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.

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 Measuring the mass of the supermassive black hole of the lenticular galaxy NGC 4546

2020 ◽  
Vol 495 (3) ◽  
pp. 2620-2629
Author(s):  
T V Ricci ◽  
J E Steiner
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Near Infrared ◽  
Velocity Dispersion ◽  
Hubble Space Telescope ◽  
Anisotropy Parameter ◽  
Stellar Structure ◽  
Stellar Kinematics ◽  
Supermassive Black Hole ◽  
Integral Field

ABSTRACT Most galaxies with a well-structured bulge host a supermassive black hole (SMBH) in their centre. Stellar kinematics models applied to adaptive optics (AO) assisted integral field unit observations are well-suited to measure the SMBH mass (MBH) and also the total mass-to-light ratio [(M/L)TOT] and possible anisotropies in the stellar velocity distribution in the central region of galaxies. In this work, we used new AO assisted Near-Infrared Integral Field Spectrometer (NIFS) observations and also photometric data from the Hubble Space Telescope Legacy Archive of the galaxy NGC 4546 in order to determine its SMBH mass. To do this, we applied the Jeans Anisotropic Modelling (JAM) method to fit the average second velocity moment in the line of sight $(\overline{v^2_{\mathrm{ los}}})$ of the stellar structure. In addition, we also obtained (M/L)TOT and the classical anisotropy parameter βz = 1-(σz/σR)2 for this object within a field of view of 200 × 200 pc2. Maps of the stellar radial velocity and of the velocity dispersion were built for this galaxy using the penalized pixel fitting (ppxf) technique. We applied the Multi Gaussian Expansion procedure to fit the stellar brightness distribution. Using JAM, the best-fitting model for $\overline{v^2_{\mathrm{ los}}}$ of the stellar structure was obtained with (M/L)TOT = 4.34 ± 0.07 (Johnson’s R band), MBH = (2.56 ± 0.16) × 108 M⊙ and βz = −0.015 ± 0.03 (3σ confidence level). With these results, we found that NGC 4546 follows the MBH × σ relation. We also measured the central velocity dispersion within a radius of 1 arcsec of this object as σc = 241 ± 2 km s−1.

scholarly journals The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

2011 ◽  
Vol 2011 ◽  
pp. 1-8 ◽  
Author(s):  
Marc S. Seigar
Keyword(s):  
Black Hole ◽  
Dark Matter ◽  
Density Profile ◽  
Pitch Angle ◽  
Rotation Curve ◽  
Dark Matter Halo ◽  
Black Hole Mass ◽  
Supermassive Black Hole ◽  
Virial Mass ◽  
Spiral Arm

We investigate the dark matter halo density profile of M33. We find that the HI rotation curve of M33 is best described by an NFW dark matter halo density profile model, with a halo concentration of and a virial mass of . We go on to use the NFW concentration of M33, along with the values derived for other galaxies (as found in the literature), to show that correlates with both spiral arm pitch angle and supermassive black hole mass.

scholarly journals Supermassive black hole mass regulated by host galaxy morphology

2009 ◽  
Vol 400 (4) ◽  
pp. 1803-1807 ◽  
Author(s):  
Y. Watabe ◽  
N. Kawakatu ◽  
M. Imanishi ◽  
T. T. Takeuchi
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Supermassive Black Hole ◽  
Galaxy Morphology

scholarly journals Observations of the γ-ray emitting narrow-line Seyfert 1, SBS 0846+513, and its host galaxy

2021 ◽  
Author(s):  
Timothy S Hamilton ◽  
Marco Berton ◽  
Sonia Antón ◽  
Lorenzo Busoni ◽  
Alessandro Caccianiga ◽  
...  
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Host Galaxy ◽  
Narrow Line ◽  
Black Hole Mass ◽  
Residual Structure ◽  
Line Region ◽  
Resolution Imaging ◽  
Γ Ray ◽  
Adaptive Optics System

Abstract The γ-ray emitting galaxy SBS 0846 + 513 has been classified as a Narrow-Line Seyfert 1 (NLS1) from its spectroscopy, and on that basis would be thought likely to have a small central black hole hosted in a spiral galaxy. But very few of the γ-ray NLS1 have high-resolution imaging of their hosts, so it is unknown how the morphology expectation holds up for the γ-emitting class. We have observed this galaxy in the J-band with the Large Binocular Telescope’s LUCI1 camera and the ARGOS adaptive optics system. We estimate its black hole mass to lie between $4.2\times 10^7 \le \frac{\text{M}}{\text{M}_\odot } \le 9.7\times 10^7$, using the correlation with bulge luminosity, or $1.9\times 10^7 \le \frac{\text{M}}{\text{M}_\odot } \le 2.4\times 10^7$ using the correlation with Sérsic index. Our favoured estimate is 4.2 × 107M⊙, putting its mass at the high end of the NLS1 range in general but consistent with others that are γ-ray emitters. These estimates are independent of the Broad Line Region viewing geometry and avoid any underestimates due to looking down the jet axis. Its host shows evidence of a bulge + disc structure, from the isophote shape and residual structure in the nuclear-subtracted image. This supports the idea that γ-ray NLS1 may be spiral galaxies, like their non-jetted counterparts.

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 Universal interferometric signatures of a black hole’s photon ring

2020 ◽  
Vol 6 (12) ◽  
pp. eaaz1310 ◽  
Author(s):  
Michael D. Johnson ◽  
Alexandru Lupsasca ◽  
Andrew Strominger ◽  
George N. Wong ◽  
Shahar Hadar ◽  
...  
Keyword(s):  
General Relativity ◽  
Black Hole ◽  
Event Horizon ◽  
Infinite Sequence ◽  
High Order ◽  
Black Hole Mass ◽  
Tests Of General Relativity ◽  
Supermassive Black Hole ◽  
The Galaxy ◽  
Self Similar

The Event Horizon Telescope image of the supermassive black hole in the galaxy M87 is dominated by a bright, unresolved ring. General relativity predicts that embedded within this image lies a thin “photon ring,” which is composed of an infinite sequence of self-similar subrings that are indexed by the number of photon orbits around the black hole. The subrings approach the edge of the black hole “shadow,” becoming exponentially narrower but weaker with increasing orbit number, with seemingly negligible contributions from high-order subrings. Here, we show that these subrings produce strong and universal signatures on long interferometric baselines. These signatures offer the possibility of precise measurements of black hole mass and spin, as well as tests of general relativity, using only a sparse interferometric array.

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