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Vital Statistics: 1.8 Ms ½ 160 ksec 1761 sources Dec 06-June 07 Catalog: Elvis et al., 2009, ApJS 184, 158 Martin Elvis, Francesca Civano, Aldcroft.

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Presentation on theme: "Vital Statistics: 1.8 Ms ½ 160 ksec 1761 sources Dec 06-June 07 Catalog: Elvis et al., 2009, ApJS 184, 158 Martin Elvis, Francesca Civano, Aldcroft."— Presentation transcript:

1 Vital Statistics: 1.8 Ms ½ 160 ksec 1761 sources Dec 06-June 07 Catalog: Elvis et al., 2009, ApJS 184, 158 Martin Elvis, Francesca Civano, Aldcroft T., Fruscione A., Harvard Smithsonian Center for Astrophysics Salvanto M.,Vignali C., Puccetti S., Zamorani G., Brusa M., Cappelluti N., Fiore F., Comastri A., Salvato M., Mainieri V., Lanzuisi, G., and the COSMOS TEAM The Chandra COSMOS X-ray Survey 1.Wedding Cake Sweet Spot 2.Galaxies 3.SEDs: Elvis was right! 4.Dust Poor AGNs (mostly) 5.Recoiling BH 6.New Proposals: Chandra, HST

2 Chandra COSMOS hits a Sweet Spot Faint AREA Flux CDFs COSMOS XBootes in the Cosmic Wedding Cake Champ 1.Faint enough to find not just more AGNs 2.Not too deep to get IDs, SEDs, spectra 3.Big enough to have large samples, find rare objects

3 Chandra-COSMOS Sweet Spot SEDs IDs? Spectra

4 Chandra-COSMOS Sweet Spot SEDs IDs? Spectra

5 C-COSMOS Galaxies L X >10 42 erg/s AGN? Log X/O (2-10keV) Lanzuisi et al., 2010, in preparation X-ray luminous & heavily obscured when enough counts Keck/DEIMOS spectra: AGN + Starburst + Wind Feruglio et al., in prep.

6 Spectroscopic Redshifts So far: 631 spec-z (SDSS, zCOSMOS, IMACS, Keck) Mostly XMM sources Only 13 BL AGN not in XMM 214 total 153 new Keck z coming soon Mostly: red (R-K)>~4 faint, i>22 Candidates: double lines z > 5 High z Samples in dozens: 22 sources at z spec >3 58 sources at z phot >3 z phot z spec

7 z>3 Quasars z=5.4 Highest z X-ray selected quasar z=6.8 candidate Salvato et al. BUT…

8 z>3 Quasars

9 COSMOS Type 1 AGN SEDs XMM Hot DustAccretion Disk α nir α opt

10 Quasar-Host-Reddening Mixing Diagram (Polletta et al. 2007) Host Dominated AGN Dominated Reddening Dominated ??? E(B-V)

11 COSMOS AGN on Mixing Diagram α opt

12 Consistent with mean E94+HOST+Reddening COSMOS AGN on Mixing Diagram E94 mean SED works in 90% of COSMOS Quasars (Hao et al. 2010) α opt

13 Hot-Dust Poor AGNs Number of Sources: 42/402 α opt Hao et al. 2010: Letter circulated to COSMOS team

14 Hot-Dust Poor AGNs Number of Sources: 42/402 α opt Hao et al E94

15 Bolometric Luminosity vs Redshift z< %±0.8% 1.51.5 Evolution Hao et al. 2010

16 Hot Dust Covering Factor Dust temperature =1500 K Emission Area =0.15 pc 2 Sublimation radius =0.81 pc (Barvainis, 1987) Covering factor ~ 0.2 Cf 75% for type1:type2 ratio Hao et al. 2010

17 Accretion Disk Outer Radius T c ~ R -3/4 K Measure: T c =1800 K R out =0.24 pc 6000 R s >> Gravitational Instability radius (r gi few 100 R s, Goodman et al. 2003) Either: 1) Not R out 2) Or something stabilizes disk Hao et al. 2010

18 SED Fitting & M- Relation E94 AGN Starburst Merloni et al Hao et al M-σ relation: basis of co-evolution Higher M bh /M host at z~1? Merloni et al Depends on SED fitting: e.g (z=1.53) = extreme Starburst, if E94 SED required If Hot-dust-Poor Quasar: Lower M host Higher M bh Test: em. line EW Moves points away from M- Need new AGN templates with separate Big Blue Bump and Hot Dust components

19 What are Hot-Dust Poor Quasars? Torus not yet formed? (Jiang et al. 2010: 2 z~6 HDPs) NO plenty of cosmic time at z~2 (1-2Gyr) Accretion rate too low to drive wind? (Elitzur & Ho 2009) NO L bol too low? (Elitzur & Schlosman 2006) NO Hot dust destroyed: 1.Radiation: Eddington Outburst? Inflow/formation time 2.Dynamically: during merger? Consistent with evolution to low HDP fraction at z < 1.5 Hao et al. 2010

20 Civano et al. 2010, Ap.J. in press, arXiv C (see also Elvis 2009 and Comerford et al. 2009) 15x15 HST+ Chandra N E CID-42 3 times peculiar COSMOS source: 1.2 sources in the optical image 2.2 nuclear emission line system 3.Large velocity offset: 1100 km/s Too large for a merger 4.Variable redshifted X-ray iron line in absorption Very RARE, 1 in 2600 Gravitational wave recoil? Slingshot from triple BH system? The best case of GW recoil BH with both Imaging and Spectroscopic signatures 2.5kpc CID-42: GW or Slingshot Recoiling BH? Resolved with HST but NOT with Chandra!

21 New DEIMOS/Keck spectrum R~2700 (1.4 x Comerford) ; 47 mins; Seeing 0.6 Slit oriented in the direction of the nuclei Confirms offset broad H Narrow offset component nuclei unresolved Keck/IFU done (Hai Fu) HST/STIS [proposed] Chandra/HRC [proposed]

22 SNLS/COSMOS AGN variability Sumin Tang (Harvard) 240 type 1 AGNs, ~120 type 2 AGNs 4 years Used to select variable AGNs for MMT/Hectospec bulk reverberation program (see J.Trump talk)

23 ECHOES: Extended Chandra Cosmic Evolution Survey Chandra Cycle 12 ECHOES: 1.4 Msec (out of 3Ms for VLP) ~doubles coverage: 100ksec 1.4sq.deg ~HST area 200ksec 0.9sq.deg ~ deep area Alternative: 800ksec on MCT 3 ACIS fields, 2.4Ms TAC meeting June Results by end-August

24 HST Cycle 18 GO Proposal: The Dark Side of Accretion: The Obscured AGN/Starburst Phase in COSMOS WFC/IR-grism + imaging 75 DOGS, 2.5/field 1.16 < z < 2.39 (4000A break, [OIII]) 60 MIPS selected 15 Chandra X-ray selected 60 orbits Virtually no overlap w. MCT Faber/Ferguson program Connecting galaxy and obscured BH growth L(AGN) from L[OIII]: BH growth rate Stellar age from 4000A break Merger state, bulge mass from IR imaging

25 UV Imaging of COSMOS with the XMM Optical Monitor Millions of seconds of neglected UV data 2 HPD (c.f. 6 GALEX) Multiple epochs – variability Simultaneous w X-ray: OX Intermediate wavelength: SEDs Partly funded by SI Proposal in to NASA ADA XMM-OM filters

26 Vital Statistics: 1.8 Ms ½ 160 ksec 1761 sources Dec 06-June 07 Catalog: Elvis et al., 2009, ApJS 184, 158 Martin Elvis, Francesca Civano, Aldcroft T., Fruscione A., Harvard Smithsonian Center for Astrophysics Salvanto M.,Vignali C., Puccetti S., Zamorani G., Brusa M., Cappelluti N., Fiore F., Comastri A., Salvato M., Mainieri V., Lanzuisi, G., and the COSMOS TEAM The Chandra COSMOS X-ray Survey 1.Wedding Cake Sweet Spot 2.Galaxies 3.SEDs: Elvis was right! 4.Dust Poor AGNs (mostly) 5.Recoiling BH 6.New Proposals: Chandra, HST

27 Dust Obscured Galaxies - DOGs Most C-COSMOS galaxies are DOGs: 50% have NeV = obscured AGN 60% of NeV have v from [OII] km/s :Winds Keck/DEIMOS spectra: AGN + Starburst + Wind (low ionization) Now >15 cases (Feruglio et al., in prep.) More in latest DEIMOS spectra v


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