The Spectral Energy Distributions of Narrow-line Seyfert 1 Galaxies. Karen M. Leighly The University of Oklahoma. Summary. The spectral energy distribution, as either the origin or the consequence , is key for understanding Narrow-line Seyfert 1 galaxies. ASCA Observations of NLS1s.
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Karen M. Leighly
The University of Oklahoma
Emission region size
~black hole mass
Absolute accretion rate
Alphaxx is a measure of the strength of the soft excess
XMM-Newton observation 10/2000
Exposure ~ 40 ks
Boller et al. 2002
XMM-Newton observation 12/2000
Exposure ~30 ks
Vaughan et al. 20021H 0707-495 Ton S180
Andrea Crews, Carnegie Mellon
Chiho Matsumoto, OU
Prominent soft excess. Galaxies
Well modeled by a single blackbody
Subtle soft excess
Modeled as two Comptonized spectra by Vaughan et al.Spectral Properties
High variance Galaxies
Variance roughly independent of energy.
Variance roughly independent of energy.Light Curves
2-10 keV structure function appears Galaxiesharder than other bands on short time scales.
3-10 keV structure function appears similar to other bands on short time scales.Structure Function Analysis
Hard X-rays show additional short time scale variability
Implication: two physically distinct components
Hard X-rays and soft X-rays show nearly identical variability.
Implication: components are not distinct. Perhaps a distribution of optical depths and temperatures.Energy-sliced Light Curves
Qualitatively similar to behavior during XMM-Newton observation.
Also true in I Zw 1, in which a hard flare was observed? (See poster by Luigi Gallo)Chandra Observation of 1H 0707-495
John Moore, OU
Strong low-ionization lines Galaxies
High SiIII]/CIII] ratio
Strongly blueshifted, low equivalent width CIV line.
Strong high-ionization lines
Moderate SiIII]/CIII] ratio
Weakly blueshifted, high equivalent width CIV.UV Spectra
X-rays relatively strong compared with UV
X-rays relatively weak compared with UV
Casebeer & Leighly, in prep.
Darrin Casebeer, OU
Leighly, Halpern & Jenkins in prep.
Nominal NLS1 photon index (2.25) plus black body - rules out absorption
Ratio of the two spectra reveal evidence for spectral variabilityIntrinsically X-ray Weak
No clear evidence for intrinsic absorption on CIV - small feature has equivalent width of 0.2 angstroms.
PHL 1811 is very unusual compared with other soft X-ray weak AGNsNo Evidence for Absorption
CIV line is blueshifted, as expected. feature has equivalent width of 0.2 angstroms.
NV line may be blueshifted also.PHL 1811
Modeling done by Yair Krongold and Fabrizio Nicastro (CfA). feature has equivalent width of 0.2 angstroms.
First component: U=1.14 logNH=21.92 Vout=24,000 km/s
Second component: U=1.47 logNH=22.4 Vout=45,000 km/s
Also Pounds et al.X-ray Outflows in 1H 0707-495