The SAMI Galaxy Survey: Early Data Release

被引：132

作者：

Allen, J. T. ^{[1
,2
]}

Croom, S. M. ^{[1
,2
]}

Konstantopoulos, I. S. ^{[2
,3
]}

Bryant, J. J. ^{[1
,2
,3
]}

Sharp, R. ^{[4
]}

Cecil, G. N. ^{[5
]}

Fogarty, L. M. R. ^{[1
,2
]}

Foster, C. ^{[3
]}

Green, A. W. ^{[3
]}

Ho, I. -T. ^{[6
]}

Owers, M. S. ^{[3
]}

Schaefer, A. L. ^{[1
,2
,3
]}

Scott, N. ^{[1
,2
]}

Bauer, A. E. ^{[3
]}

Baldry, I. ^{[7
]}

Barnes, L. A. ^{[1
]}

Bland-Hawthorn, J. ^{[1
,2
]}

Bloom, J. V. ^{[1
,2
]}

Brough, S. ^{[3
]}

Colless, M. ^{[4
]}

Cortese, L. ^{[8
]}

Couch, W. J. ^{[3
]}

Drinkwater, M. J. ^{[9
]}

Driver, S. P. ^{[10
,11
]}

Goodwin, M. ^{[3
]}

Gunawardhana, M. L. P. ^{[12
]}

Hampton, E. J. ^{[4
]}

Hopkins, A. M. ^{[3
]}

Kewley, L. J. ^{[4
]}

Lawrence, J. S. ^{[3
]}

Leon-Saval, S. G. ^{[13
]}

Liske, J. ^{[14
]}

Lopez-Sanchez, A. R. ^{[3
,15
]}

Lorente, N. P. F. ^{[3
]}

McElroy, R. ^{[1
,2
]}

Medling, A. M. ^{[4
]}

Mould, J. ^{[8
]}

Norberg, P. ^{[12
]}

Parker, Q. A. ^{[3
,15
,16
]}

Power, C. ^{[2
,10
]}

Pracy, M. B. ^{[1
]}

Richards, S. N. ^{[1
,2
,3
]}

Robotham, A. S. G. ^{[10
]}

Sweet, S. M. ^{[4
,9
]}

Taylor, E. N. ^{[17
]}

Thomas, A. D. ^{[9
]}

Tonini, C. ^{[8
]}

Walcher, C. J. ^{[18
]}

机构：

[1] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia

[2] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2016, Australia

[3] Australian Astron Observ, N Ryde, NSW 1670, Australia

[4] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia

[5] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA

[6] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[7] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England

[8] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

[9] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia

[10] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia

[11] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland

[12] Univ Durham, Dept Phys, ICC, Durham DH1 3LE, England

[13] Univ Sydney, Sch Phys, IPOS, Sydney, NSW 2006, Australia

[14] European So Observ, D-85748 Garching, Germany

[15] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia

[16] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia

[17] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia

[18] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 446卷 / 02期

基金：

澳大利亚研究理事会;

关键词：

techniques: imaging spectroscopy; galaxies: evolution; galaxies: kinematics and dynamics; galaxies: structure; MASS ASSEMBLY GAMA; STAR-FORMATION RATE; SURFACE BRIGHTNESS; OPTIMAL EXTRACTION; REDSHIFT SURVEY; EVOLUTION; CALIFA; SPECTROSCOPY; METALLICITY; MORPHOLOGY;

D O I：

10.1093/mnras/stu2057

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the Early Data Release of the Sydney-AAOMulti-object Integral field spectrograph (SAMI) Galaxy Survey. The SAMI Galaxy Survey is an ongoing integral field spectroscopic survey of similar to 3400 low-redshift (z < 0.12) galaxies, covering galaxies in the field and in groups within the Galaxy And Mass Assembly (GAMA) survey regions, and a sample of galaxies in clusters. In the Early Data Release, we publicly release the fully calibrated data cubes for a representative selection of 107 galaxies drawn from the GAMA regions, along with information about these galaxies from the GAMA catalogues. All data cubes for the Early Data Release galaxies can be downloaded individually or as a set from the SAMI Galaxy Survey website. In this paper we also assess the quality of the pipeline used to reduce the SAMI data, giving metrics that quantify its performance at all stages in processing the raw data into calibrated data cubes. The pipeline gives excellent results throughout, with typical sky subtraction residuals in the continuum of 0.9-1.2 per cent, a relative flux calibration uncertainty of 4.1 per cent (systematic) plus 4.3 per cent (statistical), and atmospheric dispersion removed with an accuracy of 0.09 arcsec, less than a fifth of a spaxel.

引用

页码：1567 / 1583

页数：17

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