The evolution of galaxies resolved in space and time: an inside-out growth view from the CALIFA survey

0.61 MB·English

by  E. Pérez

Draftversion January10,2013
PreprinttypesetusingLATEXstyleemulateapjv.5/2/11
THE EVOLUTION OF GALAXIES RESOLVED IN SPACE AND TIME: AN INSIDE-OUT GROWTH VIEW
FROM THE CALIFA SURVEY
E. P´erez1, R. Cid Fernandes1,2, R. M. Gonza´lez Delgado1, R. Garc´ıa-Benito1, S. F. Sa´nchez1,3, B. Husemann4,
D. Mast1,3, J.R. Rodo´n1, D. Kupko4, N. Backsmann4, A.L. de Amorim2, G. van de Ven5, J. Walcher4, L.
Wisotzki4, C. Cortijo-Ferrero1, and CALIFA collaboration6
1InstitutodeAstrof´ısicadeAndaluc´ıa(CSIC), GlorietadelaAstronom´ıas/n,E-18008Granada,Spain.
2Departamento deF´ısica,UniversidadeFederaldeSantaCatarina,P.O.Box476,88040-900, Florianpolis,SC,Brazil
3CentroAstron´omicoHispanoAlem´an,CalarAlto,(CSIC-MPG),Jesu´sDurb´anRemo´n2-2,E-04004Almer´ıa,Spain
3 4Leibniz-InstitutfrAstrophysikPotsdam,AnderSternwarte16,D-14482Potsdam,Germany
1 5Max-Planck-Institutfu¨rAstronomie,K¨onigstuhl17,D-69117Heidelberg,Germanyand
0 6CALIFAInternational Collaborationhttp://califa.caha.es
2 (Received 2012 October 23; Accepted 2012 December 24)
Draft version January 10, 2013

n
a ABSTRACT
J
Thegrowthofgalaxiesisoneofthekeyproblemsinunderstandingthestructureandevolutionofthe

8 universeanditsconstituents. Galaxiescangrowtheirstellarmassbyaccretionofhaloorintergalactic
gas clouds, or by merging with smaller or similar mass galaxies. The gas available translates into a
]
rate of star formation,which controlsthe generationofmetals in the universe. The spatially resolved
O
history of their stellar mass assembly has not been obtained so far for any given galaxy beyond the
C
Local Group. Here we demonstrate how massive galaxies grow their stellar mass inside-out. We
. report the results from the analysis of the first 105 galaxies of the largest to date three-dimensional
h
spectroscopicsurveyofgalaxiesinthe localuniverse(CALIFA). We applythe fossilrecordmethodof
p
stellar population spectral synthesis to recover the spatially and time resolved star formation history
-
o of each galaxy. We show, for the first time, that the signal of downsizing is spatially preserved, with
r both inner and outer regions growing faster for more massive galaxies. Further, we show that the
t
s relative growth rate of the spheroidal component, nucleus and inner galaxy, that happened 5–7 Gyr
a ago,showsamaximumatacriticalstellarmass∼7×1010M⊙. Wealsofindthatgalaxieslessmassive
[ than ∼ 1010 M⊙ show a transition to outside-in growth, thus connecting with results from resolved
1 studies of the growth of low mass galaxies.
v Subject headings: galaxies: bulges — galaxies: evolution — galaxies: fundamental parameters —
9 galaxies: stellar content — galaxies: structure
7
6
1 1. INTRODUCTION matches its spectrum (Walcher et al. 2011, and refer-
1. The stellar mass of a galaxy, M⋆, is one of its most ences therein). This fossil record method has been ap-
plied to images (e.g. Brinchmann & Ellis 2000; Bell &
0 fundamental properties as it provides a measure of the
de Jong 2000; P´erez-Gonza´lez et al. 2008; Hansson et
3 galaxy evolution process. Elucidating how it evolves in
al. 2012) with good spatial coverage but poor spectral
1 spaceandtime,andinrelationtoothergalaxiesiscentral
resolution. It has also been applied to Sloan Digital Sky
: tounderstandingtheprocessesthatgoverntheefficiency
v Survey (SDSS) spectra of many galaxies (Heavens et al.
andtimingofstarformationingalaxies. Look-backtime
i 2004; Brinchmann et al. 2004; Gallazzi et al. 2005; Cid
X studies of galaxy evolution determine the spatially re-
Fernandes et al. 2005, 2011; Panter et al. 2007), al-
solved star formation rate (SFR) at a range of redshifts
r though SDSS provides just a single spectrum per galaxy
a as a proxy for the averagehistory of a particular type of
with varying spatial coverage with redshift. The CAL-
galaxy (Lilly et al. 1996; Madau et al. 1996; Folkes et
IFAsurvey(S´anchezetal. 2012)providesasetofspectra
al. 1999; York et al. 2000; Bell et al. 2004; Moles et
that covers the extent of each galaxy with good spatial
al. 2008; Ilbert, et al. 2009; P´erez-Gonza´lezet al. 2008;
and spectral sampling. Here we report on the spatially
Nelson et al. 2012). A major handicap of this approach
resolvedgrowthwithcosmictimefor105galaxies,which
is the inability to follow the evolution of any one galaxy
sampleawiderangeofpropertiesinthecolormagnitude
over time (Faber et al. 2007). In this work we follow an
diagram(CMD), drawn from the full CALIFA survey of
alternativeapproach. Foranewsetofintegralfieldspec-
600 galaxies.
troscopic (IFS) data of a large sample of galaxies in the
local universe, we recover their spatially resolved indi-
vidualstarformationhistories(SFH)bymeansofstellar 2. SAMPLEANDMETHODS
population spectral synthesis. Details of the CALIFA survey, sample selection, re-
Beyond the Local Group, where individual stars are duction and calibration methods and analysis pipeline
not resolved, a powerful method to reverse engineer the are provided by Sa´nchez et al. (2012), Husemann et
SFH of a galaxy is to find the most plausible combi- al. (2012), Husemann et al. (2013, CALIFA first pub-
nation of evolved single stellar populations (SSP) that lic data release DR1), Cid Fernandes et al. (2013), and
J. Walcher et al. (2013, in preparation). Here we use
[email protected] thespectraldatacubescombiningbothsetups,V500and
2 P´erez et al.
[ht!]
Figure 1. Stellar mass surface density (M⊙ pc−2) in the galaxies CMD. Absolute magnitude in SDSS r, Mr, versus SDSS u−r
color,whereeachgalaxyisrepresentedwithitspresent-daystellarmassdensitydistribution. Holesinsomegalaxiesresultfromremoving
foregroundstars. Theupperhorizontalaxisindicatesapproximatevaluesofthestellarmass,fromalinearfittotheMr–log(M⋆)relation.
Thetimeevolutionofthestellarmassbuildupofeachgalaxyinthisdiagramcanbeseeninhttp://www.iaa.es/∼eperez/CALIFA/CMD.
V1200gratings,with median limiting sensitivity 1.0and 3. RESULTS
2.2×10−18ergs−1 cm2 ˚A−1 arcsec−2,spectralresolution Figure1showsthe(Mr,u−r)CMD,whereeachgalaxy
∼6˚Aintherange∼3650–7500˚A,medianspatialresolu- is representedwith its present-day distribution of stellar
tion3′.′7,andspectrophotometriccalibrationbetterthan mass density (in logarithmic units of M⊙ pc−2). Since
15%. the absolute magnitude Mr of galaxies is roughly pro-
For each galaxy the data are spatially rebinned to a portionalto their total log(M⋆) (a maindriver of galaxy
minimumsignal-to-noiseratioof20inacontinuumband physics)andtheu−rcolorworksasaroughevolutionary
at 5635±40˚A (Cid Fernandes et al. 2012). The stellar clock,theCMDencapsulatesgalaxyevolutionandthedi-
spectralsynthesis code starlight(Cid Fernandesetal. versityofgalaxiesinasimple andobservationallyconve-
2005)is then used to recoverthe SFH, including a value nientform. Furthermore,givenitswidespreaduseinthe
for the stellar extinction, from each spectrum. Here we literature(Faberetal. 2007;Blanton&Moustakas2009)
use a set of SSPs sampling the 1Myr – 14Gyr age range and the fact the CALIFA sample was defined to coverit
with 40 age bins and four metallicities between 0.2 and as uniformly as possible, the CMD provides a natural
2.5 solar (S. Charlot & G. Bruzual 2007, private com- framework to present and analyze our results. The gen-
munication), assuming a Chabrier initial mass function. eral trend in Figure 1 shows more luminous galaxies to
This method provides spatially resolvedSFHs for ∼200- be redder, while the color coded mass density image of
2000 regions per galaxy, which we use to derive a three- eachgalaxyshowsthatmoreluminousoneshaveahigher
dimensional buildup of mass (with two spatial and one
temporal coordinates).
The evolution of galaxies resolved in space and time: an inside-out growth view from the CALIFA survey 3
centralstellarsurface density andsteeper gradients;1 we
now see these trends spatially resolved over a five mag-
nitude range in Mr.
Spatially resolved mass distributions have been com-
puted for some galaxies from broad band imaging (e.g.
Zibettietal. 2009;Wuytsetal. 2012). Sincewehavethe
spatially resolved SFH for each galaxy, we can also see
the time evolution of the CMD. This is shown in the
animation http://www.iaa.es/∼eperez/CALIFA/CMD,
with the 10000-250 Myr age plotted in the top right-
handcorner,stoppingatatimewhengalaxieshavemost
of their M⋆ in place. For clarity, and to emphasize the
wayM⋆ grows,galaxiesarekeptattheirpresentlocation
in the CMD, even though their luminosities and colors
would actually change with time. The most luminous,
redder, massive galaxies have transformed an important
part of their mass into stars already 10 Gyr ago (e.g.
P´erez-Gonza´lezet al. 2008),particularly in their central
regions, while many of the less massive galaxies show a Figure 2. Relativestellarmassgrowthoffourmainspatialcom-
lower stellar surface density. ponents (nucleus, inner 0.5R50 and 1R50 and outer >1R50) for
Although we can derive the time evolution of the stel- two galaxy mass bins, the lowest (dashed, log M⋆ [M⊙]∼ 9.58)
lar populations at their present day location, it is not and an intermediate (full line, log M⋆ [M⊙]∼ 10.83). Each com-
ponent is normalized to its final M⋆. To compute a growth rate,
feasible to trace their spatial location at earlier epochs, ahorizontalgraylineat0.8markswheneachcomponentachieves
i.e., we cannot follow the evolution of their motions. If 80% of its final M⋆. At the lowest mass, galaxies outskirts grow
the stars undergo major spatial shuffling over their lives faster(dashedbluelinesteeper), butathighermassesthegrowth
proceedsinside-out(fullblacklinesteeper).
then our analysis would be hampered. Breaks in the ex-
parts.
ponential distribution of disk outer regions (e.g. Pohlen
& Trujillo 2006; Erwin et al. 2008) have been inter- Figure3showsataglancethetrendsforallmassbins.
The horizontalaxis represents log time (bottom) or red-
preted as evidence of radial migration, although there is
no general consensus. Numerical simulations show that, shift (top; H0 = 71, ΩM = 0.27, ΩΛ = 0.73); the ver-
for secular evolution, the consequences of radial migra- tical axis represents the present day total M⋆. Panels
tion are only significant in the outer parts of galaxies, show grayscale coded the relative growth of each of the
four spatial components, normalized to its final stellar
beyond about 2-3 scale lengths (Figure 2 in Roˇskar et
al. 2008; Figures 15 and 16 in Sa´nchez-Bl´azquez et al. mass, so that all components grow up to mass unity
2009; Behroozi et al. 2012). Here we partition galaxies (i.e. grayscale and contours in Figure 3 represent for
all mass bins the growth curves shown for two example
into four radial zones to compare their histories, so that
the outer regions (at severaleffective radii) where radial mass bins in Figure 2; the black contour line in each
migration may have an impact on the SFH do not have panel marks 0.8M⋆). Thus, the relative growthof differ-
a significant contribution to the results in the analysis entpartsofthegalaxycanbeassessed. ThreeM⋆growth
that follows. cuts are plotted corresponding to three mass bins (low-
est, intermediate,and highest, in blue, greenand red, as
3.1. Spatially Resolved Growth of Stellar Mass M⋆ colored in their axis mass value). The right-hand side
panel shows that outer reaches (>1R ) of less massive
The animated CMD is a visually compelling tool, but 50
lacks the quantitative information needed to probe the galaxies (log mass[M⊙]∼9.58, in the lower part of the
plot) achieve 0.8M⋆ about 1 Gyr ago, while more mas-
spatial growth of the stellar mass assembly. A more
quantitativeanalysisinFigures2-5showthetime evolu- sive ones (log mass[M⊙]∼11.26) had 0.8M⋆ already ∼5
tion for four galaxy regions: the nucleus (left, defined as Gyrago. ThesystematicsofthisoutergalaxyM⋆growth
isclearlyseenfromthe lessmassiveupto the mostmas-
the central0.1R 2),the regioninside 0.5R , theregion
50 50 sive galaxies in the sample. The central panels show a
inside 1R50, and the region outside 1R50. To make the similarbehaviorfortheinnerregions(1R and0.5R ),
growth of M⋆ more visible, galaxies are normalized to a but with a steeper growth at higher galax5y0 masses. T50he
common radial scale in units of R , and then stacked
50 left panel shows a similar behavior for the nuclei, with
in seven equally populated bins (15 galaxies each) of
aneven steeper slope for galaxiesmore massive than log
increasing present-day galaxy M⋆. Figure 2 shows the mass[M⊙]∼10.5. Thus there is a clear systematic se-
rMel⋆atbivines,gtrhoewtlohwoefstth(deafsohuerd,slpoagtiMal⋆c[oMm⊙p]o∼n9en.5t8s)faonrdtwano qisuternacnesofofrMm⋆edgrinowtothstfarrosmmtuhcehinesairdleieoruwt,itwhhiner0e.5thRem.ass
intermediate mass (full line, log M⋆ [M⊙]∼10.83). To 50
compute the M⋆ growth rate, a gray line marks when 3.2. Spatially Resolved Mean Age of the Stellar
eachcomponentachieves80%ofits finalM⋆. Clearly,at Populations
higher M⋆ the growth proceeds inside-out, while at the
lowestM⋆ galaxiesoutskirtsgrowfasterthantheirinner To better understand this result, for each of the spa-
tial regions we compute the age at 0.8M⋆ (as indicated
1 With few exceptions, such as the outstanding low surface in Figures 2 and 3). These are represented color coded
brightnessgalaxyat(-21.87,2.76). in Figure 4 (in Gyr, also shown in each box), with the
2 R50 isthecircularhalflightradiusin5635±40˚A presentdaystellarmassofthegalaxyintheverticalaxis
4 P´erez et al.
Figure 3. Inside-outstellarmassgrowthandspatiallyresolveddownsizing. Panelsshowthenormalizedgrowth(grayscaleintenintervals
of 10%, with the 80% contour inblack) in timein the four zones of Figure2. To avoid number statistics biases, the galaxies are stacked
inseven equally populated bins of 15galaxies each, sorted by present day total stellar mass; this implies that the vertical axis infigs. 3,
4,5isnotuniforminlogmass. Foreachspatialcomponent thegrowthisnormalizedtoitstotal finalstellarmass(i.e. thegrowthcurves
ofFigure2arecuts fortwoofthe massbinsthroughthe grayscaleandcontours). For eachzone, threeexamplemassbins growthcurves
areplotted(lowest,intermediateandhighest,inblue,greenandred)showinghowthesignalofdownsizingisspatiallypreserved(thefour
bluelinesherecorrespondtothefourdashedlinesinFigure2,whilethefourgreenlinesherecorrespondtothefourfulllinesinFigure2);
theaxiscorrespondingtothesecutsisthesameasthegrayscale,i.e. thescale0.0-1.0ontherighthandside. Foragivengalaxymass,the
progressivesteepening ofthe growthfromtheouter (>1R50)towards the nucleus shows theinside-outgrowthtrend withthe total mass
ofthegalaxy. Atthesametime,foragivengalaxyregion,moremassivegalaxiesgrowfasterthanlessmassiveones,andthisissustained
systematicallyfromtheinnertotheouterzones.
Figure 4. Inside-outstellarmassgrowth: ages. UsingthesameverticalaxisasinFigure3,thisfigurecolorcodestheageatwhicheach
spatialcomponent growsto80%ofitsfinal stellarmass;theage (inGyr)isshownwithineach box. Foragivenmass,thehorizontal run
ofcolorgivesthesystematicagingfromtheouter(right)totheinnerregions(left). Conversely,foragivengalaxyregion,theverticalrun
givesthesystematicagingofthatzonewithincreasinggalaxytotalstellarmass. Thereisasystematicchangebothwithmassandlocation
forallcases,withtheexceptionoftheverylowmassgalaxies(bottomrow)forwhichthereisnoinside-outgrowth(theageat80%growth
isapproximatelythe sameinallfourspatial components). Thesediagramsshow clearlythedifferential inside-outgrowthand itsexplicit
dependence ongalaxymassandgalactocentric radius.
The evolution of galaxies resolved in space and time: an inside-out growth view from the CALIFA survey 5
and the spatial zone in the horizontal. Arising from the 4. DISCUSSION ANDSUMMARY
number of galaxies, statistical errors in the age for each
Previous studies have revealed a special mass or mass
box amount to 0.23dex, while systematic errors intro- range (referred to as critical or pivotal) around M⋆ ∼
dgaudceodetbyal.th2e00ch5o)iacereo0f.0o5thdeerxS(RSP. Mba.sGiso(nGz´aolnezza´DleezlgDaedlo- 6 × 1010 M⊙ (Kauffmann et al. 2003; Mateus et al.
2006; Leauthaud et al. 2012, and references therein).
et al. 2013, in preparation). At a glance it is clear that:
Leauthaud et al study the stellar-to-halo mass relation
(1) running verticallyfor a givengalaxyzone, olderages
(SHMR) using COSMOS data and find that this mass
(red) correspond to more massive galaxies, and (2) run-
marks where the accumulated stellar growth of the cen-
ninghorizontallyforagivengalaxymass,olderages(red)
tral galaxy has been the most efficient. On the mod-
correspondto the centralzones. The trends areclearfor
eling side, Shankar et al. (2006) discuss the shape of
all masses and spatial regions,except for the lower mass
the SHMR as a change of dominance of two feedback
bin, where there is no evidence of inside-out growth. In
mechanisms, with stellar winds and supernova (SN) effi-
fact, the evidence atthe lowermassesis thatgalaxiesdo
ciently removing the gas and quenching the star forma-
growoutside-in(Figure2),connectingwiththe behavior
tion at lower galaxy masses, while active galactic nu-
seeninstudiesofdwarfgalaxies(e.g. Gallartetal. 2008;
cleus (AGN) winds become more powerful in massive
Zhang et al. 2012, and references therein).
galaxiesthus loweringstarformationefficiency athigher
The increase in mean stellar ages with increasing M⋆
masses. There is still much to be understood about the
reflects the downsizing phenomenon previously estab-
self-consistentcombinedeffectsofAGNandSNfeedback
lished on the basis of fossil record analyses of spatially
(Stinson et al. 2013; Booth & Schaye 2012). Recent
unresolveddata (Heavens et al. 2004;P´erez-Gonza´lezet
papers try to reproduce the observed SHMR from cos-
al. 2008). Figures 3 and 4 show, for the first time, that
mological simulations (cf. Figure 14 in Behroozi et al.
the signal of downsizing is preserved in a radial fashion,
withbothinnerandouterregionsgrowingfasterformore 2012),withvaluesof∼2−10×1010 M⊙ inthepeakeffi-
ciencyofconversionofhalogasintostellarmass. Cosmo-
massive galaxies. At the same time, these figures show
logical models of star formation with negative feedback
thatdifferentspatialregionsinagalaxygrowatdifferent
do not allow yet for a more precise value of this critical
paces.
mass for optimal growth (De Lucia & Borgani 2012).
3.3. Spatially Resolved Growth Rate of the Stellar Inshort,thereisclearmountingevidencefromaseries
Populations of independent studies, both observationally and from
numerical simulations, of a special galaxy mass range
To examine the relative growth of inner and outer re-
wherethe SFR reacheshigher valuesfaster. Ourresults,
gionsmoreclosely,wecomputegrowthratesfromthein-
Figure 5, show that the physical process(es) responsible
verseofthe cosmictime spancorrespondingto the build
up of 0.8M⋆. This is done for each spatial component for this peak efficiency also leave a strong imprint in the
spatial assembly of stars in galaxies. From our spatially
ofeachgalaxy,andthe resultingratesexpressedinunits
resolvedstudywecanseethatthisisrestrictedtothein-
of the growth rate of the galaxy as a whole, obtained by
nerreachesofgalaxieswiththispivotalmass. Thiswould
integrating over its full spatial extent. Thus we derive
implythattheeffectisseeninthespheroidalcomponent,
the relative growth rates shown in Figure 5. The right
which dominates the central mass distribution of galax-
panel, with coordinates as in Figure 4, codes in color
iesatthisstellarmassrange,andthatthishappened5-7
this relative growth rate. The left panel plots vertical
Gyr ago (a redshift ∼0.5–1; Figure 4).
cuts through the four locations within the galaxy, as a
We can also tentatively frame our results in the con-
function of total present day stellar mass. This figure
text of secular versus merger driven evolution. A pos-
showsatoncethatnotonlytheinnerpartsofmoremas-
sthivaetginalagxaileasxigersemwoMre⋆mfaassstievre(tahsanin5F×ig1u0re104M),⊙buthtealisno- swibitlhe Msce⋆n&ar5io×to10i1n0teMrp⊙rehtaovuergfironwdinngqsuiicskltyhatthegiralianxnieers
part by means of a merger at ages 5-9 Gyr ago (such as
ner regions grew as much as 50%-100% faster than the
galaxy-wide average. The relative growth rate for 1R M31), while lower mass galaxies are dominated by secu-
(magenta line) is close to unity, meaning that R be5s0t lar evolution (such as the Milky Way). Although we do
50 nothavethemeanstotestthis,itiscompatiblewiththe
represents the stellar mass growth in the galaxy as a
results obtained by Puech et al. (2012), and with the
whole.
studiesofM31andtheMilkyWay(Hammeretal. 2007,
Although we have grouped 105 galaxies (105123 spec-
2010;Cignoni et al. 2006;Vergely et al. 2002;McMillan
tra in total) in just a few mass bins to obtain robust re-
2011).
sults,whenthecompleteCALIFAsampleof600galaxies
Our analysis of the SFH in 105 galaxies of the CAL-
isobservedandanalyzedtheseresultswillbeestablished
IFA survey provides a direct powerful probe of the rates
with a finer detail. The most striking aspect of Figure
5 is the peak at M⋆ ∼ 6 − 7 × 1010 M⊙. At masses and efficiency of spatially resolved stellar mass growth
in galaxies, as derived from the information encoded
below this the relative growth rates of inner and outer
in their present-day spectra. We demonstrate spatially
regions slowly convergeto the galaxy average,becoming
resolved downsizing, with galaxies more massive than
essentially indistinguishable at the lowest galaxy masses
sampled. A convergence towards spatially uniform his- M⋆ ∼ 5×109 M⊙ growing inside-out while lower mass
galaxies grow outside-in. We find an optimal growth for
tories is also seen at masses above the critical mass, but
the inner regions still grow faster than the outer ones the galaxy stellar mass around ∼7×1010 M⊙.
at the highest masses. The largest differences peak at
∼6−7×1010 M⊙,where the nucleus growsabouttwice This Letter is based on data obtained by the CALIFA
faster than the outer regions. survey (http://califa.caha.es), funded by the Span-
6 P´erez et al.
Figure 5. Stellarmassassemblyrate. WiththesameaxesofFigure4,therightpanelcolorcodestherelativegrowthrateat80%mass,
foragivengalaxymassandzone,normalizedtothetotalgalaxygrowthrateat80%. Theresultindicatesthatformostofthegalaxies,on
average,therelativerate(withineachgalaxy)oftransforminggasintostarsissimilarinallparts,exceptforthecentralregions(<0.5R50)
ofgalaxies moremassivethan∼5×1010 M⊙,whichareuptoafactor of∼2faster. Theleftpanelshows verticalcuts through thefour
zones,includinguncertaintybands computedin1000iterationsofrandomlyremovingfivedifferentgalaxiesatatime.
ishMINECOgrantsICTS-2009-10,AYA2010-15081,and Heavens,A.,Panter,B.,Jimenez,R.,&Dunlop,J.2004,Nature,
the CAHA operated jointly by the Max-Planck IfA and 428,625
the IAA (CSIC). We benefited from discussions during Husemann,B.,Kamann,S.,Sandin,C.,etal.2012,A&A,545,
137
the CALIFA busyweeks. The CALIFA Collaboration
Husemann,B.,Jahnke, K.,S´anchez, S.F.,etal.2013,A&A,549,
also thanks the CAHA staff for the dedication to this A87(CALIFADataRelease1(DR1))
project. Ilbert,O.,Capak,P.,Salvato,M.,etal.2009,ApJ,690,1236
Kauffmann,G.,Heckman,T.M.,White,S.D.M.,etal.2003,
MNRAS,341,54
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