AGN Unification Viewed in the mid-IR
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Transcript of AGN Unification Viewed in the mid-IR
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AGN Unification AGN Unification Viewed in the mid-IR Viewed in the mid-IR
Lei HaoLei HaoCornell UniversityCornell University
Spectra
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Why Mid-IRWhy Mid-IR
Seyfert2s, Type II
Seyfert1s, Quasars, Type I
Narrow emission lines
Broad emission lines
Silicate dust absorption
Silicate dust emission
Dust in ISM:
•oxygen-rich silicates
•carbon-rich grains
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Why Mid-IRWhy Mid-IR
Seyfert2s, Type II
Seyfert1s, Quasars, Type I
Narrow emission lines
Broad emission lines
Silicate dust absorption
Silicate dust emission
Dust in ISM:
•oxygen-rich silicates
•carbon-rich grains
Low resolution modules (SL,LL)Low resolution modules (SL,LL) 5-405-40m wavelength coveragem wavelength coverage Resolution: 64-128Resolution: 64-128
High resolution modules (SH, High resolution modules (SH, LH)LH) 9-389-38m wavelength coveragem wavelength coverage Resolution: 600Resolution: 600
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Mid-IR spectra examples
QSO
ULIRG
Seyfert
StarburstSilicate
features
Si-O stretchin
g
O-Si-O bending
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AGN mid-IR spectraAGN mid-IR spectra
ULIRGs quasars
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Seyfert1
Seyfert2
AGN mid-IR spectraAGN mid-IR spectra
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Spitzer archival available, complete Spitzer archival available, complete low-res spectra, z<0.5low-res spectra, z<0.5
Optical classification adopted from Optical classification adopted from Veron-Cetty & Veron (2006) Veron-Cetty & Veron (2006)
24 quasars (3 ULIRGs), 45 Seyfert 1s 24 quasars (3 ULIRGs), 45 Seyfert 1s (7 ULIRGs), 47 Seyfert 2s (7 ULIRGs) (7 ULIRGs), 47 Seyfert 2s (7 ULIRGs) and 98 ULIRGs.and 98 ULIRGs.
A sample of local AGNs and A sample of local AGNs and ULIRGsULIRGs
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Mid-IR average spectraMid-IR average spectra
Hao et al. 2007, ApJ, 655, L77
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Mid-IR average spectraMid-IR average spectra
(Brandl et al., 2006)
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• Deep silicate absorption
in ULIRGs
SE SA
)10()10(ln10 mfmfS
cont
obs
Hao et al. 2007, ApJ, 655, L77
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Silicate features in Seyferts are Silicate features in Seyferts are weekweek
Deo et al. 2007, /0709.3076/
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• Many Seyfert 1s show
absorptions: • Clumpy unification• Host galaxy
contamination• The probability of
Seyfert 1s showing SA is larger than the probabilities of Seyfert 2s showing SE.
SE SA
)10()10(ln10 mfmfS
cont
obs
Hao et al. 2007, ApJ, 655, L77
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SE SA
Hao et al. 2007, ApJ, 655, L77
Silicate features Silicate features in Quasars are in Quasars are mainly in mainly in emissionemission
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1414Maiolino et al. 2007, A&A, 468 979
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Silicate features in AGNSilicate features in AGN We finally detected the emission feature We finally detected the emission feature
in QSOs.in QSOs.Caution: does the emission come from the Caution: does the emission come from the
torus or host galaxies?torus or host galaxies?Emission vs. absorption for Type I and Emission vs. absorption for Type I and
Type II are clearer for high-luminosity Type II are clearer for high-luminosity AGN.AGN.
Seyferts have weak silicate features, Seyferts have weak silicate features, many Seyfert 1s have silicate many Seyfert 1s have silicate absorptions.absorptions.
Hao et al. 2005c, ApJ, 625, L75
See also Siebenmorgen et al. 2005, Sturm et al., 2005
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1616PAH (Polycyclic Aromatic Hydrocarbon)emissions (C-H and C-C stretching and bending
modes)
Mid-IR spectra examples
QSO
ULIRG
Seyfert
Starburst
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Weedman, et al. 2005
PAH strength trace the PAH strength trace the Starformation in the hostsStarformation in the hosts
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Unification: Type I and Type II AGN Unification: Type I and Type II AGN should have comparable PAH should have comparable PAH
strength.strength.
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Mid-IR average spectraMid-IR average spectra
(Brandl et al., 2006)
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Mid-IR average spectraMid-IR average spectra PAH emissions are stronger in Seyfert
2s than in Seyfert 1s Similar in Buchanan et al. (2006) and
Deo et al. (2007) Need a control sample
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PAH stronger in Seyfert 2s?PAH stronger in Seyfert 2s?
Over 60 optically selected Seyfert 1s and Seyfert 2s sampled over their [OIII] luminosities.
Seyfert 2sSeyfert 1s
Hao et al., in preparation
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Mid-IR spectra examples
QSO
ULIRG
Seyfert
Starburst
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SinceSince IR is less sensitive to IR is less sensitive to extinction, extinction, ThenThen, Unification: Type I , Unification: Type I and Type II AGN have comparable and Type II AGN have comparable
IR emission line properties?IR emission line properties?
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2424Deo et al. 2007
Mid-IR atomic emission linesMid-IR atomic emission linesDeo et al. (2007): Seyfert 1s have
stronger [OIV]25.89/[NeII]12.81, [NeIII]15.56/[NeII]12.81, and [NeV]14.32/[NeII]12.81 than Seyfert 2s.
Enhanced [NeII] emission in Seyfert 2s?Dudik et al. (2007): Seyfert 2s have
lower [NeV]14.3/[NeV]24.3 ratios than Seyfert 1s: extinction to [NeV] emitting region?
Dudik et al. 2007
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Conclusion Conclusion Mid-IR spectrum is a power tool in Mid-IR spectrum is a power tool in
testing and constraining the unified view testing and constraining the unified view of AGN: silicate features, PAH emissions, of AGN: silicate features, PAH emissions, atomic lines, continuum…atomic lines, continuum…
In general, the observations support type In general, the observations support type II AGN have more obscuration.II AGN have more obscuration.
But the dust structure in AGN is more But the dust structure in AGN is more complicated.complicated.
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Conclusion Conclusion Mid-IR spectrum is a power tool in Mid-IR spectrum is a power tool in
testing and constraining the unified view testing and constraining the unified view of AGN: silicate features, PAH emissions, of AGN: silicate features, PAH emissions, atomic lines, continuum…atomic lines, continuum…
In general, the observations support type In general, the observations support type II AGN have more obscuration.II AGN have more obscuration.
But the dust structure in AGN is more But the dust structure in AGN is more complicated.complicated.
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Conclusion Conclusion Mid-IR spectrum is a power tool in Mid-IR spectrum is a power tool in
testing and constraining the unified view testing and constraining the unified view of AGN: silicate features, PAH emissions, of AGN: silicate features, PAH emissions, atomic lines, continuum…atomic lines, continuum…
In general, the observations support type In general, the observations support type II AGN have more obscuration.II AGN have more obscuration.
But the dust structure in AGN is more But the dust structure in AGN is more complicated.complicated.