Refining the Radius – Luminosity Relationship for Active Galactic Nuclei
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Transcript of Refining the Radius – Luminosity Relationship for Active Galactic Nuclei
Refining the Radius–Luminosity Relationship
for Active Galactic Nuclei
Misty BentzThe Ohio State University
October 19, 2006
Collaborators: Brad Peterson, Kelly Denney, Rick Pogge, Marianne Vestergaard
Talk Outline
• Review of Radius—Luminosity Relationship
• Host-galaxy starlight images
• New BLR radii from reverberation-mapping
• Summary and future plans
Radius—Luminosity Relationship
Kaspi, S. et al. 2000 ApJ, 533, 631
Long lags, some not well constrained
Bright, nearby galaxies with faint AGNs and substantial starlight
HST Imaging Program
Cycle 12 SNAP Program
• 14 objects (12 Seyferts, 2 PG quasars)
• ACS HRC camera, F550M filter
• set of 3 exposures (120s, 300s, 600s) for each object
Goal – Measure host galaxy contribution to luminosity
Examples: Aperture Geometry
Examples: Galfit 2-D Image Decompositionsfit
sresiduals
Image Decompositions, cont…fit
sresiduals
PSF Subtractions
Bentz, M. C., et al. 2006, ApJ, 644, 133
Revised Radius—Luminosity Relationship
Excluded Points:
NGC 3516, NGC 7469,IC 4329A: awaiting HST imaging
NGC 4051, NGC 3227: significant nuclear structure & reddening
PG 2130+099: suspicious lag
NGC 4151
NGC 4151τcent = 6.6 +/- 0.9 d σline = 2680 +/- 64 km s-1
MBH = 4.57 +/- 0.52 x 107 M☼
(Bentz, M. C., et al. 2006, ApJ, in press)
NGC 4593 τcent = 3.76 +/- 0.76 days σline = 1547 +/- 53 km s-1
MBH = 9.6 +/- 2.0 x 106 M☼
(Denney, K. D., et al. 2006, ApJ, in press)
New Reverberation Mapping ProgramSpring ’05 Program – Remeasure Hβ Lag Time
6 targets: 2 varied substantially, 1 marginally
See poster by Kelly Denney
HST Imaging Program #2
Cycle 14 GO Program
• 4 Seyferts:NGC3516, NGC4593,
NGC7469, and IC4329A
• Same observational setup as before
• Same techniques employed
New monitoring program Fall ‘06
HST Cycle 15 Program: ACS HRC imaging of last 17 objects
HST imagingJuly ‘06
New monitoring program Spring ‘07
Implications• R-L relationship holds for 5 orders of magnitude• low luminosity objects have masses ~3x previous estimates• significant outliers can be expected to have physical differences that separate them from the typical population
R-L relationship now diagnostic tool