Lijiang - August, 2005 DEEP2 Galaxy Redshift Survey and Post-Starburst galaxies at z~1 Renbin Yan...

Lijiang - August, 2005

DEEP2 Galaxy Redshift Surveyand

Post-Starburst galaxies at z~1Renbin Yan

University of California, Berkeley

And The DEEP2 Team

The DEEP2 Collaboration

U.C. BerkeleyM. Davis (PI)

A. Coil

M. Cooper

B. Gerke

R. Yan

C. Conroy

LBNL J. Newman

U. Hawaii N. Kaiser

U.C. Santa Cruz S. Faber (Co-PI)

D. Koo P. Guhathakurta

D. Phillips C. Willmer B. Weiner

R. Schiavon K. Noeske A. Metevier

L. Lin N. Konidaris

G. Graves

The DEEP2 Galaxy Redshift Survey, which uses the DEIMOS spectrograph on the Keck II telescope, is studying both galaxy

properties and large-scale structure at z=1.

JPL P. Eisenhardt

Princeton D. Finkbeiner

U. Pitt. A. Connolly

K survey (Caltech) K. Bundy

C. Conselice R. Ellis


Comparison with Other Surveys

1.00E+03

1.00E+04

1.00E+05

1.00E+06

1.00E+05 1.00E+06 1.00E+07 1.00E+08

Volume ( h -3 Mpc 3)

Number of Galaxies z~0z~1

DEEP2

SDSS

2dF

CFA+SSRS

LCRS

PSCZ

DEEP2 was designed to have comparable size and density to previous generation local redshift surveys and is >50 times larger than previous surveys at z~0.3-1.

DEEP2 is similar to LCRS in sample

size but at z=1 - with a very

different geometry:

~20801000 h-3 Mpc3 per field

(LCDM)


A Redshift Survey at z=1:

Observational details:

• 3 sq. degrees • 4 fields (0.5o x <2o)• primary z~0.75-1.4 (pre-selected using BRI photometry)• >40,000 redshifts• ~5·106 h-3 Mpc3

• 80 Keck nights• One-hour exposures• RAB=24.1• 1200 l/mm: ~6500-9200 Å• 1.0” slit: FWHM 68 km/s

Studying Evolution:

•Age of the Universe = 13.7 Gyr• z=0.7 - ~6.0 Gyr ago• z=1.0 - ~7.5 Gyr ago• z=1.4 - ~8.5 Gyr ago

Within DEEP2 we are surveying 2.5 Gyr or ~20% of the history of the Universe, and SDSS/2dF comparisons give ~3x this baseline


Coordinated observations ofthe Extended Groth Strip (EGS)

Spitzer MIPS, IRAC

DEEP2 spectra and Caltech / JPL Ks imaging

HST/ACSV,I (Cycle 13)

Background: 2 x 2 degfrom POSS

DEEP2/CFHTB,R,I

GALEX NUV+FUV

Chandra & XMM: Past coverage Awarded (1.4Ms)

Plus VLA (6 & 21 cm), SCUBA, etc….


Redshift Distribution of Data: z~0.7-1.4

Status: - Designed as a

three-year survey- Began summer 2002- 80 night UC time allocation is now complete-Finished 3 of 4 fields, 4th >75% done (will complete in S06)

Our color cuts are very successful! ~90% of our targets are at z>0.75 and we miss only 3% of high-z objects.


Redshift Maps in 4 Fields: z=0.7-1.2

Cone diagram of 1/12 of the full DEEP2 sample


DEEP2 sees the same color bi-modality as SDSS, COMBO-17, etc. to z~1.4

Our R-band magnitude limit corresponds to ~4000Å rest-frame at z=0.7, ~2800 Å at z=1.4 . As redshift increases, red galaxies of a given luminosity fall out before blue ones.

Willmer et al. 2005


Post-Starburst Galaxies (E+A or K+A)Post-starburst galaxies

show little on-going star-formation (lack of

emission lines) but strong Balmer absorption

features due to recent star-formation (within 1 Gyr) - ‘post-starburst galaxies’. Their spectra can be well

modeled by the combination of two

components: an old stellar population and an A-star

population.


Post-starburst Mysteries• Do all red sequence galaxies come from post-

starbursts? • What is the abundance at high-z; Cluster vs.

field?• What is their origin? Merger remnant? Satellite

harassment? Superwind? Ram-Pressure Stripping?

DEEP2 covers a large enough volume to find a large statistical sample. EGS will add multiwavelength SEDs and morphologies. We will be able to shed light on these issues.


The Selection of E+A galaxies

We use H instead of [OII] because [OII] in red galaxies is heavily contaminated by AGN or LINERs.

(Yan et al. in prep, see poster)


Color of Post-Starburst Galaxies

These galaxies populate the ‘gap’ in the color bi-modality and part of the red sequence - they may provide clues as to how galaxies move onto the red sequence. We are

investigating their morphologies and

environments.


Other recent and upcoming papers include:• Angular clustering of galaxies : Coil et al., 2004, ApJ, 617, 765• DEEP2 survey strategy & dark energy: Davis et al.,astro-ph/0408344• Evolution of close-pairs/merger rates: Lin et al., 2004, ApJ, 617, 9• Satellite galaxy kinematics: Conroy et al., astro-ph/0409305• Measuring environment in deep redshift surveys: Cooper et al., submitted• Luminosity function: Willmer et al. & Faber et al., submitted.• Group correlation function: Coil et al., submitted.• Void statistics in the DEEP2 sample: Conroy et al., submitted.• Overview of the DEEP2 sample: Faber et al., in prep.

First semester’s data is now public: http://deep.berkeley.edu/DR1


Poster:Poster: AGN Origin of [O II] in Red Galaxies AGN Origin of [O II] in Red Galaxies------ Implications for post-starburst galaxy studiesImplications for post-starburst galaxy studies

Conclusions1) Galaxies display bimodality in [O II]/Hα ratios, which corresponds

to the bimodality in rest-frame colors.

2) Line-emitting red galaxies have line ratios following those of AGN or LINERs.

3) Post-starburst galaxies identified in the SDSS dataset using Hα often exhibit significant [O II] EW; their position in [O II]-Hα plot suggest they might be AGN or LINERs.

4) [O II] emission in LINERs can be as strong as in star-forming galaxies. Locally, it is only a proxy for SFR in blue galaxies.

5) post-starburst samples defined using [O II] will be very incomplete, especially if AGN rates and intensity were higher in the past. We recommend using H as an alternative for high redshift.


Thank You


Pre-selection of high-z targets with using colors

• Plotted are the colors of some galaxies with known redshifts in our fields; those at low redshift are plotted as blue, those at high redshift as red. We use a simple color cut defined by three line segments to select galaxies at z>0.75.

•We do not apply these color cuts in the EGS!


DEEP2 slitmask spectroscopy

Using custom-milled slitmasks with DEIMOS we are obtaining spectra of ~150 targets at a time. A total of 400 slitmasks will be required for the survey; we can tilt slits up to 30 degrees to obtain rotation curves.

position


Surveys of distant galaxies can constrain both cosmology and galaxy evolution

• The evolution of large-scale structure is strongly dependent on the underlying cosmology.

• By comparing the universe at high redshift to what is seen by large local surveys such as SDSS, one can perform many unique cosmological tests and simultaneously study galaxy formation and evolution.


Scientific Goals of the DEEP2 Galaxy Redshift Survey

1. Characterize the properties of galaxies (colors, sizes, linewidths, luminosities, etc.) at z~1 for comparison to z~0

2. Study the clustering statistics (2- and 3-pt. correlations) of galaxies as a function of their properties, illuminating the nature of the galaxy bias

3. Determine N(z) of groups and clusters at high redshift, providing constraints on m and w

4. Measure the small-scale “thermal” motions of galaxies at z~1, providing a mass scale for halo models (measuring m and bias, in the paradigm when DEEP2 was designed)


DEEP2 has been made possible by DEIMOS, a new instrument on Keck II

DEIMOS (PI: Faber) and Keck provide a unique combination of wide-field multiplexing (up to 160 slitlets over a 16’x4’ field), high resolution (R~5000), spectral range (~2600 Å at highest resolution), and collecting area.


And HST ACS VI imaging finished last month!

Currently reduced mosaic 0.2% of the upcoming EGS dataset


Finding groups in DEEP2 We find groups using the locations of galaxies in redshift space - no photometric information is used, just the overdensity in the 3d galaxy

distribution.

position

Group in early DEEP2 data

In particular, we are using the Voronoi-

Delaunay Method of Marinoni et al. (2002),

which has been optimized for use at high z and

performs well. (For our purposes, “clusters” are just especially massive

groups.)


First DEEP2 Group Catalog

Gerke et al. 2005, astro-ph/0410721

We currently have group catalogs for 3 fields


Galaxy Properties and Environment We measure galaxy environments using projected 3rd-nearest neighbor

distance, shown to be near-optimal in Cooper et al. 2005 (submitted). There are strong trends of galaxy density with restframe color and [OII] equivalent width (a proxy for star formation rate); the color trend can explain the [OII] one.

Cooper et al. 2005blue color red

log

dens

ity

[OII] equivalent width (SFR)


Color vs. Equivalent Width of [OII]

Red galaxies have low [OII] equivalent width, while blue galaxies span a wide range. It appears that the scatter in this relation is most likely not due to environment. We are currently matching the DEEP2 colors and magnitudes to SDSS to look for evolution in environmental dependence between z=1 and z=0.


Environment over the CMD

Trends from z~0 studies persist at z~1: e.g. redder or brighter galaxies are preferentially found in dense environments.

Cooper et al. 2005

brighter

redder

SDSS, z~0.1 DEEP2, 0.75<z<1.05

Lijiang - August, 2005 DEEP2 Galaxy Redshift Survey and Post-Starburst galaxies at z~1 Renbin Yan...

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