Talk at Extreme Astrophysics Group, University of Michigan, Michigan, MI, USA, October 31, 2019, https://doi.org/10.6084/m9.figshare.13699300

1. Relativistic Compact Outflows
in Radio-quiet AGN
Image
Credit:
NASA/JPL-Caltech
Image
Credit:
NASA/JPL-Caltech
Ashkbiz Danehkar
Department of Astronomy, University of Michigan
danehkar@umich.edu
In collaborations with: Mike Nowak (MIT), Gerard Kriss (STSI), Julia Lee (Harvard),
In collaborations with: Mike Nowak (MIT), Gerard Kriss (STSI), Julia Lee (Harvard),
Randall Smith (SAO) and et al.
Randall Smith (SAO) and et al.
Extreme Astrophysics Group, University of Michigan, Michigan, USA, October 31st
, 2019

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Outline

Introduction
 Radio-quiet AGN Class
 Ultra-Fast Outflow (UFO)
 X-ray Absorbers

PG 1211+143
 Previous XMM-Newton Observations
 Chandra X-ray and Hubble UV Observations in 2015
 Photoionization Modeling (Parallelization with MPI)
 Confidence MCMC Maps of Measured Parameters

Future Direction for UFO in AGN
 Unified AGN Outflow Model
 A Possible Angular Momentum-UFO Correlation

Summary

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AGN Classification
AGN Unified Model (radio-loud & -quiet AGN, Seyfert I & II Galaxies)
Beckmann & Shrader 2012,
Active Galactic Nuclei
Unified Models for AGNs
Antonucci, ARA&A, 1993, 31, 473
Unified Schemes for AGNs
Megan Urry & Padovani, 1995, PASP, 107, 803
(Bernie Fanaroff &
Julia Riley 1974)
AGN Unified Model
• Radio-Quiet AGN
 Seyfert I (BLR+NLR,
compact outflows)
 Seyfert II (NLR)
• Radio-Loud AGN
 FR I (compact radio jets)
 FR II (extended radio jets)
 Blazar (relativistic beams)
(Carl Seyfert 1942)

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AGN Classification
Dermer & Giebles 2016
radio-loud & -quiet AGN, Seyfert I & II Galaxies
Blandford, Netzer, Woltjer 1990, Active Galactic Nuclei

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X-ray Feature of AGN
Disk
Black-
body
Hot Corona
Warm
Absorbers
K-shell Iron
Beckmann & Shrader 2012
Risaliti & Elvis 2004
(bbody + powerlaw + ∑ emis) x ∏ abs

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X-ray Absorbers

Ultra-fast Outflows (UFOs):
 hard X-ray blue-shifted absorption lines
 H-like & He-like Fe Ions
 Velocity > 10,000 km/s (0.03c)
 high velocity ~ 0.1– 0.4c
(Pounds + 2003, Cappi 2006, Braito + 2007)
 Recently observed in 30% of radio-quite and -loud AGN
(Tombest + 2010,2011,2012,2014)

Warm Absorbers (WAs):
 soft X-ray blue-shifted absorption lines
 H-like & He-like O, Ne, Mg, Si, S Ions
 Velocity < 10,000 km/s (0.03c)
 Observed in 50% of Seyfert I galaxies
(Reynold & Fabian 1995, Reynold 1997, George + 1998)
6
Tombesi + 2013

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PG 1211+143

A Narrow-line Quasi-Stellar Object (QSO)

In a radio-quite (Seyfert I) galaxy (z = 0.0809)

Strong soft excess

Mildly relativistic outflows – 0.06c and 0.13c (XMM-Newton)

redshifted aborbers at 0.2-0.4c: infall to the black hole

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PG 1211+143: XMM-Newton
 UFOs vout
~ -0.07c (Pounds + 2003)
 UFOs vout
~ -0.13c (Pounds+ 2006,2007,2009)
 UFOs vout
~ -0.06c and -0.13c (Pounds + 2016)

H- and He-like O, Ne, Mg, Si, S, Ar and Fe ions

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PG 1211+143: Chandra
X-ray Chandra Observations

High Energy Transmission Grating
(HETG; PI: J.C. Lee, 2015 April)

6 observations over 9 days ~ 433 ks

H- and He-like Ne, Mg, S ions: -0.06c
PG 1211+143 Chandra Observations (PI J.C. Lee)

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PG 1211+143: Hubble
Hubble UV Observations

Cosmic Origins Spectrograph (COS)
PG 1211+143 Chandra Observations (PI J.C. Lee)

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PG 1211+143: Low Varibility

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PG 1211+143: Photoionization Model
• XSTARDB & XSTAR2XSPEC
• Set parameters
 Number density (log n ~12)
 Ionizing SED (Radio+IR+Opt+UV+X-ray)

Physical Conditions (free parameters):
 Column density (NH
)
 Ionization parameter (ξ)

Photo-emission, Ionized absorption
XSTAR (Kallman + 1996, 2004) or CLOUDY (Ferland + 1998)

(bbody + powerlaw + ∑ photemis) x ∏ warmabs

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PG 1211+143: Photoionization Model

MPI_XSTAR Parallelization: github.com/xstarkit/mpi_xstar
(Danehkar + 2018, PASP, 130, 024501)
XSTAR (Kallman + 1996, 2004)
XSTAR XSTAR XSTAR XSTAR XSTAR
XSTAR

produce table model files:
 absorption spectrum imprinted onto continuum (xout_mtable.fits)
 reflected emission spectrum in all directions (xout_ain.fits)
 emission spectrum in transmitted direction of the absorpter (xout_aout.fits)

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PG 1211+143: Photoionization Model
Ionized Absorber at -0.06c
Ionized
Absorber
Danehkar + 2018, ApJ 853:165
Ionization parameter
Gas
density
Luminosity (13.6 eV-13.6 keV)
Radius
Column
density
Shell thickness
Outflow velocity
BH mass

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PG 1211+143: Photoionization Model

Absorpti
on -0.06c

HST Cosmic Origins Spectrograph (COS)

UV Lyα wide absorption line,
possible counterpart to X-ray absorber

The same outflow velocity (-0.06c)
 log NH I
> 14.5 (log NH
~ 21)

log ξ ~ 2.9
Kriss + 2018, ApJ 853:166

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PG 1211+143: MCMC Confidence Maps
Danehkar + 2018, ApJ 853:165

~ -0.06c

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PG 1211+143: Thermal Stability
Thermal Stability Curve and Ion Fraction Plots

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Ultra-fast Outflow in AGN
Detection of relativistic outflows in X-ray
●
Seyfert I PDS 456
Ionized outflow at -0.24c and -0.48 c
Biossay-Malaquin, Danehkar + 2019

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Ultra-fast Outflow in AGN
Detection of UFO in radio-quite AGN
Cappi 2006

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Unified AGN Outflow Model
Absorption Measure Distribution (AMD): similar to Emission Measure Distribution (EMD)
n(r) ~ r -1.4
density profile
Behar 2009

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Unified AGN Outflow Model
Unification of UFOs and WAs
Tombesi + 2013
(Ultra-fast outflows)
(Warm Absorbers)

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Unified AGN Outflow Model
Non-Unification of UFOs and WAs
Tombesi + 2013
(Ultra-fast outflows)
(Warm Absorbers)

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Unified AGN Outflow Model
Black Hole Spin Implication for a Unified AGN Model?
Garofalo + 2010
Beckmann & Shrader 2012,
Active Galactic Nuclei
AGN Unified Model
- Radio-Quiet AGN: Seyfert I, Seyfert II
- Radio-Loud AGN: FR I, FR II (extended radio jets)

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Supermassive Black Hole Spin
Black Hole Spin Measurement (see Brenneman 2013)
●
Thermal Continuum Fitting (UV observation)
– stellar-mass black hole
– AGN (may problematic due to UV absorption lines!)
●
Inner Disk Reflection Modeling
– AGN (X-ray)
●
High Frequency Quasi-Periodic Oscillations
– AGN + stellar-mass black hole (fully not developed)
●
X-ray Polarimetry
– Need sensitive X-ray polarimter (not available now!)
●
Imaging the Event Horizon Shadow
– Need Very Long Baseline Interferometry (in development)
– Suitable only for Sgr A* and M87
a = J c / G M2
(a: BH spin, J: angular momentum, M: BH mass, G: gravitational constant, c: speed of light)

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Supermassive Black Hole Spin
Relativistically broadened Kα iron line (6.4 keV)
Compton hump (> 10keV)
Black Hole Spin Measurement from X-ray
a = - 1
a = 0
a = 1
Image credit: NASA/JPL-Caltech

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Supermassive Black Hole Spin
BH Spin from Reflection Modeling
●
kerrconv (Brenneman & Reynold 2006)
●
relline (Dauser + 2010)
●
xillver (Garcia + 2010,11,13)
●
relxill (Garcia + 2014)
Dauser & Garcia + 2014

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Supermassive Black Hole Mass
BH Mass from Reverberation Mapping Technique (Kaspi + 2000)
●
Variation in light curves of broad emission line region (BLR) in Seyfert I AGN
●
Time delay in variation of BLR luminosity (Hb 4861A) relative to
variation of accretion disk luminosity (continuum 5100A)
www.techfreaq.de
Bentz + 2006

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SMBH Spin Implication
Black Hole Spin Implication for a Unified AGN Model?
Danehkar +

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Theories for UFO in AGN
●
strong magnetic field in accretion flow/disk
of rotating BH
– Blandford-Znajek process (1977) for strong jets from flow
– Blandford-Payne process (1982) for slow winds from disk
●
frame dragging (gravitomagnetism indirectly)
– Penrose process (1971)
– Kerr spacetime of rotating BH
– extracting black-hole rotational energy
●
frame dragging + magnetic field
(e.g. Narayan & Quataert 2005)
●
gravitomagnetism
Frame dragging+magnetic
(Narayan & Quataert 2005)
Blandford-Znajek process
(Thorne 1995)

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Theories for UFO in AGN
For local gravitational filed, these are Einstein field equations:
For non-local gravitational fields, there are dynamical formulas from Bianchi
identities in General Relativity:
Newtonian Tidal force
Non-Newtonian effect
Gravitational waves
shear current
angular momentum
Trumper 1964, Hawking 1966, Ellis 1971

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Summary

X-ray ionized Absorbers
 WAs: typically H-like & He-like O, Ne, Mg, Si & S ions, low velocity < 10,000 km/s
 UFOs: typically H-like & He-like Fe, high velocity > 10,000 km/s, usually ~ 0.05– 0.45c

The Quasar PG1211+143
 XMM-Newton observations: UFOs vout
~ -0.06c and -0.13c
 Chandra observations together with Hubble UV, VLA radio observations in 2015

Photoionization Modeling of PG1211+143
 X-ray ionized absorber: outflow velocity -0.06c
 UV Lyα absorption: outflow velocity -0.06c, possible counterpart to X-ray absorber
 MPI-based parallelization for supercomputers: MPI_XSTAR

Unified AGN Outflow Model
 Ionization parameter-Outflow velocity correlations (Tombesi + 2013)
 A possible correlation between UFO and angular momentum?

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Image
Credit:
NASA/JPL-Caltech
Image
Credit:
NASA/JPL-Caltech
Thank you for your attention
Thank you for your attention