Active Galactic Nuclei SEDs as a function of type and luminosity

Active Galactic Nuclei SEDs as a function of type and luminosity Mari Polletta (IASF-INAF Milan) Collaborators: L. Chiappetti (IASF-INAF), L. Maraschi, M. Giorgetti, G. Trinchieri (Brera-INAF), B. Wilkes (SAO), R. Kilgard (Wesleyan University) 1

Key questions Q: What is the range of AGN SEDs? Well sampled multi-λ SEDs of AGNs (e.g. Elvis et al. 1994) Q: What physical components and processes are at the origin of AGN SEDs? Model both the host and the AGN (e.g. Silva et al. 2004) Q: Do AGN SEDs behave as predicted by current models (evolutionary model, receding torus, unification model)? Investigate dependency of main parameters (e.g. Maiolino et al. 2007) Q: Do we have the data, and the techniques to do all of the above? 2

AGN emitting components Torus Obscuration Accretion disk + BLR+NLR Infrared Optical Type 1 Unobscured Type 2 Obscured Host galaxy Elliptical (Hönig et al. 2006) Illustration: CXC/Weiss Spiral Starburst ULIRG X 3

Do AGN properties depend on their evolutionary stage? AGN: Obscured AGN Obscured QSO Unobscured AGN Merger of large galaxies Host: Star-forming galaxy Starburst Elliptical AGN luminosity and absorption evolution (Hopkins et al. 2005) AGN feedback Fuel exhaustion Halt of star-formation Starburst Bulge & SMBH growth (Di Matteo et al. 2005)

X-ray selected AGN sample XMM-Newton Medium Deep Survey (Chiappetti et al. 2005; Polletta et al. 2007) 02h 30m, -5 (SWIRE/XMM-LSS) F(2-10 kev)>10-14 erg cm -2 s -1 227 sources 71 spectroscopic z + 156 photo-z Chandra/SWIRE Survey (Polletta et al. 2006; Trouille et al. 2008) 10h 46m, +59 (SWIRE/Lockman Hole) F(0.3-8 kev)>3x10-15 erg cm -2 s -1 775 sources 309 spectroscopic z Multi-λ data: Ugriz J(H)K Spitzer (3.6-160μm) VLA (20cm) XMDS Chandra/SWIRE 5

Spectral Energy Distribution Classification Galaxy & AGN template Library Spirals & Ellipticals Starbursts & Seyferts Stars Dust Stars Dust Acc. + Disk Disk QSOs Dust (Polletta et al. 2007; Silva et al. 1998; Berta et al. 2003; 2005; Hatziminaoglou et al. 2005) 6

X-ray selected AGN SEDs Star-forming like AGN SEY1.8 & AGN2 AGN1 Elliptical (2%) Sey1.8 (10%) AGN1 (26%) Star-forming galaxy (33%) AGN2 (29%) (Polletta et al. 2007) 7

Optical-IR SEDs vs X-ray properties Median XOI SEDs of X-ray selected AGNs Type 1 QSO template (Elvis et al. 1994) AGN1 Sey1.8 AGN2 Star-forming like AGN ELL Dominant energy source vs λ Class Optical Infrared X-ray AGN1 AGN AGN Unabsorbed Sey1.8 Host galaxy AGN Unabsorbed 543 X-ray selected AGNs from the XMDS & Chandra/SWIRE surveys (Chiappetti et al. 2005; Polletta et al. 2006) AGN2 Host galaxy AGN Absorbed SFG Host galaxy Host galaxy Very absorbed ELL Host galaxy Host galaxy Unabs. & Weak 8

Gas absorption vs Type Overall the SED classification correlates with the absorption in the X-rays (N H ) N H from X-ray spectral fitting or Hardness Ratio AGN1 Sey1.8 AGN2 Star-forming like AGN 9

Median X-ray-Optical-Infrared SEDs vs X-ray Luminosity AGN1 Sey1.8 L(X) vs L(MIR) Bluer? Log(L X )<44.46 44.46<Log(L X )<44.89 Log(L X )>44.89 Log(L X )<43.67 43.67<Log(L X )<44.21 Log(L X )>44.21 AGN2 Redder? Star-forming like AGN Host type Log(L X )<43.70 44.70<Log(L X )<44.48 Log(L X )>44.48 Log(L X )<43.55 43.55<Log(L X )<44.35 Log(L X )>44.35 10

SED Modeling (separating AGN and Host) Input : rest-frame SED [4-13 points] QSO template (Elvis et al. 1994) Model: - Host (26 templates: ell, spirals, starbursts) - type 1 AGN (3 templates) (Polletta et al. 2007, Silva et al. 1998, da Cunha et al. 2008) Model parameters [5]: L(Host), Host type, L(AGN), AGN type, AGN extinction (A V ) 11

AGN SED type vs Luminosity & Redshift AGN1 AGN dominates at all wavelengths and it is unobscured. Host consistent with early-type spiral. L Host galaxy scales with L AGN All Log(L X )<44.46 44.46<Log(L X )<44.89 Log(L X )>44.89 12

AGN SED type vs Luminosity & Redshift SEY18 AGN dominates atλ>2μm, Host dominates at optical & near-ir λ, similar contributions in the UV Host consistent with late-type spiral. L AGN /L Host increases with LX All Log(L X )<43.67 43.67<Log(L X )<44.21 Log(L X )>44.21 13

AGN SED type vs Luminosity & Redshift AGN2 AGN dominates atλ>2μm, Host dominates at λ<2μm if AGN is moderately - luminous. AGN might dominate at all wavelengths if highly luminous. AGN is heavily obscured. Host consistent with late-type spiral. L AGN /L Host increases with LX All Log(L X )<43.70 44.70<Log(L X )<44.48 Log(L X )>44.48 14

AGN SED type vs Luminosity & Redshift Star-forming like AGN AGN dominates atλ>3-5μm. AGN is characterized by a wide range of obscuration. Host consistent with star-forming galaxy. L AGN /L Host increases with LX All Log(L X )<43.55 43.55<Log(L X )<44.35 Log(L X )>44.35 15

Summary: AGN SED type vs Luminosity & Redshift 1) L(AGN)/L(Host) increases with L X in all types, but at different rates AGN1 Sey1.8 AGN2 SFG 16

Summary: AGN SED type vs Luminosity & Redshift 1) L(AGN)/L(Host) increases with L X in all types, but at different rates 2) No or little obscuration in AGN1 and Sey1.8, high obscuration in AGNs, wide range of obscuration in SFGs A V applied to AGN template in SED modeling AGN1 Sey1.8 AGN2 Star-forming like AGN 17

Summary: AGN SED type vs Luminosity & Redshift 1) L(AGN)/L(Host) increases with L X in all types, but at different rates 2) No or little obscuration in AGN1 and Sey1.8, high obscuration in AGNs, wide range of obscuration in SFGs 3) Host galaxy: AGN1 Sey1.8 & AGN2 SFG early spiral late spiral star-forming 4) AGN vs Host AGN1: AGN > host SEY1.8: AGN>Host atλ>2 μm and AGN Host in the UV AGN2: AGN>Host atλ>2 μm at low L(AGN), at all λ at high L(AGN) SFG: AGN>Host atλ>3-5 μm 18

From large sample studies to specific cases (small sub-samples with a bit more data) Mid-infrared spectra warm dust (torus) properties Study case: 21 Spitzer-selected AGN2 at high luminosity Far-infrared data cool/cold dust (starburst, cirrus) component Study case: 10 Spitzer-selected AGN2 at high luminosity detected at 70μm, 160μm or 1.2mm 19

Mid-infrared SEDs and spectra of obscured QSOs Model: Clumpy Torus (Hönig et al. 2006) Elliptical (host) (Silva et al. 1998) Total (host+torus) (Polletta et al. 2008a) 20

Mid-infrared SEDs and spectra of obscured QSOs Model: Clumpy Torus (Hönig et al. 2006) Elliptical (host) (Silva et al. 1998) Total (host+torus) (Polletta et al. 2008a) 21

Modeling failures and solution Torus+Host+ COLD Torus ABSORBER Host Torus Host External obscuration already proposed by Keel 1980; Lawrence & Elvis 1982; see also Rigby et al. 2006; Brand et al. 2007, Urrutia et al. 2007; Sajina et al. 2007. Cold Absorber: Galactic center extinction curve (Chiar & Tielens 2006) SED Fitting 23 Workshop 22

Fitting the far-infrared emission of obscured QSOs AGNs detected at 70 or 160μm evidence for starburst component M 82 Torus Elliptical Total Log(νLν) (erg s -1 ) Log(νLν) (erg s -1 ) Rest-frame Log(λ) (μm) Rest-frame Log(λ) (μm) Rest-frame Log(λ) (μm) Rest-frame Log(λ) (μm) Starburst with L(FIR) 10 12.5-13.2 L SFR 600-3000 M /yr (Polletta et al., 2008a) 23

Far-infrared/mm emission of obscured QSOs High-z obscured QSOs detected at mm wavelengths BUT Need far-ir data to constrain the FIR emission? z=3.867 1.2mm? z=3.427 1.2mm (Polletta et al. 2008b) L(AGN) ~ 10 13 L & L(SB) ~ 10 12.5-13.2 L 24

Summary X-ray-Optical-Infrared SEDs of 536 X-ray selected AGNs from the XMDS and SWIRE/ Chandra surveys SED classification based on fitting the SEDs with templates Median XOI SEDs built for each type and as a function of L X Optical-IR SEDs modeled with 2 components: host galaxy + AGN and 5 parameters (host type and luminosity, AGN type, extinction, and luminosity) SEDs cover a broad range of types (AGN1, SEY18, AGN2, SFG, ELL) mostly due to a combination of L(Host)/L(AGN), and AGN obscuration (not to the host type) Optical-Infrared SED types correlate with the X-ray spectrum (absorption) and dust extinction The SEDs change with the X-ray luminosity because of changes in the AGN/Host ratio (not observed in AGN1) Detailed modeling of AGN dust components is becoming possible. Study cases presented on hot/warm dust and cool/cold dust. Good perspectives to constrain torus models and AGN dust properties with mid-ir spectroscopy (IRS) and far-ir/sub-mm/mm sensitive observations (Herschel, SCUBA2) 25