amd absorption measure distribution evidence for thermal instability? by tomer holczer cambridge, ma...
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![Page 1: AMD Absorption Measure Distribution Evidence for Thermal Instability? By Tomer Holczer Cambridge, MA July 2007](https://reader030.vdocument.in/reader030/viewer/2022032522/56649d615503460f94a43b92/html5/thumbnails/1.jpg)
AMDAbsorption Measure DistributionEvidence for Thermal Instability?
By
Tomer Holczer
Cambridge, MA July 2007
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Outline
• Interesting Questions about AGN outflows
• Absorption Measure Distribution analysis – The method
• Results
• Thermal Instability?
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Some Interesting Questions
• Where is the wind?
How close is it to the engine?
• Are there several absorbing components or
a continuous distribution?
• Is the absorber in pressure equilibrium?
• Do thermal instabilities play a role?
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Fig 1 : NGC 3783 flux –
absorption lines from all charge states
From neutral to H-like (5 orders in )
The Data
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Outflow Model : Method• Determine continuum
• Identify absorption lines; determine outflow and broadening velocity
• Obtain column densities from data of each individual ion
by fitting all its lines
• Reconstruct the Absorption Measure Distribution (as a function of )
Fig 2 : IRAS 13349+2438 line profile of Fe+16 resonance
at 15 Å (in black) and model in red. Fitting the
broadening (width) and outflow (shift) velocity.
)(2Rn
L
H
=
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Absorption Measure Distribution , A New Method(analogous to emission measure distribution)
• Improvement on multi-component models
• AMD – Absorption Measure Distribution –
is the gas column-density (NH) distribution in
ionization parameter ξ : AMD
€
N ion = Az f ion (ξ )∂NH (ξ )
∂ξ
⎛ ⎝ ⎜
⎞ ⎠ ⎟∫ dξ
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Measuring Nion from HETG data
Fig 3 : NGC 3783 (left panel), IRAS 13349+2438 (middle panel), and MCG -6-30-15 (right
panel). spectra in black, model in red.
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Iron ion fractional abundances
0
0.1
0.2
0.3
0.4
0.5
0.6
-1.0 -0.5 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0
Ionization Parameter log (\xi) [erg cm s -1]
Fractional Abundance
Fe+16
Fe+24
Fe+5 NGC 3783
Fig 4: Iron ion’s relative abundances for NGC 3783 using XSTAR (Kallman & Krolik 1995)
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Fig 5 : AMD of IRAS 13349+2438.
The lower panel is the integrated
column density.
For IRAS 13349+2438 NH ~ 1022 cm-2 .
d
NfAN Hionzion ∫ ⎟⎟
⎠
⎞⎜⎜⎝
⎛∂
∂=
)()(
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Abundance Ratios Compared to Sun
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Fig 6 : AMD of NGC 7469.
(Blustin et al. 2007).
NH ~ 3 1021 cm-2.
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Fig 7 : AMD of NGC 3783.
The cyan bins in NGC 3783
are the Krongold et al.
model (with a bin width) and
the green bins Netzer et al.
model .
NH ~ 4 1022 cm-2.
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Photo-ionized Plasma Models for NGC 3783
red squares represent the observed gap
ION (Netzer et al. 2003)
XSTAR (Used by Holczer et al. 2007)
CLOUDY (Krongold et al. 2003)
TITAN (Goncalves et
al. 2006)
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Cooling Curves
Cooling rates at different values of ξ/T (Krolik et al. 1981))
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Conclusions• All outflows in the AGN’s we’ve checked are missing gas
at logT ~ 4.5 - 5 K
• We believe this is evidence for thermal instability in this
region
• Observed unstable region is not produced exactly by
codes
• Moreover, there are discrepancies between the different
models
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THE END
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Fig 6 : Preliminary AMD of
MCG -6-30-15. MCG -6-30-
15 have total column
density around 7 1021 cm-2.
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2±0.5
1.2±0.3
1.7±0.7
0.7±0.2
3.7±2
MCG -6-15-30 (Az/AFe)/
(Az/AFe)O
0.7 ±0.78.71 ±1.41Carbon
4.3±2.68.38 ±5.620.6±0.52.14±0.38Nitrogen
1.9±0.42.3±0.811±91.15±0.17Silicon
1.0 ±0.3 6±5.50.49±0.08Sulfur
1.5 ±0.51.4±0.51.0±0.91.20±0.29Magnesium
1.9 ±0.630±201.20±0.29Sodium
1.4±0.51.3 ±0.83.0±1.32.64±0.44Neon
1.0±0.21.3 ±0.51.3±0.52.64±16.22
Oxygen
NGC 3783 (Az/AFe)/
(Az/AFe)O
IRAS 13349+2438 (Az/AFe)/
(Az/AFe)O
NGC 7469 (Az/AFe)/
(Az/AFe)O
Sun Ratios (Az/AFe)O
from Asplund et al. 2005
Element