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The Chandra COSMOS X-ray Survey
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The Chandra COSMOS X-ray Survey

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  1. VitalStatistics: 1.8 Ms ½sq.deg @160 ksec 1761 sources Dec ’06-June ’07 Catalog: Elvis et al., 2009, ApJS 184, 158 Wedding Cake Sweet Spot ‘Galaxies’ SEDs: Elvis was right! Dust Poor AGNs (mostly) Recoiling BH New Proposals: Chandra, HST The Chandra COSMOS X-raySurvey Martin Elvis, Francesca Civano, Aldcroft T., Fruscione A., Harvard Smithsonian Center forAstrophysics SalvantoM.,Vignali C., Puccetti S., Zamorani G., Brusa M., Cappelluti N., Fiore F., Comastri A., Salvato M., Mainieri V., Lanzuisi, G., and the COSMOS TEAM

  2. Chandra COSMOS hits a SweetSpot in the “CosmicWeddingCake” Faint CDFs COSMOS Flux XBootes AREA Faint enough to find ‘not just more AGNs’ Not too deep to get IDs, SEDs, spectra Big enough to have large samples, find rare objects Champ

  3. Chandra-COSMOS Sweet Spot IDs? SEDs Spectra

  4. Chandra-COSMOS Sweet Spot IDs? SEDs Spectra

  5. C-COSMOS Galaxies • X-rayluminous & heavilyobscured • whenenoughcounts LX>1042 erg/s AGN? • Keck/DEIMOS spectra: • AGN + Starburst + Wind • Feruglio et al., in prep. Log X/O (2-10keV) Lanzuisiet al., 2010, in preparation

  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 zcoming soon • Mostly: • red (R-K)>~4 • faint, i>22 • Candidates: • double lines • z > 5 • High z Samples in dozens: • 22 sources at zspec>3 • 58 sources at zphot>3 zphot • 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 αnir αopt Hot Dust Accretion Disk XMM

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

  11. COSMOS AGN on Mixing Diagram αopt

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

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

  14. Hot-Dust Poor AGNs E94 E94 E94 Number of Sources: 42/402 Hao et al. 2010 αopt

  15. Bolometric Luminosity vsRedshift Larger Fraction At z>1.5 Evolution z<1.5 4.9%±0.8% 1.5<z<3 15.9%±3% Hao et al. 2010

  16. Hot Dust Covering Factor Dust temperature =1500 K Emission Area =0.15 pc2 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 Tc~R-3/4 K Measure: Tc=1800 K Rout=0.24 pc ≈ 6000 Rs >> Gravitational Instability radius (rgi≈ few 100 Rs, Goodman et al. 2003) Either: 1) Not Rout 2) Or something stabilizes disk Hao et al. 2010

  18. SED Fitting & M-s Relation • M-σ relation: basis of co-evolution • Higher Mbh/Mhost at z~1? • Merloni et al. 2010 • Depends on SED fitting: • e.g. 817202(z=1.53) = extreme Starburst, if E94 SED required • If Hot-dust-Poor Quasar: • LowerMhost • HigherMbh • Test: em. line EW • Moves points away from M-s • Need new AGN templates with separate Big Blue Bump and Hot Dust components Merloni et al. 2010 Starburst E94 AGN Hao et al. 2010

  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 • Lboltoo low? (Elitzur & Schlosman 2006)NO • Hot dust destroyed: • Radiation: Eddington Outburst? Inflow/formation time • Dynamically: during merger? • Consistent with evolution to low HDP fraction at z < 1.5 Hao et al. 2010

  20. CID-42:GW or Slingshot Recoiling BH? N E 15”x15” HST+Chandra • 3 times peculiar COSMOS source: • 2 sources in the optical image • 2 nuclear emission line system • Large velocity offset: 1100 km/s • Too large for a merger • 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 CID-42 Civano et al. 2010, Ap.J. in press, arXiv1003.0020C (see also Elvis 2009 and Comerford et al. 2009) 2.5kpc Resolved with HST but NOT with Chandra!

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

  22. SNLS/COSMOS AGN variabilitySumin Tang (Harvard) 240type 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 21-25 • Results by end-August

  24. HST Cycle 18 GO Proposal: The Dark Side of Accretion: The Obscured AGN/Starburst Phase in COSMOS • 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 • 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

  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: aOX • Intermediate wavelength: SEDs • Partly funded by SI • Proposal in to NASA ADA XMM-OM filters

  26. VitalStatistics: 1.8 Ms ½sq.deg @160 ksec 1761 sources Dec ’06-June ’07 Catalog: Elvis et al., 2009, ApJS 184, 158 Wedding Cake Sweet Spot ‘Galaxies’ SEDs: Elvis was right! Dust Poor AGNs (mostly) Recoiling BH New Proposals: Chandra, HST The Chandra COSMOS X-raySurvey Martin Elvis, Francesca Civano, Aldcroft T., Fruscione A., Harvard Smithsonian Center forAstrophysics SalvantoM.,Vignali C., Puccetti S., Zamorani G., Brusa M., Cappelluti N., Fiore F., Comastri A., Salvato M., Mainieri V., Lanzuisi, G., and the COSMOS TEAM