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Galaxy Evolution Studies & the NOAO Deep Wide-Field Survey

Galaxy Evolution Studies & the NOAO Deep Wide-Field Survey. Arjun Dey National Optical Astronomy Observatory (for the NDWFS Team). NDWFS Co-Investigators.

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Galaxy Evolution Studies & the NOAO Deep Wide-Field Survey

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  1. Galaxy Evolution Studies & the NOAO Deep Wide-Field Survey Arjun Dey National Optical Astronomy Observatory (for the NDWFS Team)

  2. 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 90 249 Arjun Dey

  3. WMAP Motivation ? M. Steinmetz Arjun Dey Lacey & Cole COBE

  4. The Power of Wide-Field Surveys Statistical approach to complex problems Large samples define population trends statistically precise measurements rare populations Wide area large scale clustering less sensitive to cosmic variance For example …

  5. t=1Gyr BC03/Salpeter BW-drops z~3.5-4.2 Red envelope population Features in the Color-Color Diagram 6.0 BW-R ~0.6M galaxies 0 2.5 -0.5 R-I Arjun Dey

  6. Magnitude Slices in Color-Color Space 17-18 20-21 23-24 18-19 21-22 24-25 BW-R 19-20 22-23 25-26 R-I Arjun Dey

  7. The Redshift Distribution in the Color-Color Plane Arjun Dey

  8. 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) • (t-models with high zF are a reasonable fit; spectra show [OII]) • A well-defined sample … and photo-z’s work well! Arjun Dey

  9. Our Photometric vs Spectroscopic zs (see M. Brown’s talk for clustering results and K. Brand’s talk for accretion history) Arjun Dey

  10. The Red Galaxy Sample: The Future 1.3 sq deg -> 18 sq deg! Wow! Arjun Dey

  11. LALA Bw-R R-I High-redshift galaxies in NDWFSz~3.7 “BW-drops” BW-R > 2.5 BW-R > 2(R-I)+1.7 R < 25 Arjun Dey

  12. Comparisons with other high-z surveys So stay tuned … Arjun Dey

  13. Spectroscopic Campaigns in the NDWFS Fields • 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)

  14. 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 R19.2 mag (completed 4200 of 5500) • random 20% of galaxies 19.2<R20 (completed 750 of 1400) • for all galaxies 19.2<R20 completed 2100 of 7200 • NDWFS BW band (BW20.5, completed 2300 of 3000) • SST/MIPS (Soifer) • 24m (F1mJy, completed 1100 of 1400) • including point sources off stellar locus • redshifts for 3100 24m sources in total (so far) • SST/IRAC (Eisenhardt) • 3.6m (15.2mag, completed 1900 of 2300) • 4.5m (15.2mag, completed 2500 of 3000) • 5.8m (14.7mag, completed 1300 of 1600) • 8.0m (13.2mag, completed 1600 of 2100) • redshifts for 7000 IRAC sources in total (so far) • CXO/ACIS (Murray) • FX41015ergs/cm2/s (completed 600 of 1000) C. Kochanek

  15. ~7100 redshifts so far; ~11,000 by June 1 Quasars redshift Galaxies 14 20 R mag Color = template used to get redshift Galaxy templates include absorption, star formation and Seyfert components C. Kochanek

  16. 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 planned facility http://www.noao.edu/kaos/ Arjun Dey

  17. Thanks!

  18. Motivation How do galaxy formation and evolution depend upon (or perhaps influence?) the formation and evolution of large-scale structure? Complexity of problem => statistical approaches 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

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