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 Independent Estimation of Black Hole Mass for the γ-ray-detected Archetypal Narrow-line Seyfert 1 Galaxy 1H 0323+342 from X-Ray Variability

2018 ◽  
Vol 866 (1) ◽  
pp. 69 ◽  
Author(s):  
Hai-Wu Pan ◽  
Weimin Yuan ◽  
Su Yao ◽  
S. Komossa ◽  
Chichuan Jin
Keyword(s):  
Black Hole ◽  
Narrow Line ◽  
Black Hole Mass ◽  
X Ray ◽  
Γ Ray

scholarly journals Black hole mass estimation for active galactic nuclei from a new angle

2019 ◽  
Vol 487 (3) ◽  
pp. 3404-3418 ◽  
Author(s):  
Dalya Baron ◽  
Brice Ménard
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Cosmic Time ◽  
Galactic Nuclei ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Mass Estimation ◽  
Line Region

Abstract The scaling relations between supermassive black holes and their host galaxy properties are of fundamental importance in the context black hole-host galaxy co-evolution throughout cosmic time. In this work, we use a novel algorithm that identifies smooth trends in complex data sets and apply it to a sample of 2000 type 1 active galactic nuclei (AGNs) spectra. We detect a sequence in emission line shapes and strengths which reveals a correlation between the narrow L([O iii])/L(H β) line ratio and the width of the broad H α. This scaling relation ties the kinematics of the gas clouds in the broad line region to the ionization state of the narrow line region, connecting the properties of gas clouds kiloparsecs away from the black hole to material gravitationally bound to it on sub-parsec scales. This relation can be used to estimate black hole masses from narrow emission lines only. It therefore enables black hole mass estimation for obscured type 2 AGNs and allows us to explore the connection between black holes and host galaxy properties for thousands of objects, well beyond the local Universe. Using this technique, we present the MBH–σ and MBH–M* scaling relations for a sample of about 10 000 type 2 AGNs from Sloan Digital Sky Survey. These relations are remarkably consistent with those observed for type 1 AGNs, suggesting that this new method may perform as reliably as the classical estimate used in non-obscured type 1 AGNs. These findings open a new window for studies of black hole-host galaxy co-evolution throughout cosmic time.

scholarly journals A REVISED BROAD-LINE REGION RADIUS AND BLACK HOLE MASS FOR THE NARROW-LINE SEYFERT 1 NGC 4051

2009 ◽  
Vol 702 (2) ◽  
pp. 1353-1366 ◽  
Author(s):  
K. D. Denney ◽  
L. C. Watson ◽  
B. M. Peterson ◽  
R. W. Pogge ◽  
D. W. Atlee ◽  
...  
Keyword(s):  
Black Hole ◽  
Broad Line ◽  
Narrow Line ◽  
Black Hole Mass ◽  
Broad Line Region ◽  
Line Region ◽  
Ngc 4051

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 Relativistic Jets in Gamma-Ray-Emitting Narrow-Line Seyfert 1 Galaxies

Galaxies ◽  
2019 ◽  
Vol 7 (4) ◽  
pp. 87 ◽  
Author(s):  
Filippo D’Ammando
Keyword(s):  
Black Hole ◽  
Gamma Ray ◽  
Broad Band ◽  
Jet Physics ◽  
Host Galaxy ◽  
Narrow Line ◽  
Relativistic Jets ◽  
Large Area ◽  
Small Black Hole ◽  
Γ Ray

Before the launch of the Fermi Gamma-ray Space Telescope satellite only two classes of active galactic nuclei (AGN) were known to generate relativistic jets and thus to emit up to the γ -ray energy range: blazars and radio galaxies, both hosted in giant elliptical galaxies. The discovery by the Large Area Telescope (LAT) on-board the Fermi satellite of variable γ -ray emission from a few radio-loud narrow-line Seyfert 1 galaxies (NLSy1) revealed the presence of an emerging third class of AGN with powerful relativistic jets. Considering that NLSy1 are usually hosted in late-type galaxies with relatively small black hole masses, this finding opened new challenging questions about the nature of these objects, the disc/jet connection, the emission mechanisms at high energies, and the formation of relativistic jets. In this review, I will discuss the broad-band properties of the γ -ray-emitting NLSy1 included in the Fourth Fermi LAT source catalog, highlighting major findings and open questions regarding jet physics, black hole mass estimation, host galaxy and accretion process of these sources in the Fermi era.

scholarly journals On the black hole mass of the γ-ray emitting narrow-line Seyfert 1 galaxy 1H 0323+342

2016 ◽  
Vol 464 (3) ◽  
pp. 2565-2576 ◽  
Author(s):  
H. Landt ◽  
M. J. Ward ◽  
M. Baloković ◽  
D. Kynoch ◽  
T. Storchi-Bergmann ◽  
...  
Keyword(s):  
Black Hole ◽  
Narrow Line ◽  
Black Hole Mass ◽  
Γ Ray

scholarly journals On the Relation Between Black Hole Mass and Velocity Dispersion in Type 1 and Type 2 AGN

2009 ◽  
Vol 5 (S267) ◽  
pp. 172-176
Author(s):  
Kalliopi M. Dasyra ◽  
Bradley M. Peterson ◽  
Linda J. Tacconi ◽  
Hagai Netzer ◽  
Luis C. Ho ◽  
...  
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Near Infrared ◽  
Velocity Dispersion ◽  
High Resolution Spectroscopy ◽  
Host Galaxy ◽  
Line Region ◽  
High Ionization

AbstractWe present results from infrared spectroscopic projects that aim to test the relation between the mass of a black hole MBH and the velocity dispersion of the stars in its host-galaxy bulge. We demonstrate that near-infrared, high-resolution spectroscopy assisted by adaptive optics is key in populating the high-luminosity end of the relation. We show that the velocity dispersions of mid-infrared, high-ionization lines originating from gas in the narrow-line region of the active galactic nucleus follow the same relation. This result provides a way of inferring MBH estimates for the cosmologically significant population of obscured, type 2 AGN that can be applicable to data from spectrographs on next-generation infrared telescopes.

Probing black hole - host galaxy scaling relations with obscured type II AGN

2019 ◽  
Vol 15 (S356) ◽  
pp. 365-365
Author(s):  
Dalya Baron
Keyword(s):  
Black Hole ◽  
Cosmic Time ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Type I ◽  
Type Ii ◽  
Black Hole Mass ◽  
Ionization State ◽  
Line Region ◽  
Black Hole Masses

AbstractThe scaling relations between supermassive black holes and their host galaxy properties are of fundamental importance in the context black hole-host galaxy co-evolution throughout cosmic time. Beyond the local universe, such relations are based on black hole mass estimates in type I AGN. Unfortunately, for this type of objects the host galaxy properties are more difficult to obtain since the AGN dominates the observed flux in most wavelength ranges. In this poster I will present a new correlation we discovered between the narrow L([OIII])/L(Hβ) line ratio and the FWHM(broad Hα). This scaling relation ties the kinematics of the gas clouds in the broad line region to the ionization state of gas in the narrow line region, connecting the properties of gas clouds kiloparsecs away from the black hole to material gravitationally bound to it on sub-parsec scales. This relation can be used to estimate black hole masses from narrow emission lines only, and thus brings the missing piece required to estimate black hole masses in obscured type II AGN. Using this technique, we estimate the black hole mass of about 10,000 type II AGN, and present, for the first time, M(BH)-sigma and M(BH)-M(stars) scaling relations for this population. These relations are remarkably consistent with those observed for type I AGN, suggesting that this new method may perform as reliably as the classical estimate used in non-obscured type I AGN. These findings open a new window for studies of black hole-host galaxy co-evolution throughout cosmic time.

Substructure in black hole scaling diagrams and implications for the coevolution of black holes and galaxies

2019 ◽  
Vol 15 (S359) ◽  
pp. 37-39
Author(s):  
Benjamin L. Davis ◽  
Nandini Sahu ◽  
Alister W. Graham
Keyword(s):  
Black Hole ◽  
Stellar Mass ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Physical Processes ◽  
Stellar Velocity ◽  
Galaxy Sample ◽  
Evolutionary Paths ◽  
Black Hole Masses

AbstractOur multi-component photometric decomposition of the largest galaxy sample to date with dynamically-measured black hole masses nearly doubles the number of such galaxies. We have discovered substantially modified scaling relations between the black hole mass and the host galaxy properties, including the spheroid (bulge) stellar mass, the total galaxy stellar mass, and the central stellar velocity dispersion. These refinements partly arose because we were able to explore the scaling relations for various sub-populations of galaxies built by different physical processes, as traced by the presence of a disk, early-type versus late-type galaxies, or a Sérsic versus core-Sérsic spheroid light profile. The new relations appear fundamentally linked with the evolutionary paths followed by galaxies, and they have ramifications for simulations and formation theories involving both quenching and accretion.

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