Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 509, Issue 2, Pages 2920-2939Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab3016
Keywords
Galaxy: disc; galaxies: ISM; galaxies: kinematics and dynamics; galaxies: nuclei; ISM: molecules; (galaxies:) quasars: supermassive black holes
Categories
Funding
- International University -Vietnam National University in Ho Chi Minh City
- National Astrononical Observatory of Japan (NAOJ)
- National Institute of Natural Sciences (NINS)
- consolidated grants Astrophysics at Oxford from the United Kingdom Research Councils [ST/H002456/1, ST/K00106X/1]
- European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme [724857]
- Science and Technology Facilities Council (STFC) [ST/S00033X/1]
- Royal Society University Research Fellowship (RSURF)
- Japan Society for the Promotion of Science (JSPS) KAKENHI grant [17K14247, 19J00892]
- USNaval Research Laboratory
- Grants-in-Aid for Scientific Research [19J00892] Funding Source: KAKEN
Ask authors/readers for more resources
The study utilized ALMA observations to measure the mass of the supermassive black hole in the nearby galaxy NGC 3593, revealing a circumnuclear molecular gas disc and a massive core of cold molecular gas. The mass distribution of the CND and NSC confirmed the presence of the SMBH and aligned with the compiled mass relation.
As part of the Measuring Black Holes in below Milky Way-mass (M*) galaxies (MBHBM*) Project, we present a dynamical measurement of the supermassive black hole (SMBH) mass in the nearby lenticular galaxy NGC 3593, using cold molecular gas 12CO(2-1) emission observed at an angular resolution of approximate to 0.'' 3 (approximate to 10 pc) with the Atacama Large Millimeter/submillimeter Array (ALMA). Our ALMA observations reveal a circumnuclear molecular gas disc (CND) elongated along the galaxy major axis and rotating around the SMBH. This CND has a relatively low-velocity dispersion (less than or similar to 10 km s(-1)) and is morphologically complex, with clumps having higher integrated intensities and velocity dispersions (less than or similar to 25 km s(-1)). These clumps are distributed along the ridges of a two-arm/bi-symmetric spiral pattern surrounded by a larger ring-like structure (radius r approximate to 10 arcsec or approximate to 350 pc). This pattern likely plays an important role to bridge the molecular gas reservoirs in the CND and beyond (10 less than or similar to r less than or similar to 35 arcsec or 350 pc less than or similar to r less than or similar to 1.2 kpc). Using dynamical modelling, the molecular gas kinematics allow us to infer an SMBH mass M-BH = 2.40(-1.05)(+1.87) x 10(6) M-circle dot (only statistical uncertainties at the 3 sigma level). We also detect a massive core of cold molecular gas (CMC) of mass MCMC = (5.4 +/- 1.2) x 10(6) M-circle dot and effective (half-mass) radius r(CMC,e) = 11.2 +/- 2.8 pc, co-spatial with a nuclear star cluster (NSC) of mass M-NSC = (1.67 +/- 0.48) x 10(7) M-circle dot and effective radius r(NSC,e) = 5.0 +/- 1.0 pc (or 0.'' 15 +/- 0 '' 03). The mass profiles of the CMC and NSC are well described by Sersic functions with indices 1-1.4. Our M-BH and MNSC estimates for NGC 3593 agree well with the recently compiled M-BH-MNSC scaling relation. Although the MNSC uncertainty is twice the inferred M-BH, the rapid central rise of the rotation velocities of the CND (as the radius decreases) clearly suggests an SMBH. Indeed, our dynamical models show that even if MNSC is at the upper end of its allowed range, the evidence for a BH does not vanish, but remains with a lower limit of M-BH > 3 x 10(5) M-circle dot.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available