1. WISDOM: Supermassive Black Hole Mass Measurements in NGC1097 and NGC3665
Kyoko Onishi
SOKENDAI (The Graduate University for Advanced Studies)
M., Bureau, T., Davis, M., Cappellari, M.,Sarzi,
L., Blitz, and S., Iguchi (WISDOM group)
K. Khono, K., Sheth

2. WISDOM?
mm-Wave Interferometric Survey of Dark Object Masses We weigh BH mass! with molecular gas!

3. Supermassive black hole
BH/galaxy evolution
Supermassive black hole
resides in
most giant galaxies
(Kormendy & Ho 2013, etc.)

4. BH/galaxy evolution Black holes and galaxies seem to
evolve hand-in-hand
(Kormendy & Ho 2013, etc.)

5. BHmass VS. galaxy properties (e.g., M-sigma)
Larger galaxy, heavier BH
larger sample needed
SMBH mass – velocity dispersion (M-sigma), galaxy luminosity, bulge mass, etc.
Ferrarese & Merrit 2000, McConnel & Ma 2013, Kormendy & Ho 2013, Läsker+ 2014, Savrognan+ 2015, etc. for obs.
Silk & Rees 1998, Di Matteo+ 2008, Barai etc. for numerical simulations

6. SMBH mass measuring method
molecular gas dynamics
settled to be a disk
easily trace its rotation
many targets in ALMA era
Davis et al. 2013: NGC 4256
Onishi et al. 2015: NGC 1097
Barth et al. 2016: NGC 1332
Onishi et al. in prep. : NGC 3665

7. SMBH mass measurement w/ HCN kinematics
ALMA Cycle 0 (PI: K. Kohno)
1”.6×2”.2 synth. beam
HCN(1-0) line integrated for minutes

8. SMBH mass estimation w/ HCN kinematics
NGC 1097, Onishi+15
Estimate the mass model
stars(Luminosity*M/L)+SMBH
Set fitting parameters
M/L, SMBH mass
Calculate rotation to compare with obs.
Determine the best fit

9. SMBH mass estimation w/ HCN kinematics
NGC 1097, Onishi+15
Estimate the mass model
stars(Luminosity*M/L)+SMBH
Set fitting parameters
M/L, SMBH mass
Calculate rotation to compare with obs.
Determine the best fit
Multi Gaussian Expansion, Emsellem+ 1994, Cappellari +2002

10. SMBH mass estimation w/ HCN kinematics
NGC 1097, Onishi+15
Estimate the mass model
Set fitting parameters
Calculate rotation to compare with obs.
cut position-velocity diagram
Determine the best fit
chi-square contour
MGE_circular _velocity,
Cappellari +2002
Kinematic Molecualr Simlation,
Davis+ 2013

11. SMBH mass estimation w/ HCN kinematics
NGC 1097, Onishi+15
Estimate the mass model
Set fitting parameters
Calculate rotation to compare with obs.
cut position-velocity diagram
Determine the best fit
chi-square contour

12. SMBH mass estimation w/ HCN kinematics
NGC 1097, Onishi+15
Collapsed the velocity field into spectra along galaxy major axis : losing data Some critical information was not included as fitting parameters
PVD fitting → cube fitting?
parameters
M/L, MBH → add parameters
inclination, disk properties, etc.?

13. refined method; Onishi+in prep.
NGC 3665: SA0 with dust lane CARMA beam 0”.63x0”.59 (~100pc) for CO(2-1)

14. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.
PVD fitting → cube fitting!

15. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.
parameters
M/L, MBH → add parameters
inclination, disk properties, etc.
More parameters Bayesian analysis

16. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.
mass model of the galaxy (NGC 3665)

17. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.
central position of the calculated cube

18. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.
molecular gas disk properties

19. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.
likelihood
M/L
BH mass (×108Msun)
M/L

20. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.
More parameters Bayesian analysis

21. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.

22. refined method; Onishi+in prep.
NGC3665, Onishi+in prep.
result
SMBH mass=( )x108Msun
M/L ratio=1.52 Msun/Lsun

23. going back to the old method..
NGC3665, Onishi+in prep.
best fit:
SMBH mass=
M/L ratio=
Consistent values from
different fitting methods!
(using PVD or data cube)
NB: molecular gas disk parameters are taken by the cube fitting!

24. going back to the old method..
NGC3665, Onishi+in prep.

25. NGC 3665 radio jet
NGC3665, Onishi+in prep.
a jet observed with VLA (1.5 GHz), perpendicular to the CO disk!
log(LX/Ledd)=-6.73:
requires radiatively inefficient flows
→ consistent with the presence of the jet!
LX=7.19e39 erg/s (Liuzzo+2011)
Ledd=6.98e46 erg/s
Nyland et al in prep.

26. Future Prospects Sensible SMBH mass detected with the method,
(no matter how the fit is done!)
however for
small number of targets.
McConnell & Ma 2013
Ferrarese & Merrit 2000
molecular gas method
McConnell et al. 2011,
McConnell & Ma, 2013

27. Some more (10+ objects) data coming in from Cycle 2 and 3..
Future Prospects
Some more (10+ objects) data coming in from Cycle 2 and 3..
other Cycle obj.
S (PI: K Onishi) 6 obj.
Cycle obj.
CARMA several
Cycle 0 N1097

28. Summary
Consistent SMBH mass measured by fitting molecular gas dynamics both in 3D cube and in PVD.
The method will bring more galaxies to the empirical M-sigma relation
e.g., NGC 1097: late-type Seyfert, NGC 3665: early-type radio jet
Larger sample possibly help one to better understand the relation and co-evolutionary process of galaxy and BH.