Download - Buried AGNs in nearby ULIRGs
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Buried AGNs in nearby ULIRGs
Masa Imanishi
(National Astronomical Observatory of Japan)
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Ultraluminous Infrared Galaxies ( ULIRGs )
L(IR)>10^12Lsun Powerful energy source is hidden behind dust
Compact cores (<500pc)are dominant
Very compact starburstor AGN ?
opticalIR(12um)
Soifer et al. 2000
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AGNs in ULIRGs are buried
AGNs obscured by torus-shaped dust
Detectable via optical spectroscopy
NLR
ULIRGs have a large amount of nuclear gas and dust
Buried AGNs are elusive
Sy2
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Infrared 3-4 um spectroscopy
IRCS on Subaru 8.2m telescope
Optically non-Seyfert ULIRGs
1. Spectral shape (PAH vs dust absorption)
2. Geometry of energy sources and dust
Methods:
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PAHPAHs are excited in starburst PDRs but destroyed near an AGN
1. 3-4 um spectral shape
EW(PAH)~100nm
starburst
3.3um PAH
Buried AGN
featureless
3.4um/3.1um
EW(PAH)<<100nm
composite
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3-4 um
starburst
Subaru
Strong PAH
Buried AGN AGN/SB composite
Abs. feature Low EW(PAH)
Ice3.1um
Bare3.4um
Bare3.4um
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2. dust/energy-source geometry
(Imanishi & Maloney 2003 ApJ 588 165)
Buried AGN
Foreground screendust model
strong
exp(-τλ)
starburst
Mixed dust model
Dust absorption feature: weak
Tau(3.1) < 0.3
Tau(3.4) < 0.2
1-exp(-τλ)τλ
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3-4 umStarburst
PAH strong (starburst):Dust absorption weak
Buried AGN composite
PAH weak (AGN):Dust absorption strong
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5-35 umStarburst
Spitzer
PAH strong :Silicate abs. weak
Buried AGN Composite
PAH weak:Silicate abs. strong
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Strong dust temperature gradient
Av(3um) > Av(10um) > Av(20um)
Av(3um)=120 mag
Av(10um)=50 mag
Av(20um)<20 mag
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17/27 (63%) LINER ULIRGs
3/13 (23%) HII-region ULIRGs
(statistically complete)
(complete at RA=10-22hr)
Results
Buried AGN signatures:
Pure buried AGNsshow LINER spectra
Powerful buried AGNs fraction: LINER > HII(see also Nagar et al. 2003)
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NLR
Our line-of-sight obscuration: Non-Sy >> Sy2
Sy2:Absweak
Non-Sy:strong
Amount of nuclear dust: Non-Sy >> Sy2
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Buried AGNs: both warm/cool FIR colors
pure buried AGN
F25/F60=0.16(cool)
larger dust column
cool FIR color
NLRwarm
cool == starburst
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Summary
1. Buried AGNs fraction: LINER > HII-region
2. Nuclear dust amount: non-Sy ULIRGs > Sy2 ULIRGs
Optical Sy (non-)detectability depends on the amount of nuclear dust
It is important to understand optically-elusive buried AGNs in ULIRGs.
( Imanishi et al. 2005, submitted )
warm & cool
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Just for reference After this slide
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Ice : inside dense molecular gas
HCN (= dense gas tracer) is concentrated to nuclei
Strong ice absorption is nuclear core origin(not ISM in an edge-on host galaxy)
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starburst Buried AGN
Centrally-concentratedenergy source
Strong dust temperature gradient
Av(3um) > Av(10um) > Av(20um)
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Weak PAH ULIRGs:Dust temperature gradient
Av(3um) > Av(10um) > Av(20um)
Av(3um)=120 mag
Av(10um)=50 mag
Av(20um)<20 mag
Strong dust temperature gradient