scholarly journals Toward Precision Measurement of Central Black Hole Masses

2009 ◽  
Vol 5 (S267) ◽  
pp. 151-160 ◽  
Author(s):  
Bradley M. Peterson
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Host Galaxy ◽  
Reverberation Mapping ◽  
Line Region ◽  
The Masses ◽  
The Relationship ◽  
Black Hole Masses ◽  
Intrinsic Scatter ◽  
Direct And Indirect Methods

AbstractWe review briefly direct and indirect methods of measuring the masses of black holes in galactic nuclei, and then focus attention on supermassive black holes in active nuclei, with special attention to results from reverberation mapping and their limitations. We find that the intrinsic scatter in the relationship between the AGN luminosity and the broad-line region size is very small, ~0.11 dex, comparable to the uncertainties in the better reverberation measurements. We also find that the relationship between reverberation-based black hole masses and host-galaxy bulge luminosities also seems to have surprisingly little intrinsic scatter, ~0.17 dex. We note, however, that there are still potential systematics that could affect the overall mass calibration at the level of a factor of a few.

scholarly journals Uncertainties of the masses of black holes and Eddington ratios in AGN

2006 ◽  
Vol 2 (S238) ◽  
pp. 111-116
Author(s):  
Suzy Collin
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Reverberation Mapping ◽  
Line Region ◽  
Region I ◽  
Accretion Rates ◽  
Unknown Structure ◽  
The Masses ◽  
Empirical Size ◽  
Black Hole Masses

AbstractBlack hole masses in Active Galactic Nuclei have been determined in 35 objects through reverberation mapping of the emission line region. I mention some uncertainties of the method, such as the “scale factor” relating the Virial Product to the mass, which depends on the unknown structure and dynamics of the Broad Line Region.When the black hole masses are estimated indirectly using the empirical size-luminosity relation deduced from this method, the uncertainties can be larger, especially when the relation is extrapolated to high and low masses and/or luminosities. In particular they lead to Eddington ratiosof the order of unity in samples of Narrow Line Seyfert 1. As the optical-UV luminosity is provided by the accretion disk, the accretion rates can be determined and are found to be much larger than the Eddington rates.So, accretion must be performed at a super-critical rate through a slim disk, resulting in rapid growth of the black holes. The alternative is that the mass determination is wrong at this limit.

scholarly journals SUPER

2020 ◽  
Vol 644 ◽  
pp. A175
Author(s):  
G. Vietri ◽  
V. Mainieri ◽  
D. Kakkad ◽  
H. Netzer ◽  
M. Perna ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Line Profile ◽  
Host Galaxy ◽  
X Ray ◽  
Bolometric Luminosity ◽  
Line Region ◽  
The Masses ◽  
Black Hole Masses

Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) was designed to conduct a blind search for AGN-driven outflows on X-ray-selected AGNs at redshift z ∼ 2 with high (∼2 kpc) spatial resolution, and to correlate them with the properties of their host galaxy and central black hole. The main aims of this paper are: (a) to derive reliable estimates for the masses of the black holes and accretion rates for the Type-1 AGNs in this survey; and (b) to characterise the properties of the AGN-driven winds in the broad line region (BLR). Methods. We analysed rest-frame optical and UV spectra of 21 Type-1 AGNs. We used Hα, Hβ, and MgII line profiles to estimate the masses of the black holes. We used the blueshift of the CIV line profile to trace the presence of winds in the BLR. Results. We find that the Hα and Hβ line widths are strongly correlated, as is the line continuum luminosity at 5100 Å with Hα line luminosity, resulting in a well-defined correlation between black hole masses estimated from Hα and Hβ. Using these lines, we estimate that the black hole masses for our objects are in the range Log (MBH/M⊙) = 8.4–10.8 and are accreting at λEdd = 0.04–1.3. Furthermore, we confirm the well-known finding that the CIV line width does not correlate with the Balmer lines and the peak of the line profile is blueshifted with respect to the [OIII]-based systemic redshift. These findings support the idea that the CIV line is tracing outflowing gas in the BLR for which we estimated velocities up to ∼4700 km s−1. We confirm the strong dependence of the BLR wind velocity on the UV-to-X-ray continuum slope, the bolometric luminosity, and Eddington ratio. We infer BLR mass outflow rates in the range 0.005–3 M⊙ yr−1, revealing a correlation with the bolometric luminosity consistent with that observed for ionised winds in the narrow line region (NLR), and X-ray winds detected in local AGNs, and kinetic power ∼10−7 − 10−4 × LBol. The coupling efficiencies predicted by AGN-feedback models are much higher than the values reported for the BLR winds in the SUPER sample; although it should be noted that only a fraction of the energy injected by the AGN into the surrounding medium is expected to become kinetic power in the outflow. Finally, we find an anti-correlation between the equivalent width of the [OIII] line and the CIV velocity shift, and a positive correlation between this latter parameter and [OIII] outflow velocity. These findings, for the first time in an unbiased sample of AGNs at z ∼ 2, support a scenario where BLR winds are connected to galaxy-scale detected outflows, and are therefore capable of affecting the gas in the NLR located at kiloparsec scale distances.

scholarly journals Accurate AGN Black Hole Masses and the Scatter in the MBH–Lbulge Relationship

2009 ◽  
Vol 5 (S267) ◽  
pp. 203-203 ◽  
Author(s):  
C. Martin Gaskell
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Velocity Dispersion ◽  
High Luminosity ◽  
Lower Mass ◽  
Reverberation Mapping ◽  
The Masses ◽  
Black Hole Masses ◽  
The Continuum

AbstractA new empirical formulae is given for estimating the masses of black holes in AGNs from the Hβ velocity dispersion and the continuum luminosity at 5100 Å. It is calibrated to reverberation-mapping and stellar-dynamical estimates of black hole masses. The resulting mass estimates are as accurate as reverberation-mapping and stellar-dynamical estimates. The new mass estimates show that there is very little scatter in the MBH–Lbulge relationship for high-luminosity galaxies, and that the scatter increases substantially in lower-mass galaxies.

A Photoionization Method for Estimating Black Hole Masses in Quasars

2018 ◽  
Vol 14 (S342) ◽  
pp. 270-271
Author(s):  
C. Alenka Negrete ◽  
Deborah Dultzin ◽  
Paola Marziani ◽  
Jack W. Sulentic ◽  
M. L. Martínez-Aldama
Keyword(s):  
Black Hole ◽  
High Redshift ◽  
Broad Line ◽  
Reverberation Mapping ◽  
Physical Conditions ◽  
Broad Line Region ◽  
Supermassive Black Hole ◽  
Line Region ◽  
Black Hole Masses

AbstractWe present a method that uses photoionization codes (CLOUDY) to estimate the supermassive black hole masses (MBH) for quasars at low and high redshift. This method is based on the determination of the physical conditions of the broad line region (BLR) using observational diagnostic diagrams from line ratios in the UV. We also considered that the density and metallicity of the BLR in quasars at high z could be different from those at the nearby Universe. The computed black hole masses obtained using this method are in agreement with those derived from the method of reverberation mapping.

scholarly journals New Reverberation Mapping Results from the Lick AGN Monitoring Project

2009 ◽  
Vol 5 (S267) ◽  
pp. 197-197
Author(s):  
Misty C. Bentz ◽  
Keyword(s):  
Black Hole ◽  
Reverberation Mapping ◽  
Scaling Relationships ◽  
Mapping Experiment ◽  
The Masses ◽  
Black Hole Masses

AbstractEight new black hole masses have been derived from a recent reverberation-mapping experiment carried out at Lick Observatory. The masses lie in the range ~ 106–107M⊙ and will allow us to extend the low end of AGN scaling relationships by a factor of ~10.

scholarly journals Black hole masses from X-rays

2012 ◽  
Vol 8 (S290) ◽  
pp. 371-372
Author(s):  
Xin-Lin Zhou ◽  
Roberto Soria
Keyword(s):  
Black Hole ◽  
X Rays ◽  
X Ray ◽  
Reverberation Mapping ◽  
Photon Index ◽  
Bolometric Correction ◽  
Black Hole Masses ◽  
Intrinsic Scatter

AbstractWe discuss two methods to estimate black hole (BH) masses using X-ray data only: from the X-ray variability amplitude and from the photon index Γ. The first method is based on the anti-correlation between BH mass and X-ray variability amplitude. Using a sample of AGN with BH masses from reverberation mapping, we show that this method shows small intrinsic scatter. The second method is based on the correlation between Γ and both the Eddington ratio Lbol/LEdd and the bolometric correction Lbol/L2−10keV.

scholarly journals Reverberation Mapping Measurements of Black Hole Masses and Broad-line Region Kinematics in Mrk 817 and NGC 7469

2021 ◽  
Vol 918 (2) ◽  
pp. 50
Author(s):  
Kai-Xing Lu ◽  
Jian-Guo Wang ◽  
Zhi-Xiang Zhang ◽  
Ying-Ke Huang ◽  
Liang Xu ◽  
...  
Keyword(s):  
Black Hole ◽  
Broad Line ◽  
Reverberation Mapping ◽  
Broad Line Region ◽  
Line Region ◽  
Black Hole Masses ◽  
Ngc 7469

Quasar black hole masses and accretion rates across cosmic time

2019 ◽  
Vol 15 (S359) ◽  
pp. 57-61
Author(s):  
Michael Brotherton ◽  
Jaya Maithil ◽  
Adam Myers ◽  
Ohad Shemmer ◽  
Brandon Matthews ◽  
...  
Keyword(s):  
Black Hole ◽  
High Redshift ◽  
Cosmic Time ◽  
Small Samples ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Reverberation Mapping ◽  
Scaling Relationships ◽  
Accretion Rates ◽  
Black Hole Masses

AbstractQuasar black hole masses are most commonly estimated using broad emission lines in single epoch spectra based on scaling relationships determined from reverberation mapping of small samples of low-redshift objects. Several effects have been identified requiring modifications to these scaling relationships, resulting in significant reductions of the black hole mass determinations at high redshift. Correcting these systematic biases is critical to understanding the relationships among black hole and host galaxy properties. We are completing a program using the Gemini North telescope, called the Gemini North Infrared Spectrograph (GNIRS) Distant Quasar Survey (DQS), that has produced rest-frame optical spectra of about 200 high-redshift quasars (z = 1.5–3.5). The GNIRS-DQS will produce new and improved ultraviolet-based black hole mass and accretion rate prescriptions, as well as new redshift prescriptions for velocity zero points of high-z quasars, necessary to measure feedback.

Recent results of measuring black hole masses via reverberation mapping

2019 ◽  
Vol 15 (S356) ◽  
pp. 116-121
Author(s):  
Shai Kaspi
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Line Emission ◽  
Galactic Nuclei ◽  
Continuum Emission ◽  
Mapping Technique ◽  
Reverberation Mapping ◽  
Line Region ◽  
Almost All ◽  
Black Hole Masses

AbstractOver the past three decades more than 100 Active Galactic Nuclei (AGNs) were measured using the reverberation mapping technique. This technique uses the response of the line emission in the Broad Line Region (BLR) to continuum emission variation and yields a measure for the distance of the BLR from the central Black Hole (BH). This in turn is used to measure the BH’s mass. Almost all of these measurements are of low-luminosity AGNs while for quasars with luminosities higher than 1046 rg s−1 there are hardly any attempts of reverberation mapping. This contribution reports on recent results from a two-decades campaigns to measure the BH mass in high-luminosity quasars using the reverberation mapping technique. BLR distance from the BH, BH mass, and AGN UV luminosity relations over eight orders of magnitude in luminosity are presented, pushing the luminosity limit to the highest point so far.

scholarly journals Tidal disruption events in galactic centers

2013 ◽  
Vol 9 (S303) ◽  
pp. 427-428
Author(s):  
Resha Parajuli ◽  
Dieter H. Hartmann
Keyword(s):  
Black Holes ◽  
Stellar Dynamics ◽  
Close Correlation ◽  
Host Galaxy ◽  
Causal Process ◽  
Reverberation Mapping ◽  
Energy And Momentum ◽  
Coevolution Process ◽  
The Masses ◽  
Tight Correlation

Supermassive black holes (106–109 M⊙) are now known to be present at the centers of most galaxies, but they are also found to have a close correlation with the host galaxy they live in. The masses of the supermasssive black holes (SMBHs) have been rigorously calculated using stellar dynamics (e.g., Gillessen et al. 2009) for the Milky Way, gas dynamics (e.g., Davis et al. 2013) for NGC 4526, water maser emissions, reverberation mapping, etc. In comparison, the mass of the SMBH seems to be tightly correlated with the galactic bulge it resides in. The tight correlation between the mass of the BH and the velocity dispersion of the stars in the bulge, known as the M-σ relation, (Ferrarese & Merritt, 2000; Tremaine et al. 2002), and the 2:1000 mass of BH - mass of bulge ratio suggests some sort of co-evolution process. A feedback driven coevolution process would suggest that the BH directly controls galaxy properties via energy and momentum feedback (Kormendy & Ho, 2013). However, since correlation does not necessarily imply causation, the evolution may be a non-causal process that occurs in tandem, where the BH and bulge grow independently. In such a process, star formation in the bulge and growth of SMBH occur in separate periods and are self regulating (Cen, 2012).

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