Black hole mass measurement in nearby galaxy using molecular gas dynamics

2016 ◽  
Author(s):  
Kyoko Onishi ◽  
Satoru Iguchi ◽  
Timothy Davis ◽  
Martin Bureau ◽  
Michele Cappellari ◽  
...  
Keyword(s):  
Black Hole ◽  
Gas Dynamics ◽  
Mass Measurement ◽  
Molecular Gas ◽  
Nearby Galaxy ◽  
Black Hole Mass

scholarly journals A black-hole mass measurement from molecular gas kinematics in NGC4526

Nature ◽  
2013 ◽  
Vol 494 (7437) ◽  
pp. 328-330 ◽  
Author(s):  
Timothy A. Davis ◽  
Martin Bureau ◽  
Michele Cappellari ◽  
Marc Sarzi ◽  
Leo Blitz
Keyword(s):  
Black Hole ◽  
Mass Measurement ◽  
Molecular Gas ◽  
Black Hole Mass ◽  
Gas Kinematics

scholarly journals WISDOM project – I. Black hole mass measurement using molecular gas kinematics in NGC 3665

2017 ◽  
Vol 468 (4) ◽  
pp. 4663-4674 ◽  
Author(s):  
Kyoko Onishi ◽  
Satoru Iguchi ◽  
Timothy A. Davis ◽  
Martin Bureau ◽  
Michele Cappellari ◽  
...  
Keyword(s):  
Black Hole ◽  
Mass Measurement ◽  
Molecular Gas ◽  
Black Hole Mass ◽  
Gas Kinematics

Central kiloparsec of NGC 1326 observed with SINFONI

2020 ◽  
Vol 638 ◽  
pp. A53
Author(s):  
Nastaran Fazeli ◽  
Gerold Busch ◽  
Andreas Eckart ◽  
Françoise Combes ◽  
Persis Misquitta ◽  
...  
Keyword(s):  
Black Hole ◽  
Galaxy Evolution ◽  
Near Infrared ◽  
Velocity Fields ◽  
Molecular Gas ◽  
Nearby Galaxy ◽  
Stellar Content ◽  
Stellar Rotation ◽  
Supermassive Black Hole ◽  
Integral Field Spectrograph

Gas inflow processes in the vicinity of galactic nuclei play a crucial role in galaxy evolution and supermassive black hole growth. Exploring the central kiloparsec of galaxies is essential to shed more light on this subject. We present near-infrared H- and K-band results of the nuclear region of the nearby galaxy NGC 1326, observed with the integral-field spectrograph SINFONI mounted on the Very Large Telescope. The field of view covers 9″ × 9″ (650 × 650 pc2). Our work is concentrated on excitation conditions, morphology, and stellar content. The nucleus of NGC 1326 was classified as a LINER, however in our data we observed an absence of ionised gas emission in the central r ∼ 3″. We studied the morphology by analysing the distribution of ionised and molecular gas, and thereby detected an elliptically shaped, circum-nuclear star-forming ring at a mean radius of 300 pc. We estimate the starburst regions in the ring to be young with dominating ages of < 10 Myr. The molecular gas distribution also reveals an elongated east to west central structure about 3″ in radius, where gas is excited by slow or mild shock mechanisms. We calculate the ionised gas mass of 8 × 105 M⊙ completely concentrated in the nuclear ring and the warm molecular gas mass of 187 M⊙, from which half is concentrated in the ring and the other half in the elongated central structure. The stellar velocity fields show pure rotation in the plane of the galaxy. The gas velocity fields show similar rotation in the ring, but in the central elongated H2 structure they show much higher amplitudes and indications of further deviation from the stellar rotation in the central 1″ aperture. We suggest that the central 6″ elongated H2 structure might be a fast-rotating central disc. The CO(3–2) emission observations with the Atacama Large Millimeter/submillimeter Array reveal a central 1″ torus. In the central 1″ of the H2 velocity field and residual maps, we find indications for a further decoupled structure closer to a nuclear disc, which could be identified with the torus surrounding the supermassive black hole.

scholarly journals WISDOM Project – III. Molecular gas measurement of the supermassive black hole mass in the barred lenticular galaxy NGC4429

2017 ◽  
Vol 473 (3) ◽  
pp. 3818-3834 ◽  
Author(s):  
Timothy A. Davis ◽  
Martin Bureau ◽  
Kyoko Onishi ◽  
Freeke van de Voort ◽  
Michele Cappellari ◽  
...  
Keyword(s):  
Black Hole ◽  
Molecular Gas ◽  
Black Hole Mass ◽  
Supermassive Black Hole ◽  
Gas Measurement

scholarly journals WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

2017 ◽  
Vol 468 (4) ◽  
pp. 4675-4690 ◽  
Author(s):  
Timothy A. Davis ◽  
Martin Bureau ◽  
Kyoko Onishi ◽  
Michele Cappellari ◽  
Satoru Iguchi ◽  
...  
Keyword(s):  
Black Hole ◽  
Molecular Gas ◽  
Black Hole Mass ◽  
Supermassive Black Hole ◽  
Gas Measurement

scholarly journals Revealing the intermediate-mass black hole at the heart of the dwarf galaxy NGC 404 with sub-parsec resolution ALMA observations

2020 ◽  
Vol 496 (4) ◽  
pp. 4061-4078 ◽  
Author(s):  
Timothy A Davis ◽  
Dieu D Nguyen ◽  
Anil C Seth ◽  
Jenny E Greene ◽  
Kristina Nyland ◽  
...  
Keyword(s):  
Black Hole ◽  
Dwarf Galaxy ◽  
Elliptical Galaxy ◽  
Continuum Emission ◽  
Molecular Gas ◽  
Black Hole Mass ◽  
Stellar Kinematics ◽  
Intermediate Mass ◽  
Gas Kinematics ◽  
Stellar Kinematic

ABSTRACT We estimate the mass of the intermediate-mass black hole at the heart of the dwarf elliptical galaxy NGC 404 using Atacama Large Millimetre/submillimetre Array (ALMA) observations of the molecular interstellar medium at an unprecedented linear resolution of ≈0.5 pc, in combination with existing stellar kinematic information. These ALMA observations reveal a central disc/torus of molecular gas clearly rotating around the black hole. This disc is surrounded by a morphologically and kinematically complex flocculent distribution of molecular clouds, that we resolve in detail. Continuum emission is detected from the central parts of NGC 404, likely arising from the Rayleigh–Jeans tail of emission from dust around the nucleus, and potentially from dusty massive star-forming clumps at discrete locations in the disc. Several dynamical measurements of the black hole mass in this system have been made in the past, but they do not agree. We show here that both the observed molecular gas and stellar kinematics independently require a ≈5 × 105 M⊙ black hole once we include the contribution of the molecular gas to the potential. Our best estimate comes from the high-resolution molecular gas kinematics, suggesting the black hole mass of this system is 5.5$^{+4.1}_{-3.8}\times 10^5$ M⊙ (at the 99 per cent confidence level), in good agreement with our revised stellar kinematic measurement and broadly consistent with extrapolations from the black hole mass–velocity dispersion and black hole mass–bulge mass relations. This highlights the need to accurately determine the mass and distribution of each dynamically important component around intermediate-mass black holes when attempting to estimate their masses.

scholarly journals Testing the robustness of black hole mass measurements with ALMA and MUSE

2019 ◽  
Vol 14 (S353) ◽  
pp. 199-202
Author(s):  
Sabine Thater ◽  
Davor Krajnović ◽  
Dieu D. Nguyen ◽  
Satoru Iguchi ◽  
Peter M. Weilbacher
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Molecular Gas ◽  
Black Hole Mass ◽  
Stellar Kinematics ◽  
Mass Measurements ◽  
Massive Black Hole ◽  
Gas Kinematics ◽  
Ongoing Work ◽  
Black Hole Masses

AbstractWe present our ongoing work of using two independent tracers to estimate the supermassive black hole mass in the nearby early-type galaxy NGC 6958; namely integrated stellar and molecular gas kinematics. We used data from the Atacama Large Millimeter/submillimeter Array (ALMA), and the adaptive-optics assisted Multi-Unit Spectroscopic Explorer (MUSE) and constructed state-of-the-art dynamical models. The different methods provide black hole masses of (2.89±2.05)×108M⊙ from stellar kinematics and (1.35±0.09)×108M⊙ from molecular gas kinematics which are consistent within their 3σ uncertainties. Compared to recent MBH - σe scaling relations, we derive a slightly over-massive black hole. Our results also confirm previous findings that gas-based methods tend to provide lower black hole masses than stellar-based methods. More black hole mass measurements and an extensive analysis of the method-dependent systematics are needed in the future to understand this noticeable discrepancy.

scholarly journals Black hole mass measurement using ALMA observations of [CI] and CO emissions in the Seyfert 1 galaxy NGC 7469

2021 ◽  
Author(s):  
Dieu D Nguyen ◽  
Takuma Izumi ◽  
Sabine Thater ◽  
Masatoshi Imanishi ◽  
Taiki Kawamuro ◽  
...  
Keyword(s):  
Black Hole ◽  
Mass Measurement ◽  
Emission Lines ◽  
Black Hole Mass ◽  
X Ray ◽  
Carbon Abundance ◽  
Line Region ◽  
Order Of Magnitude ◽  
Ngc 7469 ◽  
Co Emission

Abstract We present a supermassive black hole (SMBH) mass measurement in the Seyfert 1 galaxy NGC 7469 using Atacama Large Millimeter/submillimeter Array (ALMA) observations of the atomic-[CI](1-0) and molecular-12CO(1-0) emission lines at the spatial resolution of ≈0${_{.}^{\prime\prime}}$3 (or ≈ 100 pc). These emissions reveal that NGC 7469 hosts a circumnuclear gas disc (CND) with a ring-like structure and a two-arm/bi-symmetric spiral pattern within it, surrounded by a starbursting ring. The CND has a relatively low σgas/V ≈ 0.35 (r ≲ 0${_{.}^{\prime\prime}}$5) and ≈0.19 (r &gt; 0${_{.}^{\prime\prime}}$5), suggesting that the gas is dynamically settled and suitable for dynamically deriving the mass of its central source. As is expected from X-ray dominated region (XDR) effects that dramatically increase an atomic carbon abundance by dissociating CO molecules, we suggest that the atomic [CI](1-0) emission is a better probe of SMBH masses than CO emission in AGNs. Our dynamical model using the [CI](1-0) kinematics yields a $M_{\rm BH}=1.78^{+2.69}_{-1.10}\times 10^7$ M⊙ and $M/L_{\rm F547M}=2.25^{+0.40}_{-0.43}$ (M⊙/L⊙). The model using the 12CO(1-0) kinematics also gives a consistent MBH with a larger uncertainty, up to an order of magnitude, i.e. $M_{\rm BH}=1.60^{+11.52}_{-1.45}\times 10^7$ M⊙. This newly dynamical MBH is ≈ 2 times higher than the mass determined from the reverberation mapped (RM) method using emissions arising in the unresolved broad-line region (BLR). Given this new MBH, we are able to constrain the specific RM dimensionless scaling factor of $f=7.2^{+4.2}_{-3.4}$ for the AGN BLR in NGC 7469. The gas within the unresolved BLR thus has a Keplerian virial velocity component and the inclination of i ≈ 11.0○$_{-2.5}^{+2.2}$, confirming its face-on orientation in a Seyfert 1 AGN by assuming a geometrically thin BLR model.

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