Reverberation Mapping
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Transcript of Reverberation Mapping
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Methods of Measuring Black Hole Masses:
Reverberation Mapping
Misty C. Bentz
Georgia State UniversityMonday, September 12, 2011
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Dynamical methods generally not feasible in AGNs AGNs rare = distant, poor spatial resolution AGNs are bright, outshine the test particles
Use variability instead!Reverberation mapping
relies on time resolution instead of spatial resolution
R size of emission region
V velocity of gas in that region
f order unity scale factor
Black Hole Masses in AGNs
RM Assumptions:1. R (continuum emission region)
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AGN Unified Model
Broad-lineAGNs (Type 1)
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AGN Unified Model
Narrow-lineAGNs (Type 2)
Broad-lineAGNs (Type 1)
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AGN Unified ModelBlazars
Narrow-lineAGNs (Type 2)
Broad-lineAGNs (Type 1)
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AGN Unified ModelBlazars
Narrow-lineAGNs (Type 2)
Broad-lineAGNs (Type 1)
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Inner Solar System
Orbit of Sedna
aphelion = 928AU
= 5.4 light days
AGN Scales or Why Its Hard to Study the BLR in Detail
Radius of Seyfert BLR
~5 light days
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Inner Solar System
Orbit of Sedna
aphelion = 928AU
= 5.4 light days
Embedded in the center of a galaxy
~40Mpc away (z~0.01)
AGN Scales or Why Its Hard to Study the BLR in Detail
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Telescope AGN
Red = continuum
Purple = broad line
Measuring the BLR Radius -- RM Cartoon
BH
Broad Line Region
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Example Data NGC 4151
Cross-correlation"time delay of
broad line response to continuumvariations
Bentz et al. 2006, ApJ, 651, 775
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Time delay (c!) "average BLR radius R
measured for ~50 AGNs
width of variable line emission "line-of-sight BLR gas velocity (V)
fincludes BLR physical details(e.g., inclination, geometry, kinematics)
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Woo et al. 2010
The Fudge Factor f
population average: = 5.2 +/- 1.1
Assume MBH- # relationship
is same for AGNs andquiescent galaxies
#difficult to measure forhigh-L AGNs (z > 0.1)
Morphological biases in #measurements?
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Virial Behavior in the BLR
Peterson & Wandel 2002
V!"-1/2
where measurementsexist for multipleemission lines
Bentz et al. 2010Kollatschny 2003
Mrk110
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Consistency with Dynamical Masses
Stellar and gas dynamical
measurements for 2 AGNswith RM masses
Dynamical and RMmasses aregenerally consistent for
NGC 4151 andNGC 3227
More direct comparisons areneeded, limited by AGN
distances
Davies et al. 2006, Onken et al. 2007,Hicks & Malkan 2008
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Simple RM:
log MBH= 6.82 +/- 0.07
(Bentz et al. 2009)
vs.
Bayesian modeling:
log MBH= 6.51 +/- 0.28
(Brewer et al. 2011)
Brewer et al. 2011
Bayesian Modeling of RM Data
Fits RM datasets withplausible BLR models
i=90defined as
face-on
Models are still simplistic
Need to study more objects
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Echo Mapping - BLR Transfer Function
Bentz et al. 2010
recovered transfer function rulesout outflow
possible evidence for inflow
rotation inflow outflow
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M-L relationship
AGN Lbulgefrom 2-Ddecomposition of optical
HST images
AGN M-L relationship
and
M-L relationship foronly early type
quiescent galaxies
are consistent
Needs to be studied in NIR tominimize dust
AGNs
Bentz et al. 2011, in prep
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Single Epoch MBHEstimates
R Lrelationship yields black
hole mass with onespectrumand twomeasurements: 1. emission line width (V) 2. AGN L!proxy for R
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Single Epoch MBHEstimates
R Lrelationship yields black
hole mass with onespectrumand twomeasurements: 1. emission line width (V) 2. AGN L!proxy for R
V
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Si l E h M E i
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Single Epoch MBHEstimates
R Lrelationship yields black
hole mass with onespectrumand twomeasurements: 1. emission line width (V) 2. AGN L!proxy for R
L
RV
ALLmass estimates for AGNsusing emission lines are based
on the local observed
R L relationship for H$Monday, September 12, 2011
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NGC 4051
z = 0.00234
PG 0953+414
z = 0.234
Large slit (i.e. 4x10) used to minimize aperture effects!strong starlight contamination at low z
5 x 5 images
AGN Luminosities Host Galaxy Starlight
Mrk 79
z =0.0222
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Updates to RM Database
LAMP 2008
Bentz et al. 2009
MDM 2007
Denney et al. 2010
1 new object
3 replacements2 additions
H$Results Summary:
7 new objects
1 addition
H$Results Summary:
HST Cycle 17 WFC3
Imaging CampaignMonday, September 12, 2011
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CIV R L R l ti hi
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Kaspi et al. 2007
CIV R-L Relationship
Only 7 AGNs,and 5 have similar
luminosities
Slope of CIV R-Lis consistent
with slope of H$R-L
Not enough MgIImeasurements forR-L relationship
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S
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Summary
%Reverberation mapping substitutes time resolution for spatialresolution and probes the gravity of the BH
%RM masses consistent with dynamics and with Bayesian modeling
%We are just beginning to acquire data that could soon allow directconstraints on the detailed physics of the BLR gas
%The R-L relationship provides a convenient method for estimating MBHin any broad-lined AGN
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