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Vital Statistics: 1.8 Ms
½ sq.deg @160 ksec
1761 sourcesDec ’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 Spot2. ‘Galaxies’3. SEDs: Elvis was right!4. Dust Poor AGNs (mostly)5. Recoiling BH6. New Proposals: Chandra, HST
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
Chandra-COSMOS Sweet Spot
SEDs
IDs?
Spectra
Chandra-COSMOS Sweet Spot
SEDs
IDs?
Spectra
C-COSMOS Galaxies
LX>1042 erg/s
AGN?
Log X/O (2-10keV)
Lanzuisi et al., 2010, in preparation
X-ray luminous & heavily obscuredwhen enough counts
•Keck/DEIMOS spectra:• AGN + Starburst + Wind
Feruglio et al., in prep.
Spectroscopic RedshiftsSo far:• 631 spec-z(SDSS, zCOSMOS, IMACS, Keck)Mostly XMM sources
• Only 13 BL AGN not in XMM214 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 zspec>358 sources at zphot>3
z phot
z spec
z>3 Quasars
z=5.4Highest zX-ray selectedquasar
z=6.8 candidateSalvato et al.
BUT…
z>3 Quasars
COSMOS Type 1 AGN SEDs
XMM
Hot Dust Accretion Disk
αnir αopt
Quasar-Host-Reddening Mixing Diagram
(Polletta et al. 2007)Host Dominated
AGN Dominated
Reddening Dominated
???
E(B-V)
COSMOS AGN on Mixing Diagram
αopt
Consistent with meanE94+HOST+Reddening
COSMOS AGN on Mixing DiagramE94 mean SED works in 90% of COSMOS Quasars
(Hao et al. 2010)
αopt
Hot-Dust Poor AGNs
Number of Sources: 42/402
αopt
Hao et al. 2010: Letter circulated to COSMOS team
Hot-Dust Poor AGNs
Number of Sources: 42/402
αopt
Hao et al. 2010
E94E94 E94
Bolometric Luminosity vs Redshift
z<1.54.9%±0.8%
1.5<z<315.9%±3%
Larger Fraction At z>1.5Evolution
Hao et al. 2010
Hot Dust Covering Factor
Dust temperature =1500 KEmission 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
Accretion Disk Outer Radius
Tc~ R-3/4 KMeasure: Tc=1800 KRout=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
SED Fitting & M-s Relation
E94 AGN
Starburst
Merloni et al. 2010
Hao et al. 2010
• 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:
Lower Mhost
Higher Mbh
• Test: em. line EW• Moves points away from M-s• Need new AGN templates with separate Big Blue Bump and Hot Dust components
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
• Lbol 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
Civano et al. 2010, Ap.J. in press, arXiv1003.0020C(see also Elvis 2009 and Comerford et al. 2009)
15”x15” HST+ Chandra
N
E
CID-42
• 3 times peculiar COSMOS source: 1. 2 sources in the optical image2. 2 nuclear emission line system3. Large velocity offset: 1100 km/s
• Too large for a merger4. 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
2.5kp
c
CID-42: GW or Slingshot Recoiling BH?
Resolved with HST but NOT with Chandra!
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 Hb• Narrow offset component• nuclei unresolved
Keck/IFU done (Hai Fu)HST/STIS [proposed]Chandra/HRC [proposed]
SNLS/COSMOS AGN variabilitySumin 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)
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 area200ksec 0.9sq.deg ~ deep area
• Alternative: 800ksec on MCT3 ACIS fields, 2.4Ms
• TAC meeting June 21-25Results by end-August
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
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-OMfilters
Vital Statistics: 1.8 Ms
½ sq.deg @160 ksec
1761 sourcesDec ’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 Spot2. ‘Galaxies’3. SEDs: Elvis was right!4. Dust Poor AGNs (mostly)5. Recoiling BH6. New Proposals: Chandra, HST
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