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Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 1 AGN and Star Formation at High Redshift Anton Koekemoer (Space Telescope.

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Presentation on theme: "Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 1 AGN and Star Formation at High Redshift Anton Koekemoer (Space Telescope."— Presentation transcript:

1 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 1 AGN and Star Formation at High Redshift Anton Koekemoer (Space Telescope Science Institute) + CDFS/GOODS-AGN (Alexander, Brandt, Bergeron, Conselice, Chary, Cristiani, Dickinson, Elbaz, Grogin, Mainieri, Schreier, Treister, Urry, Wiklind...) +COSMOS-AGN (Brusa, Carilli, Capak, Civano, Comastri, Daddi, Elvis, Fiore, Hasinger, Ilbert, Impey, Jahnke, Mainieri, Martinez-Sansigre, Mobasher, Murayama, Nagao, Oyama, Salvato, Sanders, Sasaki, Schinnerer, Scoville, Smolcic, Treister, Taniguchi, Trump, Urry, Zamorani)

2 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 2 Black holes in context: Likely tracer of hierarchical dark matter halos Provide hard ionizing continuum, relevant to low-  reionization May regulate galaxy growth / SFR via feedback M-  relation suggests intimate connection between BH/galaxy formation and growth To date: At z ~ 6 - 6.5, already have supermassive BHs to ~ 10 9 M o ( Fan et al 2001-06; Willott et al. 2003; Vestergaard et al. 2004 ) AGN LF evolves strongly from z~6 to z~2; PLE is ruled out ( Fan et al. 2001+; Richards et al. 2006 ) Faint end of AGN LF steepens at z~6 ( Jiang et al 2009, Fan et al. (Richards et al. 2006)

3 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 3 Instead of PLE, AGN appear to follow “anti-hierarchical evol” -- luminosity-dependent density evolution “LDDE” at least for XLF ( Ueda et al. 2003, Hasinger et al. 2005; Gilli, Comastri, Hasinger 2006), QSO LF (Richards et al. 2006 ); also Merloni et al. (2004) : –luminous AGN peak earlier (z~2-3) –fainter AGN peak more recently (z~1) (XLF; Hasinger et al. 2005) (QSO LF, Richards et al. 2006)

4 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 4 Below L X ~ 10 44 erg s -1, density evolution is drastically different from higher-lum sources, peaking at lower z higher-lum sources show essentially pure density evolution suggests possible difference in accretion / galaxy evolution as a function of luminosity (Hasinger et al. 2005)

5 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 5

6 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 6 Questions: How do the most massive BHs form within < 1 Gyr? How does BH growth influence the M-  relation? What is the ionizing budget of AGN integrated over the LF beyond z ~ 6, and its contribution to reionization? (How) does obscured/unobsc. AGN ratio evolve at high z? Our knowledge has been limited by the following: only the top of the AGN LF has been studied at z ~ 6 no AGN previously confirmed at z > 7 Approach: Understand AGN / SFR evolution at z ~ 2 - 5 Set out to quantify the faint end of AGN LF at z ~ 6 Search for more luminous AGN at z > ~ 6 - 7

7 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 7 F Opt (mag) log F X (erg s -1 cm -2 ) AGN Require Wide+Deep X-ray / Optical / IR Surveys: Depth probes faint/moderate-lum AGN to high z Area probes high-lum AGN at high z (Hard) X-rays penetrate obscuring torus, IR probes rest-frame optical emission from AGN + host galaxy New part of parameter space: Combined optical + X-ray depth allows wider exploration of F X /F Opt :

8 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 8 Some current relevant surveys AreaFx (cgs)R(AB)I(AB)z(AB)J(AB)K(AB) f(3.6 ) X-Bootes9.34.0e-1525.524.9-21.020.65.0 COSMOS27.0e-1626.826.225.2-21.60.9 HELLAS2XMM0.97.5e-1525.0---19.115.0 XMM/SWIRE/ELAIS-S10.61.0e-1324.5 -21.020.03.7 SXDF/UKIDSS-UDS0.51.3e-1527.2-24.022.622.53.7 ECDFS/MUSYC0.253.9e-1625.824.723.623.523.00.8 AEGIS0.28.2e-1626.526.025.024.022.61.0 GOODS0.22.4e-1726.227.126.625.525.10.17

9 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 9 GOODS COSMOS ECDFS SXDF AEGIS

10 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 10 A Brief Selection of Extragalactic Survey Fields UDF: –3’x3’ HST/ACS (B,V,i,z) + NICMOS (JH) –Other coverage same as CDFS GOODS/CDFS+CDFN: –2x 10’x16’ HST/ACS (B,V,i,z) –Chandra 1Ms, Spitzer (3-70  m), ATCA, VLA, VLT, KPNO GEMS/ECDFS: –30’x30’ HST/ACS (i,z) –Chandra 1Ms+4x 250ks, Spitzer, ATCA, CTIO EGS: –10’ x 1 o HST/ACS (i,z) –Chandra 7x50ks, CFHT (UBVRIz) COSMOS: –1.4 o x 1.4 o HST/ACS (z) + NICMOS (J,H) –Subaru (UBVRiz), XMM, Spitzer, VLA

11 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 11 CDFS/GOODS-S+N survey: powerful combination of wide area and depth, opt/Xray: CDFS + CDFN have 1 & 2 Msec Chandra depth respectively –X-ray depth sufficient for AGN LF faint end (L X ~10 43-44 erg s -1 ) up to z ≥ 6 - 7 –area sufficient (0.1 sq deg) to provide number statistics on AGN LF at these redshifts More than 800 AGN from Chandra in GOODS-N & S (> 600 covered by HST/ACS and Spitzer) Extensive optical spectroscopic coverage Deep multi-band optical/NIR/Spitzer coverage: –JHK + Spitzer/IRAC 3.6 – 8  m observations trace host stellar mass for z > 1-2 –Spitzer/MIPS 24  m data helps constrain thermal dust emission

12 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 12 GOODS = G reat O bservatories O rigins D eep S urvey (Hubble, Chandra, Spitzer) Centered on CDFS, CDFN Supporting observations: VLT, Gemini, Keck, Subaru, KPNO, CTIO, VLA, ATCA, JCMT Goals: Extensive, deep multi- coverage Large enough area to probe both galaxy and AGN evolution Two fields reduce impact of cosmic variance

13 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 13 Advantages of X-ray selection: avoid obscuration effects in optical/IR at z > 2-3, hard X-rays are redshifted into soft observed X-ray bandpass, allows a more complete selection of obscured AGN (except for Compton thick sources) allows selection of more AGN than radio selection. Other wavelengths needed: deep optical to ensure good identification of dropouts: –at least R,I, preferably also z deep near-IR to provide detections relative to optical: –at least K, preferably also J,H Spitzer data to allow SED fitting: –at least IRAC 3.6 - 8 micron, preferably also MIPS 24 micron

14 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 14 Starformation in obscured AGN: IRAC colours Significant fraction (~50%) of z~2-4 obscured AGN show strong SFR signatures (Brusa et al. 2009): –S(8.0)/S(4.5) < 2 classified as SFR-dominated (Pope et al. 2008) (Brusa et al. 2009) Green points: 24  m selected field galaxies Blue points: AGN L X < 10 43 erg s -1 Red points: AGN L X > 10 43 erg s -1 Purple, yellow: other samples of high-z obscured AGN (Pozzi et al 2008, Pope et al 2008)

15 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 15 Starformation in obscured AGN: SFR Comparison with field galaxies: –For 65% of the obscured AGN, find significant SFR (>10M  /yr) –Result is robust for both optically and MIR-selected samples (Brusa et al. 2009) Upper panel: optically-selected field galaxies, AGN Lower panel: MIPS 24  m-selected field galaxies, AGN (Brusa et al. 2009)

16 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 16 Starformation in obscured AGN: SSFR Significant fraction of AGN still have active SSFR w.r.t mass (Alonso-Herrero et al. 2008, Busa et al. 2009) Red colours likely due to dust (not stellar population age)

17 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 17 Increased warm dust in z~1-2 obscured AGN: Lanzuisi et al (2009) sample: SWIRE sources, F24/Fopt > 1000 X-ray spectral properties used to compare with AGN in the local universe (yellow shaded region) Result: majority of the AGN have significant MIR excess wrt intrinsic Lx: requires excess dust component relative to local

18 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 18 Compton-Thick AGN Redshift Evolution Red: Lx > 1043 erg/s Blue: Lx > 1044 erg/s LFs: Della Ceca et al (2009) Yencho et al (2009) Normalized to Treister et al Steep rise above z~2 relative to non-CT AGN Treister et al. (2009)

19 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 19 Expected contributions of AGN & starbursts to LIR Examine triggering of AGN and starbursts in mergers (Hopkins et al 2009) - how significant is the contribution from AGN to the MIR LF? Find that, for log(LIR)>12-13, both starburst & AGN dominate LF To a similar extent, up to z~3

20 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 20 HST Morphologies of MIR Excess AGN

21 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 21 High-z AGN Candidates: “EXOs” Based on SED change with z: –Drop-outs in z 850lp (>27) –Anomalous Fx/Fopt (>100) –Red z 850lp - K (>4) Expect mostly obscured sources, but unobscured AGN are not excluded Highest F X /F Opt : found in several studies so far (Koekemoer et al 2002,2004; Brusa et al. 2004; Treister et al 2006; Koekemoer et al 2009) EXO’s - Extreme X-ray / Optical sources –Only revealed by extending optical depth below ~27 –Optically faint sources with anomalously high F X /F Opt >100 –Typically have extremely red z-K > 4-6 –Appear to have no comparable analogs in the local universe CDFS (Brandt et al, Koekemoer et al, Treister et al) u u u u u u u FX/Fopt = 0.1 FX/Fopt = 10

22 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 22 Candidate high-z AGN: X-z-K selection: X-ray properties: Well-detected by Chandra (~10 -16 -10 -15 erg s -1 cm -2 ) F X /F Opt is a lower limit, and is > ~100x above the average for AGN Generally have soft and hard X-ray emission (excludes z<2 obscured AGN) Redder z-K colour: most AGN with F X /F Opt ~ 0.1 - 10 have fairly tight z-K ~1-2, with some slight scatter: –z-K ~ -1 to 2 for quasars/Seyferts –z-K ~ 2 to 4 for ERO’s However, the EXO high-z candidates generally have z-K >4

23 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 23 CDFS EXOs

24 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 24 EXO/high-z candidates from GOODS N+S HST/ACS VLT+NOAO SPITZER/IRAC MIPS

25 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 25 EXO Close-up (contours = Chandra 0.5-8 keV)

26 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 26 SED Fitting Overall parameterization: Use CB03, Maraston06, vary IMF, metallicity  - stellar mass formed as SSP / CSP  - reddening (Fall & Charlot; Calzetti; SMC; LMC) Fits driven by two observational features: red opt/NIR - IRAC colours within IRAC General results: Use the fits to identify plausible z~2-3 interlopers Down-select to the remainder that are not well fit by z~2-3: –Follow these up with NIR spectroscopy (Subaru/Gemini/VLT) –Use their number counts to directly constrain high-z logN-logS

27 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 27 total ~2 million galaxies, ~1300 AGN (XMM: Hasinger et al, Brusa et al 2007) + radio (Schinnerer et al 2007) ~1.4°

28 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 28 COSMOS X-Ray Observations (Comastri, Brusa 2007) : XMM dataset: 53 pointings, ~1.6 sq deg (Brusa et al) Chandra dataset (1.8 Msec) ~1.4 sq deg, deeper than XMM Total of ~1300 sources in XMM, ~1800 in Chandra Limiting fluxes: –F(0.5-2 keV) ~ 1 x 10 -15 erg cm -2 s -1 –F(2-10 keV) ~ 5 x 10 -15 erg cm -2 s -1 Full survey: Combined XMM + Chandra ~2500 sources to date identify with ACS sources remove ambiguous IDs Finally, produce sample of EXOs: detect a total of 35 EXOs (cf ~7 for GOODS/CDFS) Likely a mixture of z~2-4 sources and z>~6 candidates, similar to GOODS

29 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 29 ACS- i K SPITZER/IRAC1,2,3,4 EXO/high-z candidates from COSMOS

30 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 30 ACS- i K SPITZER/IRAC1,2,3,4 (cont’d)

31 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 31 Constraining high-z AGN LF: Use hard X-ray XLF to estimate expected number of optically unidentified sources as a function of redshift: –Most of the optically unidentified AGN are evolved interlopers at intermediate z > 2 Compare with observed number of undetected sources: –use existing X-ray detection limits –apply optical detection cut-off (z(AB) ~ 27.5 for ACS) Integrate over X-ray luminosities at each redshift bin: –Use the difference to calculate cumulative number N(>6) –Compare with N(>6) from XLF

32 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 32 Number of optically unID’d sources N(z) based on z(AB)=27.5 limit, for current Chandra catalogs, using: –X-ray sensitivity –Optical flux limits –Spitzer flux limits LDDE predicts total of ~5 AGN at z>7 in GOODS+COSMOS (out of all the X-ray sources with ACS coverage): After removing low-z interlopers, currently have 4 likely z~7 candidates in GOODS+COSMOS - rough agreement with LDDE

33 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 33 New results - MOIRCS Spectroscopy (special thanks to Yoichi Oyama!) NIR spectroscopy of remaining high-z candidates Subaru - MOIRCS: ~4 hours/mask; objects faint (K~23+) Data reduction currently in progress One example EXO spectrum (no lines detected so far..):

34 Anton Koekemoer (STScI) Black Holes - STScI Spring Symposium, 23-26 Apr 2007 34 Summary: New results by several groups on z~2-4 AGN: –Many AGN are now found to have strong MIR SFR signatures –May be seeing “pre/post-blowout” QSO phase in action Overall number of high-z candidate AGN found in GOODS+COSMOS supports steepening of LF at z~6-7: –Intermediate-z interlopers successfully accounted for, and removed from dropout samples –Not clear yet whether faint-end slope needs to change as well or whether evolution can be accounted for by change in L* Next steps: –larger/deeper coverage at MIR with Spitzer and Herschel to better constrain rest-frame opt/IR and dust SEDs MAIN QUESTION: –What observational signatures to look for in determining the direction of causality for BH / bulge growth?

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