harvey-Smith and S.~Hay and D.~B.~Hayman and I.~Heywood and A.~W.~Hotan and S.~Hoyle and B.~Humphreys and B.~Indermuehle and C.~Jacka and C.~A.~Jackson and S.~Jackson and K.~Jeganathan and S.~Johnston and J Joseph and P.~Kamphuis and M.~Leach and E.~Lenc and E.~Lensson and S.~Mackay and M.~Marquarding and J.~Marvil and N.~McClure-Griffiths and D.~McConnell and M.~Meyer and P.~Mirtschin and S.~Neuhold and A.~Ng and R.~P.~Norris and J.~O'Sullivan and J.~Pathikulangara and S.~Pearce and C.~Phillips and A.~Popping and R.~Y.~Qiao and J.~E.~Reynolds and P.~Roberts and R.~J.~Sault and A.~E.~T.~Schinckel and R.~Shaw and T.~W.~Shimwell and L.~Staveley-Smith and M.~Storey and A.~W.~Sweetnam and E.~Troup and A.~Tzioumis and M.~A.~Voronkov and T.~Westmeier and M.~Whiting and C.~Wilson and O.~I.~Wong and X.~Wu}, title = {{ASKAP} {HI} imaging of the galaxy group {IC} 1459}, year = {2015}, eprint = {1506.04399}, note = {arXiv:1506.04399v1} }
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We present HI imaging of the galaxy group IC 1459 carried out with six antennas of the Australian SKA Pathfinder equipped with phased-array feeds. We detect and resolve HI in eleven galaxies down to a column density of $\sim10^{20}$ cm$^{-2}$ inside a ~6 deg$^2$ field and with a resolution of ~1 arcmin on the sky and ~8 km/s in velocity. We present HI images, velocity fields and integrated spectra of all detections, and highlight the discovery of three HI clouds -- two in the proximity of the galaxy IC 5270 and one close to NGC 7418. Each cloud has an HI mass of $10^9$ M$_\odot$ and accounts for ~15% of the HI associated with its host galaxy. Available images at ultraviolet, optical and infrared wavelengths do not reveal any clear stellar counterpart of any of the clouds, suggesting that they are not gas-rich dwarf neighbours of IC 5270 and NGC 7418. Using Parkes data we find evidence of additional extended, low-column-density HI emission around IC 5270, indicating that the clouds are the tip of the iceberg of a larger system of gas surrounding this galaxy. This result adds to the body of evidence on the presence of intra-group gas within the IC 1459 group. Altogether, the HI found outside galaxies in this group amounts to several times $10^9$ M$_\odot$, at least 10% of the HI contained inside galaxies. This suggests a substantial flow of gas in and out of galaxies during the several billion years of the group's evolution.
Discovery of HI gas in a young radio galaxy at $z = 0.44$ using the Australian Square Kilometre Array Pathfinder
J. R. Allison, E. M. Sadler, V. A. Moss, M. T. Whiting, R. W. Hunstead, M. B. Pracy, S. J. Curran, S. M. Croom, M. Glowacki, R. Morganti, S. S. Shabala, M. A. Zwaan, G. Allen, S. W. Amy, P. Axtens, L. Ball, K. W. Bannister, S. Barker, M. E. Bell, D. C.-J. Bock, et al (83)
Mar 05 2015 astro-ph.GA arXiv:1503.01265v2

@misc{1503.01265, author = {J.~R.~Allison and E.~M.~Sadler and V.~A.~Moss and M.~T.~Whiting and R.~W.~Hunstead and M.~B.~Pracy and S.~J.~Curran and S.~M.~Croom and M.~Glowacki and R.~Morganti and S.~S.~Shabala and M.~A.~Zwaan and G.~Allen and S.~W.~Amy and P.~Axtens and L.~Ball and K.~W.~Bannister and S.~Barker and M.~E.~Bell and D.~C.-J.~Bock and R.~Bolton and M.~Bowen and B.~Boyle and R.~Braun and S.~Broadhurst and D.~Brodrick and M.~Brothers and A.~Brown and J.~D.~Bunton and C.~Cantrall and J.~Chapman and W.~Cheng and A.~P.~Chippendale and Y.~Chung and F.~Cooray and T.~Cornwell and D.~DeBoer and P.~Diamond and P.~G.~Edwards and R.~Ekers and I.~Feain and R.~H.~Ferris and R.~Forsyth and R.~Gough and A.~Grancea and N.~Gupta and J.~C.~Guzman and G.~Hampson and L.~Harvey-Smith and C.~Haskins and S.~Hay and D.~B.~Hayman and I.~Heywood and A.~W.~Hotan and S.~Hoyle and B.~Humphreys and B.~T.~Indermuehle and C.~Jacka and C.~Jackson and S.~Jackson and K.~Jeganathan and S.~Johnston and J.~Joseph and R.~Kendall and M.~Kesteven and D.~Kiraly and B.~S.~Koribalski and M.~Leach and E.~Lenc and E.~Lensson and S.~Mackay and A.~Macleod and M.~Marquarding and J.~Marvil and N.~McClure-Griffiths and D.~McConnell and P.~Mirtschin and R.~P.~Norris and S.~Neuhold and A.~Ng and J.~O'Sullivan and J.~Pathikulangara and S.~Pearce and C.~Phillips and A.~Popping and R.~Y.~Qiao and J.~E.~Reynolds and P.~Roberts and R.~J.~Sault and A.~Schinckel and P.~Serra and R.~Shaw and M.~Shields and T.~Shimwell and M.~Storey and T.~Sweetnam and E.~Troup and B.~Turner and J.~Tuthill and A.~Tzioumis and M.~A.~Voronkov and T.~Westmeier and C.~D.~Wilson}, title = {{D}iscovery of {HI} gas in a young radio galaxy at $z = 0.44$ using the {A}ustralian {S}quare {K}ilometre {A}rray {P}athfinder}, year = {2015}, eprint = {1503.01265}, note = {arXiv:1503.01265v2} }
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We report the discovery of a new 21-cm HI absorption system using commissioning data from the Boolardy Engineering Test Array of the Australian Square Kilometre Array Pathfinder (ASKAP). Using the 711.5 - 1015.5 MHz band of ASKAP we were able to conduct a blind search for the 21-cm line in a continuous redshift range between $z = 0.4$ and 1.0, which has, until now, remained largely unexplored. The absorption line is detected at $z = 0.44$ towards the GHz-peaked spectrum radio source PKS B1740$-$517 and demonstrates ASKAP's excellent capability for performing a future wide-field survey for HI absorption at these redshifts. Optical spectroscopy and imaging using the Gemini-South telescope indicates that the HI gas is intrinsic to the host galaxy of the radio source. The narrow OIII emission lines show clear double-peaked structure, indicating either large-scale outflow or rotation of the ionized gas. Archival data from the \emphXMM-Newton satellite exhibit an absorbed X-ray spectrum that is consistent with a high column density obscuring medium around the active galactic nucleus. The HI absorption profile is complex, with four distinct components ranging in width from 5 to 300 km s$^{-1}$ and fractional depths from 0.2 to 20 per cent. In addition to systemic HI gas, in a circumnuclear disc or ring structure aligned with the radio jet, we find evidence for a possible broad outflow of neutral gas moving at a radial velocity of $v \sim 300$ km s$^{-1}$. We infer that the expanding young radio source ($t_{\rm age} \approx 2500$ yr) is cocooned within a dense medium and may be driving circumnuclear neutral gas in an outflow of $\sim$ 1 $\mathrm{M}_{\odot}$ yr$^{-1}$.
The Australian Square Kilometre Array Pathfinder: System Architecture and Specifications of the Boolardy Engineering Test Array
A. W. Hotan, J. D. Bunton, L. Harvey-Smith, B. Humphreys, B. D. Jeffs, T. Shimwell, J. Tuthill, M. Voronkov, G. Allen, S. Amy, K. Ardern, P. Axtens, L. Ball, K. Bannister, S. Barker, T. Bateman, R. Beresford, D. Bock, R. Bolton, M. Bowen, et al (81)
Sep 05 2014 astro-ph.IM arXiv:1409.1325v1

@misc{1409.1325, author = {A.~W.~Hotan and J.~D.~Bunton and L.~Harvey-Smith and B.~Humphreys and B.~D.~Jeffs and T.~Shimwell and J.~Tuthill and M.~Voronkov and G.~Allen and S.~Amy and K.~Ardern and P.~Axtens and L.~Ball and K.~Bannister and S.~Barker and T.~Bateman and R.~Beresford and D.~Bock and R.~Bolton and M.~Bowen and B.~Boyle and R.~Braun and S.~Broadhurst and D.~Brodrick and K.~Brooks and M.~Brothers and A.~Brown and C.~Cantrall and G.~Carrad and J.~Chapman and W.~Cheng and A.~Chippendale and Y.~Chung and F.~Cooray and T.~Cornwell and E.~Davis and L.~de Souza and D.~DeBoer and P.~Diamond and P.~Edwards and R.~Ekers and I.~Feain and D.~Ferris and R.~Forsyth and R.~Gough and A.~Grancea and N.~Gupta and JC.~Guzman and G.~Hampson and C.~Haskins and S.~Hay and D.~Hayman and S.~Hoyle and C.~Jacka and C.~Jackson and S.~Jackson and K.~Jeganathan and S.~Johnston and J.~Joseph and R.~Kendall and M.~Kesteven and D.~Kiraly and B.~Koribalski and M.~Leach and E.~Lenc and E.~Lensson and L.~Li and S.~Mackay and A.~Macleod and T.~Maher and M.~Marquarding and N.~McClure-Griffiths and D.~McConnell and S.~Mickle and P.~Mirtschin and R.~Norris and S.~Neuhold and A.~Ng and J.~O'Sullivan and J.~Pathikulangara and S.~Pearce and C.~Phillips and RY.~Qiao and J.~E.~Reynolds and A.~Rispler and P.~Roberts and D.~Roxby and A.~Schinckel and R.~Shaw and M.~Shields and M.~Storey and T.~Sweetnam and E.~Troup and B.~Turner and A.~Tzioumis and T.~Westmeier and M.~Whiting and C.~Wilson and T.~Wilson and K.~Wormnes and X.~Wu}, title = {{T}he {A}ustralian {S}quare {K}ilometre {A}rray {P}athfinder: {S}ystem {A}rchitecture and {S}pecifications of the {B}oolardy {E}ngineering {T}est {A}rray}, year = {2014}, eprint = {1409.1325}, note = {arXiv:1409.1325v1} }
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This paper describes the system architecture of a newly constructed radio telescope - the Boolardy Engineering Test Array, which is a prototype of the Australian Square Kilometre Array Pathfinder telescope. Phased array feed technology is used to form multiple simultaneous beams per antenna, providing astronomers with unprecedented survey speed. The test array described here is a 6-antenna interferometer, fitted with prototype signal processing hardware capable of forming at least 9 dual-polarisation beams simultaneously, allowing several square degrees to be imaged in a single pointed observation. The main purpose of the test array is to develop beamforming and wide-field calibration methods for use with the full telescope, but it will also be capable of limited early science demonstrations.
The Northern HIPASS catalogue - Data presentation, completeness and reliability measures
O. I. Wong, E. V. Ryan-Weber, D. A. Garcia-Appadoo, R. L. Webster, L. Staveley-Smith, M. A. Zwaan, M. J. Meyer, D. G. Barnes, V. A. Kilborn, R. Bhathal, W. J. G. de Blok, M. J. Disney, M. T. Doyle, M. J. Drinkwater, R. D. Ekers, K. C. Freeman, B. K. Gibson, S. Gurovich, J. Harnett, P. A. Henning, et al (15)
Jul 24 2006 astro-ph arXiv:astro-ph/0607491v1

@misc{astro-ph/0607491, author = {O.~I.~Wong and E.~V.~Ryan-Weber and D.~A.~Garcia-Appadoo and R.~L.~Webster and L.~Staveley-Smith and M.~A.~Zwaan and M.~J.~Meyer and D.~G.~Barnes and V.~A.~Kilborn and R.~Bhathal and W.~J.~G.~de Blok and M.~J.~Disney and M.~T.~Doyle and M.~J.~Drinkwater and R.~D.~Ekers and K.~C.~Freeman and B.~K.~Gibson and S.~Gurovich and J.~Harnett and P.~A.~Henning and H.~Jerjen and M.~J.~Kesteven and P.~M.~Knezek and B.~S.~Koribalski and S.~Mader and M.~Marquarding and R.~F.~Minchin and J.~O'Brien and M.~E.~Putman and S.~D.~Ryder and E.~M.~Sadler and J.~Stevens and I.~M.~Stewart and F.~Stootman and M.~Waugh}, title = {{T}he {N}orthern {HIPASS} catalogue - {D}ata presentation, completeness and reliability measures}, year = {2006}, eprint = {astro-ph/0607491}, howpublished = {Mon.Not.Roy.Astron.Soc.371:1855-1864,2006}, doi = {10.1111/j.1365-2966.2006.10846.x}, note = {arXiv:astro-ph/0607491v1} }
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The Northern HIPASS catalogue (NHICAT) is the northern extension of the HIPASS catalogue, HICAT (Meyer et al. 2004). This extension adds the sky area between the declination range of +2 deg < dec. < +25.5 deg to HICAT's declination range of -90 deg < dec. < +2 deg. HIPASS is a blind HI survey using the Parkes Radio Telescope covering 71% of the sky (including this northern extension) and a heliocentric velocity range of -1,280 km/s to 12,700 km/s . The entire Virgo Cluster region has been observed in the Northern HIPASS. The galaxy catalogue, NHICAT, contains 1002 sources with v_hel > 300 km/s . Sources with -300 km/s < v_hel < 300 km/s were excluded to avoid contamination by Galactic emission. In total, the entire HIPASS survey has found 5317 galaxies identified purely by their HI content. The full galaxy catalogue is publicly-available at <http://hipass.aus-vo.org>.
Data storage, processing and visualisation for the ATCA
T. Murphy, P. Lamb, C. Owen, M. Marquarding
Jan 18 2006 astro-ph arXiv:astro-ph/0601354v1

@misc{astro-ph/0601354, author = {T.~Murphy and P.~Lamb and C.~Owen and M.~Marquarding}, title = {{D}ata storage, processing and visualisation for the {ATCA}}, year = {2006}, eprint = {astro-ph/0601354}, note = {arXiv:astro-ph/0601354v1} }
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We present three Virtual Observatory tools developed at the ATNF for the storage, processing and visualisation of ATCA data. These are the Australia Telescope Online Archive, a prototype data reduction pipeline, and the Remote Visualisation System. These tools were developed in the context of the Virtual Observatory and were intended to be both useful for astronomers and technology demonstrators. We discuss the design and implementation of these tools, as well as issues that should be considered when developing similar systems for future telescopes.
The HIPASS Catalogue: III - Optical Counterparts & Isolated Dark Galaxies
Marianne T. Doyle, M. J. Drinkwater, D. J. Rohde, K. A. Pimbblet, M. Read, M. J. Meyer, M. A. Zwaan, E. Ryan-Weber, J. Stevens, B. S. Koribalski, R. L. Webster, L. Staveley-Smith, D. G. Barnes, M. Howlett, V. A. Kilborn, M. Waugh, M. J. Pierce, R. Bhathal, W. J. G. de Blok, M. J. Disney, et al (21)
May 31 2005 astro-ph arXiv:astro-ph/0505591v1

@misc{astro-ph/0505591, author = {Marianne T.~Doyle and M.~J.~Drinkwater and D.~J.~Rohde and K.~A.~Pimbblet and M.~Read and M.~J.~Meyer and M.~A.~Zwaan and E.~Ryan-Weber and J.~Stevens and B.~S.~Koribalski and R.~L.~Webster and L.~Staveley-Smith and D.~G.~Barnes and M.~Howlett and V.~A.~Kilborn and M.~Waugh and M.~J.~Pierce and R.~Bhathal and W.~J.~G.~de Blok and M.~J.~Disney and R.~D.~Ekers and K.~C.~Freeman and D.~A.~Garcia and B.~K.~Gibson and J.~Harnett and P.~A.~Henning and H.~Jerjen and M.~J.~Kesteven and P.~M.~Knezek and S.~Mader and M.~Marquarding and R.~F.~Minchin and J.~O'Brien and T.~Oosterloo and R.~M.~Price and M.~E.~Putman and S.~D.~Ryder and E.~M.~Sadler and I.~M.~Stewart and F.~Stootman and A.~E.~Wright}, title = {{T}he {HIPASS} {C}atalogue: {III} - {O}ptical {C}ounterparts & {I}solated {D}ark {G}alaxies}, year = {2005}, eprint = {astro-ph/0505591}, howpublished = {Mon.Not.Roy.Astron.Soc.361:34,2005}, doi = {10.1111/j.1365-2966.2005.09159.x}, note = {arXiv:astro-ph/0505591v1} }
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We present the largest catalogue to date of optical counterparts for HI radio-selected galaxies, Hopcat. Of the 4315 HI radio-detected sources from the HI Parkes All Sky Survey (Hipass) catalogue, we find optical counterparts for 3618 (84%) galaxies. Of these, 1798 (42%) have confirmed optical velocities and 848 (20%) are single matches without confirmed velocities. Some galaxy matches are members of galaxy groups. From these multiple galaxy matches, 714 (16%) have confirmed optical velocities and a further 258 (6%) galaxies are without confirmed velocities. For 481 (11%), multiple galaxies are present but no single optical counterpart can be chosen and 216 (5%) have no obvious optical galaxy present. Most of these 'blank fields' are in crowded fields along the Galactic plane or have high extinctions. Isolated 'Dark galaxy' candidates are investigated using an extinction cut of ABj < 1 mag and the blank fields category. Of the 3692 galaxies with an ABj extinction < 1 mag, only 13 are also blank fields. Of these, 12 are eliminated either with follow-up Parkes observations or are in crowded fields. The remaining one has a low surface brightness optical counterpart. Hence, no isolated optically dark galaxies have been found within the limits of the Hipass survey.
The 1000 Brightest HIPASS Galaxies: HI Mass Function and Omega_HI
M. A. Zwaan, L. Staveley-Smith, B. S. Koribalski, P. A. Henning, V. A. Kilborn, S. D. Ryder, D. G. Barnes, R. Bhathal, P. J. Boyce, W. J. G. de Blok, M. J. Disney, M. J. Drinkwater, R. D. Ekers, K. C. Freeman, B. K. Gibson, A. J. Green, R. F. Haynes, H. Jerjen, S. Juraszek, M. J. Kesteven, et al (20)
Feb 22 2003 astro-ph arXiv:astro-ph/0302440v2

@misc{astro-ph/0302440, author = {M.~A.~Zwaan and L.~Staveley-Smith and B.~S.~Koribalski and P.~A.~Henning and V.~A.~Kilborn and S.~D.~Ryder and D.~G.~Barnes and R.~Bhathal and P.~J.~Boyce and W.~J.~G.~de Blok and M.~J.~Disney and M.~J.~Drinkwater and R.~D.~Ekers and K.~C.~Freeman and B.~K.~Gibson and A.~J.~Green and R.~F.~Haynes and H.~Jerjen and S.~Juraszek and M.~J.~Kesteven and P.~M.~Knezek and R.~C.~Kraan-Korteweg and S.~Mader and M.~Marquarding and M.~Meyer and R.~F.~Minchin and J.~R.~Mould and J.~O'Brien and T.~Oosterloo and R.~M.~Price and M.~E.~Putman and E.~Ryan-Weber and E.~M.~Sadler and A.~Schroeder and I.~M.~Stewart and F.~Stootman and B.~Warren and M.~Waugh and R.~L.~Webster and A.~E.~Wright}, title = {{T}he 1000 {B}rightest {HIPASS} {G}alaxies: {HI} {M}ass {F}unction and {O}mega_{HI}}, year = {2003}, eprint = {astro-ph/0302440}, howpublished = {Astron.J.125:2842,2003}, doi = {10.1086/374944}, note = {arXiv:astro-ph/0302440v2} }
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We present a new accurate measurement of the HI mass function of galaxies from the HIPASS Bright Galaxy Catalog, a sample of 1000 galaxies with the highest HI peak flux densities in the southern hemisphere (Koribalski et al. 2003). This sample spans nearly four orders of magnitude in HI mass (from log M_HI/M_sun=6.8 to 10.6, H0=75) and is the largest sample of HI selected galaxies to date. We develop a bivariate maximum likelihood technique to measure the space density of galaxies, and show that this is a robust method, insensitive to the effects of large scale structure. The resulting HI mass function can be fitted satisfactorily with a Schechter function with faint-end slope alpha=-1.30. This slope is found to be dependent on morphological type, with later type galaxies giving steeper slopes. We extensively test various effects that potentially bias the determination of the HI mass function, including peculiar motions of galaxies, large scale structure, selection bias, and inclination effects, and quantify these biases. The large sample of galaxies enables an accurate measurement of the cosmological mass density of neutral gas: Omega_HI=(3.8 +/- 0.6) x 10^-4. Low surface brightness galaxies contribute only 15% to this value, consistent with previous findings.
The Large Scale Distribution of Neutral Hydrogen in the Fornax Region
Meryl Waugh, M. J. Drinkwater, R. L. Webster, L. Staveley-Smith, V. A. Kilborn, D. G. Barnes, R. Bhathal, W. J. G. de Blok, P. J. Boyce, M. J. Disney, R. D. Ekers, K. C. Freeman, B. K. Gibson, P. A. Henning, H. Jerjen, P. M. Knezek, B. Koribalski, M. Marquarding, R. F. Minchin, R. M. Price, et al (5)
Oct 09 2002 astro-ph arXiv:astro-ph/0210170v1

@misc{astro-ph/0210170, author = {Meryl Waugh and M.~J.~Drinkwater and R.~L.~Webster and L.~Staveley-Smith and V.~A.~Kilborn and D.~G.~Barnes and R.~Bhathal and W.~J.~G.~de Blok and P.~J.~Boyce and M.~J.~Disney and R.~D.~Ekers and K.~C.~Freeman and B.~K.~Gibson and P.~A.~Henning and H.~Jerjen and P.~M.~Knezek and B.~Koribalski and M.~Marquarding and R.~F.~Minchin and R.~M.~Price and M.~E.~Putman and S.~D.~Ryder and E.~M.~Sadler and F.~Stootman and M.~A.~Zwaan}, title = {{T}he {L}arge {S}cale {D}istribution of {N}eutral {H}ydrogen in the {F}ornax {R}egion}, year = {2002}, eprint = {astro-ph/0210170}, howpublished = {Mon.Not.Roy.Astron.Soc. 337 (2002) 641}, doi = {10.1046/j.1365-8711.2002.05942.x}, note = {arXiv:astro-ph/0210170v1} }
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Using HIPASS data, we have searched for HI in a ~25x25 sq.deg. region centred on the Fornax cluster. Within a velocity search range of 300 - 3700 km/s and a lower flux limit of ~40 mJy, 110 galaxies with HI emission were detected, one of which is previously uncatalogued. None of the detections has early-type morphology. Previously unknown velocities for 14 galaxies have been determined, with a further 4 velocity measurements being significantly dissimilar to published values. Identification of an optical counterpart is relatively unambiguous for more than ~90% of our HI galaxies. The galaxies appear to be embedded in a sheet at the cluster velocity which extends for more than 30 deg across the search area. At the nominal cluster distance of ~20 Mpc, this corresponds to an elongated structure more than 10 Mpc in extent. A velocity gradient across the structure is detected, with radial velocities increasing by \~500 km/s from SE to NW. The clustering of galaxies evident in optical surveys is only weakly suggested in the spatial distribution of our HI detections. Our results suggest a considerable deficit of HI-rich galaxies in the centre of the cluster. However, relative to the field, there is a 3(+/-1)-fold excess of HI-rich galaxies in the outer parts of the cluster where galaxies may be infalling towards the cluster for the first time.
HIPASS Detection of an Intergalactic Gas Cloud in the NGC 2442 Group
S. D. Ryder, B. Koribalski, L. Staveley-Smith, V. Kilborn, D. Malin, G. Banks, D. Barnes, R. Bhatal, W. de Blok, P. Boyce, M. Disney, M. Drinkwater, R. Ekers, K. Freeman, B. Gibson, P. Henning, H. Jerjen, P. Knezek, M. Marquarding, R. Minchin, et al (9)
Mar 08 2001 astro-ph arXiv:astro-ph/0103099v1

@misc{astro-ph/0103099, author = {S.~D.~Ryder and B.~Koribalski and L.~Staveley-Smith and V.~Kilborn and D.~Malin and G.~Banks and D.~Barnes and R.~Bhatal and W.~de Blok and P.~Boyce and M.~Disney and M.~Drinkwater and R.~Ekers and K.~Freeman and B.~Gibson and P.~Henning and H.~Jerjen and P.~Knezek and M.~Marquarding and R.~Minchin and J.~Mould and T.~Oosterloo and R.~Price and M.~Putman and E.~Sadler and I.~Stewart and F.~Stootman and R.~Webster and A.~Wright}, title = {{HIPASS} {D}etection of an {I}ntergalactic {G}as {C}loud in the {NGC} 2442 {G}roup}, year = {2001}, eprint = {astro-ph/0103099}, doi = {10.1086/321453}, note = {arXiv:astro-ph/0103099v1} }
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We report the discovery, from the HI Parkes All-Sky Survey (HIPASS), of a gas cloud associated with the asymmetric spiral galaxy NGC 2442. This object, designated HIPASS J0731-69, contains ~10^9 M_sun of HI, or nearly one-third as much atomic gas as NGC 2442 itself. No optical counterpart to any part of HIPASS J0731-69 has yet been identified, consistent with the gas being diffuse, and with its stream-like kinematics. If the gas in HIPASS J0731-69 was once part of NGC 2442, then it was most likely a fairly recent tidal encounter with a moderately massive companion which tore it loose, although the possibility of ram-pressure stripping cannot be ruled out. This discovery highlights the potential of the HIPASS data for yielding new clues to the nature of some of the best-known galaxies in the local universe.
An Extragalactic HI Cloud with No Optical Counterpart?
V. A. Kilborn, L. Staveley-Smith, M. Marquarding, R. L. Webster, D. F. Malin, G. D. Banks, R. Bhathal, W. J. G. de Blok, P. J. Boyce, M. J. Disney, M. J. Drinkwater, R. D. Ekers, K. C. Freeman, B. K. Gibson, P. A. Henning, H. Jerjen, P. M. Knezek, B. Koribalski, R. F. Minchin, J. R. Mould, et al (8)
May 15 2000 astro-ph arXiv:astro-ph/0005267v1

@misc{astro-ph/0005267, author = {V.~A.~Kilborn and L.~Staveley-Smith and M.~Marquarding and R.~L.~Webster and D.~F.~Malin and G.~D.~Banks and R.~Bhathal and W.~J.~G.~de Blok and P.~J.~Boyce and M.~J.~Disney and M.~J.~Drinkwater and R.~D.~Ekers and K.~C.~Freeman and B.~K.~Gibson and P.~A.~Henning and H.~Jerjen and P.~M.~Knezek and B.~Koribalski and R.~F.~Minchin and J.~R.~Mould and T.~Oosterloo and R.~M.~Price and M.~E.~Putman and S.~D.~Ryder and E.~M.~Sadler and I.~Stewart and F.~Stootman and A.~E.~Wright}, title = {{A}n {E}xtragalactic {HI} {C}loud with {N}o {O}ptical {C}ounterpart?}, year = {2000}, eprint = {astro-ph/0005267}, doi = {10.1086/301542}, note = {arXiv:astro-ph/0005267v1} }
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We report the discovery, from the HI Parkes All-Sky Survey (HIPASS), of an isolated cloud of neutral hydrogen which we believe to be extragalactic. The HI mass of the cloud (HIPASS J1712-64) is very low, 1.7 x 10^7 Msun, using an estimated distance of ~3.2 Mpc. Most significantly, we have found no optical companion to this object to very faint limits (mu(B)~ 27 mag arcsec^-2). HIPASS J1712-64 appears to be a binary system similar to, but much less massive than, HI 1225+01 (the Virgo HI Cloud) and has a size of at least 15 kpc. The mean velocity dispersion, measured with the Australia Telescope Compact Array (ATCA), is only 4 km/s for the main component and because of the weak or non-existent star-formation, possibly reflects the thermal linewidth (T<2000 K) rather than bulk motion or turbulence. The peak column density for HIPASS J1712-64, from the combined Parkes and ATCA data, is only 3.5 x 10^19 cm^-2, which is estimated to be a factor of two below the critical threshold for star formation. Apart from its significantly higher velocity, the properties of HIPASS J1712-64 are similar to the recently recognised class of Compact High Velocity Clouds. We therefore consider the evidence for a Local Group or Galactic origin, although a more plausible alternative is that HIPASS J1712-64 was ejected from the interacting Magellanic Cloud/Galaxy system at perigalacticon ~ 2 x 10^8 yr ago.