probing agn outflows with variability
DESCRIPTION
Probing AGN Outflows with Variability. Smita Mathur Ohio State. Collaborators: Yair Krongold, Fabrizio Nicastro, Anjali Gupta Nancy Brickhouse, Martin Elvis. Outburst in NGC 2617. Seyfert 1.8 Seyfert 1. Swift monitoring. + XMM. Outflows are ubiquitous. - PowerPoint PPT PresentationTRANSCRIPT
Probing AGN Outflows with Probing AGN Outflows with VariabilityVariability
Smita MathurSmita MathurOhio StateOhio State
Collaborators: Yair Krongold, Fabrizio Nicastro, Anjali Gupta Nancy Brickhouse, Martin Elvis
Outburst in NGC 2617Outburst in NGC 2617
Seyfert 1.8 Seyfert 1.8 Seyfert 1 Seyfert 1
Swift monitoringSwift monitoring
+ XMM
Outflows are ubiquitousOutflows are ubiquitous
Seen in 50% of Seyfert galaxies.Seen in 50% of Seyfert galaxies.
NGC 3783 HST and FUSE
Kaspi +
Physical models of outflowPhysical models of outflow
Accretion disk winds: Accretion disk winds: Proga et al. Proga et al.
- - small physical scalesmall physical scale Winds off obscuring torus: Winds off obscuring torus: Krolik & Krolik &
KrissKriss
- on pc to 10s of pc scale - on pc to 10s of pc scale
Outflowing NLROutflowing NLR Host galaxy ISMHost galaxy ISM
Disk windsDisk winds
Elvis 2000
Proga +
AGN outflowsAGN outflows
UbiquitousUbiquitous Location, physical properties not well Location, physical properties not well
known until recentlyknown until recently Accretion disk winds?Accretion disk winds? Dependence on black hole mass/ Dependence on black hole mass/
Eddington luminosity ratioEddington luminosity ratio
What is the distance of the What is the distance of the absorber from the nucleus?absorber from the nucleus?
Proposals span a factor of > Proposals span a factor of > 10106 6
from accretion disk to Kpc from accretion disk to Kpc scalescale
narrow line regionnarrow line regionn R2
How to measure the How to measure the density?density?
Metastable absorption lines.Metastable absorption lines.
- He I- He I**, , C IIC II**, , C IIIC III* *
- low ionization lines : distinct - low ionization lines : distinct parameter parameter
spacespace
- Non-detection NOT constraining- Non-detection NOT constraining
VariabilityVariability
VariabilityVariability
Density Distance
There There cancan be variability due to be variability due to absorber crossing line of sight.absorber crossing line of sight.
ButBut
Absorber Absorber mustmust vary in responses to vary in responses to changes in ionizing continuum.changes in ionizing continuum.
Why is this a hard Why is this a hard measurement?measurement?
X-rays: Integration times too largeX-rays: Integration times too large
(one day = 86.4 ks)(one day = 86.4 ks)
UV: need many observations with UV: need many observations with dense time sampling dense time sampling lots of HST lots of HST orbitsorbits
XMM Observations of NGC XMM Observations of NGC 40514051
RGS RGS High resolution spectrum High resolution spectrum
EPIC EPIC Variability Variability
The Powerful UTAThe Powerful UTA
Time 104 s
0 2 10
Log U
Log U
Log c
ount
rate
Krongold et al. 2007
R (HIP) = 0.5-1.0 lt days. (2300-4600 RS)
R (LIP) = < 3.5 lt days. (< 15800 RS)
BH mass in NGC 4051 is 2 x 106 M⊙
The outflow is clearly The outflow is clearly compactcompact
……consistent with an accretion disk origin.consistent with an accretion disk origin.
Rule out various models:Rule out various models: - wind off torus edge - wind off torus edge (Krolik & Kriss)(Krolik & Kriss)
- continuous range of ionization - continuous range of ionization
parameter parameter (Ogle et al.)(Ogle et al.)
Mass & Energy outflow ratesMass & Energy outflow rates
HIP & LIP mass outflow rates: HIP & LIP mass outflow rates:
~ 1 x 10~ 1 x 10-4 -4 MM⊙ ⊙
yryr-1-1
c.f. accretion rate: ~ 5 x 10c.f. accretion rate: ~ 5 x 10-3 -3 MM⊙⊙ yr yr-1-1
Kinetic power released: ~10Kinetic power released: ~1038 38 erg/s erg/s
c.f. bolometric luminosity: 2.5 x 10c.f. bolometric luminosity: 2.5 x 1043 43
erg/serg/s
Energy injection rate in the surrounding medium is significantly smaller than that required by feedback models
ScannapiecoSilk
Observational evidence for Observational evidence for accretion disk winds is accretion disk winds is
scarcescarce
Short time-scale variability remains an unexplored region of the parameter space.
Sparse sampling naturally leads to Sparse sampling naturally leads to large radial distance.large radial distance.
Often radial distance is Often radial distance is assumedassumed to to be that with escape velocity = be that with escape velocity = outflow velocity. outflow velocity.
Distance derived from metastable Distance derived from metastable states is states is assumedassumed for high ionization for high ionization outflow. outflow.
……..But what about luminous ..But what about luminous quasars?quasars?
Dietrich et al. in prep.
L
Z
MergerMerger
SecularSecular
Seyferts are NOT scaled down Quasars
Future directionsFuture directions
Intra-day time resolved spectroscopyIntra-day time resolved spectroscopy X-ray: XMM advantageX-ray: XMM advantage
-- CCD and gratings-- CCD and gratings UV: HST COSUV: HST COS
-- exquisite sensitivity-- exquisite sensitivity
Discovery of relativistic Discovery of relativistic outflows in soft X-raysoutflows in soft X-rays
Robust detectionRobust detection
V ~ 0.1c
Gupta et al.2013
Magneto-hydrodynamic Magneto-hydrodynamic wind?wind?
Gupta et al.2013b
Stay tuned….Stay tuned….