Galaxy formation in the Planck cosmology - I. Matching the observed evolution of star formation rates, colours and stellar masses

被引：552

作者：

Henriques, Bruno M. B. ^{[1
]}

White, Simon D. M. ^{[1
]}

Thomas, Peter A. ^{[2
]}

Angulo, Raul ^{[3
]}

Guo, Qi ^{[4
]}

Lemson, Gerard ^{[1
]}

Springel, Volker ^{[5
,6
]}

Overzier, Roderik ^{[7
]}

机构：

[1] Max Planck Inst Astrophys, D-85741 Garching, Germany

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

[3] Ctr Estudios Fis Cosmos Aragon, E-44001 Teruel, Spain

[4] Chinese Acad Sci, Natl Astron Observ, Max Planck Inst Astrophys, Partner Grp, Beijing 100012, Peoples R China

[5] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany

[6] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany

[7] Observ Nacl MCTI, BR-20921400 Rio De Janeiro, RJ, Brazil

来源：

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

基金：

英国科学技术设施理事会; 欧洲研究理事会;

关键词：

methods: analytical; methods: statistical; galaxies: evolution; galaxies: formation; galaxies: high-redshift; DIGITAL-SKY-SURVEY; DARK-MATTER HALOS; SEMIANALYTIC MODELS; FORMATION HISTORIES; POPULATION SYNTHESIS; QUIESCENT GALAXIES; SATELLITE GALAXIES; LUMINOSITY FUNCTION; PHYSICAL-PROPERTIES; FORMING SEQUENCE;

D O I：

10.1093/mnras/stv705

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have updated the Munich galaxy formation model to the Planck first-year cosmology, while modifying the treatment of baryonic processes to reproduce recent data on the abundance and passive fractions of galaxies from z=3 down to z=0. Matching these more extensive and more precise observational results requires us to delay the reincorporation of wind ejecta, to lower the surface density threshold for turning cold gas into stars, to eliminate ram-pressure stripping in haloes less massive than similar to 10(14) M-circle dot, and to modify our model for radio mode feedback. These changes cure the most obvious failings of our previous models, namely the overly early formation of low-mass galaxies and the overly large fraction of them that are passive at late times. The new model is calibrated to reproduce the observed evolution both of the stellar mass function and of the distribution of star formation rate at each stellar mass. Massive galaxies (log M-star/M-circle dot >= 11.0) assemble most of their mass before z = 1 and are predominantly old and passive at z = 0, while lower mass galaxies assemble later and, for log M-star/M-circle dot <= 9.5, are still predominantly blue and star forming at z = 0. This phenomenological but physically based model allows the observations to be interpreted in terms of the efficiency of the various processes that control the formation and evolution of galaxies as a function of their stellar mass, gas content, environment and time.

引用

页码：2663 / 2680

页数：18

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