A new look at AGN X-ray spectra - the imprint of massive and energetic outflows Ken Pounds...
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![Page 1: A new look at AGN X-ray spectra - the imprint of massive and energetic outflows Ken Pounds University of Leicester Prague August 2006.](https://reader035.fdocuments.us/reader035/viewer/2022081603/5697bfb71a28abf838c9e936/html5/thumbnails/1.jpg)
A new look at AGN X-ray spectra
- the imprint of massive and energetic outflows
Ken Pounds
University of Leicester
Prague August 2006
![Page 2: A new look at AGN X-ray spectra - the imprint of massive and energetic outflows Ken Pounds University of Leicester Prague August 2006.](https://reader035.fdocuments.us/reader035/viewer/2022081603/5697bfb71a28abf838c9e936/html5/thumbnails/2.jpg)
1H 0419
NGC 509
NGC 5548
Mkn 766
L2-10 (1042 ergs/s)
570
175
40
6
most obvious feature is the ‘soft excess’ - a function of luminosity ?
also fluorescent Fe K line, sometimes with ‘red wing’
XMM-EPIC spectra for sample of type 1 AGN
![Page 3: A new look at AGN X-ray spectra - the imprint of massive and energetic outflows Ken Pounds University of Leicester Prague August 2006.](https://reader035.fdocuments.us/reader035/viewer/2022081603/5697bfb71a28abf838c9e936/html5/thumbnails/3.jpg)
but the same spectral features (and changes) are seen for individual AGN example - the luminous Seyfert 1 PG1211+143
XMM pn data from 2001 (black) and 2004 (red) observations
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Appearances can be deceptive - compare the unmodelled data
difference lies between ~0.7 and ~2 keV
due to a change in photoionised absorption?
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Spectral ratio supports change in ionised absorption as cause of spectral difference
Gierlinski and Done (2004) and Chevallier et al (2006) have explored this idea as an explanation of strong soft excesses.
Problems with relativistically smeared absorber and with ‘fine tuning’
2001/2004 data
![Page 6: A new look at AGN X-ray spectra - the imprint of massive and energetic outflows Ken Pounds University of Leicester Prague August 2006.](https://reader035.fdocuments.us/reader035/viewer/2022081603/5697bfb71a28abf838c9e936/html5/thumbnails/6.jpg)
difference spectra showed: dominant spectral change due to steep power law component (Gamma ~ 2.4)
Fluxed spectra of the highly variable Seyfert 1H 0419-577 (*)
Could another component be moderating the spectral change?
Pounds et al, ApJ 2004
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PG1211 exhibits a high velocity outflow which, unless highly collimated, has a mechanical energy comparable to the bolometric luminosity (more strictly ~ v/c if continuum driven) *
Could this power the steep, variable continuum component ?
Pounds et al MN 2003 King and Pounds ApJ 2003
But lower velocity claimed by Kaspi and Behar, ApJ 2006
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analysis of higher resolution XMM MOS data has improved constraints on high energy outflow (*)
K-shell absorption from H- and He-like ions of Ne, Mg, Si, S and Fe
>> v~0.14+/-0.01c
Pounds and Page (astro-ph 0607099)
![Page 9: A new look at AGN X-ray spectra - the imprint of massive and energetic outflows Ken Pounds University of Leicester Prague August 2006.](https://reader035.fdocuments.us/reader035/viewer/2022081603/5697bfb71a28abf838c9e936/html5/thumbnails/9.jpg)
Developing a new spectral model
components include:
power law continuum from disc-corona
absorption by high and moderate ionisation gas
re-emission from ionised gas components
second (power law) continuum powered by outflow
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the result
- an excellent spectral fit to the EPIC data (chi_sq ~ 840/830 dof) - - with no ‘smearing’
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Compare energies and luminosities as further test of model
•Absorption by warm absorber ~ 8.4 x 1043 ergs/s from PL1 and 5.3 x 1042 ergs/s from PL2 >>> 9 x 1043 ergs/s
•Absorption by high Xi absorber ~ 1.4 x 1043 ergs/s from PL1 and 5 x 1042 ergs/s from PL2 >>> 1.9 x 1043 ergs/s
Luminosity of warm emitter ~ 1.7 x 1043 ergs/s >>> CF ~ 0.2
Luminosity of high Xi emitter ~ 1.4 x 1042 ergs/s >>> CF ~ 0.1
•Luminosity (0.35-10) in second power law ~ 6 x 1043 ergs/s
while mechanical energy in fast flow and CF of 0.1 ~ 6 x 1044 ergs/s >>> efficiency ~ 10%
NB warm emission ~ 35 x that of NGC1068 (but only 5-10 x higher Lbol)
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Critical fit to high resolution RGS data - yes, but requires emission lines to be strongly broadened
Steep power law continuum consistent with EPIC model
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the broadened emission line structure in the RGS spectral fit
N, O, Ne, Mg removed from XSTAR model
Fe also removed, to leave continuum only
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Finally - how does the same model fit the 2004 data?
primarily by increase in weakly absorbed power law
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Summary
• blue-shifted absorption lines in the luminous Seyfert 1 galaxy PG1211+143 show highly ionized outflow at v ~ 0.14c
• the mechanical energy in the high velocity outflow is sufficient to power a second X-ray continuum component perhaps via internal shocks in the flow (NB efficiency similar to GRB ?)
• re-emission of the absorbed flux from primary power law visible in the soft X-ray spectrum (strong line broadening)
• the need for a relativistic Fe K line is reduced or removed by the spectral curvature caused by continuum absorption
• similar spectral features in other luminous AGN suggest PG1211 + 143 may be characteristic of a high accretion ratio
NB. outflow of 1 MSun/ yr for ~ 5x107 yr will carry mechanical energy to host galaxy ~ 1060 ergs ( cf binding energy ~ 1059 erg of galactic bulge with M ~ 1011 MSun and velocity dispersion ~ 300 km/ s; >>> major effect on growth of host galaxy
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Warm absorber/emitter
Ionisation parameter >>> n.r2~1043.7/35 ~ 2 x 1042 column density >>> n.d ~ 8 x 1022 assume d ~ 0.1r >>> r ~ 2 x 1018 cm and n ~ 5 x 105 cm-3
Emission measure ~ 1066 cm-3 from observed luminosity spherical shell with above parameters >>> n2 . volume ~ 3 x 1066 cm-3
>>> CF ~ 0.3
High Xi absorber/emitter Ionisation parameter >>> n.r2~1043/750 ~ 1.3 x 1041 column density >>> n.d ~ 6 x 1022 assume d ~ 0.1r >>> r ~ 2 x 1017 cm and n ~ 4 x 106 cm-3
Emission measure ~ 2 x 1065 cm-3 from observed luminosity spherical shell with above parameters >>> n2 . volume ~ 2 x 1064 cm-3 >>> CF ~ 0.1
Scaling the ionised outflow components
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EPIC (and RGS) spectra show evidence for outflowing matter with wide range of ionisation parameter.
Unless tightly collimated the high velocity implies:
(1) a high mass rate with Mdot.out ~ 1.0 MSun/yr, comparable to Mdot.Edd ~ 1.2 MSun/yr for a BH mass of 3 x 107 MSun accreting at an efficiency of 0.1, and
(2) an energetic outflow ~ 2 x 1044 erg/s (~v/c x LEdd) with mechanical energy significantly larger than the luminosity of the X-ray PL
NB. outflow of 1 MSun/ yr for ~ 5x107 yr will carry mechanical energy to host galaxy ~ 1060 ergs ( cf binding energy ~ 1059 erg of galactic bulge with M ~ 1011 MSun and velocity dispersion ~ 300 km/ s; hence will have a major effect on growth of host galaxy
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But is the spectrum compatible with no strong narrow lines in RGS?
- model fit (PO2 + EM1) requires smoothing to get acceptable chi-sq- find similar ratio of line emission to continuum and PL slope is again steep (Gamma ~ 3)
However, best-fit sigma ~ 18 eV at 0.5 keV
Corresponds to v ~ 25000 km s-1 FWHM
additional broadening from line saturation, turbulence or spread in ionisation parameter?
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PG1211+143 is a bright, narrow emission line quasar at z ~ 0.0809
Lbol~ 6 x 1045 ergs/s (H0 = 75) MBH ~ 3 x 107 MSun
suggesting accretion rate ~ Eddington rate
Pre-XMM observations showed a strong `soft excess’ over a PL of photon index ~ 2, with some evidence for a broad Fe K line
XMM made a ~ 60 ks observation of PG1211+143 in June 2001 and second similar observation in June 2004
Consider the case of PG1211+143 - where an energetic outflow is well established
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Lyman-alpha of FeXXVI MgXII SXVI
* * *
Identification of narrow absorption lines in EPIC pn and MOS with resonance lines of H- like ions of Fe, S, and Mg, consistent with high ionisation, high column density outflow of v ~0.08 – 0.1c
see also IC4329A (Markowicz et al astro-ph/0604353)
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in particular the absorption features at ~ 1.5 and 2.7 keV are both resolved into two lines
a closer look at the MOS data for PG1211
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best fit now if 7 keV feature is identified with 1s-2p resonance absorption line of Fe XXV
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Finally - testing the new model with 2004 pn data
abundances fixed at 2001 valuesfit acceptable (chi-sq / dof ~ 1.1)
• reduced absorption modelled mainly by stronger steep power law component
• weaker soft X-ray emission as indicated by difference spectrum
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The initial analysis used 4 of the 5 most significant absorption features to find an outflow velocity of v~0.09c.
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- ignoring absorption near the Si edge and an ‘emission line’
![Page 27: A new look at AGN X-ray spectra - the imprint of massive and energetic outflows Ken Pounds University of Leicester Prague August 2006.](https://reader035.fdocuments.us/reader035/viewer/2022081603/5697bfb71a28abf838c9e936/html5/thumbnails/27.jpg)
Addition of a trace absorber affecting PO2 improved chi-sq from 877/817 to 832/814
NH~1.2x1021 cm-2 log Xi~ 1.95 v_out~ 0.07 – 0.10 c
Removing absorber shows absorption due to Fe-L and UTA
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Initial ratio of 2004 data to 2001 model
New fit with increase in PO2 and weaker soft X-ray line emission
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conventional plot with PL fit at 1-10 keV
-more spectral structure seen below ~ 3 keV
a closer look at the MOS data for PG1211
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1H 0419-577 in
bright, high flux state
and faint, low flux state
But, individual AGN show very similar spectral variations
Perhaps accretion rate is the key?
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Conventional analysis of EPIC spectrum (pn black; MOS red) reported in 2003 paper*
Power law fit at 1-10 keV found a photon index ~ 1.85 and a strong SX
1-10 keV spectrum modelled with a power law plus an extreme relativistic line Fe K emission line (EW ~ 1.4 keV)
Plus narrow absorption features at ~1.5, ~2.7, ~7 and ~8 keV
* (MNRAS, 345, 705, 2003)
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MOS has equally good statistics at medium and low energies – and better energy resolution (1 sigma~34 eV at 1 keV)
Part of MOS spectrum of NGC 1068
(MNRAS, 368, 707, 2006)
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Chi-sq plot shows high significance of the 5 absorption lines and (the same) emission lines (*) as seen in pn data
higher resolution MOS spectra confirms the strong, highly ionised outflow in PG1211 + 143, albeit with velocity increased to v~0.12c
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The fitted model includes power law continua with photon indices ~ 2.1 and ~3
plus high ionisation absorber A1 and warm absorber A2 affecting both power laws
E1,E2 re-emission from absorbing gas
NH~2x1023 A1 log Xi~ 2.9 v_out~ 0.120+/-0.005c
NH~3x1022 A2 logXi~ 1.5 v_out~ 0.05+/-0.02c
logXi~ 1.4 E1 v_out~ 3000+/-1000 km/s
logXi~ 2.9 E1 v_out~ 3000+/-1000 km/s
Chi-sq/d.o.f. ~ 820/820
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the main spectral change appears to be an increase in flux between ~ 0.7 – 2 keV
narrow absorption lines remain, but weaker
Does model describe spectral change in 2004 ?
-- the plot shows pn data from 2001 (black) and 2004 (red)
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2-10
~45%
1-2
~40%
0.3-1
~25%
~32% flare over ~104 sec in full 0.3-10 keV light curve
variation least in soft X-ray band as expected for significant re-processed flux
Footnote: Variability of EPIC light curve also supports model