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dc.contributor.authorSerra, P.
dc.contributor.authorKoribalski, B.
dc.contributor.authorKilborn, V.
dc.contributor.authorAllison, J.
dc.contributor.authorAmy, S.
dc.contributor.authorBall, L.
dc.contributor.authorBannister, K.
dc.contributor.authorBell, M.
dc.contributor.authorBock, D.
dc.contributor.authorBolton, R.
dc.contributor.authorBowen, M.
dc.contributor.authorBoyle, B.
dc.contributor.authorBroadhurst, S.
dc.contributor.authorBrodrick, D.
dc.contributor.authorBrothers, M.
dc.contributor.authorBunton, J.
dc.contributor.authorChapman, J.
dc.contributor.authorCheng, W.
dc.contributor.authorChippendale, A.
dc.contributor.authorChung, Y.
dc.contributor.authorCooray, F.
dc.contributor.authorCornwell, T.
dc.contributor.authorDeBoer, D.
dc.contributor.authorDiamond, P.
dc.contributor.authorForsyth, R.
dc.contributor.authorGough, R.
dc.contributor.authorGupta, N.
dc.contributor.authorHampson, G.
dc.contributor.authorHarvey-Smith, L.
dc.contributor.authorHay, S.
dc.contributor.authorHayman, D.
dc.contributor.authorHeywood, I.
dc.contributor.authorHotan, A.
dc.contributor.authorHoyle, S.
dc.contributor.authorHumphreys, B.
dc.contributor.authorIndermuehle, B.
dc.contributor.authorJacka, C.
dc.contributor.authorJackson, Carole
dc.contributor.authorJackson, S.
dc.contributor.authorJeganathan, K.
dc.contributor.authorJohnston, S.
dc.contributor.authorJoseph, J.
dc.contributor.authorKamphuis, P.
dc.contributor.authorLeach, M.
dc.contributor.authorLenc, E.
dc.contributor.authorLensson, E.
dc.contributor.authorMackay, S.
dc.contributor.authorMarquarding, M.
dc.contributor.authorMarvil, J.
dc.contributor.authorMcClure-Griffiths, N.
dc.contributor.authorMcConnell, D.
dc.contributor.authorMeyer, M.
dc.contributor.authorMirtschin, P.
dc.contributor.authorNeuhold, S.
dc.contributor.authorNg, A.
dc.contributor.authorNorris, R.
dc.contributor.authorO'Sullivan, J.
dc.contributor.authorPathikulangara, J.
dc.contributor.authorPearce, S.
dc.contributor.authorPhillips, C.
dc.contributor.authorPopping, A.
dc.contributor.authorQiao, R.
dc.contributor.authorReynolds, J.
dc.contributor.authorRoberts, P.
dc.contributor.authorSault, R.
dc.contributor.authorSchinckel, A.
dc.contributor.authorShaw, R.
dc.contributor.authorShimwell, T.
dc.contributor.authorStaveley-Smith, L.
dc.contributor.authorStorey, M.
dc.contributor.authorSweetnam, A.
dc.contributor.authorTroup, E.
dc.contributor.authorTzioumis, A.
dc.contributor.authorVoronkov, M.
dc.contributor.authorWestmeier, T.
dc.contributor.authorWhiting, M.
dc.contributor.authorWilson, C.
dc.contributor.authorWong, O.
dc.contributor.authorWu, X.
dc.identifier.citationSerra, P. and Koribalski, B. and Kilborn, V. and Allison, J. and Amy, S. and Ball, L. and Bannister, K. et al. 2015. ASKAP HI imaging of the galaxy group IC 1459. Monthly Notices of the Royal Astronomical Society. 452 (3): pp. 2680-2691.

© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. We present HI imaging of the galaxy group IC 1459 carried out with six antennas of the Australian Square Kilometre Array Pathfinder equipped with phased-array feeds. We detect and resolve HI in 11 galaxies down to a column density of ~1020 cm-2 inside a ~6 deg2 field and with a resolution of ~1 arcmin on the sky and ~8 kms-1 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 ~109 M? and accounts for ~15 per cent 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 intragroup gas within the IC 1459 group. Altogether, the HI found outside galaxies in this group amounts to several times 109 M?, at least 10 per cent 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.

dc.titleASKAP HI imaging of the galaxy group IC 1459
dc.typeJournal Article
dcterms.source.titleMonthly Notices of the Royal Astronomical Society

This article has been accepted for publication in Monthly Notices of The Royal Astronomical Society, © 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

curtin.departmentCurtin Institute of Radio Astronomy (Physics)
curtin.accessStatusOpen access

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