type 1 agn seds in the cosmos a single form, mixing diagram, and outliers

Type 1 AGN SEDs in the COSMOSA Single Form, Mixing Diagram,

and Outliers Heng Hao (SISSA)

Martin Elvis (CFA)and COSMOS Team

INAF-OABO Seminar

2012-10-25

10%

90%

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 1963First 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 dust2.Type 2 AGNs: narrow emission lines only generally heavily abscured

According to power of nuclei:

1. Quasars2. Seyferts

SED Ref for other type of AGNs:1) LLAGN: Ho 19992) Red quasar: Young+20083) …

1995

Wavelength Ordered Strips

Wavelength Ordered Strips from Peter Capak

u IB427 B IB565 g IB505 V IB574 r IB709 NB711 i NB816 IB827 z K 1IRAC

3 4 24um2



3 4 24um2




3 4 24um2

NB816 IB827 z K IRAC1 IRAC3 IRAC4IRAC2


MIPS IRAC K H J Subaru SDSS CFHT GALEX

XMM

SED Example

Elvis 94

Galaxy

(Elvis, Hao + 2012)

Quasar Spectral Energy Distribution

Elvis et al., 1994, ApJS, 95, 1

FIR Opt-UVRadio EUV X-rayNIRConstant power per decade

1 dex



Big Blue Bump (0.1~1μm)

Soft Excess (~0.1 keV)

1μm inflection

mm break (~100μm)

Compton Hump

(~10-30keV)

Lν = ν-3 (dust)

Radio-loud

Radio-quiet

jet synchrotron

Mechanism hot dust from ‘torus’

accretion disk

corona-Comptonized

FIR Opt-UVRadio EUV X-rayNIR





1μm inflection

mm break (~100μm)

Compton Hump

(~10-30keV)

Lν = ν-3 (dust)

Radio-loud

Radio-quiet

jet synchrotron


accretion disk

corona-Comptonized


Review by Harris & Krawczynski (2006)

Radio Loudness Distr.: bimodal (e.g. Kellermann +1989, Miller+1990)

continuous (e.g. Cirasuolo +2003)

Typical RL Fraction ~10% (e.g. Kellermann +1989; Urry & Padovani 1995)

RL Fraction evolve with z or i magnitude (Balokovic + 2012)

RL (L/LEdd)-1 for

L/LEdd>0.001 (Sikora + 2007)

Radio Loudness Definitions:RL =log(f5GHz/fB)>1

q24= log(f24μm/f1.4GHz)<0

R*uv= log(f5GHz/f2500Å)>1

Ri=log(f1.4GHz/fi)>1

logP5GHz(W/Hz/Sr)>23.7

RX=log(νLν(5GHz)/LX)>-3

where LX is the luminosity in 2-10 keV

*Affected by reddening

Radio Loudness

€

∝

COSMOS RL fraction ~4%, 9% (Ri)•5/413 RL in common for all definitions•8/413 RL in common for two

definitions

(Hao + 2012 in prep)

RQ

RL

Small Radio Loud Fraction

COSMOS sources are at the high accretion tail of the Sikora + 2007 plot show no similar trend.





1μm inflection

mm break (~100μm)

Compton Hump

(~10-30keV)

Lν = ν3 (dust)

Radio-loud

Radio-quiet

jet synchrotron


accretion disk

corona-Comptonized


Lack Observation Data; ALMA✔Grey Body:Fν ν∝ 3+β/(ehν/kT − 1), where β~1-2(Silva + 1998, Dunne & Eales 2001)





1μm inflection

mm break (~100μm)

Compton Hump

(~10-30keV)

Lν = ν3 (dust)

Radio-loud

Radio-quiet

jet synchrotron


accretion disk

corona-Comptonized


Observation: Spitzer, Herschel, WISETorus model: Smooth (eg. Fritz + 2006)

Clumpy (eg. Nenkova + 2008)

2-phase (eg. Stalevski + 2012)

• Maximum dust temperature: 1400K - 1900K (eg. Laor & Drain 1993)• Inner radius of dust sublimation: 0.01 - 0.1pc (10~100 light days) (Suganuma+ 2006)

Dust Property• Dust extinct λ~2πa most• AGN extinction curve SMC like(Czerny + 2004; Gaskell + 2004; Crenshaw+2001, 2002—Seyferts; Hopkins +2004 —SDSS+2MASS; )

Reddening of E94: E(B-V)=0~1





1μm inflection

mm break (~100μm)

Compton Hump

(~10-30keV)

Lν = ν3 (dust)

Radio-loud

Radio-quiet

jet synchrotron


accretion disk

corona-Comptonized


BBB comes from Accretion Disk(Shields 1978)Simple α disk fits well Fν ν∝ ⅓

(Frank+2002)





1μm inflection

mm break (~100μm)

Compton Hump

(~10-30keV)

Lν = ν3 (dust)

Radio-loud

Radio-quiet

jet synchrotron


accretion disk

corona-Comptonized


Milky Way OpaqueDefine αox= -log[L2keV/L2500Å]/2.605





1μm inflection

mm break (~100μm)

Compton Hump

(~10-30keV)

Lν = ν3 (dust)

Radio-loud

Radio-quiet

jet synchrotron


accretion disk

corona-Comptonized


Quasar Continuum is Hard to StudyVeritas

Fermi

Chandra

Hubble

Spitzer

SMA

VLA

• Needs many telescopes• Several Quasar Properties Affect: (Variability, BEL, …)• Reddening• Host Galaxy Contamination

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 Continuum3) SMBH and Galaxy Co-evolution / Black Hole Growth4) …

Note: SED Fitting usually use Bruzual & Charlot (2003)Gal SEDs (no dust feature)

AGN Selection

Elvis 94RQ RL

16 SWIRE Galaxy Template (Polletta+2007)

normalized at UKIDSS L*(Cirasuolo + 2007)

1) Selected in certain band(s):

a) Radio Luminosity (RL is rare, biased towards RL)b) Near Infrared (Lacy / Stern Wedge, obs frame, missing)c) Optical color (e.g. U-B, biased toward blue quasar)d) X-ray Luminosity (most complete)

2) Emission Lines (e.g. BPT Diagram)

Outline

Introduction: Definition and Important Questions XMM-COSMOS SEDs


• Evolution Track




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

26

QUASAR phase

High L/Ledd

2 accretion modes 2 SEDs

Hopkins et al. 2008 ApJS, 175, 356

Star formation rate

SMBH luminosity

Time from Merger (Gyr)

Seyfert phase Low L/Ledd

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

1<z<2.2

Merloni +(2010)

Δlog(MBH/M*)=(0.68±0.12)log(1+z)

Similar Results, e.g.Peng+2006Schields+2006Ho+2007

Silverman et al. 2005

Qua

sar

Expect SED differences: 4. Number Density Evolution

Elv

is 9

4

COSMOS80%


Opt-UV



1μm inflection

mm break (~100μm)

Radio

Compton Hump

(~10-30keV)

Lν = ν-3 (dust)

EUV

Radio-loud

Radio-quiet

X-ray

Is Elvis94 SED correct? - at ALL 6 decades of L? - at ALL z? 13 Gyr - at ALL L/LEdd?

Quasar Spectral Energy Distributionjet

synchrotronMechanism hot dust from

‘torus’accretion

diskcorona-

Comptonized

FIR NIR

Outline


XMM-COSMOS SEDs


• Evolution Track




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

Elvis 94 Sample SDSS Sample COSMOS Sample

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 0.1-4.3

Photometry 14(Low S/N) 10 35

Reference Elvis et al. 1994 Richards et al. 2006 Brusa et al. 2010Elvis, Hao et al. 2012

Elvis 94 Richards 06 XMM-COSMOS

COSMOS Type 1 AGN Sample

MIPS IRAC K H J Subaru SDSS CFHT GALEX

XMM

Elvis 94

Galaxy

Elvis 94

XMM-COSMOSMean SED

(Elvis, Hao + 2012)

Before Any Correction

Mean SED

• Galactic Extinction Correction• Variability Restriction• Broad Emission Line Correction• Host Galaxy Correction

Before Any Correction

Galaxy normalized at UKIDSS L*(Cirasuolo + 2007)

After First Corrections *

OPT-UV

*Galactic Extinction Variability Restriction Em. Line Correction

Elvis 94

XMM-COSMOSMean SED

(Elvis, Hao + 2012)Mean SED

Luo+2010

XMM

(Elvis, Hao + 2012)Host Galaxy Correction

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-COSMOSMean SED(203/413)

(Elvis, Hao + 2012)Mean SED With Host Correction

Elvis+1994Richards+2006Hopkins+2007Shang+2011Elvis, Hao+2012

z, Lbol, logMBH and logλE Parameter Space

z, Lbol, log(MBH/M), logλE=log(Lbol/LEdd)

Host Corrected 203 Quasars

Radio Loud

(46.1, 47.3]

(45.7 46.1]

(45.4 45.7]

(44.3 45.4]

Mean SED

Elvis 94

Elliptical

(Hao + 2012a)

Similarity of Mean SED in logLbol bins

logLbol

Mean SED in z, logLbol, logMBH, logλE bins (norm)z logLbol

logλE

1.5 2

logMBH1.51.5

(Hao + 2012a)

SED Dispersion in z, Lbol, MBH, λE bins (norm)z logLbol

logλElogMBH

E94 Dispersion

(Hao + 2012a)

The Luminosity Dependence at Fixed z

The SED shape has no obvious dependence on bolometric luminosity at similar redshifts.

(Hao + 2012a)

The Redshift Dependence at Fixed Lbol

The SED shape has no obvious dependence on redshift at similar bolometric luminosity.

(Hao + 2012a)

SED Partial Dependence (Hao + 2012a)

Quasar Growth Physics invariant with z, Lbol, MBH, L/LEdd

Gross quasar structure within the torus does not change; But the M-σ is evolving, feeding must be changing.

z~2 merger dominated epoch

z~0.3 secular growth modehas the same SED as

Intrinsic Quasar SED Exists

Outline


XMM-COSMOS SEDs

Mixing Diagram: HR Diagram in AGN Evolution?• Evolution Track




Summary

Quasar and Galaxy SEDs

Elvis 94RQ RL

16 SWIRE Galaxy (Polletta+2007)

norm. at UKIDSS L*

in K band(Cirasuolo + 2007)

Ell2Ell5Ell13S0SaSbScSdSdmSpi4NGC6090M82Arp220IRAS 20551-4250IRAS 22491-1808NGC6240

XMM

Hot Dust Accretion Disk

αNIR αOPT

0.3-1μm1-3μm

(Hao + 2012b)

Disentangling Quasar and Host

Host Dominated

AGN DominatedReddening

Dominated

???

E(B-V)

AGN Dominated

(Hao + 2012b)Quasar-Host-Reddening Mixing Diagram

Host Dominated

Reddening Dominated

Consistent with meanE94+Host+Reddening

E94 mean SED works in 90% of COSMOS Quasars(Hao et al. 2012a)

(Hao + 2012b)COSMOS AGN on Mixing Diagram

Outline


XMM-COSMOS SEDs





Summary

Appl. a) Evolutionary Tracks: “cosmic cycle”

HR Diagram in AGN Evolution? (Hao+ 2011b)

Outline


XMM-COSMOS SEDs





Summary

(Hao + 2012b)

Appl. b) Inferred Host Galaxy Fraction

f g

(Hao + 2012b)Appl. b) Host Galaxy Fraction ComparisionG

alax

y Fr

actio

nG

alax

y L

umin

osity

MD vs MH MD vs C C vs MH

Outline


XMM-COSMOS SEDs





Summary

(Hao + 2012b)Appl. c) Inferred Reddening E(B-V)

Correlation Coefficient = 0.54 Correlation Coefficient = -0.62

(Hao + 2012b)Appl. c) Inferred Reddening E(B-V)

Correlation Coefficient = 0.40 Correlation Coefficient = -0.035

Outline


XMM-COSMOS SEDs





Summary

(Hao + 2010, 2011) APPL d) Outliers Identification

α=-0.5 - 2

• Maximum dust temperature: 1400K - 1900K (eg. Laor & Drain 1993)• Inner radius of dust sublimation: 0.01 - 0.1pc (10~100 light days) (Suganuma+ 2006)

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 )

• 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)?

J0303-0019z=6.07

J0005-0006z=5.85

Richards et al. 2006 Richards et al. 2006

4 1 0.4 4 1 0.4

IR IR1μm 1μmOPT OPT

Jiang et al. 2008, 2010

No Dust in z~6 Quasars

# of HDP : 41/404

(Hao + 2010)Hot-Dust Poor Outliers

missing hot dust

E94

extension of acc. disk

E94

???

E94

Physical Properties: 1. Hot Dust Covering Factor

XID=2105, z=1.509

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)

Dust Temperature= 1500 K

Black Body Normalization

Radius = 0.83 pc Area = 1.76 pc2

Covering Factor fc = 20%

1. Tc=7.8×105α-⅕η-3/10M811/20λE

3/10R-3/4f6/5 K assumed α=0.1, η=0.1 (Frank+2002)2.Rgi ≈ few×102 Rs (Goodman 2003)

XID=96, z=2.117

Physical Properties: 2. Accretion Disk Size

Tc

(3200 K)

Accretion Disk Outer Edge

Tc ~ R-3/4

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

Torus not yet formed? (Jiang + 2010)

Not enough accretion rate to drive wind? (Elitzur & Ho 2009)

Too low Lbol? (Elitzur & Schlossman 2006)

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)

No

No

plenty of cosmic time at z~2, No

What are Hot-Dust Poor Quasars?

14%

HDP QuasarsHDP Quasars

Geometric Origin: “tilted disks”

Dust Covering Factor: fc=A/(4πre2),

where dust evaporation radius:re=1.3Luv,46

1/2T1500-2.8 pc (Barvainis 1987)

αOPT>0.3

Lawrence & Elvis (2010)Tilted Disk Model

(Hao + 2012d in prep)






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)

No

No



6%20%

Volonteri & Madau (2008)

<

Evolutionary Tracks: “cosmic cycle”

HR Diagram in AGN Evolution?






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)

Evolution—Hot Dust Destroyed: HDPs are quasars on the transition phase?

No

No



Larger HDP sample (e.g. SDSS+WISE+UKIDSS)Optical and X-ray Spectrum of HDPs

All XMM-COSMOS Point Source

• Galaxy• Type 2 AGN• Type 1 AGN

Hot Dust Rich

XID=2532 z=1.297 XID=5607 z=1.359

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 DiagramEvolutionary Tracks

Inferred Host Fraction

Inferred Reddening E(B-V)

Outliers: Hot-Dust-Poor Quasars: dust covering factor; outer disk radius

Hot-Dust-Rich Quasars

Quasar

90% COSMOS quasarConsistent with meanE94+Host+Reddening

10% quasar are hot-dust-poor

Other outliers:eg hot-dust-rich

Mixing Diagram (Hao + 2010, 2011, 2012a, 2012b; Elvis, Hao + 2012)

Backup

XMM-COSMOS Survey

XMM-Newton53 Fields

Large Area

2.13 deg2

Large Sample1856 sources>90% IdentifiedBrusa + 2007, 2010 413 Type 1 AGN

X-ray Moon to scale

Magellan Survey: IMACS/Baade ~ 2,000 redshiftsTrump+ 2007, 2009

COSMOS Spectroscopic Survey

zCOSMOS: ESO-VLT ~ 30,000 redshifts Lilly+ 2007, 2009

Keck for Faint SourcesMasters+ in prep.

Main COSMOS Data Sets

Hubble – 2 deg2 optical images (600 orbits) Scoville

XMM – 2 deg2 Xray imaging (1.5 Msec) Hasinger

Galex – ultraviolet imaging Schiminovich

Spitzer – Mid IR w/ IRAC (620 hrs) Sanders

Chandra – 1 deg2 high-res X-ray imaging Elvis

Herschel – GTO Lutz

Subaru – multiple color imaging Taniguchi

VLA – radio imaging (~300 hrs) Schinnerer

MAMBO – 1.2 mm survey Bertoldi

ESO-VLT – zCOSMOS LP ~ 30,000 gal. Lilly

Magellan – optical spectr. ~ 5,000 redshifts Impey

CFHT, NIR – NOAO, UH88, UKIRT …

Spa

ceG

roun

d

XMM

(Elvis, Hao + 2012)The Galactic Extinction

<E(B-V)>=0.019Schlegel, Finkbeiner, & Davis, 1998

XMM

Variability Restriction

All data: 2001-2007Restricted Dates: 2004-2007

OPT SED Quadratic Fitting

All data:2001-2007

(Elvis, Hao + 2012)

Restricted Dates:2004-2007

(Elvis, Hao + 2012)Broad Emission Line Correction

EW of SDSS DR7

Line σ>10(avoid the lines at the edge of the spectrum)

Line # of QuasarsLyα: 8068 CIV: 36350CIII]: 35650MgII: 36730Hγ: 15722Hβ: 23063OIII4960: 11027OIII5008: 20567Hα: 12060

Gaussian FitLog Normal FitEW Measurementfrom Spectra×200

(Elvis, Hao + 2012)Broad Emission Line Correction

Broad Emission Line

(Hao + 2012a)XMM-COSMOS, R06, E94 Mixing Diagram

σint2=σdis

2-Err2

σint, OPT=0.20σint, NIR=0.36



(Hao + 2012a)XMM-COSMOS, R06, E94 Mixing Diagram

αOPT

αNIR

Bayesian method (Kelly + 2007)

Same Intrinsic Dispersion

# of HDP: 17/195

(Hao + 2011)SDSS-Spitzer Hot-Dust Poor Quasars

E94 E94

Appl. a) Evolutionary Tracks on Mixing Diagram Preliminary Results: ULIRG

In collaboration with Chris Hayward

0.00 Gyr0.49 Gyr0.98 Gyr

two z=3 disk(Hao + 2012d in prep)

Appl. a) Evolutionary Tracks on Mixing Diagram Preliminary Results: Quasar Phase?

10×AGN luminosity100 obs directions: no direction has quasar phase

Extreme Example

XID=2532 Spectra (z=1.297)

CIII] FWHM:~20Å~1400 km/s

CIII

CII

MgI

I

Other Mixing Diagram Outliers II. ULIRG/Quasar

logLbol~47Lbol~1014LHyper-LIRG

HST Spitzer-IRAC1

type 1 agn seds in the cosmos a single form, mixing diagram, and outliers

Documents

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