A Self-Consistent, Dynamic Model for the Evolution of the Galaxy-Dark Matter Connection across Cosmic Time. Frank van den Bosch.

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1 A Self-Consistent, Dynamic Model for the Evolution of the Galaxy-Dark Matter Connection across Cosmic Time Frank van den Bosch Yale University In collaboration with: Marcello Cacciato (HU), Surhud More (KICP), Xiaohu Yang (SHAO), Houjun Mo (UMass), Youcai Zhang (SHAO), Jiaxin Han (SHAO)

2 Static Methods Sub-Halo Abundance Matching Galaxy Clustering Vale & Ostriker 24, 26; Conroy et al. 26; Shankar et al. 26; Conroy & Wechsler 29; Moster et al. 21; Behroozi et al. 21; Wetzel & White 21 Satellite Kinematics Jing, et al. 1998; Peacock & Smith 2; Berlind & Weinberg 22; Zheng 24; Yang, Mo & vdb 23; vdb, Yang & Mo 23; Tinker et al. 25; vdb et al. 27 Galaxy-Galaxy Lensing Zaritsky & White 1994; McKay et al 22; Prada et al. 23; vdb et al. 24; Conroy et al. 25; Norberg, Frenk & Cole 28; More et al. 29, 211; Galaxy-Group Catalogues Guzik & Seljak 22; Seljak et al. 25; Mandelbaum et al. 26; Yoo et al. 26 Cacciato et al. 29; van Uitert et al. 211; Leauthaud et al. 212; Frank van den Bosch Eke et al. 24; Yang et al. 25, 27, 28, 29; vdb et al. 28; Weinmann et al. 26a,b; Pasquali et al. 21, 212; Wetzel et al. 212 Yale University

3 New Insights from Galaxy Group Catalogues Group Catalogues allow distinction between centrals and satellites. Comparing centrals to satellites provides insight into satellite-specific processes. Source: Yang, Mo & vdb et al. 29, ApJ, 695, 9 SAMs over-quench satellites 1 12 h 1 M See also: vdb et al. 28; Kimm et al.29; Wetzel et al Source: Weinmann, vdb et al. 26, MNRAS, 372, 1161

4 The Abundance of Satellite Galaxies SDSS Y7 GC DB7 true DB7 GC Source: Liu, Yang Mo, vdb & Springel, 21, ApJ, 712, 734 Semi-Analytical Models predict too many satellite galaxies See also: Conroy, Ho & White 27; Conroy, Wechsler & Kravtsov 29; Kang & vdb 28; Yang, Mo & vdb 29; Henriques & Thomas 29

5 Stellar Metallicities of Centrals and Satellites Source: Pasquali et al. 21, MNRAS, 47, 937 Satellites have higher metallicity than centrals of same stellar mass. Satellites of given M have higher metallicity in more masive host halo

6 Stellar Metallicities of Centrals and Satellites Source: Pasquali et al. 21, MNRAS, 47, 937 Satellites have higher metallicity than centrals of same stellar mass. Satellites of given M have higher metallicity in more masive host halo Satellite Galaxies experience large amount of mass stripping

7 A Dynamic, Self-Consistent Model central galaxies Φ c (M M,z) = 1 2πσ c EXP (log M /M ) 2 2σ 2 c M = M (M,z) σ c = σ c (z) Yang et al. 211, ApJ, 741, 13 Yang et al. 212, ApJ, 752, 41 } 9 free parameters Frank van den Bosch Yale University

8 A Dynamic, Self-Consistent Model central galaxies Φ c (M M,z) = 1 2πσ c EXP (log M /M ) 2 2σ 2 c M = M (M,z) σ c = σ c (z) Yang et al. 211, ApJ, 741, 13 Yang et al. 212, ApJ, 752, 41 } 9 free parameters satellite galaxies are centrals at infall: Φ s (M M,z) = dm,a M dm a dz a M dm a 1 dη Φ c (M,a m a,z a ) n sub (m a,z a M,z) z P (M,z M,a,z a ; m a ; M a,η) P (M a,z a M,z) P (η) Frank van den Bosch Yale University

9 A Dynamic, Self-Consistent Model central galaxies Φ c (M M,z) = 1 2πσ c EXP (log M /M ) 2 2σ 2 c M = M (M,z) σ c = σ c (z) Yang et al. 211, ApJ, 741, 13 Yang et al. 212, ApJ, 752, 41 } 9 free parameters satellite galaxies are centrals at infall: M M 1 Φ s (M M,z) = dm,a dm a dz a dm a dη Φ c (M,a m a,z a ) n sub (m a,z a M,z) z P (M,z M,a,z a ; m a ; M a,η) P (M a,z a M,z) P (η) a simplified model for the evolution of satellites: P (M,z M,a,z a ; m a ; M a,η)= { δd (M M ) if t <αt df (m, M, z, η) otherwise M =(1 c) M,a + c M,c (m a,z) α `satellite disruption parameter c `satellite mass growth parameter Frank van den Bosch Yale University

10 Fit to Stellar Mass Functions across Cosmic Time Data: Yang et al (29; z~.1) Perez-Gonzales et al. (28) Fit : α= --> no sats Source: Yang et al. 212, ApJ, 752, 41 Fit 1 : α= --> no evolution 2PCF : fit to Φ(M ) + 2PCF CSMF : fit to Φ(M ) + Φ(M M,z=)

11 Fit to Two-Point Correlation Functions at z=.1 Data: SDSS DR7 (Yang et al. 212) Fit : α= --> no sats Source: Yang et al. 212, ApJ, 752, 41 Fit 1 : α= --> no evolution 2PCF : fit to Φ(M ) + 2PCF CSMF : fit to Φ(M ) + Φ(M M,z=)

12 Fit to Conditional Stellar Mass Functions at z=.1 Data: SDSS Galaxy Group Catalogues (Yang et al. 29) best-fit value for c ~.95 +/-.5 indicating that sats continue to grow in stellar mass after accretion, in excellent agreement with recent results by Wetzel et al. (212) Fit : α= --> no sats Source: Yang et al. 212, ApJ, 752, 41 Fit 1 : α= --> no evolution 2PCF : fit to Φ(M ) + 2PCF CSMF : fit to Φ(M ) + Φ(M M,z=)

13 Source: Yang et al. 212, ApJ, 752, 41 Comparison of Stellar Mass - Halo Mass Relations Main uncertainty arises from uncertainties in observational constraints on stellar mass functions at high redshift SMF1: Perez-Gonzales et al. (28) SMF2: Drory et al. (25)

14 Stellar Assembly Histories of Galaxies centrals surviving satellites accreted satellites stellar halo Source: Yang et al. 212, ApJ, 752, 41

15 The Stellar Assembly History of Central Galaxies Stellar Mass Growth is truncated ones halo mass reaches 1 12 h 1 M

16 Wetzel et al. 212 (arxiv: ) Mass growth, quenching & stripping Central galaxies grow in stellar mass until host halo mass 1 12 h 1 M Tidal disruption of satellite galaxies is an important ingredient. It explains both satellite abundances and ICL/stellar halos. Mihos et al (25) See also: Conroy et al. 27; Kang & vdbosch 28; Yang, Mo & vdbosch 29; Pasquali et al. 21 Yang et al. 212, ApJ, 752, 41 Satellites continue to grow in stellar mass after accretion for 2-4 Gyr. After that they quench rapidly (in Gyr). See also: Weinmann et al. 26, 29; vdb et al. 28; Kimm et al. 29; Wetzel et al. 212

17 CONCLUSIONS Satellite Galaxies are very different from Central Galaxies. We presented the first fully self-consistent, dynamic model of the galaxy-dark matter connection across cosmic time. The model accurately matches all data (stellar mass functions, correlation functions, conditional stellar mass functions) Limiting factor is accuracy of stellar mass functions at high z. Time scale for satellite disruption ~ dynamical friction time. Satellites continue to grow in stellar mass very much like centrals of the same stellar mass (see also Wetzel et al. 212) 12 Central galaxies `quench once halo mass reaches ~1 Msun Stellar mass growth is COMPLETELY decoupled from halo mass growth; 12 star formation only happens over ~1 decade in halo mass: 1-1 Msun 11