Quenching and morphological transformation in semi-analytic models and CANDELS

被引：65

作者：

Brennan, Ryan ^{[1
]}

Pandya, Viraj ^{[2
]}

Somerville, Rachel S. ^{[1
]}

Barro, Guillermo ^{[3
]}

Taylor, Edward N. ^{[4
]}

Wuyts, Stijn ^{[5
]}

Bell, Eric F. ^{[6
]}

Dekel, Avishai ^{[7
]}

Ferguson, Henry C. ^{[8
]}

McIntosh, Daniel H. ^{[9
]}

Papovich, Casey ^{[10
]}

Primack, Joel ^{[11
]}

机构：

[1] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA

[2] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[3] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA

[4] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia

[5] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[6] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[7] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel

[8] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[9] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA

[10] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA

[11] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 451卷 / 03期

关键词：

galaxies: bulges; galaxies: evolution; galaxies: interactions; galaxies: star formation; EARLY-TYPE GALAXIES; MASS ASSEMBLY GAMA; DIGITAL SKY SURVEY; STAR-FORMATION HISTORIES; SUPERMASSIVE BLACK-HOLES; DARK-MATTER HALOS; STELLAR MASS; QUIESCENT GALAXIES; LAMBDA-CDM; PHYSICAL-PROPERTIES;

D O I：

10.1093/mnras/stv1007

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We examine the spheroid growth and star formation quenching experienced by galaxies since z similar to 3 by studying the evolution with redshift of the quiescent and spheroid-dominated fractions of galaxies from the CANDELS (Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey) and GAMA(Galaxy and Mass Assembly) surveys. We compare the observed fractions with predictions from a semi-analytic model which includes prescriptions for bulge growth and AGN feedback due to mergers and disc instabilities. We facilitate direct morphological comparison by converting our model bulge-to-total stellar mass ratios to Sersic indices. We then subdivide our population into the four quadrants of the specific star formation rate-Sersic index plane and study the build-up of each of these subpopulations. We find that the fraction of star-forming discs declines steadily, while the fraction of quiescent spheroids builds up over cosmic time. The fractions of star-forming spheroids and quiescent discs are both non-negligible, and stay nearly constant over the period we have studied. Our model is qualitatively successful at reproducing the evolution of the two 'main' populations (star-forming discs and quiescent spheroids), and approximately reproduces the relative fractions of all four types, but predicts a stronger decline in star-forming spheroids, and increase in quiescent discs, than is seen in the observations. A model with an additional channel for bulge growth via disc instabilities agrees better overall with the observations than a model in which bulges can grow only through mergers. We also examine the relative importance of these different physical drivers of transformation (major and minor mergers and disc instabilities).

引用

页码：2933 / 2956

页数：24

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