The AGN and Galaxy Evolution Survey (AGES)

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

2. AGES is a redshift survey of the 9 deg2 NOAO Deep Wide-Field Survey Bootes field. Ic<20 for galaxies (roughly i<20.5). Ic<21.5 for AGN (going to 22.5 this spring). 20,000 redshifts. Observations complete. ~3 mag fainter than SDSS. Superb imaging NDWFS Bw, Rc, Ic 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 What is AGES?

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. • BW, R, J, K, IRAC Ch 1-4, MIPS 24 mm, X-ray • 13k redshifts for 26k I<20 galaxies. Highly complete. • Largest spectroscopic sample of Spitzer objects. • After correction, can think of this as an Ic<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 deg2.

6. AGN Target Selection • AGN were selected by X-ray, mid-IR (red in IRAC or 24 mm detect.), and radio, with limited GALEX and optical selection. • I<21.5 for point sources (I<22.5 limited coverage) • I<20 for extended sources (I<22.5 limited coverage). • At least 2000 AGN in 9 deg2. 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, Ha star formation rates. • 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. • AGN properties from z = 6 to today. • 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. • Leveraging of imaging catalogs • Photo-z training for Spitzer, NDWFS, and SDSS. • Cross-correlations to fainter galaxies.

8. Rest-Frame Optical Properties • Ic to r0.1 • BW to u0.1 • 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 a 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, Ha, and radio for star formation. • Near-IR for stellar masses. • X-ray and mid-IR for nuclear activity. • 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 mm 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. • 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!