Kyoko Onishi SOKENDAI (The Graduate University for Advanced Studies)

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Presentation transcript:

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

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

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

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

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+ 2014 etc. for numerical simulations

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

SMBH mass measurement w/ HCN kinematics ALMA Cycle 0 (PI: K. Kohno) 1”.6×2”.2 synth. beam HCN(1-0) line integrated for 105.24 minutes

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

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

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

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

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.?

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

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

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

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

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

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

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

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

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

refined method; Onishi+in prep. NGC3665, Onishi+in prep. result SMBH mass=(5.5+0.96-0.71)x108Msun M/L ratio=1.52 Msun/Lsun

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!

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

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.

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

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 3 10 obj. 2015.1.00466.S (PI: K Onishi) 6 obj. Cycle 2 3 obj. CARMA several Cycle 0 N1097

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.