The AGN and Galaxy The AGN and Galaxy Evolution SurveyEvolution Survey

(AGES)(AGES)

Daniel EisensteinDaniel EisensteinUniversity of ArizonaUniversity of Arizona

What is AGES?What is AGES?

AGES is a redshift AGES is a redshift survey of the 9 degsurvey of the 9 deg22 NOAO Deep Wide-Field NOAO Deep Wide-Field Survey Bootes field.Survey Bootes field. IIcc<20 for galaxies <20 for galaxies

(roughly (roughly ii<20.5).<20.5). IIcc<21.5 for AGN (going to <21.5 for AGN (going to

22.5 this spring).22.5 this spring). 20,000 redshifts.20,000 redshifts. Observations complete.Observations complete. ~3 mag fainter than ~3 mag fainter than

SDSS. SDSS.

Superb imagingSuperb imaging NDWFS NDWFS BBww, , RRcc, , IIcc to 25– to 25–

26 mag.26 mag. NDWFS NDWFS KK to 19 Vega to 19 Vega FLAMEX FLAMEX JJ & & KK deeper deeper

over half the fieldover half the field Spitzer IRAC and MIPS, Spitzer IRAC and MIPS,

similar to SWIRE depth.similar to SWIRE depth. Chandra (5 ksec)Chandra (5 ksec) GALEX planned to 25 ABGALEX planned to 25 AB Radio dataRadio data

Who is AGES?Who is AGES?

PIs: Chris Kochanek, Daniel Eisenstein, Steve MurrayPIs: Chris Kochanek, Daniel Eisenstein, Steve Murray Special mention: Nelson Caldwell, Richard CoolSpecial mention: Nelson Caldwell, Richard Cool NDWFS: Brand, Brown, Dey, R. Green, JannuziNDWFS: Brand, Brown, Dey, R. Green, Jannuzi Chandra: P. Green, Jones-Forman, ShieldsChandra: P. Green, Jones-Forman, Shields IRAC: Brodwin, Eisenhardt, Fazio, J. Huang, Pahre, Stern IRAC: Brodwin, Eisenhardt, Fazio, J. Huang, Pahre, Stern MIPS/IRS: Dole, Egami, Le Floc'h, Kuraszkiewicz, MIPS/IRS: Dole, Egami, Le Floc'h, Kuraszkiewicz,

Papovich, Perez-Gonzalez, M. Rieke, Soifer, Weedman, Papovich, Perez-Gonzalez, M. Rieke, Soifer, Weedman, WillmerWillmer

SO/SAO: Fan, Falco, Huchra, Impey, Moustakas, ZaritskySO/SAO: Fan, Falco, Huchra, Impey, Moustakas, Zaritsky GALEX: Martin, HeckmanGALEX: Martin, Heckman OSU: Kollmeier, Watson OSU: Kollmeier, Watson

Galaxy Target SelectionGalaxy Target Selection

Target selection is heavily Target selection is heavily multi-wavelength.multi-wavelength.

For galaxies, 100% to I<18.5, For galaxies, 100% to I<18.5, then sparse-sampled to I<20, then sparse-sampled to I<20, with heavier sampling for with heavier sampling for objects that pass flux cuts in objects that pass flux cuts in other bands.other bands.

BBWW, R, J, K, IRAC Ch 1-4, MIPS , R, J, K, IRAC Ch 1-4, MIPS

24 24 m, X-raym, X-ray 13k redshifts for 26k I<20 13k redshifts for 26k I<20

galaxies. Highly complete.galaxies. Highly complete. Largest spectroscopic Largest spectroscopic

sample of Spitzer objects.sample of Spitzer objects.

After correction, can think of After correction, can think of this as an this as an IIcc<20 sample, with <20 sample, with sparse sampling of “typical” sparse sampling of “typical” galaxies and better (often full) galaxies and better (often full) sampling for rare galaxies.sampling for rare galaxies.

Galaxy Redshift DistributionGalaxy Redshift Distribution

Blue: Main sampleBlue: Main sample Grey: Reweighted.Grey: Reweighted. Red: “Filler” sample.Red: “Filler” sample.

Reach L* at Reach L* at z z = 0.5.= 0.5.

Complementary to DEEP-2, Complementary to DEEP-2, which does not target z<0.7 which does not target z<0.7 galaxies, save for 0.5 deggalaxies, save for 0.5 deg22..

AGN Target SelectionAGN Target Selection

AGN were selected by AGN were selected by X-ray, mid-IR (red in X-ray, mid-IR (red in IRAC or 24 IRAC or 24 m m detect.), and radio, with detect.), and radio, with limited GALEX and limited GALEX and optical selection.optical selection. I<21.5 for point sources I<21.5 for point sources

(I<22.5 limited (I<22.5 limited coverage)coverage)

I<20 for extended I<20 for extended sources (I<22.5 limited sources (I<22.5 limited coverage).coverage).

At least 2000 AGN in 9 degAt least 2000 AGN in 9 deg22. . 1250 at z>1, 208 at z>2.5.1250 at z>1, 208 at z>2.5.

3 AGN at 5.1<z<5.8 3 AGN at 5.1<z<5.8 (Cool et al., 2006).(Cool et al., 2006).

AGES ScienceAGES Science Evolution of galaxy properties from Evolution of galaxy properties from zz~0.8 to today.~0.8 to today.

Optical luminosity function, color-luminosity distribution, stellar Optical luminosity function, color-luminosity distribution, stellar populations, mass-metallicity, Hpopulations, mass-metallicity, H star formation rates. star formation rates.

Mid-IR properties and evolution, e.g. luminosity functions in Mid-IR properties and evolution, e.g. luminosity functions in IRAC and MIPS, hidden star formation, stellar masses.IRAC and MIPS, hidden star formation, stellar masses.

Multi-wavelength distributions of galaxy properties, including Multi-wavelength distributions of galaxy properties, including versus environment.versus environment.

AGN properties from AGN properties from z z = 6 to today.= 6 to today. Study of diversity of SEDs, impact on selection, and implications Study of diversity of SEDs, impact on selection, and implications

for AGN physics.for AGN physics. Black hole masses, radiation rates, build-up of BHs, particularly Black hole masses, radiation rates, build-up of BHs, particularly

for lower luminosity AGN.for lower luminosity AGN. Leveraging of imaging catalogsLeveraging 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.

Rest-Frame Optical PropertiesRest-Frame Optical Properties

IIcc to to rr0.10.1

BBWW to to uu0.10.1

Color bimodality is obvious.Color bimodality is obvious.

As observed.

Optical Luminosity FunctionOptical Luminosity Function

Evolution is clear. Low redshift matches SDSS.Evolution is clear. Low redshift matches SDSS.

Split blue vs. Split blue vs. red galaxies, red galaxies, using a redshift using a redshift dependent cut.dependent cut.

Luminosity-Luminosity-color bimodal color bimodal distribution distribution clearly seen at clearly seen at all redshifts.all redshifts.

Red vs. Blue GalaxiesRed vs. Blue Galaxies

Low redshift luminosity functions match those Low redshift luminosity functions match those from SDSS.from SDSS.

Clear evolution in both sets.Clear evolution in both sets.

Evolution of the Optical LFEvolution of the Optical LF

Fit Schechter forms to the LFs, holding Fit Schechter forms to the LFs, holding fixed at the fixed at the SDSS value.SDSS value.

Luminosity density is near constant for red galaxies, Luminosity density is near constant for red galaxies, increasing for blue galaxies. L* increases for both sets.increasing for blue galaxies. L* increases for both sets.

A Multiwavelength View of GalaxiesA Multiwavelength View of Galaxies

The pan-chromatic imaging in the The pan-chromatic imaging in the Bootes field offers a marvelous Bootes field offers a marvelous opportunity to use multiwavelength opportunity to use multiwavelength data to study galaxy properties.data to study galaxy properties.

UV, Spitzer, HUV, Spitzer, H, and radio for star , and radio for star formation.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 Now have the redshifts to translate these observed quantities into rest-these observed quantities into rest-frame properties.frame properties.

QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.

Mid-Infrared PropertiesMid-Infrared Properties

Red points are upper

limits.

Galaxy 24 Galaxy 24 m Luminosity Functionm Luminosity Function

Preliminary: No Mid-IR

K-corrections

Q is at least 2.5; K corrections will enhance this.Q is at least 2.5; K corrections will enhance this.

Where are the Mid-IR Luminous Galaxies?Where are the Mid-IR Luminous Galaxies?

Imposing a 24 micron to optical color cut.Imposing a 24 micron to optical color cut.

Optical LF seems UnchangedOptical LF seems Unchanged

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

Mid-IR Galaxies are Mid-IR Galaxies are slightly offset in optical colorslightly offset in optical color

Hectospec Lessons from AGESHectospec Lessons from AGES

Rolling inspections with monthly re-design of Rolling inspections with monthly re-design of configurations.configurations.

F star sentinals for spectrophotometry.F star sentinals for spectrophotometry. Fiber collisions were severe; required many Fiber collisions were severe; required many

visits to reach completeness goals. Density-visits to reach completeness goals. Density-dependent sparse sampling might be better.dependent sparse sampling might be better.

We were lucky not to get stuck “mid-sweep” with We were lucky not to get stuck “mid-sweep” with weather losses; this would have compromised weather losses; this would have compromised survey completeness.survey completeness.

ConclusionsConclusions

We have completed a large galaxy and AGN We have completed a large galaxy and AGN redshift survey.redshift survey.

Superb imaging from space and ground.Superb imaging from space and ground. Many different science analyses are underway.Many different science analyses are underway.

Measuring evolution of galaxies from Measuring evolution of galaxies from zz=0.8 to today.=0.8 to today. General data release coming ASAP, but we're General data release coming ASAP, but we're

open to new collaborations now.open to new collaborations now.

Thanks to the Hectospec instrument team, the Thanks to the Hectospec instrument team, the robot operators, and the MMT staff!robot operators, and the MMT staff!