1. Black Hole Growth in the Local Universe
Jenny E. Greene (Hubble/Princeton-Carnegie Fellow)
Luis C. Ho (Carnegie), Aaron J. Barth (UC Irvine)

2. Local BH Mass Functions
Marconi et al. 2004
Galaxy luminosity function→BH mass function
Primary mode of BH growth
AGN lifetimes, radiative efficiency

3. BHs Growing Today Broad-line AGNs - masses from AGN physics
Heckman et al. 2004
All BHs (active+inactive)
Narrow-line AGNs
Distribution of L[OIII]
Broad-line AGNs
- masses from AGN physics
- compare broad and narrow line AGNs
- sensitive to low-mass (<106 M⦿) BHs

4. Only means to probe this regime is using AGNs, since current resolution inadequate for dynamical detection
But isn’t this a neglible fraction of total
BH mass and radiated lumiminosity?
Haehnelt 2004

5. Disproportionate ImportGC
dSph dE E
Merritt et al. 2004
Gravitational Recoil
Primordial Seeds
Bromm & Loeb
Gravitational
radiation
LISA

6. Low-mass BHs are rare? All galaxies Active galaxies (narrow-line)
Stellar Mass
Greene & Ho 2004
found only 19 broad-line
AGNs in DR1 (<106 M⦿)
All galaxies
Active galaxies
(narrow-line)
Groves et al. astroph/

7. The Search z<0.35 broad-line AGNs from SDSS
Galaxy Survey: r < 17.77; extended (e.g. Hao et al. 2005, Heckman et al. 2004)
AGN Survey: 15 < i < 19.1; color-selected
PCA (Hao et al. 2005)
Modeling (Greene & Ho 2004)
[S II] λλ6716, 6731
Hα + [N II] λλ6548, 6583

8. Standard scaling relations (BLR radius and AGN luminosity)
~8000 AGNs, 2000 from main galaxy sample
LHα
FWHMHα
MBH
Lbol/LEdd
Standard scaling relations
(BLR radius and AGN luminosity)
Greene & Ho 2005

9. Lbol/LEdd 0.01 0.03 0.1 0.3 1 SDSS bright limit Greene & Ho in prep

10. Hα Luminosity Function
broad Hα luminosity function
8300 broad-line AGNs
Vmax method
Greene & Ho in prep
Contaminants
Ho 2004

11. BH Mass Functions
Greene & Ho in prep ?
“Cosmic Downsizing”
MBH *
Text

12. CF with Hasinger et al 2005 CF with Heckman et al. 2004
All T2s from SDSS
Greene & Ho in prep
Seyfert T2s
Broad-line AGNs
CF with Heckman et al. 2004
CF with Hasinger et al 2005
Soft X-ray LF
Inferred from optical
using αox

13. Monte Carlo Real turnover at the low-mass end OR low-mass BHs are
z=0.05
z < 0.02
z =0.1
0.01 < L/LEdd<0.1
0.1 < L/LEdd<0.3
0.3< L/LEdd<3
log (MBH/M⦿)
Real turnover at the low-mass end OR
low-mass BHs are
quiescent
incorrect galaxy luminosities

14. Greene, Barth, & Ho in prep
3 kpc
8 kpc
7 kpc
10 kpc
4 kpc
20 kpc
GH02
GH08
GH05
GH17
GH04
GH09
19 AGNs (<106 M⦿) Greene & Ho 2004 HST/ACS: F435W (B), F814W (I), 1 orbit/source
Greene, Barth, & Ho in prep
7 kpc

15. Greene, Barth, & Ho in prep
MBH-LBulge
Marconi & Hunt (2003)
Greene & Ho 2004
NGC 4395
Pox 52
5 mag
GALFIT
Peng et al. 2002
PSF + 1 Sersic fit
13 have n<1.5 in Single-Sersic fits
8 have clear disks/spiral structure
To convert to b-band used the conversion of Fukugita 1995 for an Scd galaxy - b=i+1.57
Barth, Greene, & Ho 2005
Barth et al. 2004
Filippenko & Ho 2003
Greene, Barth, & Ho in prep

16. Lauer et al. 2006/astroph
Ferrarese et al. 2006
Star-cluster mass correlated with galaxy mass (see also Wehner & Harris 2006, Rossa et al. 2006)

17. Conclusions (preliminary)
We construct BH mass functions using local broad-line AGNs from SDSS
We investigate, for the first time, the space density of the lowest-mass AGNs known (<106 M⦿)
Preliminary evidence that low-mass BHs are truly rare (or inactive)
Alternate search techniques are desirable: deeper nuclear optical spectroscopic surveys, X-ray stacking, deep radio searches, tidal disruptions (LSST)

18. Greene, Barth, & Ho in prep
MBH-LBulge
Marconi & Hunt (2003)
Greene & Ho 2004
NGC 4395
Pox 52
5 mag
GALFIT
Peng et al. 2002
PSF + 1 Sersic fit
13 have n<1.5 in Single-Sersic fits
8 have clear disks/spiral structure
To convert to b-band used the conversion of Fukugita 1995 for an Scd galaxy - b=i+1.57
Barth et al. 2004
Filippenko & Ho 2003
Greene, Barth, & Ho in prep

19. N 1068m
N 4261
N 821
N 1023
N 2778
N 3115
N 3377
N 3379
N 3384
N 3608
N 4291
N 4473
N 4649
N 7457
N 7052g
N 6251g
N 2787G
M87G
IC 1459
N 3245
N 4697
N 4596g
N 4564
N 4459g
N 4258m
M 32
M31 MW
MBH
MGal
32 galaxies from Tremaine et al 2002, I’m missing 3:

20. Monte Carlo Distribution of MBH, L, z
Corresponding galaxy luminosities using MBH-Lbulge relations
Realistic S/N using SDSS
Spectroscopic completeness using simulations

21. Unreliable BH Masses

22. Bulge/Total ratio poorly constrained
z=0.02
z=0.05
z=0.1
Lbol/LEdd = 0.01
Lbol/LEdd = 0.1
Bulge/Total ratio poorly constrained
for low-mass BHs
- Just bulge, assuming targeted as a galaxy
Lbol/LEdd = 1

23. Real incompleteness at the low-mass end OR biased galaxy sample
z=0.05
z=0.02
z=0.1
L/LEdd=0.01
L/LEdd=0.1
L/LEdd=1
log (MBH/M⦿)
Real incompleteness
at the low-mass end OR
biased galaxy sample
low-mass BHs are
quiescent

24. Maximum-Likelihood

26. Contaminants

27. Contaminants

28. Contaminants

30. Marconi et al. 2004

31. Which BHs are growing Today?
Narrow-line AGNs
SDSS Galaxies
Heckman et al. 2004

32. Fundamental Plane?