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Refining the Radius-Luminosity Relationship for Active Galactic Nuclei

This presentation by Misty Bentz from The Ohio State University outlines a refined understanding of the radius-luminosity relationship (R-L) for active galactic nuclei (AGNs). It reviews previous studies, discusses host galaxy contributions to luminosity, and presents new reverberation mapping results. Collaborators include Brad Peterson, Kelly Denney, Rick Pogge, and Marianne Vestergaard. Emphasis is placed on new imaging programs and significant findings, highlighting potential implications for understanding black hole masses and the behavior of low luminosity AGNs.

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Refining the Radius-Luminosity Relationship for Active Galactic Nuclei

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  1. Refining the Radius–Luminosity Relationship for Active Galactic Nuclei Misty Bentz The Ohio State University October 19, 2006 Collaborators: Brad Peterson, Kelly Denney, Rick Pogge, Marianne Vestergaard

  2. Talk Outline • • Review of Radius—Luminosity Relationship • • Host-galaxy starlight images • • New BLR radii from reverberation-mapping • •Summary and future plans

  3. Radius—Luminosity Relationship Bright, nearby galaxies with faint AGNs and substantial starlight Long lags, some not well constrained Kaspi, S. et al. 2000 ApJ, 533, 631

  4. 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

  5. Examples: Aperture Geometry

  6. Examples: Galfit 2-D Image Decompositions fits residuals

  7. Image Decompositions, cont… fits residuals

  8. PSF Subtractions

  9. 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 Bentz, M. C., et al. 2006, ApJ, 644, 133

  10. New Reverberation Mapping Program Spring ’05 Program – Remeasure Hβ Lag Time 6 targets: 2 varied substantially, 1 marginally NGC 4151 τcent = 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) See poster by Kelly Denney

  11. HST Imaging Program #2 Cycle 14 GO Program • 4 Seyferts: NGC3516, NGC4593, NGC7469, and IC4329A •Same observational setup as before •Same techniques employed

  12. New monitoring program Fall ‘06 HST imaging July ‘06 New monitoring program Spring ‘07 HST Cycle 15 Program: ACS HRC imaging of last 17 objects

  13. 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

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