1. UV/Optical Detections of Candidate Tidal Disruption Events by GALEX and CFHTLS
Gezari et al. 2007
Looking for detections of stellar material accreting onto quiescent black hole
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2. SMBH Mass Function How are SMBH masses derived? Outstanding questions
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 yrs between events
For too large a mass, RT < RS
Can use tD to constrain MBH
Aquire tD from power-law decay in consumption rate (n=5/3)
From energy argument
K is related to spinup k=1 no spinup, k=3 near breakup speed
M6=MBH/106

4. Previous Candidates NGC 4552 has a “mini-AGN”
In 1995 experienced UV flare L ~ 1039 ergs/s
ROSAT ( ) 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
Do not have monotonic decreases in UV flux

7. Ruled Out Type II SNe
Only 2 candidates left

8. Candidate D1-9 BC03 fits early-type galaxy at z=0.326
I-band contours from CFHTLS
UV/optical variable in center

9. Candidate D1-9 Solid line is 5/3rds power law => 2004.0
Dashed line is with fixed tD at , n=1.1
n allowed to vary =
td =
Dot dash line is detection of soft x-ray source

10. Candidate D3-13
Z=0.3698

11. Candidate D3-13 With n=5/3, tD = 2003.3
With variable n = 3+-2, tD =
With tD fixed to , n = 0.82

12. Black Hole Masses D1-9 on left, D3-13 on right
Vertical line is min mass of star from mass accreted
In maximally spinning BH, Rms=Rg
Rbb>Rg gives max BH Mass
Max mass is also consistent with MBH<Mcrit for solar type star

13. Spectral Energy Densities
Two black-body spectra fit with solid lines

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