Comparing l-galaxies, galform and eagle

Transcription

1 V. Gonzalez-Perez /9 Comparing l-galaxies, galform and eagle Violeta Quan Guo (Postdam), Qi Guo (Beijing), Matthieu Schaller (Durham), Michelle Furlong (Durham), Richard Bower (Durham), Shaun Cole (Durham), Rob Crain (Liverpool), Carlos Frenk (Durham), John Helly (Durham), Cedric Lacey (Durham), Claudia Lagos (ICRAR), Peter Mitchell (Durham), Joop Schaye (Leiden), Tom Theuns (Durham), Carlton Baugh (Durham) and Peder Norberg (Durham)

2 The processes that need modelling: gravity alone is not enough. Gonzalez-Perez 2/9 log(φ/dlogm Mpc 3 h 3 ) Panter+07 Schechter fit M halo,db *0.04/0.308 Normalised M halo,db f b Baldry log 0 (M/M h ) If we assume a simple approach: There are more DM halos than galaxies at the faint and bright ends. ( Galaxy formation is an inefficient process!

3 The processes that need modelling: gravity alone is not enough. Gonzalez-Perez 2/9 If we assume a simple approach: There are more DM halos than galaxies at the faint and bright ends. ( Galaxy formation is an inefficient process! Galaxies are NOT shaped only by gravity. Gas physics, stellar formation and feedback, mergers, etc., also shape galaxies.

4 How to proceed? V. Gonzalez-Perez 3/9 a) In parallel: hydrodynamical simulations b) In series: SAMs, SHAMs, HOD modelling

5 The eagle simulation V. Gonzalez-Perez 4/9 Hydro simulation using gadget-3 (SPH) + anarchy 00 Mpc box with a 0 6 M gas mass resolution Planck cosmology

6 The l-galaxies semi-analytical model V. Gonzalez-Perez 5/9 ΛCDM Cosmology DM Merger trees

7 The galform semi-analytical model (G6) ΛCDM Cosmology DM Merger trees Using analytical equations, containing free parameters, galform calculates the physical processes affecting the evolution of galaxies: Gas cooling Disk formation Galaxy mergers Spheroids SF & Feedback Chemical Evolution Stellar population & Extinction Parameter GP4 G6 IMF Kennicutt Chabrier Yield Recycle fraction SPS model BC99 Conroy+0 Stripping of hot gas in satellite galaxies Instantaneous Gradual α cool V. Gonzalez-Perez 6/9

8 The effect of changing the mass resolution. Gonzalez-Perez 7/9 0 log(φ/h 3 Mpc 3 mag ) 2 3 MS-W7 haloes > 0 0 M /h EagleDM haloes > 0 8 M /h 4 GP GP4+Eagle+Cha GP4+Eagle+Cha, Mhalo>0 GP4+Eagle+Cha+GRP GP4+Eagle+Cha+GRP, Mhalo>0 Baldry+202, z< log(m /M h )

9 Starting point: the stellar mass function V. Gonzalez-Perez 8/9 Schaye+5 See also Somerville and Dave 205

10 Compared mass functions log(dn/dlog 0 (M h )/Mpc 3 ) z = 0 z = 2 GALFORM EAGLE L-GALS z = 0 GALFORM 2.0 EAGLE 2.5 L-GALS log 0 (M halo /M ) log 0 (M /M ) V. Gonzalez-Perez 9/9 log 0 (dn/dlog 0 (M /M )/Mpc 3 ) Baldry+ 202 Li&White 2009 Muzzin+ 3 (.0<z<.5) Muzzin+ 3 (0.5<z<.0) Ilbert+ 3 (0.8<z<.) Ilbert+ 3 (.<z<.5).5 z = 2 Muzzin+ 3 (2.0<z<2.5) Muzzin+ 3 (.5<z<2.0) Ilbert+ 3 (2.0<z<2.5) Ilbert+ 3 (.5<z<2.0)

11 The M M halo relation log 0 (M /M ) z = 0 z = 2 GALFORM L-GALS EAGLE log 0 (M halo /M ) V. Gonzalez-Perez 0/9

12 The SF sequence from different models EAGLE z = 0 GALFORM 0 L-GALS ) log 0 (ssfr/gyr z= z= V. Gonzalez-Perez dp/dlog 0 (M ) dlog 0 (ssfr) log 0 (M /M ) log 0 (M /M ) -3.5 log 0 (M /M ) /9

13 The SFRD and ssfr evolution ssfr t growth z < log 0 (M /M ) < 0. 0 EAGLE SF L-GALS SF GALFORM (Grad.) SF GALFORM (Instant.) SF 0. 0 < log 0 (M /M ) < < log 0 (M /M ) < Gonzalez-Perez t lb /Gyr 2/9 log 0 ( ρ /M yr Mpc 3 ) t growth (Gyr ) = dm/dt M(z) M(z) = M 0 (+z) α e βz t lb /Gyr GALFORM EAGLE L-GALS Gilbank+ 0 (H α ) Karim+ (radio) Rodighiero+ 0 (24µm) Cucciati+ 2 (FUV) Burgarella+ 3 (FUV+IR)

14 The evolution of the ssfr compared with observations V. Gonzalez-Perez 3/9

15 The passive fractions Passive Fraction z = log 0 (M /M ) All Satellites Centrals log 0 (M /M ) z = 2 GALFORM (Instant.) GALFORM (Grad.) EAGLE L-GALS log 0 (M /M ) V. Gonzalez-Perez 4/9

16 The GSMF split in to passive and star-forming galaxies log 0 (dn/dlog 0 (M /M )/Mpc 3 ) SF Centrals Reclassified z = log 0 (M /M ) Passive Centrals z = 0 log 0 (M /M ) SF Satellites z = 0 log 0 (M /M ) Passive Satellites EAGLE L-GALS z = 0 GALFORM (Instant.) GALFORM (Grad.) log 0 (M /M ) V. Gonzalez-Perez 5/9

17 Metallicity z = z = GALFORM L-GALS EAGLE Zahid+ 3 (z=0.08) Tremonti+ 04 L-GALS EAGLE GALFORM log 0 (Z ) log 0 (O/H) Zahid+ 3 (z=0.78) Zahid+ 3 (z=.4) z = z = Zahid+ 3 (z=2.26) log 0 (M /M ) log 0 (M /M ) V. Gonzalez-Perez 6/9

18 Sizes.0 z = GALFORM EAGLE L-GALS log 0 (r 50 /kpc) z = V. Gonzalez-Perez /9

19 Conclusions V. Gonzalez-Perez 8/9 The stellar mass assembly history closely follows that of the dark matter, which is not the case for observations. The GSMF and SF sequence in SAMs have very similar evolution to hydrodynamical simulations. The modelling of sizes needs a major improvement. The problem is: sizes affect everything! The observed mass-metallicity relation is not reproduced by models which points to a excesively crude modelling of flows. Guo, Gonzalez-Perez et al., 206.

20 The luminosity function of [OII] emitters at 0.6 < z < log 0 (Φ/Mpc 3 dlog 0 L) All, z=0.76 F >0 6 erg s cm 2 Dr< 23.5 R< 24. Di< 22.5 log 0 (Φ/Mpc 3 dlog 0 L) All, z=0.99 F >0 6 erg s cm 2 Dr< 23.5 R< Di< 24.0 VVDS-DEEP, 0.65<z< Di< 22.5 Di< 24.0 VVDS-WIDE, 0.65<z< Comparat+4, z= log 0 (L[OII]/erg s ) log 0 (L[OII]/erg s ) 2 2 log 0 (Φ/Mpc 3 dlog 0 L) All, z=.7 F >0 6 erg s cm 2 6 Dr< 23.5 R< 24. Di< Di< 24.0 Comparat+4, z=.2 Comparat+4, z= log 0 (L[OII]/erg s ) log 0 (L[OII]/erg s ) V. Gonzalez-Perez 9/9 log 0 (Φ/Mpc 3 dlog 0 L) All, z=.5 F >0 6 erg s cm 2 6 Dr< 23.5 R< 24. Di< Di< 24.0