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UV/Optical Detections of Candidate Tidal Disruption Events by GALEX and CFHTLS

UV/Optical Detections of Candidate Tidal Disruption Events by GALEX and CFHTLS. Gezari et al. 2007. TexPoint fonts used in EMF. Read the TexPoint manual before you delete this box.:. SMBH Mass Function. How are SMBH masses derived? OIII kinematics – M- σ *

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UV/Optical Detections of Candidate Tidal Disruption Events by GALEX and CFHTLS

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  1. UV/Optical Detections of Candidate Tidal Disruption Events by GALEX and CFHTLS Gezariet al. 2007 TexPoint fonts used in EMF. Read the TexPoint manual before you delete this box.:

  2. SMBH Mass Function • How are SMBH masses derived? • OIII kinematics – M-σ* • Relations with bulge mass / luminosity – M-L* • Reverberation mapping • Only good for nearby (or bright) stuff • Only good if active • Outstanding questions • How do they coevolve with their hosts? • How does mass scale with redshift?

  3. Tidal Disruption • Magorrian & Tremaine predict 103-105 yrs between events • For too large a mass, RT < RS • Can use tD to constrain MBH • Aquire tDfrom power-law decay in consumption rate (n=5/3)

  4. Previous Candidates • NGC 4552 has a “mini-AGN” • In 1995 experienced UV flare L ~ 1039 ergs/s • ROSAT (1990-91) detected several soft X-ray flares • L ~ 1042 – 1044 ergs/s • No previous AGN activities in hosts • Derived rate of 10-5 yr-1 per galaxy • Agrees with Magorrian & Tremaine rate

  5. Searching for New Candidates • GALEX DIS • Optical counterparts in CFHTLS • 80 deg2 coverage (0.02 sr) • Rule out hard X-ray emitters (AGNs) • Must rule out type II SNe • Fit to power law decay (n=5/3, monotonic) • Find tD=> MBH

  6. Ruled Out UV Outbursts

  7. Ruled Out Type II SNe

  8. Candidate D1-9 • BC03 fits early-type galaxy at z=0.326

  9. Candidate D1-9

  10. Candidate D3-13

  11. Candidate D3-13

  12. Black Hole Masses

  13. Spectral Energy Densities

  14. Things I Did Not Cover • The full energy argument getting to MBH • Expected detection rates

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