2017/03/14 by Kyoko Onishi, K. Onishi, S. Iguchi +10 · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Mass ratio #Millimeter #Physics #Radio Astronomy Observations and Technology #Supermassive black hole #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stx631
Accepted to MNRAS
openalex publication_date 2017/03/14 · arxiv created 2017/03/21 · arxiv updated 2017/03/22 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
As a part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project, we present an estimate of the mass of the supermassive black hole (SMBH) in the nearby fast-rotator early-type galaxy NGC 3665. We obtained the Combined Array for Research in Millimeter Astronomy (CARMA) B and C array observations of the 12CO(J = 2 − 1) emission line with a combined angular resolution of 0.59 arcsec. We analysed and modelled the three-dimensional molecular gas kinematics, obtaining a best-fitting SMBH mass |M\rm BH=5.75+1.49-1.18 × 108| M⊙, a mass-to-light ratio at H-band (M/L)H = 1.45 ± 0.04 (M/L)⊙,H and other parameters describing the geometry of the molecular gas disc (statistical errors, all at 3σ confidence). We estimate the systematic uncertainties on the stellar M/L to be ≈0.2 (M/L)⊙,H, and on the SMBH mass to be ≈0.4 × 108 M⊙. The measured SMBH mass is consistent with that estimated from the latest correlations with galaxy properties. Following our older works, we also analysed and modelled the kinematics using only the major-axis position–velocity diagram, and conclude that the two methods are consistent.