Galaxy and Mass Assembly (GAMA): maximum-likelihood determination of the luminosity function and its evolution

被引：58

作者：

Loveday, J. ^{[1
]}

Norberg, P. ^{[2
]}

Baldry, I. K. ^{[3
]}

Bland-Hawthorn, J. ^{[4
]}

Brough, S. ^{[5
]}

Brown, M. J. I. ^{[6
]}

Driver, S. P. ^{[7
,8
]}

Kelvin, L. S. ^{[9
]}

Phillipps, S. ^{[10
]}

机构：

[1] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England

[2] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England

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

[4] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia

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

[6] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia

[7] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia

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

[9] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[10] Univ Bristol, HH Wills Phys Lab, Astrophys Grp, Bristol BS8 1TL, Avon, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 451卷 / 02期

基金：

欧洲研究理事会; 英国科学技术设施理事会;

关键词：

galaxies: evolution; galaxies: luminosity function; mass function; galaxies: statistics; DIGITAL SKY SURVEY; STELLAR MASS; REDSHIFT SURVEY; SURFACE BRIGHTNESS; FIELD; DENSITY; DEPENDENCE; MAGNITUDE; COUNTS;

D O I：

10.1093/mnras/stv1013

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We describe modifications to the joint stepwise maximum-likelihood method of Cole in order to simultaneously fit the Galaxy and Mass Assembly II galaxy luminosity function (LF), corrected for radial density variations, and its evolution with redshift. The whole sample is reasonably well fitted with luminosity (Q(e)) and density (P-e) evolution parameters Q(e), P-e approximate to 1.0, 1.0 but with significant degeneracies characterized by Q(e) approximate to 1.4 - 0.4 P-e. Blue galaxies exhibit larger luminosity density evolution than red galaxies, as expected. We present the evolution-corrected r-band LF for the whole sample and for blue and red subsamples, using both Petrosian and Sersic magnitudes. Petrosian magnitudes miss a substantial fraction of the flux of de Vaucouleurs profile galaxies: the Sersic LF is substantially higher than the Petrosian LF at the bright end.

引用

页码：1540 / 1552

页数：13

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