PFS - wide: a million galaxies over ten billion years

John Silverman (IPMU)PFS galaxy working group: Jim Gunn (Princeton), M. Imanishi (NAOJ),
Y.T., Lin (IPMU), M. Ouchi (Tokyo), L. Sodre Jr. (USP, Brazil), M. Strauss(Princeton), M. Takada (IPMU), N. Tamura (NAOJ), M. Tanaka (IPMU)

Outline
Motivation to push studies of the extragalactic Universe to z~2
Current, large (~104 spectra) spectroscopic surveys to z~1
Deficiencies of such narrow beam survey
Defining a strategy for a PFS survey for galaxy and AGN evolution in anenvironmental context up to z ~ 2Galaxies

SupermassiveBlack Holes

Environment

Key problems in galaxy formation

enceRed sequw/feedback
Blue, star-forming galaxy

Springel et al. 2005
Croton et al. 2006

What physical mechanism(s) is halting the growth of massive galaxies?

SDSS: a (local) benchmark for galaxy and AGN surveys

Kauffmann et al. 2003

Peng et al. 2010

Mass and environment are fundamental parameters(e.g.,Baldry et al. 2004; Thomas et al. 2009; Peng et al. 2010)

SDSS: a (local) benchmark for galaxy and AGN surveys
Type 2 AGNs: Nature’s ‘cosmic coronograph’Selection based on emission-line ratios

Urry & Padovani 1995
Kauffmann et al. 2003

SDSS: a (local) benchmark for galaxy and AGN surveys
Type 2 AGNs: Nature’s ‘cosmic coronograph’

Late

Selection based on emission-line ratios

Early

Young stellar populations are associated withstrongly accreting SMBHs
Kauffmann et al. 2003

Kewley et al. 2006

Do AGN impact the formation of stars?

Schawinski et al. 2007

SDSS: a (local) benchmark for galaxy and AGN surveys

Greene et al. 2006
How do galaxies and their black holes migrate onto local mass relations?

Need to push to higher redshift
SFRs (data points): Hopkins, A. et al. 2004
Bouwens et al. 2007

Accretion ontosupermassive black holes
LBol=ε Maccr

JDS et al. 2008

zCOSMOS and large spectroscopic surveys

zCOSMOS
20k spectra

Lilly et al. 2009
‘Bright program’
IAB < 22.5
1.7 deg2~5500-9600 Å

zCOSMOS and large spectroscopic surveys

Environmental studies of galaxies

Environments of AGNs

High ρlow ρ
JDS et al. 2009
Cucciatti et al. 2010
Environmental and mass dependence of galaxy properties
up to z~1 (see Tanaka et al. 2010 for higher-z)

zCOSMOS and large spectroscopic surveys••

Galaxy group catalog (Knobel et al. 2009)
1681 groups in 20k (577 w/ 3 or more members)
1012 < Mhalo < 1014 M☉

Practically no massive clusters!

Estimating cluster yields at 1 < z < 2• given a fixed amount of observing time, there is a one-toone correspondence between depth (zlim) and area

• maximize the number of clusters (required to have >4members)• model the number of halos as a function of cluster mass

after Tinker & Wetzel (2010), who used an HOD model toexplain the clustering of galaxies at z=1-2 in UKIDSS UDS

Kodama et al. 2008; Nagashima et al. 2005

Estimating cluster yields at 1 < z < 2• given a fixed amount of observing time, there is a one-to-one
correspondence between depth (zlim) and area

• maximize the number of clusters (required to have >4members)• model the number of halos as a function of cluster mass after
Tinker & Wetzel (2010), who used an HOD model to explain
the clustering of galaxies at z=1-2 in UKIDSS UDS

Estimating cluster yields at 1 < z < 2• we populate the “lightcone” simulation by Paul Bode (seeSehgal et al ’10) with Tinker’s HOD model, using
observed luminosity function at z~1.4 to scale thenumber of galaxies above the limiting mag• given the depth (hence area), we select halos from thelightcone at z=1-2• simulation covers an octant of the sky, resolves halos
down to 6e12 Msun

• count the number of clusters with >4 members brighter
than zlimit

based on WMAP5 cosmology (sigma8=0.8).

Cluster mass function

Expected cluster counts (1 < z < 2)

100 nights•• 6 hr science time pernight• >4 members per
halo
S/N ~3 per•resolution element

300 sq. degrees with tracer galaxies to z~22.5

Expected cluster counts (1 < z < 2)

PFS target selection
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~3 hour exposure~6000 targets per PFS footprint★

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PFS target selection
Random flux limited sample (i<22.5; z <1.4)
fieldclusters

5000

Color-selected sample (z<22.5; 1 < z <2)
cluster/group members (ACT, eROSITA)
field sample

1000
~100
900

QSOs (see Imanishi’s talk)

500

Other
X-ray, radio, IR~500

6000x(300 sq deg/PSF FOV)~106 galaxies

Comprehensive survey of the high-z Universe with PFS
106 galaxies up to z~2• Galaxy evolution (mass buildup, star formation)
SFRs up to z~2• Growth of supermassive black holes (AGNs, QSOs)
masses to z~1.6•Cluster science

Progenitors of today’s massive halos• Serendipitous discoveries
Synergy with PFS deep survey
Spectroscopic support forHSC surveys
Identify unique environmentallaboratories for detail studies withTMT and ALMA

Provide a treasure-trove of data for a generation of students in Japan