Type 1 AGN SEDs in the COSMOS
A Single Form, Mixing Diagram,
and Outliers
Heng Hao (SISSA)
Martin Elvis (CFA)
and COSMOS Team
10%
90%
INAF-OABO
Seminar
2012-10-25
Outline
 Introduction: Definition and Important Questions
 XMM-COSMOS SEDs
 Mixing Diagram: HR Diagram in AGN Evolution?
• Evolution Track
• Inferred Host Galaxy Fraction
• Inferred Reddening E(B-V)
• Outliers: Hot-Dust-Poor Quasars & Others
 Summary
49 yrs ago, in 1963
First Quasar: 3C 273 by Maarten Schmidt
3C 273: z = 0.1583
Furthest quasar now:
z=7
Unified Model
Two types of AGNs
According to Optical Emission Lines:
1.Type 1 AGNs: broad emission lines
generally unobscured by gas and dust
2.Type 2 AGNs: narrow emission lines only
generally heavily abscured
According to power of nuclei:
1. Quasars
2. Seyferts
SED Ref for other type of AGNs:
1) LLAGN: Ho 1999
2) Red quasar: Young+2008
3) …
1995
Wavelength Ordered Strips
IRAC
u IB427
B IB565
g IB505 V IB574 r IB709 NB711 i NB816 IB827 z
K
1
2
3
4 24um
Wavelength Ordered Strips from Peter Capak
Wavelength Ordered Strips
IRAC
u IB427
B IB565
g IB505 V IB574 r IB709 NB711 i NB816 IB827 z
K
1
2
3
4 24um
Wavelength Ordered Strips from Peter Capak
Wavelength Ordered Strips
IRAC
u IB427
B IB565
NB816
g IB505 V IB574 r IB709 NB711 i NB816 IB827 z
IB827
z
K
IRAC1
IRAC2
K
IRAC3
1
2
3
4 24um
IRAC4
Wavelength Ordered Strips from Peter Capak
SED Example
MIPS
IRAC
(Elvis, Hao + 2012)
K H J Subaru SDSS CFHT GALEX
Elvis 94
Galaxy
XMM
Quasar Spectral Energy Distribution
1 dex
Radio
FIR
Constant power per decade
NIR Opt-UV
Elvis et al., 1994, ApJS, 95, 1
EUV
X-ray
Quasar Spectral Energy Distribution
Mechanism
jet
synchrotron
Radio
hot dust from
‘torus’
FIR
NIR Opt-UV
EUV
Big Blue Bump
(0.1~1μm)
Radio-loud
mm break
(~100μm)
1μm
inflection
Radio-quiet
coronaComptonized
accretion
disk
Lν = ν-3 (dust)
Elvis et al., 1994, ApJS, 95, 1
X-ray
Compton
Hump
(~10-30keV)
Soft Excess
(~0.1 keV)
Quasar Spectral Energy Distribution
Mechanism
jet
synchrotron
Radio
hot dust from
‘torus’
FIR
NIR Opt-UV
Radio-loud
EUV
Big Blue Bump
(0.1~1μm)
mm break
(~100μm)
1μm
inflection
Radio-quiet
coronaComptonized
accretion
disk
Lν = ν-3 (dust)
Elvis et al., 1994, ApJS, 95, 1
X-ray
Compton
Hump
(~10-30keV)
Soft Excess
(~0.1 keV)
Radio Loudness
Radio Loudness Definitions:
 Radio Loudness Distr.:
RL =log(f5GHz/fB)>1
bimodal (e.g. Kellermann +1989, Miller+1990)
q24= log(f24μm/f1.4GHz)<0
continuous (e.g. Cirasuolo +2003)
R*uv= log(f5GHz/f2500Å)>1
 Typical RL Fraction ~10%
Ri=log(f1.4GHz/fi)>1
(e.g. Kellermann +1989; Urry & Padovani 1995)
logP5GHz(W/Hz/Sr)>23.7
RX=log(νLν(5GHz)/LX)>-3
where LX is the luminosity in
2-10 keV
*Affected by reddening
 RL Fraction evolve with z or i
magnitude (Balokovic + 2012)
 RL

(L/LEdd)-1 for
L/LEdd>0.001 (Sikora + 2007)
Small Radio Loud Fraction
(Hao + 2012 in prep)
RQ
RL
 COSMOS RL fraction ~4%, 9%
 COSMOS sources are at the high
(Ri)
accretion tail of the Sikora + 2007 plot
• 5/413 RL in common for all definitions
• 8/413 RL in common for two definitions
show no similar trend.
Quasar Spectral Energy Distribution
Mechanism
jet
synchrotron
hot dust from
‘torus’
Radio
FIR
Radio-loud
coronaComptonized
accretion
disk
NIR Opt-UV
EUV
X-ray
Compton
Lack Observation Data;
ALMA✔
Hump
Big Blue Bump
(~10-30keV)
mm breakGrey Body:
(0.1~1μm)
(~100μm) F ∝ν3+β/(ehν/kT − 1),
ν
Soft Excess
where1μm
β~1-2
inflection
(~0.1 keV)
(Silva + 1998, Dunne & Eales 2001)
Radio-quiet
Lν = ν3 (dust)
Elvis et al., 1994, ApJS, 95, 1
Quasar Spectral Energy Distribution
Mechanism
jet
synchrotron
hot dust from
‘torus’
Radio
FIR
Radio-loud
Radio-quiet
coronaComptonized
accretion
disk
NIR Opt-UV
EUV
X-ray
Compton
Observation: Spitzer, Herschel,
WISE
Hump
Big Blue Bump
(~10-30keV)
mm breakTorus model:
(0.1~1μm)
(~100μm) Smooth (eg. Fritz + 2006)
1μm (eg. Nenkova
Soft+ Excess
Clumpy
2008)
inflection
(~0.1 keV)
2-phase (eg. Stalevski + 2012)
Lν = ν3 (dust)
Elvis et al., 1994, ApJS, 95, 1
Dust Property
• Dust extinct λ~2πa most
• AGN extinction curve SMC like
(Czerny + 2004; Gaskell + 2004;
Crenshaw+2001, 2002—Seyferts;
Hopkins +2004 —SDSS+2MASS; )
• Maximum dust temperature:
1400K - 1900K
(eg. Laor & Drain 1993)
• Inner radius of dust sublimation:
0.01 - 0.1pc (10~100 light days)
(Suganuma+ 2006)
Reddening of E94: E(B-V)=0~1
Quasar Spectral Energy Distribution
Mechanism
jet
synchrotron
hot dust from
‘torus’
Radio
FIR
NIR Opt-UV
BBB comes
from Accretion Disk
Radio-loud
(Shields 1978)
Simple α disk fits
Radio-quiet
EUV
Big Blue Bump
(0.1~1μm)
mm break
well (~100μm)
Fν∝ν⅓
(Frank+2002)
coronaComptonized
accretion
disk
1μm
inflection
Lν = ν3 (dust)
Elvis et al., 1994, ApJS, 95, 1
X-ray
Compton
Hump
(~10-30keV)
Soft Excess
(~0.1 keV)
Quasar Spectral Energy Distribution
Mechanism
jet
synchrotron
hot dust from
‘torus’
Radio
FIR
coronaComptonized
accretion
disk
NIR Opt-UV
EUV
Milky WayRadio-loud
Opaque
Big Blue Bump
Define αox= -log[L2keV/L
mm2500Å
break]/2.605
(0.1~1μm)
(~100μm)
1μm
inflection
Radio-quiet
Lν = ν3 (dust)
Elvis et al., 1994, ApJS, 95, 1
X-ray
Compton
Hump
(~10-30keV)
Soft Excess
(~0.1 keV)
Quasar Spectral Energy Distribution
Mechanism
jet
synchrotron
hot dust from
‘torus’
Radio
FIR
NIR Opt-UV
Radio-loud
EUV
Big Blue Bump
(0.1~1μm)
mm break
(~100μm)
1μm
inflection
Radio-quiet
coronaComptonized
accretion
disk
Lν = ν3 (dust)
Elvis et al., 1994, ApJS, 95, 1
X-ray
Compton
Hump
(~10-30keV)
Soft Excess
(~0.1 keV)
Quasar Continuum is Hard to Study
Veritas
• Needs many telescopes
• Several Quasar Properties Affect:
(Variability, BEL, …)
• Reddening
• Host Galaxy Contamination
Fermi
Chandra
Hubble
Spitzer
SMA
VLA
Why SED is important?
Int.
1) SED-----> Total Quasar Power (Lbol) k Correction Transfer Lν to Lbol
 Accretion Rate Accretion History of the Universe
2) SED ----- AGN Structure --- Origin of Continuum
3) SMBH and Galaxy Co-evolution / Black Hole Growth
4) …
AGN Selection
Elvis 94
RQ RL
16 SWIRE Galaxy
1) Selected in certain band(s):
Template (Polletta+2007)
a) Radio Luminosity (RL is rare, biased towards RL)
normalized
b) Near Infrared (Lacy / Stern Wedge, obs frame, missing)
at UKIDSS L*
c) Optical color (e.g. U-B, biased toward blue
quasar)
(Cirasuolo
+ 2007)
d) X-ray Luminosity (most complete)
2) Emission Lines (e.g. BPT Diagram)
Note: SED Fitting usually use
Bruzual & Charlot (2003)
Gal SEDs (no dust feature)
Outline
 Introduction: Definition and Important Questions
 XMM-COSMOS SEDs
 Mixing Diagram: HR Diagram in AGN Evolution?
• Evolution Track
• Inferred Host Galaxy Fraction
• Inferred Reddening E(B-V)
• Outliers: Hot-Dust-Poor Quasars & Others
 Summary
Pre-COSMOS SED - Elvis 94
 Most studies use only mean SED
& bolometric corrections
 Yet SED spread is significant:
~1dex in UV, FIR
 No theory
 No correlations
 Small sample: 29 radio-quiet, 18
radio-loud
 Low z: 0.05 - 0.9
 Low S/N: in X-ray, UV, FIR
 Biased: Blue Quasar
 (Elvis et al. 1994)
1 dex
1 dex
Pre-COSMOS SED - Richards 06
 SDSS-selected (optical selected)
 Photometry coverage:
5 bands in optical,
limited VLA data (30/259)
limited ROSAT data (28/259)
limited GALEX data
(FUV 55/259; NUV 88/259)
 87 quasars fainter than the SDSS
spectroscopic magnitude limit
 “Gap Repair” – heavily depend
on the Elvis 1994 SED
 (Richards et al. 2006)
Expect SED differences: 1. The Galaxy/SMBH Merger Cycle
QUASAR
phase
High L/Ledd
2 accretion modes  2 SEDs
Star formation rate
Seyfert phase
Low L/Ledd
SMBH luminosity
Time from Merger (Gyr)
Hopkins et al. 2008 ApJS, 175, 356
26
Expect SED differences: 2. αox Depend on Luminosity
• αox is anticorrelated with LUV
at ~4σ.
(αox= -log[L2keV/L2500Å]/2.605)
• No significant correlation
between αox and redshift
Vignali, Brandt, & Schneider (2003)
(see also, Steffen+2006, Just+ 2007,
Young+2010, Lusso+2010)
Expect SED differences: 3. M-σ Evolution
__ Local spheroid
 direction of evolution in 300Myr
Merloni +(2010)
Δlog(MBH/M*)=
(0.68±0.12)log(1+z)
Similar Results, e.g.
Peng+2006
Schields+2006
Ho+2007
1<z<2.2
COSMOS
80%
Quasar
Elvis 94
Expect SED differences: 4. Number Density Evolution
Silverman et al. 2005
Quasar Spectral Energy Distribution
Mechanism
jet
synchrotron
Radio
Radio-loud
Radio-quiet
hot dust from
‘torus’
FIR
coronaComptonized
accretion
disk
NIR Opt-UV
EUV
X-ray
Compton
Hump
(~10-30keV)
Is Elvis94 SED
correct?
Big Blue Bump
mm -break
(0.1~1μm)
at ALL 6 decades
of L?
(~100μm)
- at ALL z? 13 Gyr
1μm
Soft Excess
- at ALL L/L
inflection
(~0.1 keV)
Edd?
Lν = ν-3 (dust)
Elvis et al., 1994, ApJS, 95, 1
Outline
 Introduction: Definition and Important Questions
 XMM-COSMOS SEDs
 Mixing Diagram: HR Diagram in AGN Evolution?
• Evolution Track
• Inferred Host Galaxy Fraction
• Inferred Reddening E(B-V)
• Outliers: Hot-Dust-Poor Quasars & Others
 Summary
References
 Hao + 2012a, MNRAS submitted, arXiv:1210.3033
 Hao + 2012b, MNRAS submitted, arXiv:1210.3044
 Elvis, Hao + 2012, ApJ, 759, 6
 Hao + 2011, ApJ, 733, 108
 Hao + 2010, ApJL, 724, 59
COSMOS Type 1 AGN Sample
Elvis 94
MIPS
Richards 06 XMM-COSMOS
Elvis 94
Sample K HSDSS
Sample
COSMOS
Sample
J Subaru
GALEX
IRAC
SDSS CFHT
Sample Size
47
259
413
Selection Method
Blue (Biased)
Optical (SDSS)
X-ray (XMM)
FWHM>2000km s-1
Redshift Range
0.05-0.9
0.1-5.2
Elvis
94
0.1-4.3
Photometry
14
(Low S/N)
10
35
Galaxy
Reference
Elvis et al. 1994
Richards et al. 2006
Brusa et al. 2010
Elvis, Hao et al. 2012
XMM
Mean SED
(Elvis, Hao + 2012)
Elvis 94
Before Any
• Galactic Extinction Correction
XMM-COSMOS
Correction
• Variability Restriction
Mean SED
• Broad Emission Line Correction
• Host Galaxy Correction
Mean SED
(Elvis, Hao + 2012)
Elvis 94
Before
AnyCorrections
Correction *
After
First
OPT-UV
XMM-COSMOS
Mean SED
Galaxy normalized
at UKIDSS L*
(Cirasuolo + 2007)
*Galactic Extinction
Luo+2010
Variability Restriction
Em. Line Correction
Host Galaxy Correction
(Elvis, Hao + 2012)
Two Host Galaxy Contamination Estimation Methods:
1. Hubble Imaging (ACS 814W) : only for z<1 (Cisternas+2011)
2. Mbulge vs MBH relationship (Marconi & Hunt 2003): needs MBH (206/413)
logLJ,gal = 0.877 log Lbol − 0.877 log λE -1.23log(1+z)+ 3.545
XMM
Mean SED With Host Correction (Elvis, Hao + 2012)
Elvis+1994
Richards+2006
Hopkins+2007
Shang+2011
Elvis, Hao+2012
XMM-COSMOS
Mean SED
(203/413)
z, Lbol, logMBH and logλE Parameter Space
z, Lbol, log(MBH/M), logλE=log(Lbol/LEdd)
Host Corrected 203 Quasars
Radio Loud
Similarity of Mean SED in logLbol bins
(Hao + 2012a)
logLbol
(46.1, 47.3]
Elvis 94
(45.7 46.1]
(45.4 45.7]
Mean SED
(44.3 45.4]
Elliptical
Mean SED in z, logLbol, logMBH, logλE bins (norm)
z
logLbol
1.5
logMBH
1.5
2
1.5
logλE
(Hao + 2012a)
SED Dispersion in z, Lbol, MBH, λE bins (norm)
z
logLbol
E94
Dispersion
logMBH
logλE
(Hao + 2012a)
The Luminosity Dependence at Fixed z
(Hao + 2012a)
The SED shape has no obvious
dependence on bolometric
luminosity at similar redshifts.
The Redshift Dependence at Fixed Lbol
(Hao + 2012a)
The SED shape has no obvious
dependence on redshift at
similar bolometric luminosity.
SED Partial Dependence
(Hao + 2012a)
Quasar Growth Physics invariant with z, Lbol, MBH, L/LEdd
z~2  merger
dominated epoch
z~0.3  secular
has the same SED as growth mode
Intrinsic Quasar SED Exists
Gross quasar structure within the torus does not change;
But the M-σ is evolving, feeding must be changing.
Outline
 Introduction: Definition and Important Questions
 XMM-COSMOS SEDs
 Mixing Diagram: HR Diagram in AGN Evolution?
• Evolution Track
• Inferred Host Galaxy Fraction
• Inferred Reddening E(B-V)
• Outliers: Hot-Dust-Poor Quasars & Others
 Summary
Quasar and Galaxy SEDs
Elvis 94
RQ RL
16 SWIRE Galaxy
(Polletta+2007)
norm. at UKIDSS L*
in K band
(Cirasuolo + 2007)
Ell2
Ell5
Ell13
S0
Sa
Sb
Sc
Sd
Sdm
Spi4
NGC6090
M82
Arp220
IRAS 20551-4250
IRAS 22491-1808
NGC6240
Disentangling Quasar and Host
(Hao + 2012b)
αNIR αOPT
Hot Dust
1-3μm
Accretion Disk
0.3-1μm
XMM
Quasar-Host-Reddening Mixing Diagram (Hao +
Host
Dominated
Host Dominated
Reddening Dominated
???
AGN Dominated
E(B-V)
Reddening
Dominated
AGN
Dominated
2012b)
COSMOS AGN on Mixing Diagram
E94 mean SED works in
90% of COSMOS Quasars
(Hao et al. 2012a)
Consistent with mean
E94+Host+Reddening
(Hao + 2012b)
COSMOS AGN on Mixing Diagram
(Hao + 2012b)
Outline
 Introduction: Definition and Important Questions
 XMM-COSMOS SEDs
 Mixing Diagram: HR Diagram in AGN Evolution?
• Evolution Track
• Inferred Host Galaxy Fraction
• Inferred Reddening E(B-V)
• Outliers: Hot-Dust-Poor Quasars & Others
 Summary
Appl. a) Evolutionary Tracks: “cosmic cycle”
HR Diagram in AGN Evolution? (Hao+ 2011b)
Outline
 Introduction: Definition and Important Questions
 XMM-COSMOS SEDs
 Mixing Diagram: HR Diagram in AGN Evolution?
• Evolution Track
• Inferred Host Galaxy Fraction
• Inferred Reddening E(B-V)
• Outliers: Hot-Dust-Poor Quasars & Others
 Summary
Appl. b) Inferred Host Galaxy Fraction
(Hao + 2012b)
(Hao + 2012b)
Galaxy
Fraction
Galaxy
Luminosity
Appl. b) Host Galaxy Fraction Comparision
MD vs MH
MD vs C
C vs MH
Outline
 Introduction: Definition and Important Questions
 XMM-COSMOS SEDs
 Mixing Diagram: HR Diagram in AGN Evolution?
• Evolution Track
• Inferred Host Galaxy Fraction
• Inferred Reddening E(B-V)
• Outliers: Hot-Dust-Poor Quasars & Others
 Summary
Appl. c) Inferred Reddening E(B-V)
Correlation Coefficient = 0.54
(Hao + 2012b)
Correlation Coefficient = -0.62
Appl. c) Inferred Reddening E(B-V)
Correlation Coefficient = 0.40
(Hao + 2012b)
Correlation Coefficient = -0.035
Outline
 Introduction: Definition and Important Questions
 XMM-COSMOS SEDs
 Mixing Diagram: HR Diagram in AGN Evolution?
• Evolution Track
• Inferred Host Galaxy Fraction
• Inferred Reddening E(B-V)
• Outliers: Hot-Dust-Poor Quasars & Others
 Summary
APPL d) Outliers Identification (Hao +
2010, 2011)
Hot Dust Universal in AGN
• Hot dust emission is characteristic
of AGN
– not seen in starbursts
• Infrared slope selects AGNs,
especially obscured ones ,
νfν=να ; α=-0.5 to +2
( Miley+ 1985….Lacy+ 2004, Stern+ 2005,
Lacy+ 2007, Donley+ 2008 )
• Maximum dust temperature:
1400K - 1900K
(eg. Laor & Drain 1993)
• Inner radius of dust sublimation:
0.01 - 0.1pc (10~100 light days)
(Suganuma+ 2006)
No Dust in z~6 Quasars
• 2/21 of 5.8<z<6.4 SDSS quasars are ‘dust-Free’
Spitzer IRAC, IRS (15.6μm), MIPS 24
• Not enough time to form ‘Torus’ (0.93 Gyr)?
IR 1μm OPT
IR 1μm OPT
Richards et al. 2006
Richards et al. 2006
J0005-0006
z=5.85
J0303-0019
z=6.07
4
1
0.4
4
1
0.4
Jiang et al. 2008, 2010
Hot-Dust Poor Outliers
missing hot dust
E94
(Hao + 2010)
extension of acc. disk
E94
???
E94
# of HDP : 41/404
Physical Properties: 1. Hot Dust Covering Factor
Dust Temperature
= 1500 K
Black Body
Normalization
Radius = 0.83 pc
Area = 1.76 pc2
Covering Factor fc = 20%
Class I HDP fc: 2% ~ 29%
• 75% from type1:type2 ratio at z=0
• 50% from type1:type2 ratio for X-
ray bright (e.g. Gilli+2007)
XID=2105, z=1.509
Physical Properties: 2. Accretion Disk Size
Accretion Disk
Outer Edge
Tc ~ R-3/4
Tc
(3200 K)
XID=96, z=2.117
Rout = 0.47 pc ≈104 × Rschwarzchild
~14×Rgi(gravitational instability radius)= 20%
Class II HDP AGNs:
Rout = (10 ~ 23)·Rgi
= 0.09pc ~ 0.99pc = (0.3 ~ 2) × 104·Rs
Not Rout
or
something stabilizes disk
1.
2.
Tc=7.8×105α-⅕η-3/10M811/20λE3/10R-3/4f6/5 K
assumed α=0.1, η=0.1 (Frank+2002)
Rgi ≈ few×102 Rs (Goodman 2003)
What are Hot-Dust Poor Quasars?
 HDP(Jiang
Quasars
 Torus not yet formed?
+ 2010)
HDP Quasars
plenty of cosmic time at z~2, No
 Not enough accretion rate to drive wind? (Elitzur & Ho 2009) No
 Too low Lbol? (Elitzur & Schlossman 2006) No
Geometry—Tilted Disk:
14%
Misaligned disks could result from isotropic accretion events. (Volonteri+2007)
Warped disks leads to a range of covering factors. (Lawrence & Elvis 2010)
Geometric Origin: “tilted disks”
(Hao + 2012d in prep)
Lawrence & Elvis (2010)
Tilted Disk Model
αOPT>0.3
Dust Covering Factor: fc=A/(4πre2),
where dust evaporation radius:
re=1.3Luv,461/2T1500-2.8 pc (Barvainis 1987)
What are Hot-Dust Poor Quasars?
 Torus not yet formed? (Jiang + 2010)
plenty of cosmic time at z~2, No
 Not enough accretion rate to drive wind? (Elitzur & Ho 2009) 20%
No
6%
 Too low Lbol? (Elitzur & Schlossman 2006) No
Geometry—Tilted Disk:
<
Misaligned disks could result from isotropic accretion events. (Volonteri+2007)
Warped disks leads to a range of covering factors. (Lawrence & Elvis 2010)
Recoiling—Off-nuclear BH:
When a SMBH recoils (or kicked-out), it is possible to bring along the
adjacent broad line region but not the further out dusty torus. (Loeb 2007)
Volonteri & Madau (2008)
Evolutionary Tracks: “cosmic cycle”
HR Diagram in AGN Evolution?
What are Hot-Dust Poor Quasars?
 Torus not yet formed? (Jiang + 2010)
plenty of cosmic time at z~2, No
 Not enough accretion rate to drive wind? (Elitzur & Ho 2009) No
 Too low Lbol? (Elitzur & Schlossman 2006) No
Geometry—Tilted Disk:
Misaligned disks could result from isotropic accretion events. (Volonteri+2007)
Larger
HDP
Warped disks
leadssample
to a range of (e.g.
coveringSDSS+WISE+UKIDSS)
factors. (Lawrence & Elvis 2010)
Optical and X-ray
Recoiling—Off-nuclear
BH:Spectrum of HDPs
When a SMBH recoils (or kicked-out), it is possible to bring along the
adjacent broad line region but not the further out dusty torus. (Loeb 2007)
Evolution—Hot Dust Destroyed:
HDPs are quasars on the transition phase?
All XMM-COSMOS Point Source
• Galaxy
• Type 2 AGN
• Type 1 AGN
XID=2532 z=1.297
XID=5607 z=1.359
Hot Dust Rich
Summary
 E94 like SED template works for majority of quasars
 No evolution in mean SED to z=2: quasar structure within
torus independent of merger/radio accretion mode
 Mixing Diagram
 Evolutionary Tracks
 Inferred Host Fraction
 Inferred Reddening E(B-V)
 Outliers:
Hot-Dust-Poor Quasars: dust covering factor; outer disk radius
Hot-Dust-Rich Quasars
Mixing Diagram
(Hao + 2010, 2011, 2012a, 2012b; Elvis, Hao + 2012)
Quasar
10% quasar are
hot-dust-poor
90% COSMOS quasar
Consistent with mean
E94+Host+Reddening
Other outliers:
eg hot-dust-rich
Backup
XMM-COSMOS Survey
Large Area
2.13 deg2
Large Sample
1856 sources
>90% Identified
Brusa + 2007, 2010
413 Type 1 AGN
X-ray Moon to scale
XMM-Newton
53 Fields
COSMOS Spectroscopic Survey
Magellan Survey: IMACS/Baade
~ 2,000 redshifts
Trump+ 2007, 2009
zCOSMOS: ESO-VLT
~ 30,000 redshifts
Lilly+ 2007, 2009
Keck for Faint Sources
Masters+ in prep.
Ground
Space
Main COSMOS Data Sets
Hubble – 2 deg2 optical images (600 orbits)
XMM – 2 deg2 Xray imaging (1.5 Msec)
Galex – ultraviolet imaging
Spitzer – Mid IR w/ IRAC (620 hrs)
Chandra – 1 deg2 high-res X-ray imaging
Herschel – GTO
Subaru – multiple color imaging
VLA – radio imaging (~300 hrs)
MAMBO – 1.2 mm survey
ESO-VLT – zCOSMOS LP ~ 30,000 gal.
Magellan – optical spectr. ~ 5,000 redshifts
CFHT, NIR – NOAO, UH88, UKIRT …
Scoville
Hasinger
Schiminovich
Sanders
Elvis
Lutz
Taniguchi
Schinnerer
Bertoldi
Lilly
Impey
The Galactic Extinction
(Elvis, Hao + 2012)
<E(B-V)>=0.019
Schlegel,
Finkbeiner, &
Davis, 1998
XMM
Variability Restriction
(Elvis, Hao + 2012)
OPT SED Quadratic Fitting
Restricted
2004-2007
All data:Dates:
2001-2007
Restricted Dates:2004-2007
All data:2001-2007
XMM
Broad Emission Line Correction (Elvis, Hao + 2012)
EW of SDSS DR7
Line σ>10
(avoid the lines at the
edge of the spectrum)
Line # of Quasars
Lyα:
8068
CIV:
36350
CIII]:
35650
MgII:
36730
Hγ:
15722
Hβ:
23063
OIII4960: 11027
OIII5008: 20567
Hα:
12060
Gaussian Fit
Log Normal Fit
EW Measurement
from Spectra×200
Broad Emission Line Correction (Elvis, Hao + 2012)
Broad Emission Line
COSMOS AGN on Mixing Diagram
(Hao + 2012b)
XMM-COSMOS, R06, E94 Mixing Diagram (Hao +
2012a)
σint2=σdis2-Err2
σint, OPT=0.20
σint, NIR=0.36
σint, OPT=0.23
σint, NIR=0.36
σint, OPT=0.25
σint, NIR=0.32
XMM-COSMOS, R06, E94 Mixing Diagram (Hao +
αOPT
αNIR
Same Intrinsic Dispersion
Bayesian method (Kelly + 2007)
2012a)
SDSS-Spitzer Hot-Dust Poor Quasars
E94
(Hao + 2011)
E94
# of HDP: 17/195
Appl. a) Evolutionary Tracks on Mixing Diagram
Preliminary Results: ULIRG
two z=3 disk
0.00 Gyr
0.49 Gyr
0.98 Gyr
In collaboration with Chris Hayward
(Hao + 2012d in prep)
Appl. a) Evolutionary Tracks on Mixing Diagram
Preliminary Results: Quasar Phase?
10×AGN luminosity
100 obs directions:
no direction has quasar phase
Extreme Example
XID=2532 Spectra (z=1.297)
MgII
CII
CIII
CIII] FWHM:~20Å~1400 km/s
Other Mixing Diagram Outliers II.
HST
logLbol~47Lbol~1014L
Hyper-LIRG
ULIRG/Quasar
Spitzer-IRAC1