The formation of massive, quiescent galaxies at cosmic noon

0.88 MB·

by  Robert Feldmann

MNRAS000,1–5(2016) Preprint20January2016 CompiledusingMNRASLATEXstylefilev3.0
The formation of massive, quiescent galaxies at cosmic
noon
Robert Feldmann1(cid:63), Philip F. Hopkins2, Eliot Quataert1,
Claude-Andr´e Faucher-Gigu`ere3, and Duˇsan Kereˇs4
1Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
2TAPIR 350-17, California Institute of Technology, Pasadena, CA 91125, USA
3Department of Physics and Astronomy and CIERA, Northwestern University, Evanston, IL 60208, USA
6 4Center for Astrophysics and Space Sciences, University of California, San Diego, CA 92093, USA
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AcceptedXXX.ReceivedYYY;inoriginalformZZZ

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ABSTRACT

8 The cosmic noon (z ∼ 1.5−3) marked a period of vigorous star formation for most
1 galaxies.However,aboutathirdofthemoremassivegalaxiesatthosetimeswerequi-

escent in the sense that their observed stellar populations are inconsistent with rapid
]
A star formation. The reduced star formation activity is often attributed to gaseous
outflows driven by feedback from supermassive black holes, but the impact of black
G
holefeedbackon galaxies intheyoung Universeisnotyet definitivelyestablished.We
. analyze the origin of quiescent galaxies with the help of ultra-high resolution, cosmo-
h
p logical simulations that include feedback from stars but do not model the uncertain
- consequencesofblackholefeedback.Weshowthatdarkmatterhaloswithspecificac-
o cretion rates below ∼0.25−0.4 Gyr−1 preferentially host galaxies with reduced star
r
t formation rates and red broad-band colors. The fraction of such halos in large dark
s matter only simulations matches the observed fraction of massive quiescent galaxies
a
(∼1010−1011 M ). This strongly suggests that halo accretion rate is the key param-
[ (cid:12)
eter determining which massive galaxies at z ∼ 1.5−3 become quiescent. Empirical

1 models that connect galaxy and halo evolution, such as halo occupation distribution
v or abundance matching models, assume a tight link between galaxy properties and
4
the masses of their parent halos. These models will benefit from adding the specific
0
accretion rate of halos as a second model parameter.
7
4 Key words: galaxies: formation – galaxies: evolution – galaxies: high-redshift
0
.
1
0
6
1 INTRODUCTION choicetotestthisproposedpicture,butuntilnownoexist-
1
: ingsimulationproducedbothagalaxysampleoftheneces-
v There is mounting evidence that star formation in galaxies sary size for statistical analysis and properly resolved and
i is tied to the accretion of gas from intergalactic distances
X modeled the relevant physical processes that take place in
(e.g., Dekel et al. 2009; Cresci et al. 2010; Lilly et al. 2013;
galaxies at z ∼ 1.5−3. In addition, cosmological, hydro-
r Sa´nchezAlmeidaetal.2014;Martinetal.2014;Rodriguez-
a dynamical simulations have a long history of struggling to
Puebla et al. 2015; Brisbin et al. 2015; Narayanan et al.
reproduce key properties of observed galaxies such as their
2015).Hence,reducedgasaccretionontogalaxiescouldpo-
typicalstellarmassesandstarformationrates(Scannapieco
tentiallyberesponsibleforthereducedstarformationrates
et al. 2012). The present study, MassiveFIRE, overcomes
(SFRs)ofquiescentgalaxies(Feldmann&Mayer2015).The
thesechallengesbyadoptingtheaccuratephysicalmodeling
reducedsupplyofgastogalaxiesandhaloswouldalsomake
of the Feedback In Realistic Environments (FIRE) project
it easier for additional processes, e.g., black hole feedback
(Hopkins et al. 2014) and by applying it, for the first time,
(e.g., Ciotti & Ostriker 1997; Di Matteo et al. 2005; Si-
to a population of massive galaxies.
jacki & Springel 2006; Teyssier et al. 2011; Kormendy &
Wehavesimulatedtheevolutionof35massivegalaxies
Ho 2013), to fully suppress any remaining star formation
for the first 4 billion years after the Big Bang (until red-
activityinquiescentgalaxies(Dekel&Birnboim2006;Cat-
shiftz≥1.67).Thegalaxysampleisextractedfrom17dis-
taneo et al. 2006). Numerical simulations are the tool of
tinct sub-regions, each containing at least one dark matter
(DM)halowithamassintherange3×1012−3×1013 M ,
(cid:12)
(cid:63) E-mail:[email protected](RF) embedded in a representative volume of the Universe. The
(cid:13)c 2016TheAuthors
2 R. Feldmann et al.
sub-regions sample the full range of cosmological assembly 1012
MassiveFIRE
histories of halos harboring massive galaxies, i.e., galaxies
z=2
lwaittihonsstealrlaerrmunaswseitshlatrhgeerhythdarondaybnoaumtic1s01a0ndMg(cid:12)r.avOituyrssoimlvuer- 1011 zz==59
GIZMO(Hopkins2015)atultra-highspatial(∼10pc)and High resolution
Medium resolution
mass resolution (m = 3.3×104 M at high resolution, 10
gas (cid:12) 10 Centrals
2.7×105 M(cid:12) at medium resolution) in P-SPH mode. The Satellites
high numerical resolution allows us to model reliably many
9
olafrtmheedrieulmevaonftgparlaoxceiesss.esSttehlalatrtfaekeedbpalcakceprinoctehsseesinstuecrhsteals- M]sun10
energy and momentum injection from supernovae, stellar M[star108
winds, photo-heating, and radiation pressure interact in a
non-linearmanner(Hopkinsetal.2012)andareallincluded
7
inoursimulationswithlittlerelianceontunableparameters. 10
Feedback from supermassive black holes (SMBH) is not in-
cluded. We will present the setup and methodology of our 6 Moster et al. 2013
simulations in more detail in Feldmann et al. in prep. 10 z=2
z=5
We showed in previous work that the computational
z=9
approach of this paper reproduces well the integral prop- 105
9 10 11 12 13 14
erties of lower mass galaxies (M∗ (cid:46) 3×1010 M ) since 10 10 10 10 10 10
(cid:12)
M [M ]
cosmicnoon.Forinstance,wereportedontheSHMR(Hop- vir sun
kins et al. 2014), on the stellar mass – metallicity relation
Figure1.Stellar-to-halo-massrelation(SHMR)ofMassiveFIRE
(Ma et al. 2015), and on the properties of galactic outflows galaxies at z = 2 (green circles), z = 5 (purple circles), and
drivenbystellarfeedback(Muratovetal.2015)findinggood z = 9 (cyan circles). Central (satellite) galaxies at each redshift
agreementwithavailableobservations.Wealsoshowedthat areshownbyfilled(empty)circles,andlarge(small)circlesdenote
theH coveringfractionsin(cid:46)1012M halosatcosmicnoon galaxiessimulatedathigh(medium)numericalresolution.Dotted
I (cid:12)
match observations (Faucher-Gigu`ere et al. 2015). We will linesshowanempiricalestimate(Mosteretal.2013)oftheSHMR
reportcorrespondingpropertiesofMassiveFIREgalaxiesin anditsextrapolationtohighredshiftsandlowstellarmasses.The
1−σ scatter of individual galaxies above and below the mean
upcoming work.
relation is about 0.2 dex (Reddick et al. 2013) (shaded region).
SatellitegalaxiestendtolietotheleftoftherelationastheirDM
2 RESULTS AND DISCUSSION halosareoftentidallystripped.MassiveFIREgalaxieshavestellar
massesinfairagreementwiththeempiricallyderivedSHMR.
Figure1comparesthestellarmassesofMassiveFIREgalax-
ies with those of actual galaxies that reside in DM halos of
similarmass.StellarmassesofMassiveFIREgalaxiesagree, servations (Lee et al. 2013). In contrast, quiescent galaxies
to within a factor of ∼ 2, with the empirically inferred es- often have an early type morphology with a more compact
timateofthestellar-to-halo-massrelation(SHMR)(Moster stellar distribution (van der Wel et al. 2014) and contain
et al. 2013) at z = 2 and its extrapolation to higher red- only low levels of dust and cold gas (bottom row of Fig. 2).
shifts. We note, however, that the exact functional form of The specific SFR for both star forming and quiescent
theSHMRrelationdifferssomewhatamongstudies(Moster galaxies in the MassiveFIRE sample is shown in Figure 3.
et al. 2013; Behroozi et al. 2013; Garrison-Kimmel et al. WemeasurethespecificSFRin5kpcradiitoroughlymimic
2014). aperture based flux measurements (Whitaker et al. 2011;
Fig. 2 shows four typical example galaxies from Mas- Schreiber et al. 2015) and to minimize potential contribu-
siveFIRE. Each panel displays a composite image (in rest- tionsfromlowmasssatellitegalaxies.SpecificSFRschange
frame U, V, and J broad-band filters) of the dust repro- typically by less than 0.1 dex if measured within a radius
cessed star light. Following conventional practice (Wuyts of 0.1 R instead. Star forming galaxies at cosmic noon
vir
et al. 2007; Williams et al. 2009; Whitaker et al. 2011) we have high specific SFRs of the order of ∼ 1 Gyr−1, while
classify galaxies as quiescent based on their U-V and V-J quiescent galaxies form stars at significantly lower specific
broadbandcolors;specifically,ifU−V >1.2,V −J <1.4, rates.WenotethatinmostcasestheSFRsofgalaxiesclas-
and U −V >0.88×(V −J)+0.59. Our sample contains 8 sified as quiescent remain low for extended periods of time
quiescentand15starformingcentralgalaxies(galaxiesthat (>3×108 yr). The specific SFRs of MassiveFIRE galaxies
dominate the central potential well of their host DM halo), are in good agreement with observations (Schreiber et al.
and 4 quiescent and 8 star forming satellites (galaxies or- 2015; Brammer et al. 2011).
bitingacentralgalaxy).Starforminggalaxieshaveyounger We fit the growth history of the (cold) baryonic mass
stellarpopulationsthanquiescentgalaxies,resultinginbluer (M = M +M +M ) of each galaxy with a modi-
bar HI H2 ∗
intrinsiccolors,althoughintersperseddustlanesextinctand fied exponential ∝ (1+z)βe−γz over an extended redshift
reddenthelightalongparticularlinesofsight(seetoppan- rangestartingfromz=7downtoeitherthefinalsimulation
els of Fig. 2). Fortunately, the color-color classification is snapshotortothelastsnapshotatwhichthegalaxyisstilla
relativelyinsensitivetotheamountofdustreddening.Most central, whichever comes first. Gas and stars within 10% of
star forming galaxies in our sample have a late type mor- the virial radius from the center of a galaxy are considered
phology with either large stellar and gas disks (half mass part of that galaxy. Our results do not change qualitatively
radii > 3 kpc) or irregular shapes, in agreement with ob- ifweusea50%largerorsmallerradiusinstead.Wesimilarly
MNRAS000,1–5(2016)
Massive, quiescent galaxies at cosmic noon 3
-8
10
-9
10
MassiveFIRE
Star forming
-1yr]10-10 Quiescent
R [ Centrals
F Satellites
S
s -11 High res.
10 Medium res.
z=2
z=1.7
Schreiber et al. 2015
-12
10
z=2
z=1.7
10 11
10 10
M [M ]
star sun
Figure 2.Color-compositeimagesoffourcentralgalaxiesinthe Figure3.SpecificSFRwithinthecentral5kpcofMassiveFIRE
MassiveFIRE sample as they would appear in rest-frame U, V, galaxies as function of stellar mass. SFRs are averaged over the
and J bands ∼ 4 billion years after the Big Bang (z = 1.67). past100Myr.Starformingandquiescentgalaxiesareshownby
Galaxiesareshownface-onwitheachimagespanning30kpcon blue and red symbols respectively (the classification is based on
each side. (Top left) a star forming, disk galaxy, (top right) a rest-frameU,V,andJbroadbandfluxes).Linesdenotetheloca-
starforming,irregulargalaxy,(bottomrow)twoexamplesofqui- tion of the star forming sequence inferred from rest-frame ultra-
escent, early type galaxies. Star forming and quiescent galaxies violetandinfraredobservations(Schreiberetal.2015).The1−σ
differintheircolors,morphologies,andlevelsofdustextinction. scatter of individual galaxies above and below the star forming
sequenceatz∼2isabout0.3dex(Daddietal.2007;Whitaker
etal.2012;Schreiberetal.2015)(shadedregion).MassiveFIRE
fit the growth of the DM mass, M , contained within the galaxies classified as star forming have specific SFRs consistent
DM
withtheobservedstarformingsequence.Starformationinquies-
virialradiusofthehalossurroundingthesegalaxies.InFig.4
centgalaxies,however,proceedsatmuchlowerratesthaninstar
we plot dlnM /dt anddlnM /dt for bothstar forming
bar DM forminggalaxiesofcomparablestellarmass.
and quiescent galaxies in MassiveFIRE, linking the growth
ofDMhalostothegrowthofgalaxiesresidingatthecenters
of those halos. The figure demonstrates that most galaxies In agreement with this analysis, dlnM /dt ∼ 0.4
bar
at cosmic noon grow on the same timescale as the DM ha- Gyr−1largelyseparatesstarformingfromquiescentgalaxies
los they live in, complementing previous work that showed intheMassiveFIREsample,asshowninFig.4.Asgalaxies
that baryonic masses and DM masses of halos assemble on andhalosgrowonverysimilartimescales(seeFig.4),wecan
similar timescales (Faucher-Gigu`ere et al. 2011). This is a re-interpret this result in terms of the specific growth rates
non-trivial result as galaxies contain only a small fraction, of DM halos, i.e., dlnM /dt (cid:46) 0.4 Gyr−1 is a necessary
DM
less than a fifth, of the baryons in halos (Papastergis et al. condition for a halo to host a quiescent galaxy at its center
2012). atcosmicnoon.Weproposethatthemajorityofmoderately
At cosmic noon, galaxies with declining SFRs are on massive, quiescent galaxies in the young Universe form via
their way to becoming quiescent. Hence, we may introduce thismechanism,i.e.,theyresideinthesub-setofhalosthat
an alternative definition of “quiescence” that is not based accretegasfromthecosmicwebatsuchlowratesthatthey
on broad-band colors, but on the star formation history of cannotmaintainSFRscharacteristicoftypicalstarforming
galaxies. In particular, by manipulating the standard equa- galaxies (Schreiber et al. 2015). As discussed more below,
tions for one-zone galaxy models including inflow, outflow, numerous halos undergoing such“cosmological starvation”
star formation, and gas build up (e.g., Lilly et al. 2013; (Feldmann&Mayer2015)shouldexistgiventhevariations
Feldmann 2015) the condition of a declining SFR can be inthegravity-drivencollapsehistoriesofDMhalos(McBride
shown to be equivalent to dlnM /dt < X ≡ [1−R+ et al. 2009).
bar crit
dt /dt]/[t +sSFR−1]. Here, t =(M +M )/SFR 35% of the central galaxies and 34% of all galaxies in
dep dep dep HI H2
is the gas depletion time, R is the return fraction of gas oursamplearequiescent.Thesenumberscomparefavorably
fromevolvedstellarpopulations,andsSFR(t)=SFR/M = with observations of quiescent fractions of 25−50% over
∗
AsSFR (M (t),t)isthespecificSFR.sSFR isthespe- a broad stellar mass range (Tomczak et al. 2014; Muzzin
MS ∗ MS
cific SFR of galaxies of the same mass on the star forming et al. 2013); see Fig. 5. We note that the cumulative frac-
sequenceandAcanbederivedfromthecriticalitycondition tion of quiescent galaxies in MassiveFIRE is lower at larger
dSFR/dt=0.Uponinsertingvaluesappropriateforgalaxies stellar masses, while the observed fraction remains remains
intheM ∼1010−1011M range,wefindthatsuchgalax- relatively flat. This difference could point towards missing
∗ (cid:12)
iesshouldbereducingtheirstarformationactivity,andthus physics in our simulations, such as black hole feedback, or
becoming quiescent, when dlnM /dt(cid:46)0.25−0.4 Gyr−1. it could be an artifact related to the low number of galax-
bar
MNRAS000,1–5(2016)
4 R. Feldmann et al.
1.5 log M [M ]
10 star sun
Star forming 10 10.5 10.8 11 11.1 11.2
] Quiescent 1
−1 1.25 Tomczak et al. 2014 z~2
yr Centrals 0.9 Muzzin et al. 2013
G
[ 1 Satellites 0.8 MassiveFIRE (hydro) simulations
dt N-body simulation + analytic model
/
)vir0.75 log10 Mstar 0.7
R 10
0.1 10.5 M) 0.6
(< 0.5 11 (>nt0.5
MH+H+starI20.25 on growth 11.5 fquiesce00..34 Xcrit x1.1
dln 0 ger bary 0.2 xx01..90
on 0.1
−0.25 str
stronger DM growth
0
−0.25 0 0.25 0.5 0.75 1 1.25 1.5 12 12.5 13 13.5 14
dlnMDM(<Rvir)/dt [ Gyr−1] log10Mvir[Msun]
Figure 4. Comparison between the growth rate of baryonic Figure5.Fractionofquiescent,centralgalaxiesresidinginhalos
masses (stars, HI, and H2) of galaxies and the DM masses of aboveagivenmass.ThefractionspredictedbyMassiveFIREare
their parent halos. Red circles and blue squares show quiescent shownbyfilledcircles.Errorbarsindicate1−σ standarddevia-
andstarforminggalaxiesinMassiveFIRE,respectively.Theclas- tionsbasedonabinomialdistributionwiththesamesamplesize
sification is based on rest-frame U-V and V-J colors (Whitaker and quiescent fraction as in MassiveFIRE. For the largest mass
etal.2011)appropriateforz∼2.Filledandemptysymbolsde- binweassumea40%quiescentfractiontocomputetheerrorbar.
note galaxies thatarecentralsorsatellitesbythefinalsnapshot Oursimulationspredictthataboutathirdofmassivegalaxiesat
ofthesimulation(z=1.7−2).Symbolsizesreflectstellarmasses. cosmic noon are quiescent. Solid lines showthe fraction of halos
Forcentralgalaxies,growthratesandcolorsarecomputedatthe withspecificgrowthratesbelowthecriticalvaluerequiredforqui-
finalsnapshotofeachsimulation.Forgalaxiesthatbecomesatel- escentgalaxies(fromFig.4),0.9−1.1×Xcrit∼0.25−0.4Gyr−1,
lites by z ∼ 2, we compute growth rates and colors in the last basedontheMillenniumN-bodysimulation(Springeletal.2005;
snapshotbeforetheyentertheirhosthalo.Thesolidlinemarksa McBride et al. 2009). These theoretical estimates agree reason-
1:1 relationship and is not a fit. Galaxies residing at the centers ablywellwiththeobservedquiescentfractionderivedfromstel-
of fast growing halos (dlnMDM/dt(cid:38)0.4 Gyr−1) are essentially larmassfunctionsofquiescentandstarforminggalaxiesoverthe
alwaysstronglystarforming.Incontrast,slowlygrowing(oreven z=1.5−2.5range(dashed(Tomczaketal.2014)anddot-dashed
shrinking)halostypicallyharborquiescentgalaxies. (Muzzinetal.2013)linesandshadedregions).
Nelsonetal.2013).Bylimitingthesupplyofgastogalaxies
ies (two) in our highest halo mass bin. Hence, whether cos-
and halos, cosmological starvation makes it much easier for
mological starvation is an effective quenching mechanisms
additionalprocesses,e.g.,feedbackfromblackholes,tofully
for galaxies residing in the most massive halos at z = 2
(M >1013 M ,n<10−5 Mpc−3)remainstobestudied counteracthotgascoolingandtoheatorejectanyremaining
halo (cid:12)
coolgas.Cosmologicalstarvationthusenablestheformation
in future work.
ofquiescentgalaxieswithredbroad-bandcolorsandreduced
Fig. 5 also plots the fraction of halos with low specific
SFRs at cosmic noon. However, it may be a necessary but
growth rates based on a large-volume cosmological N-body
not a sufficient condition for completely shutting-down star
simulation (Springel et al. 2005; McBride et al. 2009). The
formation in such galaxies.
fractionofhaloswithdlnM /dt<0.9−1.1X matches
DM crit
The different accretion histories of quiescent and star
fairly well the observed quiescent fraction. The former de-
forminggalaxiesinhalosofthesamemasshaveanumberof
clines slightly towards the largest stellar masses, indicat-
observational consequences. First, as quiescent galaxies are
ing that additional physics besides cosmological starvation
assembled earlier, they will be surrounded by more evolved
islikelyinvolvedinshuttingdownstarformationinthemost
massive galaxies (M > 1011 M ). Fig. 4 shows that there satellite populations. In particular, orbital decay and tidal
∗ (cid:12)
stripping(Zentneretal.2005)shouldreducethenumberof
is overlap between star forming and quiescent galaxies at
satellites of a given stellar mass, and the longer exposure
intermediatespecificgrowthrates.Wefindthatthefraction
(Feldmann et al. 2011) to the hot atmospheres of massive
of slowly accreting halos still matches the observed fraction
galaxiesmayexplaintheincreasedfractionofsatelliteswith
ofquiescentgalaxiesevenifasizablefractionofsuchhalos,
low SFRs (Weinmann et al. 2006). Second, we expect that
e.g., a third, host star forming galaxies.
thedominanthalosofover-denseenvironmentsshouldhave
large accretion rates and, thus, should host vigorously star
3 CONCLUSIONS
forminggalaxies.Incontrast,quiescentgalaxiesatthosered-
The star formation activity of massive galaxies in a young shiftsshouldpreferentiallyresideinaverageorbelowaverage
Universeisultimatelyfueledbytheaccretionofintergalactic environments.Thisideaiscorroboratedbyourfindingthat
gas (Kereˇs et al. 2005; Dekel et al. 2009; Dav´e et al. 2010; 50% (25%) of the quiescent central galaxies vs 13% (73%)
MNRAS000,1–5(2016)
Massive, quiescent galaxies at cosmic noon 5
of the star forming central galaxies in our sample reside in FeldmannR.,CarolloC.M.,MayerL.,2011,Astrophys. J.,736,
the lower (upper) quartile of the local environment density. 88
Third, the clustering of halos of a given mass depends on Garrison-Kimmel S., Boylan-Kolchin M., Bullock J. S., Lee K.,
their formation time, the so-called assembly bias (Wechsler 2014,Mon. Not. R. Astron. Soc.,438,2578
Hearin A. P., Watson D. F., 2013, Mon. Not. R. Astron. Soc.,
et al. 2006). As massive DM halos are less clustered if they
435,1313
collapsed earlier, we predict that massive, quiescent galax-
HopkinsP.F.,2015,Mon. Not. R. Astron. Soc.,450,53
ies at cosmic noon have a lower clustering amplitude than
HopkinsP.F.,QuataertE.,MurrayN.,2012,Mon. Not. R. As-
starforminggalaxiesresidingwithinhalosofthesamemass.
tron. Soc.,421,3522
Finally, we speculate that age-matching (Hearin & Watson Hopkins P. F., Kereˇs D., On˜orbe J., Faucher-Gigu`ere C.-A.,
2013), an empirical correlation between galaxy colors and Quataert E., Murray N., Bullock J. S., 2014, Mon. Not. R.
halo formation time, has its physical origin in cosmological Astron. Soc.,445,581
starvation. KereˇsD.,KatzN.,WeinbergD.H.,Dav´eR.,2005,Mon.Not.R.
Astron. Soc.,363,2
ACKNOWLEDGEMENTS KormendyJ.,HoL.C.,2013,Ann. Rev.Astron.Astrophys.,51,
511
RF was supported in part by NASA through Hubble Fel-
LeeB.,etal.,2013,Astrophys. J.,774,47
lowshipgrantHF2-51304.001-AawardedbytheSpaceTele- LillyS.J.,CarolloC.M.,PipinoA.,RenziniA.,PengY.,2013,
scope Science Institute, which is operated by the Associ- Astrophys. J.,772,119
ation of Universities for Research in Astronomy, Inc., for Ma X., Hopkins P. F., Faucher-Giguere C.-A., Zolman N.,
NASA, under contract NAS 5-26555, in part by the Theo- Muratov A. L., Keres D., Quataert E., 2015, preprint,
retical Astrophysics Center at UC Berkeley, and by NASA (arXiv:1504.02097)
ATP grant 12-ATP-120183. Support for PFH was provided MartinD.C.,ChangD.,MatuszewskiM.,MorrisseyP.,Rahman
S.,MooreA.,SteidelC.C.,2014,Astrophys. J.,786,106
by an Alfred P. Sloan Research Fellowship, NASA ATP
McBrideJ.,FakhouriO.,MaC.-P.,2009,Mon. Not. R. Astron.
Grant NNX14AH35G, and NSF Collaborative Research
Soc.,398,1858
Grant#1411920andCAREERgrant#1455342.CAFGwas
Moster B. P., Naab T., White S. D. M., 2013, Mon. Not. R.
supported by NSF through grants AST-1412836 and AST-
Astron. Soc.,428,3121
1517491, by NASA through grant NNX15AB22G, and by MuratovA.L.,KereˇsD.,Faucher-Gigu`ereC.-A.,HopkinsP.F.,
Northwestern University funds. DK was supported by NSF Quataert E., Murray N., 2015, Mon. Not. R. Astron. Soc.,
grantAST-1412153.EQwassupportedbyNASAATPgrant 454,2691
12-ATP-120183, a Simons Investigator award from the Si- MuzzinA.,etal.,2013,Astrophys. J.,777,18
mons Foundation, and the David and Lucile Packard Foun- NarayananD.,etal.,2015,Nature,525,496
dation.Simulationswererunwithresourcesprovidedbythe Nelson D., Vogelsberger M., Genel S., Sijacki D., Kereˇs D.,
Springel V., Hernquist L., 2013, Mon. Not. R. Astron. Soc.,
NASA High-End Computing (HEC) Program through the
429,3353
NASA Advanced Supercomputing (NAS) Division at Ames
Papastergis E., Cattaneo A., Huang S., Giovanelli R., Haynes
Research Center, proposal SMD-14-5492. Additional com-
M.P.,2012,Astrophys. J.,759,138
puting support was provided by HEC allocation SMD-14-
ReddickR.M.,WechslerR.H.,TinkerJ.L.,BehrooziP.S.,2013,
5189 and NSF XSEDE allocation TG-AST120025. Astrophys. J.,771,30
Rodriguez-Puebla A., Primack J. R., Behroozi P., Faber S. M.,
REFERENCES
2015,preprint, (arXiv:1508.04842)
Behroozi P. S., Wechsler R. H., Conroy C., 2013, Astrophys. J., Sa´nchez Almeida J., Elmegreen B. G., Mun˜oz-Tun˜´on C.,
770,57 ElmegreenD.M.,2014,Astron. Astrophys. Rev.,22,71
BrammerG.B.,etal.,2011,Astrophys. J.,739,24 ScannapiecoC.,etal.,2012,Mon.Not.R.Astron.Soc.,423,1726
Brisbin D., Ferkinhoff C., Nikola T., Parshley S., Stacey G. J., SchreiberC.,etal.,2015,Astron. Astrophys.,575,A74
Spoon H., Hailey-Dunsheath S., Verma A., 2015, Astrophys. SijackiD.,SpringelV.,2006,Mon.Not.R.Astron.Soc.,366,397
J.,799,13 SpringelV.,etal.,2005,Nature,435,629
Cattaneo A., Dekel A., Devriendt J., Guiderdoni B., Blaizot J., Teyssier R., Moore B., Martizzi D., Dubois Y., Mayer L., 2011,
2006,Mon. Not. R. Astron. Soc.,370,1651 Mon. Not. R. Astron. Soc.,414,195
CiottiL.,OstrikerJ.P.,1997,Astrophys. J. Lett.,487,L105 TomczakA.R.,etal.,2014,Astrophys. J.,783,85
Cresci G., Mannucci F., Maiolino R., Marconi A., Gnerucci A., Wechsler R. H., Zentner A. R., Bullock J. S., Kravtsov A. V.,
MagriniL.,2010,Nature,467,811 AllgoodB.,2006,Astrophys. J.,652,71
DaddiE.,etal.,2007,Astrophys. J.,670,156 WeinmannS.M.,vandenBoschF.C.,YangX.,MoH.J.,2006,
Dav´e R., Finlator K., Oppenheimer B. D., Fardal M., Katz N., Mon. Not. R. Astron. Soc.,366,2
KereˇsD.,WeinbergD.H.,2010,Mon. Not. R. Astron. Soc., WhitakerK.E.,etal.,2011,Astrophys. J.,735,86
404,1355 WhitakerK.E.,vanDokkumP.G.,BrammerG.,FranxM.,2012,
DekelA.,BirnboimY.,2006,Mon. Not. R. Astron. Soc.,368,2 Astrophys. J. Lett.,754,L29
DekelA.,etal.,2009,Nature,457,451 Williams R. J., Quadri R. F., Franx M., van Dokkum P., Labb´e
DiMatteoT.,SpringelV.,HernquistL.,2005,Nature,433,604 I.,2009,Astrophys. J.,691,1879
Faucher-Gigu`ere C.-A., KereˇsD., MaC.-P., 2011, Mon. Not. R. WuytsS.,etal.,2007,Astrophys. J.,655,51
Astron. Soc.,417,2982 ZentnerA.R.,BerlindA.A.,BullockJ.S.,KravtsovA.V.,Wech-
Faucher-Gigu`ereC.-A.,HopkinsP.F.,KereˇsD.,MuratovA.L., slerR.H.,2005,Astrophys. J.,624,505
Quataert E., Murray N., 2015, Mon. Not. R. Astron. Soc., vanderWelA.,etal.,2014,Astrophys. J.,788,28
449,987
FeldmannR.,2015,Mon. Not. R. Astron. Soc.,449,3274 ThispaperhasbeentypesetfromaTEX/LATEXfilepreparedby
Feldmann R., Mayer L., 2015, Mon. Not. R. Astron. Soc., 446, theauthor.
1939
MNRAS000,1–5(2016)