Galaxy Evolution Studies & the NOAO Deep Wide-Field Survey

Arjun Dey

National Optical Astronomy Observatory

(for the NDWFS Team)

NDWFS Co-Investigators

Taft Armandroff, Ed Ajhar (Miami), Bob Blum, Todd Boroson, Kate Brand, Michael Brown , Chuck Claver, Lindsey Davis, Ian Dell'Antonio (Brown), Mark Dickinson (STScI), Richard Elston (U.o Fla.), Richard Green, Pat Hall (Princeton), Dan Hoard, George Jacoby (WIYN), Dick Joyce, Tod Lauer , Roger Lynds, Sangeeta Malhotra (STScI), Mike Merrill, Joan Najita, Earl O'Neil (Steward), Marc Postman (STScI), Ron Probst, Travis Rector, James Rhoads (STScI), Robert Schommer, Nigel Sharp (NSF), Malcolm Smith, Paul S. Smith (Steward), Glenn Tiede, Frank Valdes, Jeff Valenti (STScI), Ted von Hippel (UofTexas), Alistair Walker, and Sidney Wolff.

Erin Ryan, Emma Hogan, Lissa Miller, Alyson Ford

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249

Arjun Dey

90

Lacey & Cole

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WMAP

COBE

?

Motivation

Arjun Dey

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M. Steinmetz

Large samplesdefine population trendsstatistically precise measurementsrare populations

Wide arealarge scale clusteringless sensitive to cosmic variance

For example …

The Power of Wide-Field Surveys

Statistical approach to complex problems

BW-dropsz~3.5-4.2

Red envelopepopulation

Features in the Color-Color Diagram

Arjun DeyR-I

BW-R

-0.5 2.50

6.0

~0.6M galaxies

=1Gyr BC03/Salpeter

20-21

25-26

24-25

23-24

22-23

21-22

19-20

18-19

17-18

R-I

BW

-R

Arjun Dey

Magnitude Slices in Color-Color Space

Arjun Dey

The Redshift Distribution in the Color-Color Plane

Some Observations

•Galaxies in red envelope constitute ~ 10-12% of the objects (I<24.5)

•Most stars in red envelope population formed at high redshift (z>5)

•Narrow loop width suggests this population formed in a narrow time interval and is coeval

•Small amounts of star formation persist to present-day:field red population is not passively evolving (<1% of

I<24.5)

-models with high zF are a reasonable fit; spectra show [OII])

A well-defined sample … and photo-z’s work well! Arjun Dey

Arjun Dey

Our Photometric vs Spectroscopic zs

(see M. Brown’s talk for clustering results and K. Brand’s talk for accretion history)

The Red Galaxy Sample: The Future

1.3 sq deg -> 18 sq deg!

Wow!

Arjun Dey

High-redshift galaxies in NDWFSz~3.7

“BW-drops”BW-R > 2.5BW-R > 2(R-I)+1.7R < 25

R-I

Bw-R

Arjun Dey

LALA

Steidel

z~3

Steidel

z~4

NDWFS

z~3.7

NDWFS

z~3.7

Area (sq deg) 0.38 0.23 0.36 18

# of candidates 2347 244 611 30,000

Spectroscopic redshifts 940 48 45

Hit rate 95.5% 65-80% 98%

Surface density (arcmin-2) 0.68 0.20 0.47

# Contiguous fields 17 10 <1> 2

Max scale (comoving) 26Mpc 29Mpc 68Mpc 1020Mpc

Comparisons with other high-z surveys

So stay tuned …Arjun Dey

• MMT/Hectospec “AGES” (R<21 + X-ray sources)

• Keck/DEIMOS & LRIS (high-z + SIRTF sources)

• Gemini/GMOS (high-z + GALEX sources)

• WIYN/Hydra (QSOs + low-z line emitters)

• WHT/WYFOS (QSOs)

• Spitzer/IRS (very red objects)

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Spectroscopic Campaigns in the NDWFS Fields

The AGN and Galaxy Evolution Survey (AGES)(C.S. Kochanek, D. Eisenstein PIs)

•Redshift survey using 300 fiber Hectospec on the MMT (Fabricant)

•Complete samples over most of NDWFS/Bootes field in:•NDWFS R band

•all galaxies R19.2 mag (completed 4200 of 5500)•random 20% of galaxies 19.2<R20 (completed 750 of 1400)•for all galaxies 19.2<R20 completed 2100 of 7200

•NDWFS BW band (BW20.5, completed 2300 of 3000)

• SST/MIPS (Soifer) •24m (F1mJy, completed 1100 of 1400)•including point sources off stellar locus•redshifts for 3100 24m sources in total (so far)

• SST/IRAC (Eisenhardt) •3.6m (15.2mag, completed 1900 of 2300)•4.5m (15.2mag, completed 2500 of 3000)•5.8m (14.7mag, completed 1300 of 1600)•8.0m (13.2mag, completed 1600 of 2100)•redshifts for 7000 IRAC sources in total (so far)

• CXO/ACIS (Murray)•FX41015ergs/cm2/s (completed 600 of 1000)

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C. Kochanek

~7100 redshifts so far; ~11,000 by June

Galaxies

Quasars

Color = template used to get redshiftGalaxy templates include absorption, star formation and Seyfert components

C. Kochanek

R mag2014

reds

hift

1

K.A.O.S.!Kilo-Aperture Optical Spectrograph

• Gemini prime focus spectrograph– 1.5 degree field of view– ~4800 fibers– 12 spectrographs (4k x 4k CCDs)– Nod-and-shuffle sky subtraction

10-100 times better than any extant or 10-100 times better than any extant or planned facilityplanned facility

Arjun Deyhttp://www.noao.edu/kaos/

Thanks!

Complexity of problem => statistical approaches

How do galaxy formation and evolution depend upon (or perhaps influence?) the formation and evolution of large-scale structure?

Need to track mass, Z, SFH, morphology, gas/stellar content, accretion history as functions of time & environment

=> large samples

Structures on ~100h-1 Mpc scales! => large area

Arjun Dey

Motivation