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 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 The Supermassive Black Hole at the Heart of Centaurus A: Revealed by the Kinematics of Gas and Stars

2010 ◽  
Vol 27 (4) ◽  
pp. 449-456 ◽  
Author(s):  
Nadine Neumayer
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Accurate Determination ◽  
Black Hole Mass ◽  
Stellar Kinematics ◽  
Supermassive Black Hole ◽  
Integral Field Spectroscopy ◽  
Very Large Telescope ◽  
Using Data ◽  
Centaurus A

AbstractAt less than 4 Mpc distance the radio galaxy NGC 5128 (Centaurus A) is the prime example to study the supermassive black hole and its influence on the environment in great detail. To model and understand the feeding and feedback mechanisms one needs an accurate determination of the mass of the supermassive black hole. The aim of this review is to give an overview of the recent studies that have been dedicated to measure the black hole mass in Centaurus A from both gas and stellar kinematics. It shows how the advancement in observing techniques and instrumentation drive the field of black hole mass measurements and concludes that adaptive optics assisted integral field spectroscopy is the key to identify the effects of the AGN on the surrounding ionised gas. Using data from SINFONI at the ESO Very Large Telescope, the best-fit black hole mass is MBH = 4.5(+1.7, −1.0) × 107 M⊙ (from H2 kinematics) and MBH = (5.5 ± 3.0) × 107 M⊙ (from stellar kinematics). This is one of the cleanest gas-versus-star comparisons of a MBH determination, and brings Centaurus A into agreement with the MBH−σ relation.

The Megamaser Cosmology Project − XII. VLBI imaging of H2O maser emission in three active galaxies and the effect of AGN winds on disc dynamics

2020 ◽  
Vol 498 (2) ◽  
pp. 1609-1627
Author(s):  
C Y Kuo ◽  
J A Braatz ◽  
C M V Impellizzeri ◽  
F Gao ◽  
D Pesce ◽  
...  
Keyword(s):  
Black Hole ◽  
Active Galaxies ◽  
Black Hole Mass ◽  
Rotating Disc ◽  
Maser Emission ◽  
Gas Kinematics ◽  
Long Baseline ◽  
Show Evidence ◽  
Black Hole Masses

ABSTRACT We present very long baseline interferometry (VLBI) images and kinematics of water maser emission in three active galaxies: NGC 5728, Mrk 1, and IRAS 08452–0011. IRAS 08452–0011, at a distance of ∼200 Mpc, is a triple-peaked H2O megamaser, consistent with a Keplerian rotating disc, indicating a black hole mass of (3.3$\pm 0.2)\times 10^{7}\, \mathrm{ M}_{\odot }$. NGC 5728 and Mrk 1 display double-peaked spectra, and VLBI imaging reveals complicated gas kinematics that do not allow for a robust determination of black hole mass. We show evidence that the masers in NGC 5728 are in a wind while the Mrk 1 maser system has both disc and outflow components. We also find that disturbed morphology and kinematics are a ubiquitous feature of all double-peaked maser systems, implying that these maser sources may reside in environments where active galactic nucleus (AGN) winds are prominent at ∼1 pc scale and have significant impact on the masing gas. Such AGNs tend to have black hole masses $M_{\rm BH}\, \lt$ 8 × 106 M⊙ and Eddington ratios $\lambda _{\rm Edd}\, \gtrsim$ 0.1, while the triple-peaked megamasers show an opposite trend.

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 Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations

2019 ◽  
Vol 625 ◽  
pp. A62 ◽  
Author(s):  
Sabine Thater ◽  
Davor Krajnović ◽  
Michele Cappellari ◽  
Timothy A. Davis ◽  
P. Tim de Zeeuw ◽  
...  
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Velocity Dispersion ◽  
Variable Mass ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Early Type ◽  
Black Hole Mass ◽  
The Impact ◽  
Black Hole Masses

Different massive black hole mass – host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black hole masses is still limited and additional measurements are necessary to understand the underlying physics of this apparent coevolution. We add six new black hole mass (MBH) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281, and NGC 7049. Our target galaxies have effective velocity dispersions (σe) between 170 and 245 km s−1, and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combined high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS3D to derive two-dimensional stellar kinematics maps. We then built both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 108 M⊙ for NGC 584, (1.0 ± 0.6) × 108 M⊙ for NGC 2784, (7.7 ± 5) × 107 M⊙ for NGC 3640, (5.4 ± 0.8) × 108 M⊙ for NGC 4281, (6.8 ± 2.0) × 107 M⊙ for NGC 4570, and (3.2 ± 0.8) × 108 M⊙ for NGC 7049 at 3σ confidence level, which are consistent with recent MBH−σe scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.

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

scholarly journals The MBHBM⋆ Project. I. Measurement of the Central Black Hole Mass in Spiral Galaxy NGC 3504 Using Molecular Gas Kinematics

2020 ◽  
Vol 892 (1) ◽  
pp. 68 ◽  
Author(s):  
Dieu D. Nguyen ◽  
Mark den Brok ◽  
Anil C. Seth ◽  
Timothy A. Davis ◽  
Jenny E. Greene ◽  
...  
Keyword(s):  
Black Hole ◽  
Spiral Galaxy ◽  
Molecular Gas ◽  
Black Hole Mass ◽  
Central Black Hole ◽  
Gas Kinematics

scholarly journals Reverberation Mapping Results from MDM Observatory

2009 ◽  
Vol 5 (S267) ◽  
pp. 201-201
Author(s):  
Kelly D. Denney ◽  
B. M. Peterson ◽  
R. W. Pogge ◽  
M. C. Bentz ◽  
C. M. Gaskell ◽  
...  
Keyword(s):  
Black Hole ◽  
Time Delay ◽  
Black Hole Mass ◽  
Mass Measurements ◽  
Reverberation Mapping ◽  
Spectroscopic Monitoring ◽  
Line Region ◽  
Optical Continuum ◽  
Black Hole Masses

Reverberation mapping takes advantage of the presence of a time delay or lag, τ, between continuum and emission line flux variations observed through spectroscopic monitoring campaigns to infer the radius of the broad-line region (BLR) and, subsequently, the central black hole mass in type 1 AGNs. We present results from a multi-month reverberation mapping campaign undertaken primarily at MDM Observatory with supporting observations from around the world. We measure BLR radii and black hole masses for six objects. The primary goal of this campaign was to obtain either new or improved Hβ reverberation lag measurements for several relatively low-luminosity AGNs. Using cross correlation techniques to measure the time delay between the mean optical continuum flux density around 5100 Å and the integrated Hβ flux, we determine the Hβ lags and black hole mass measurements listed in columns 2 and 3 of Table 1, respectively. Column 4 tells if this measurement is new, an improvement meant to replace a previous, less reliable measurement, or simply an additional measurement not used to replace a previous value. The complete results from this study are currently being prepared for publication. A subsequent velocity-resolved analysis of the Hβ response shows that three of the six primary targets demonstrate kinematic signatures (column 5) of infall, outflow, and non-radial virialized motions (see Denney et al. 2009).

Sign in / Sign up

Export Citation Format

Share Document