First DEIMOS Science Results: The DEEP2 Redshift Survey

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Galaxy and Quasar Clustering at z=1

Alison Coil

University of Arizona

April 2007

SDSS :

Large-Scale Structure

Why do galaxies cluster?

initial fluctuations in early universe

gravity

cosmology

physics: galaxy formation

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Why high redshift?

time leverage

earlier phase of galaxy evolution

additional constraint on models

DEEP2: A Redshift Survey at z=1

Collaboration b/w UC-Berkeley and UC-Santa Cruz using the DEIMOS spectrograph on the Keck II telescope to study both galaxy properties and largescale structure at z=1.

Observational details:

• 3 sq. degrees

• 4 fields on sky

• primary z~0.7-1.4

• ~7-9 Gyr ago

40k redshifts

• ~5·10 6 h -3 Mpc 3

80 Keck nights - 3 years

• One-hour exposures

R

AB

=24.1

• high resolution - robust z’s

Survey is done - data is released!

DEEP2 Redshift Survey: z=0.7-1.3

Cone diagram of 1/12 of the full DEEP2 sample

Clustering Primer

Quantify clustering:

probability of two galaxies separated by r

relative to a random unclustered distribution

large on small scales, small on large scales r

0 x

(r) follows a ~power-law prescription locally: x

(r) = (r

0

/r) g with r

0

~5 Mpc/h and g

~1.8

= scale where the prob. of a galaxy pair is 2x random larger r

0

= more clustered

Clustering Primer

Trace different physics on different scales:

- small scales (r < 100 kpc/h): mergers + galaxy-galaxy interactions

- intermediate scales (100 kpc/h < r < 2 Mpc/h): radial profiles of galaxies w/in halos / clusters

- large scales (r > 2 Mpc/h): large-scale density field / cosmology / host dark matter halo mass

Galaxies Come in 2 Distinct Types

Blue:

star-forming, gas+dust, spiral, ‘late-type’

Red: non-star-forming, little gas/dust, elliptical, ‘early-type’ red sequence

SDSS:

Blanton et al.

2003 blue cloud

Bi-modal color distribution magnitude

why?

evolution?

DEEP2: same color bi-modality to z>1 red

# density red gals blue bright faint redshift

Build-up of red galaxies since z=1 - galaxies moving from blue cloud to red sequence.

Willmer et al. 2006 ApJ / Faber et al. 2006 ApJ

Galaxy Clustering as a Function of Color

Blue

Red

Red galaxies are more clustered and have larger velocity dispersion/fingers of god: reside in overdense environments + groups.

Detect coherent infall on large scales for blue and red galaxies.

First time this has been seen at z=1! Need precise z’s.

Galaxy Clustering as a Function of Color green

Color-density relation strongly in place at z=1.

No color dependence w/in red sequence, but there is w/in blue cloud. Green galaxies as clustered as red.

blue red red: blue:

(for M

B

<-20, L>L*, z=0.7-1.0) r r

0

=5.17 (0.26) g

=1.97 (0.04)

0

=3.83 (0.19) g

=1.67 (0.05)

Which galaxies move to the red sequence by z=0?

Redder of the blue cloud + green galaxies.

Coil et al. in prep

Galaxy Clustering as a Function of Color

Quantify minimum dark matter halos mass as a function of galaxy color (for M

B

<-20): red: b=1.6, M halo

>2 10 12 M o

/h blue: b=1.3, M halo

>4 10 11 M o

/h

- important for color bimodality theories and simulations of gas accretion and star formation

Color-density relation is not caused by clusters - very few clusters at z=1. Either caused by groups or intrinsic galaxy or halo property such as age/stellar mass/halo mass.

The ‘green’ population is distinct - as clustered as red galaxies, but kinematics of blue galaxies. Shows infall on large scales likely at the edges of groups/filaments and falling in. Likely a transition population moving to red sequence.

Coil et al. in prep

QSO/AGN and Galaxy Evolution

QSO/AGN may be important in how galaxies evolve:

many/most galaxies have SMBH

m

BH

s bulge relation

simulations: feedback from AGN or SNe is needed to shut off SF and create the color-mag diagram

mergers are needed to create ellipticals - may involve quasars as disk galaxies collide

Can test galaxy and QSO/AGN formation and evolution models with observed clustering

SDSS QSOs in DEEP2 fields

36 SDSS + 16 DEEP2 spectroscopic broad-line

QSOs in the DEEP2 fields between z=0.6-1.4:

DEEP2

SDSS

(near M*)

Clustering of Galaxies around QSOs

Cross-correlation of DEEP2 galaxies and SDSS QSOs.

Errors include Poisson errors + cosmic variance.

Similar errors as surveys with

1000s of QSOs (eg. 2dF).

Divide by the clustering of

DEEP2 galaxies around DEEP2 galaxies to get the bias of QSO hosts…

Coil et al. 2007 ApJ

Relative bias of QSOs to DEEP2 galaxies

QSO relative bias = 0.9 (0.2)

QSO absolute bias = 1.2 (0.3)

Cluster more like blue galaxies than red! (2 s

) ---not what is found locally at z=0.

Constrains host type for QSOs

(blue) and QSO host halo masses:

Min. halo mass = 5x10 11 M

0

Mean halo mass = 3x10 12 M

0

No dependence is seen on magnitude or redshift.

Coil et al. 2007 ApJ

red color blue

Clustering of X-ray AGN in AEGIS

Chandra survey in the

EGS: 200 ks depth

Have ~10,000 galaxies and ~200 (so far) X-ray sources w/ redshifts.

Can measure the crosscorrelation of X-ray AGN with galaxies.

z=0.7-1.4

-16 M

B

Nandra et al. 2006 ApJL

Barger et al. 2003 AJ quasars

-24

X-ray AGN hosts are bright and on red sequence or massive end of blue cloud.

(even the faint ones:

L x

~10 42-44 erg/s, f x

~1.5 x 10 -15 erg/s/cm 2 )

Clustering of X-ray AGN in AEGIS

First results:

significant dependence with optical luminosity: brighter AGN

(-20.5>M

B

>-23) are ~50% more biased/clustered than fainter

AGN (-17.5>M

B

>-20.5)

-X-ray AGN cluster more like red than blue galaxies

-cluster more than QSOs!

-redder X-ray AGN cluster more than bluer AGN

-consistent w/ galaxies undergoing a QSO phase before settling on the red sequence w/ an AGN

Coil et al. in prep

QSO/AGN Formation and Evolution

Competing QSO/AGN formation and evolution models predict different clustering properties, through assumed accretion and lifetimes:

- all begin with major mergers

Kauffmann and Haenelt 2001 predict a strong luminositydependence to QSO clustering:

assume an exponentially declining light curve, time= t

M_B ~ gas mass accreted / t

gas mass accreted ~ host halo mass

luminosity~halo mass brighter QSOs cluster more

QSO Formation and Evolution

Lidz, Hopkins et al. 2005 predict less luminosity-dependence (but still some), as the light curve is not exponential

- bright and faint QSOs are similar objects in same halos, but in different stages of their evolution - similar clustering

- bias at z~1 is too high (b~2)

- X-ray AGN cluster like quasars

Croton et al. 2006 include a second mode for low-L AGN: if halo M > M threshold then no gas accretion (~5 10 11 M

0

)

- gas is shock heated, shuts off SF, creates color bimodality, shuts off black hole accretion - no QSO - but there is a low-L AGN

- predict blue galaxies have QSOs at z<2 and red galaxies have low-L

AGN - good qualitative agreement with our results!

Clustering of QSOs constrains lifetimes, host halo mass, host galaxy type and differentiates between formation models.

Summary

Galaxies have a bimodal color distribution at z=1, similar to z=0.

LF studies show that red galaxies have been forming since z=1.

Red galaxies are more clustered than blue galaxies at z=1, with a steeper slope and stronger fingers of god.

Galaxies that are likely to evolve from blue to red are the reddest of the blue galaxies and green galaxies.

Color-density relation is not due to clusters!

Galaxies that host QSOs at z=1 reside in the same mass halos as typical DEEP2 galaxies and have blue host galaxies.

X ray-selected AGN cluster like red galaxies at z=1 - at later stage in evolution from QSOs?

Place strong constraints on QSO/AGN formation models.

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