1. The AGN and Galaxy Evolution Survey (AGES) Daniel Eisenstein University of Arizona

2. What is AGES?  AGES is a redshift survey of the 9 deg 2 NOAO Deep Wide-Field Survey Bootes field. I c <20 for galaxies (roughly i<20.5). I c <20 for galaxies (roughly i<20.5). I c <21.5 for AGN (going to 22.5 this spring). I c <21.5 for AGN (going to 22.5 this spring). 20,000 redshifts. 20,000 redshifts. Observations complete. Observations complete. ~3 mag fainter than SDSS. ~3 mag fainter than SDSS.  Superb imaging NDWFS B w, R c, I c to 25– 26 mag. NDWFS K to 19 Vega FLAMEX J & K deeper over half the field Spitzer IRAC and MIPS, similar to SWIRE depth. Chandra (5 ksec) GALEX planned to 25 AB Radio data

3. Who is AGES?  PIs: Chris Kochanek, Daniel Eisenstein, Steve Murray  Special mention: Nelson Caldwell, Richard Cool  NDWFS: Brand, Brown, Dey, R. Green, Jannuzi  Chandra: P. Green, Jones-Forman, Shields  IRAC: Brodwin, Eisenhardt, Fazio, J. Huang, Pahre, Stern  MIPS/IRS: Dole, Egami, Le Floc'h, Kuraszkiewicz, Papovich, Perez-Gonzalez, M. Rieke, Soifer, Weedman, Willmer  SO/SAO: Fan, Falco, Huchra, Impey, Moustakas, Zaritsky  GALEX: Martin, Heckman  OSU: Kollmeier, Watson

4. Galaxy Target Selection  Target selection is heavily multi-wavelength.  For galaxies, 100% to I<18.5, then sparse-sampled to I<20, with heavier sampling for objects that pass flux cuts in other bands. B W, R, J, K, IRAC Ch 1-4, MIPS 24  m, X-ray B W, R, J, K, IRAC Ch 1-4, MIPS 24  m, X-ray 13k redshifts for 26k I<20 galaxies. Highly complete. 13k redshifts for 26k I<20 galaxies. Highly complete. Largest spectroscopic sample of Spitzer objects. Largest spectroscopic sample of Spitzer objects.  After correction, can think of this as an I c <20 sample, with sparse sampling of “typical” galaxies and better (often full) sampling for rare galaxies.

5. Galaxy Redshift Distribution  Blue: Main sample  Grey: Reweighted.  Red: “Filler” sample.  Reach L* at z = 0.5.  Complementary to DEEP-2, which does not target z<0.7 galaxies, save for 0.5 deg 2.

6. AGN Target Selection  AGN were selected by X-ray, mid-IR (red in IRAC or 24  m detect.), and radio, with limited GALEX and optical selection. I<21.5 for point sources (I<22.5 limited coverage) I<21.5 for point sources (I<22.5 limited coverage) I<20 for extended sources (I<22.5 limited coverage). I<20 for extended sources (I<22.5 limited coverage).  At least 2000 AGN in 9 deg 2. 1250 at z>1, 208 at z>2.5.  3 AGN at 5.1<z<5.8 (Cool et al., 2006).

7. AGES Science  Evolution of galaxy properties from z~0.8 to today. Optical luminosity function, color-luminosity distribution, stellar populations, mass-metallicity, H  star formation rates. Optical luminosity function, color-luminosity distribution, stellar populations, mass-metallicity, H  star formation rates. Mid-IR properties and evolution, e.g. luminosity functions in IRAC and MIPS, hidden star formation, stellar masses. Mid-IR properties and evolution, e.g. luminosity functions in IRAC and MIPS, hidden star formation, stellar masses. Multi-wavelength distributions of galaxy properties, including versus environment. Multi-wavelength distributions of galaxy properties, including versus environment.  AGN properties from z = 6 to today. Study of diversity of SEDs, impact on selection, and implications for AGN physics. Study of diversity of SEDs, impact on selection, and implications for AGN physics. Black hole masses, radiation rates, build-up of BHs, particularly for lower luminosity AGN. Black hole masses, radiation rates, build-up of BHs, particularly for lower luminosity AGN.  Leveraging of imaging catalogs Photo-z training for Spitzer, NDWFS, and SDSS. Photo-z training for Spitzer, NDWFS, and SDSS. Cross-correlations to fainter galaxies. Cross-correlations to fainter galaxies.

8. Rest-Frame Optical Properties  I c to r 0.1  B W to u 0.1  Color bimodality is obvious. As observed.

9. Optical Luminosity Function  Evolution is clear. Low redshift matches SDSS.

10.  Split blue vs. red galaxies, using a redshift dependent cut.  Luminosity- color bimodal distribution clearly seen at all redshifts.

11. Red vs. Blue Galaxies  Low redshift luminosity functions match those from SDSS.  Clear evolution in both sets.

12. Evolution of the Optical LF  Fit Schechter forms to the LFs, holding  fixed at the SDSS value.  Luminosity density is near constant for red galaxies, increasing for blue galaxies. L* increases for both sets.

13. A Multiwavelength View of Galaxies  The pan-chromatic imaging in the Bootes field offers a marvelous opportunity to use multiwavelength data to study galaxy properties. UV, Spitzer, H , and radio for star formation. UV, Spitzer, H , and radio for star formation. Near-IR for stellar masses. Near-IR for stellar masses. X-ray and mid-IR for nuclear activity. X-ray and mid-IR for nuclear activity. Optical spectroscopic diagnostics. Optical spectroscopic diagnostics.  Now have the redshifts to translate these observed quantities into rest- frame properties.

14. Mid-Infrared Properties Red points are upper limits.

15. Galaxy 24  m Luminosity Function Preliminary: No Mid-IR K-corrections  Q is at least 2.5; K corrections will enhance this.

16. Where are the Mid-IR Luminous Galaxies?  Imposing a 24 micron to optical color cut.

17. Optical LF seems Unchanged

18. Mid-IR Galaxies avoid the blue edge of the late-types.

19. Mid-IR Galaxies are slightly offset in optical color

20. Hectospec Lessons from AGES  Rolling inspections with monthly re-design of configurations.  F star sentinals for spectrophotometry.  Fiber collisions were severe; required many visits to reach completeness goals. Density- dependent sparse sampling might be better.  We were lucky not to get stuck “mid-sweep” with weather losses; this would have compromised survey completeness.

21. Conclusions  We have completed a large galaxy and AGN redshift survey.  Superb imaging from space and ground.  Many different science analyses are underway. Measuring evolution of galaxies from z=0.8 to today. Measuring evolution of galaxies from z=0.8 to today.  General data release coming ASAP, but we're open to new collaborations now.  Thanks to the Hectospec instrument team, the robot operators, and the MMT staff!

23. Hectospec & SDSS  As a SDSS project, we have observed fields from stripe 82 for z=0.8 LRGs and faint quasars.  Had hoped for 10 deg 2 but horrid weather limited us to about 5 deg 2.  LRGs selected in r-i-z color space and observed to z=20.3. Cool & DJE are analyzing luminosity function.  AGN selected to g=22.5. Faint-end LF presented by Jiang et al., 2006, in press.  Further collaborative projects here are possible.

24. MMT & Hectospec  MMT is a 6.5-meter telescope on Mt. Hopkins, south of Tucson.  Hectospec provides 300 fibers over a 1 degree field of view. 1.5" apertures 1.5" apertures R=1000 currently R=1000 currently 20-30 minute overhead per config; robot positioner. 20-30 minute overhead per config; robot positioner. PI: Dan Fabricant (CfA) PI: Dan Fabricant (CfA)

25. AGES & SDSS  AGES is intended for many different science goals.  In the SDSS context, it can characterize galaxy and AGN properties at exactly the depths of the SDSS photometry.  SDSS has imaged this region; AGES could be used to train/test SDSS photo-z's.