scholarly journals M94 as a Unique Testbed for Black Hole Mass Estimates and AGN Activity at Low Luminosities

2012 ◽  
Vol 2012 ◽  
pp. 1-14 ◽  
Author(s):  
Anca Constantin ◽  
Anil C. Seth
Keyword(s):  
Black Hole ◽  
Mass Measurement ◽  
Broad Line ◽  
Black Hole Mass ◽  
Multiple Sources ◽  
X Ray ◽  
Line Region ◽  
High Ionization ◽  
Ir Emission

We discuss the peculiar nature of the nucleus of M94 (NGC 4736) in the context of new measurements of the broadHαemission fromHST-STIS observations. We show that this component is unambiguously associated with the high-resolution X-ray, radio, and variable UV sources detected at the optical nucleus of this galaxy. These multiwavelength observations suggest that NGC 4736 is one of the least luminous broad-line (type 1) LINERs, withLbol=2.5×1040 erg s-1. This LINER galaxy has also possibly the least luminous broad-line region known (LHα=2.2×1037 erg s-1). We compare black hole mass estimates of this system to the recently measured∼7×106 M⨀dynamical black hole mass measurement. The fundamental plane andM-σ*relationship roughly agree with the measured black hole mass, while other accretion-based estimates (theM-FWHM(Hα)relation, empirical correlation of BH mass with high-ionization mid-IR emission lines, and the X-ray excess variance) provide much lower estimates (∼105 M⨀). An energy budget test shows that the AGN in this system may be deficient in ionizing radiation relative to the observed emission-line activity. This deficiency may result from source variability or the superposition of multiple sources including supernovae.

scholarly journals Exploring the diversity of Type 1 active galactic nuclei identified in SDSS-IV/SPIDERS

2020 ◽  
Vol 492 (3) ◽  
pp. 3580-3601 ◽  
Author(s):  
Julien Wolf ◽  
Mara Salvato ◽  
Damien Coffey ◽  
Andrea Merloni ◽  
Johannes Buchner ◽  
...  
Keyword(s):  
Black Hole ◽  
Optical Properties ◽  
Continuum Emission ◽  
High Signal ◽  
Broad Line ◽  
Black Hole Mass ◽  
X Ray ◽  
Broad Line Region ◽  
Line Region

ABSTRACT We present a statistical analysis of the optical properties of an X-ray-selected Type 1 active galactic nucleus (AGN) sample, using high signal-to-noise ratio (S/N>20) spectra of the counterparts of the ROSAT/2RXS sources in the footprint of the SDSS-IV/SPIDERS (Spectroscopic IDentification of eROSITA Sources) programme. The final sample contains 2100 sources. It significantly extends the redshift and luminosity ranges (z ∼ 0.01–0.80 and $L_{\rm 0.1\!-\!2.4 \, keV} \sim \rm 2.0 \times 10^{41}\!-\!1.0 \times 10^{46} \, \, erg \, s^{-1}$) used so far in this kind of analysis. By means of a principal component analysis, we derive eigenvector (EV) 1 and 2 in an eleven-dimensional optical and X-ray parameter space, which are consistent with previous results. The validity of the correlations of the Eddington ratio L/LEdd with EV1 and the black hole mass with EV2 is strongly confirmed. These results imply that L/LEdd and black hole mass are related to the diversity of the optical properties of Type 1 AGNs. Investigating the relation of the width and asymmetry of H β and the relative strength of the iron emission $r_{\rm Fe\, \small{II}}$, we show that our analysis supports the presence of a distinct kinematic region: the very broad line region. Furthermore, comparing sources with a red-asymmetric broad H β emission line to sources for which it is blue asymmetric, we find an intriguing difference in the correlation of the $\rm Fe\, \small{II}$ and the continuum emission strengths. We show that this contrasting behaviour is consistent with a flattened, stratified model of the broad-line region, in which the $\rm Fe\, \small{II}$-emitting region is shielded from the central source.

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}}$5) and ≈0.19 (r > 0${_{.}^{\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.

scholarly journals AGN orientation through the spectroscopic correlations and model of dusty cone shell

2021 ◽  
Author(s):  
M Lakićević ◽  
J Kovačević-Dojčinović ◽  
L Č Popović
Keyword(s):  
Black Hole ◽  
Spectral Properties ◽  
Alternative Explanation ◽  
Selection Effect ◽  
Broad Line ◽  
Black Hole Mass ◽  
Cone Model ◽  
Line Region ◽  
Inclination Angles ◽  
Dust Distribution

Abstract The differences between Narrow Line Seyfert 1 galaxies (NLS1s) and Broad Line AGNs (BLAGNs) are not completely understood; it is thought that they may have different inclinations and/or physical characteristics. The FWHM(Hβ)–luminosities correlations are found for NLS1s and their origin is the matter of debate. Here we investigated the spectroscopic parameters and their correlations considering a dusty, cone model of AGN. We apply a simple conical dust distribution (spreading out of broad line region, BLR), assuming that the observed surface of the model is in a good correlation with MIR emission. The dusty cone model in combination with a BLR provides the possibility to estimate luminosity dependence on the cone inclination. The FWHM(Hβ)–luminosities correlations obtained from model in comparison with observational data show similarities which may indicate the influence of AGN inclination and structure to this correlation. An alternative explanation for FWHM(Hβ)–luminosities correlations is the selection effect by the black hole mass. These FWHM(Hβ)–luminosities correlations may be related to the starburst in AGNs, as well. The distinction between spectral properties of the NLS1s and BLAGNs could be caused by multiple effects: beside physical differencies between NLS1s and BLAGNs (NLS1s have lighter black hole mass than BLAGNs), inclination of the conical AGN geometry may have important role as well, where NLS1s may be seen in lower inclination angles.

scholarly journals Modelling photometric reverberation data: a disk-like broad-line region and a potentially larger black hole mass for 3C 120

2014 ◽  
Vol 568 ◽  
pp. A36 ◽  
Author(s):  
F. Pozo Nuñez ◽  
M. Haas ◽  
M. Ramolla ◽  
C. Bruckmann ◽  
C. Westhues ◽  
...  
Keyword(s):  
Black Hole ◽  
Broad Line ◽  
Black Hole Mass ◽  
Broad Line Region ◽  
Line Region ◽  
3C 120

scholarly journals Broad spectral lines in AGNs and supermassive black hole mass measurements

2020 ◽  
Vol 29 (1) ◽  
pp. 1-14 ◽  
Author(s):  
Luka Č. Popović
Keyword(s):  
Mass Measurement ◽  
Spectral Lines ◽  
Complex Task ◽  
Black Hole Mass ◽  
Mass Measurements ◽  
X Ray ◽  
Supermassive Black Hole ◽  
Broad Emission ◽  
Absorbing Material

AbstractThe mass measurement of supermassive black holes (SMBHs) is a very complex task. Between several methods for SMBH mass measurements, some of them use the spectral lines, which indicate the motion of the emitting/absorbing material around an SMBH. Mostly, there is an assumption of virialization of line emitting gas in the region which is close to the central SMBH. In this paper we will give an overview of methods for the SMBH mass measurements using broad emission spectral lines observed in Type 1 AGNs. First we give the basic idea to use the parameters of broad lines to SMBH mass measurements. After that we give an overview of broad lines from X-ray (Fe kα) to the IR (Pashen and Brecket lines) which have been used for SMBH mass estimates. Additionally, we describe and discuss a new method for SMBH mass measurements using the polarization in the broad lines emitted from Type 1 AGNs.

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 Broad line region and black hole mass of PKS 1510-089 from spectroscopic reverberation mapping

2020 ◽  
Vol 642 ◽  
pp. A59
Author(s):  
Suvendu Rakshit
Keyword(s):  
Black Hole ◽  
Root Mean Square ◽  
Thermal Emission ◽  
Light Curves ◽  
Broad Line ◽  
Mean Square ◽  
Black Hole Mass ◽  
Broad Line Region ◽  
Line Region ◽  
The Continuum

Reverberation results of the flat spectrum radio quasar PKS 1510-089 from 8.5 years of spectroscopic monitoring carried out at Steward Observatory over nine observing seasons between December 2008 and June 2017 are presented. Optical spectra show strong Hβ, Hγ, and Fe II emission lines overlying on a blue continuum. All the continuum and emission line light curves show significant variability with fractional root-mean-square variations of 37.30 ± 0.06% (f5100), 11.88 ± 0.29% (Hβ), and 9.61 ± 0.71% (Hγ); however, along with thermal radiation from the accretion disk, non-thermal emission from the jet also contributes to f5100. Several methods of time series analysis (ICCF, DCF, von Neumann, Bartels, JAVELIN, χ2) are used to measure the lag between the continuum and line light curves. The observed frame broad line region size is found to be 61.1−3.2+4.0 (64.7−10.6+27.1) light-days for Hβ (Hγ). Using the σline of 1262 ± 247 km s−1 measured from the root-mean-square spectrum, the black hole mass of PKS 1510-089 is estimated to be 5.71−0.58+0.62 × 107 M⊙.

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 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
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