Kavli Affiliate: Luis C. Ho
| First 5 Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle
| Summary:
We present 0$.!!^{primeprime}{22}$-resolution CO(2$-$1) observations of
the circumnuclear gas disk in the local compact galaxy NGC 384 with the Atacama
Large Millimeter/submillimeter Array (ALMA). While the majority of the disk
displays regular rotation with projected velocities rising to $370$ km
s$^{-1}$, the inner $sim$0farcs{5} exhibits a kinematic twist. We develop
warped disk gas-dynamical models to account for this twist, fit those models to
the ALMA data cube, and find a stellar mass-to-light ratio in the $H$-band of
mlabstract and a supermassive black hole (BH) mass ($M_{mathrm{BH}}$) of
$M_{mathrm{BH}}$ $= (7.26^{+0.43}_{-0.48}$ [$1sigma$ statistical]
$^{+0.55}_{-1.00}$ [systematic])$times 10^8$ $M_odot$. In contrast to most
previous dynamical $M_{mathrm{BH}}$ measurements in local compact galaxies,
which typically found over-massive BHs compared to the local BH mass$-$bulge
luminosity and BH mass$-$bulge mass relations, NGC 384 lies within the scatter
of those scaling relations. NGC 384 and other local compact galaxies are likely
relics of $zsim2$ red nuggets, and over-massive BHs in these relics indicate
BH growth may conclude before the host galaxy stars have finished assembly. Our
NGC 384 results may challenge this evolutionary picture, suggesting there may
be increased scatter in the scaling relations than previously thought. However,
this scatter could be inflated by systematic differences between stellar- and
gas-dynamical measurement methods, motivating direct comparisons between the
methods for NGC 384 and the other compact galaxies in the sample.
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