Accretion disk wind in the AGN broad-line region: Spectroscopically resolved line profile variations in Mrk 110 ?

By W. Kollatschny. 2003

141 citations recorded by the source corpus.

Detailed line profile variability studies of the narrow line Seyfert 1 galaxy Mrk 110 are presented. We obtained the spectra in a variability campaign carried out with the 9.2 m Hobby-Eberly Telescope at McDonald Observatory. The integrated Balmer and helium (He i, ii) emission lines are delayed by 3 to 33 light days to the optical continuum variations respectively. The outer wings of the line profiles respond much faster to continuum variations than the central regions. The comparison of the observed profile variations with model calculations of different velocity fields indicates an accretion disk structure of the broad line emitting region in Mrk 110. Comparing the velocity-delay maps of the different emission lines among each other a clear radial stratification in the BLR can be recognized. Furthermore, delays of the red line wings are slightly shorter than those of the blue wings. This indicates an accretion disk wind in the BLR of Mrk 110. We determine a central black hole mass of $M = 1.8\times 10^{7}~M_{\odot}$. Because of the poorly known inclination angle of the accretion disk this is a lower limit only.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6fffb129ebae2ac1719226645649dab037e63697

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

THE LOW-LUMINOSITY END OF THE RADIUS–LUMINOSITY RELATIONSHIP FOR ACTIVE GALACTIC NUCLEI (2013, background): “A subset of objects in the reverberation sample have measurements for several different emission lines throughout the ultraviolet and optical portions of their spectra, and the multiple emission lines show a virial behavior (e.g., Peterson & Wandel 1999, 2000; Kollatschny 2003; Bentz et al. 2010).”
THE LICK AGN MONITORING PROJECT: BROAD-LINE REGION RADII AND BLACK HOLE MASSES FROM REVERBERATION MAPPING OF Hβ (2009, background): “The existence of a “virial” relationship between time lag and line width,v ∝ τ−0.5, has been clearly shown in NGC 5548 (Peterson & Wandel 1999), and has been in seen in numerous other objects (Peterson et al. 2000; Onken & Peterson 2002; Kollatschny 2003), upholding this basic assumption.”
Systematic effects in measurement of black hole masses by emission-line reverberation of active galactic nuclei: Eddington ratio and inclination (2006, background): “In the case of Mrk 110, Kollatschny (2003b) showed that the variable part of the broad lines of this bright NLS1 nucleus are redshifted with respect to the systemic velocity, from which he deduced a “gravitational mass” of 1.4 × 108 M , larger than the “isotropic” reverberation mass by almost one…”
Reverberation mapping of active galactic nuclei (2004, background): “The Keplerian taper of the map is seen, but other possible structure is only hinted at, as it is in other attempt to recover a velocity-delay map from real data (e.g., Wanders et al. 1995; Done & Krolik 1996; Kollatschny 2003).”
THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: TECHNICAL OVERVIEW (2014, result): “The observed relationship between time delay and velocity width for multiple emission lines in the same source is apparently consistent with this hypothesis28 (Peterson & Wandel 1999, 2000; Kollatschny 2003; Peterson et al. 2004; Bentz et al. 2010a).”
THE LICK AGN MONITORING PROJECT: REVERBERATION MAPPING OF OPTICAL HYDROGEN AND HELIUM RECOMBINATION LINES (2010, background): “Several additional AGNs have since been shown to exhibit virial behavior of their broad emission lines as well, such as NGC 3738 (Onken & Peterson 2002) and Mrk 110 (Kollatschny 2003).”
A New Sample of Low-Mass Black Holes in Active Galaxies (2007, background): “We are hopeful that an increased sample of reverberation-mappedsources (e.g., Kollatschny 2003), combined with an increase in the number of measuredσ∗ measurements in AGNs, will decrease the outstanding systematic errors in these masses in the near future.”
Central Masses and Broad-Line Region Sizes of Active Galactic Nuclei. II. A Homogeneous Analysis of a Large Reverberation-Mapping Database (2004, background): “The justification for this assumption is simply that a virial relationship between time delay and line width has already been established for several objects (Peterson & Wandel 1999, 2000; Onken & Peterson 2002; Kollatschny 2003).”
A Reverberation-based Mass for the Central Black Hole in NGC 4151 (2006, background): “In fact, this relationship has been found in NGC 5548 (Peterson & Wandel 1999) as well as a handful of other objects (Peterson et al. 2000; Onken & Peterson 2002; Kollatschny 2003).”
Measuring the Masses of Supermassive Black Holes (2014, methodology): “There were early attempts to recover velocity– delay maps (e.g., Ulrich & Horne 1996; Wanders et al. 1997; Kollatschny 2003a); these revealed some structure, but little detail.”
DWARF GALAXIES WITH OPTICAL SIGNATURES OF ACTIVE MASSIVE BLACK HOLES (2013, background): “For one thing, the BLR geometry clearly varies considerably from object to object (Kollatschny 2003; Bentz et al. 2009b; Denney et al. 2010; Barth et al. 2011), making a single geometric scaling factor suspect.”
The origin of the broad line region in active galactic nuclei (2010, background): “…of sight towards the nucleus; (ii) the medium is predominantly in Keplerian motion with additional velocity components (e.g., Done & Krolik 1996; Kollatschny 2003; Collin et al. 2006); (iii) the outer edge of the BLR is delineated the dusty/molecular torus (Netzer & Laor 1993, Suganuma et al.…”
What broad emission lines tell us about how active galactic nuclei work (2009, background): “Kollatschny (2003) found marginal evidence for some outflow in Mrk 110, and Denney et al. (2009b) have found a clearer signature of an apparent outflow component in velocity-resolved reverberation mapping of NGC 3227.”
Supermassive Black Holes in Active Galactic Nuclei. II. Calibration of the Black Hole Mass-Velocity Dispersion Relationship for Active Galactic Nuclei (2004, background): “If the BLR is modeled as a simple disk, then (MBH/f) Mgrav = sin2 i 2 ln 2 , (6) and the difference between these two measurements allows us to infer that i ≈ 30◦, slightly larger than the 21± 5 degrees found by Kollatschny (2003b).”
Evolution of broad-line emission from active galactic nuclei (2013, background): “From detailed line profile variability studies, Kollatschny (2003) finds evidence for an accretion disk wind in the BLR of the nar- row line Seyfert 1 Mrk 110.”
Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research (2004, background): “A radial flow would be reflected in a difference between the time lag measured for the blue and red wings of the line; such difference is generally not detected (e.g. Koratkar & Gaskell 1991; Wanders & Horne 1994; Wanders & Peterson 1996; O’Brien et al. 1998; Sergeev et al. 2002), although a mild ra”
RELATIONS BETWEEN CENTRAL BLACK HOLE MASS AND TOTAL GALAXY STELLAR MASS IN THE LOCAL UNIVERSE (2015, methodology): “While these parameters have been seen to vary from object to object (Kollatschny 2003; Bentz et al. 2009; Denney et al. 2010; Barth et al. 2011), a single scaling factor is generally adopted from calibrating the ensemble of reverberation-based BH masses to the MBH − σ⋆ relation (e.g., Gebhardt et…”