Galaxy And Mass Assembly (GAMA): the 0.013 < z < 0.1 cosmic spectral energy distribution from 0.1 μm to 1 mm

被引：90
|
作者：
Driver, S. P. [1 ,2 ]
Robotham, A. S. G. [1 ,2 ]
Kelvin, L. [1 ,2 ]
Alpaslan, M. [1 ,2 ]
Baldry, I. K. [3 ]
Bamford, S. P. [4 ]
Brough, S. [5 ]
Brown, M. [6 ]
Hopkins, A. M. [5 ]
Liske, J. [7 ]
Loveday, J. [8 ]
Norberg, P. [9 ]
Peacock, J. A. [10 ]
Andrae, E. [11 ]
Bland-Hawthorn, J. [12 ]
Bourne, N. [4 ]
Cameron, E. [13 ]
Colless, M. [5 ]
Conselice, C. J. [4 ]
Croom, S. M.
Dunne, L. [14 ]
Frenk, C. S. [9 ]
Graham, Alister W. [15 ]
Gunawardhana, M. [12 ]
Hill, D. T. [2 ]
Jones, D. H. [6 ]
Kuijken, K. [16 ]
Madore, B. [17 ]
Nichol, R. C. [18 ]
Parkinson, H. R. [10 ]
Pimbblet, K. A. [6 ]
Phillipps, S. [19 ]
Popescu, C. C. [20 ]
Prescott, M. [3 ]
Seibert, M. [17 ]
Sharp, R. G. [21 ]
Sutherland, W. J. [22 ]
Taylor, E. N. [12 ]
Thomas, D. [18 ]
Tuffs, R. J. [11 ]
van Kampen, E. [7 ]
Wijesinghe, D. [12 ]
Wilkins, S. [23 ]
机构：
[1] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia
[2] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland
[3] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England
[4] Univ Nottingham, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England
[5] Australian Astron Observ, Epping, NSW 1710, Australia
[6] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia
[7] European So Observ, D-85748 Garching, Germany
[8] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England
[9] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England
[10] Univ Edinburgh, Inst Astron, Royal Observ, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland
[11] Max Planck Inst Nucl Phys MPIK, D-69117 Heidelberg, Germany
[12] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia
[13] Queensland Univ Technol, Sch Math Sci, Brisbane, Qld 4001, Australia
[14] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand
[15] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia
[16] Leiden Univ, NL-2300 RA Leiden, Netherlands
[17] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA
[18] Univ Portsmouth, Inst Cosmol & Gravitat ICG, Portsmouth PO1 3FX, Hants, England
[19] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England
[20] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England
[21] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Western Creek, ACT 2611, Australia
[22] Queen Mary Univ London, Astron Unit, London E1 4NS, England
[23] Univ Oxford, Sch Phys & Astron, Oxford OX1 3RH, England
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 427卷 / 04期
基金：
美国国家航空航天局; 美国国家科学基金会;
关键词：
surveys; galaxies: fundamental parameters; galaxies: general; galaxies: luminosity function; mass function; cosmology: observations; infrared: galaxies; DIGITAL-SKY-SURVEY; EXTRAGALACTIC BACKGROUND LIGHT; LUMINOSITY FUNCTION; REDSHIFT SURVEY; STAR-FORMATION; HERSCHEL-ATLAS/GAMA; PHOTOMETRIC SYSTEM; CATALOG; CALIBRATION; EVOLUTION;
D O I：
10.1111/j.1365-2966.2012.22036.x
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We use the Galaxy And Mass Assembly survey (GAMA) I data set combined with GALEX, Sloan Digital Sky Survey (SDSS) and UKIRT Infrared Deep Sky Survey (UKIDSS) imaging to construct the low-redshift (z < 0.1) galaxy luminosity functions in FUV, NUV, ugriz and YJHK bands from within a single well-constrained volume of 3.4 x 10(5) (Mpc h(-1))(3). The derived luminosity distributions are normalized to the SDSS data release 7 (DR7) main survey to reduce the estimated cosmic variance to the 5 per cent level. The data are used to construct the cosmic spectral energy distribution (CSED) from 0.1 to 2.1 mu m free from any wavelength-dependent cosmic variance for both the elliptical and non-elliptical populations. The two populations exhibit dramatically different CSEDs as expected for a predominantly old and young population, respectively. Using the Driver et al. prescription for the azimuthally averaged photon escape fraction, the non-ellipticals are corrected for the impact of dust attenuation and the combined CSED constructed. The final results show that the Universe is currently generating (1.8 +/- 0.3) x 10(35) h W Mpc(-3) of which (1.2 +/- 0.1) x 10(35) h W Mpc-3 is directly released into the inter-galactic medium and (0.6 +/- 0.1) x 10(35) h W Mpc(-3) is reprocessed and reradiated by dust in the far-IR. Using the GAMA data and our dust model we predict the mid- and far-IR emission which agrees remarkably well with available data. We therefore provide a robust description of the pre- and post-dust attenuated energy output of the nearby Universe from 0.1 mu m to 0.6 mm. The largest uncertainty in this measurement lies in the mid- and far-IR bands stemming from the dust attenuation correction and its currently poorly constrained dependence on environment, stellar mass and morphology.
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页码：3244 / 3264
页数：21
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