Bryant, JJ and Owers, MS and Robotham, ASG and Croom, SM and Driver, SP and Drinkwater, MJ and Lorente, NPF and Cortese, L and Scott, N and Colless, M and Schaefer, A and Taylor, EN and Konstantopoulos, IS and Allen, JT and Baldry, IK and Barnes, L and Bauer, AE and Bland-Hawthorn, J and Bloom, JV and Brooks, AM et al and Brough, S and Cecil, G and Couch, W and Croton, D and Davies, R and Ellis, S and Fogarty, LMR and Foster, C and Glazebrook, K and Goodwin, M and Green, A and Gunawardhana, ML and Hampton, E and Ho, I-T and Hopkins, AM and Kewley, L and Lawrence, JS and Leon-Saval, SG and Leslie, S and McElroy, R and Lewis, G and Liske, J and Lopez-Sanchez, AR and Mahajan, S and Medling, AM and Metcalfe, N and Meyer, M and Mould, J and Obreschkow, D and O'Toole, S and Pracy, M and Richards, SN and Shanks, T and Sharp, R and Sweet, SM and Thomas, AD and Tonini, C and Walcher, CJ (2015) The SAMI Galaxy Survey: instrument specification and target selection. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 447 (3). pp. 2857-2879. ISSN 0035-8711
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1407.7335v2.pdf - Accepted Version
The SAMI Galaxy Survey will observe 3400 galaxies with the Sydney-AAO Multi- object Integral-field spectrograph (SAMI) on the Anglo-Australian Telescope (AAT) in a 3-year survey which began in 2013. We present the throughput of the SAMI system, the science basis and specifications for the target selection, the survey observation plan and the combined properties of the selected galaxies. The survey includes four volume-limited galaxy samples based on cuts in a proxy for stellar mass, along with low-stellar-mass dwarf galaxies all selected from the Galaxy And Mass Assembly (GAMA) survey. The GAMA regions were selected because of the vast array of ancillary data available, including ultraviolet through to radio bands. These fields are on the celestial equator at 9, 12, and 14.5 hours, and cover a total of 144 square degrees (in GAMA-I). Higher density environments are also included with the addition of eight clusters. The clusters have spectroscopy from 2dFGRS and SDSS and photometry in regions covered by the Sloan Digital Sky Survey (SDSS) and/or VLT Survey Telescope/ATLAS. The aim is to cover a broad range in stellar mass and environment, and therefore the primary survey targets cover redshifts 0.004 < z < 0.095, magnitudes rpet < 19.4, stellar masses 107– 1012M⊙, and environments from isolated field galaxies through groups to clusters of _ 1015M⊙.
|Additional Information:||This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record "The SAMI Galaxy Survey: instrument specification and target selection", MNRAS 447(3), pp.2857-2879 is available online at: http://dx.doi.org/10.1093/mnras/stu2635|
|Uncontrolled Keywords:||0201 Astronomical And Space Sciences|
|Subjects:||Q Science > QB Astronomy|
|Divisions:||Astrophysics Research Institute|
|Publisher:||OXFORD UNIV PRESS|
|Date Deposited:||27 Oct 2015 08:47|
|Last Modified:||27 Oct 2015 08:47|
|DOI or Identification number:||10.1093/mnras/stu2635|
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The SAMI Galaxy Survey: instrument specification and target selection. (deposited 02 Jul 2015 10:13)
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