Slide 1

A Bolometric Approach To Galaxy And AGN Evolution. L. L. Cowie Venice 2006 (primarily from Wang, Cowie and Barger 2006, Cowie and Barger 2006 and Wang 2006 thesis)

Slide 2

The Hawaii bolometric sample: To understand the star formation and accretion history we need a census of all energy-producing galaxies & supermassive black holes in the universe, including those obscured by gas & dust. Best to choose them by their bolometric light rather than at a single frequency.

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The HDF /GOODS-N /CDF-N is still the best field for this!

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Wide Hawaii HDF-N Data BandSensitivity LimitTelescope / CameraSource (5sig Jy) U0.052KPNO 4mCapak et al. (2004) B0.063Subaru / SuprimeCamCapak et al. (2004) V0.069Subaru / SuprimeCamCapak et al. (2004) R0.083Subaru / SuprimeCamCapak et al. (2004) I0.209Subaru / SuprimeCamCapak et al. (2004) z0.251Subaru / SuprimeCamCapak et al. (2004) J0.839UH2.2m / ULBCAMTrouille et al. (2006) (400 sq arcmin) H1.06UH2.2m / ULBCAMTrouille et al. (2006) 3.6 m 0.327Spitzer / IRACGOODS Spitzer Legacy Program 4.5 m 0.411Spitzer / IRACGOODS Spitzer Legacy Program 5.8 m 2.27Spitzer / IRACGOODS Spitzer Legacy Program 8.0 m 2.15Spitzer / IRACGOODS Spitzer Legacy Program 24 m 80Spitzer / MIPSGOODS Spitzer Legacy Program

Slide 5

Just under 4000 galaxies have been spectroscopically identified in the region: remainder can be assigned photometric redshifts. J and H data considerably improves the robustness at z>2. Spectroscopic redshifts (as of early 2006)

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503 X-ray sources:(purple crosses) 202 20cm Radio sources (red squares): rectangle is core GOODS region.

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HAWAII BOLOMETRIC SAMPLE: 2740 objects with 0.3-24 micron fluxes above 1.5x10^(-14) erg cm^(-2) s^(-1) in the 140 square arcminute core GOODS region. This already contains all but 5 of the 40 microJy radio sources and all but 3 of the X-ray sources (CDF-N). We add the remaining 7 sources (2 are overlapped). Goal is a near-complete spectrosopic identification of the sample: with a uniform 4000-10000A spectral database (DEIMOS spectrograph) of very high quality and spectral resolution. Sample contains all of the 24 micron sources (this determines the limiting flux).

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STATUS: Goal is a complete spectrosopic identification of the sample: currently 1890/2475 of the sources are spectroscopically identified and all but about 100 of these have high quality spectra. Red=X-ray AGN

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Redshift distribution of Z band sources

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Today I just want to focus on the analysis of the submillimeter light and its implications for the star formation

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SCUBA Survey in the GOODS HDF-N GOODS HDF-N ~110 arcmin 2 by SCUBA 0.4-4 mJy (rms) sensitivity ~ 95 hours integration 27 sources at >3.5 Wang, Cowie, & Barger (2004) HDF-proper SCUBA 850 m map HST ACS imaging

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Spectroscopy of 20cm Selected Submm Sources redshift desert radio sensitivity limit Chapman et al. (2005) 18 Keck nights ~ 100 submm sources observed ~ 70 identified 2.2 median redshift = 2.2

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Problems Submm sources that are above SCUBAs detection limit (~2 mJy) only contribute ~20% of the total submm background. Only 60% of the above 20% can be detected by radio telescopes to 40 microJy at 20cm. Chapmans radio selected submm sources only represent ~10% of the total background. Need to know about the faint ( 1. Wang, Cowie and Barger, 2006 astro-ph/512347 (ApJ upcoming) The bolometric sample will appear shortly in Cowie and Barger (2006)

Slide 25

Number Counts from Clusters 0.3-2 mJy : N(>S) = 3.5 10 3 (S 850 /2 mJy) -1.2 deg -2 = 20 (+32/-8) Jy deg -2 Cowie, Barger, & Kneib (2002)

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SuprimeCam 0.45 0.45 Capak et al. (2004) HDF-proper

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Spitzer Images GOODS Spitzer Legacy Program 20 13 Confusion limited at 3.6-4.5 m

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Extragalactic Background Light total 850 um EBL : 31-44 Jy deg -2

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AGN in the Z band sample

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Submm EBL vs Near-IR Color

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B