Reverberation mapping of active galactic nuclei

By B. Peterson, K. Horne. 2004

662 citations recorded by the source corpus.

Reverberation mapping is a proven technique that is used to measure the size of the broad emission-line region and central black hole mass in active galactic nuclei. More ambitious reverberation mapping programs that are well within the capabilities of Hubble Space Telescope could allow us to determine the nature and flow of line-emitting gas in active nuclei and to assess accurately the systematic uncertainties in reverberation-based black hole mass measurements.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fa0033fcb35a2d311b5bc43359bbf7f30cca13d4

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Citations in the corpus

Reverberation Mapping of High-Luminosity Quasars: First Results (2006, methodology): “The technique uses the light-travel time-delayed flux response of the BLR to changes in the continuum flux (for reviews, see Peterson 1993, 2006; Netzer & Peterson 1997, and references therein).”
X-ray reverberation around accreting black holes (2014, methodology): “Optical reverberation studies of AGN use time-domain techniques to measure time-lags, specifically the cross-correlation function (e.g. Peterson 1993; Peterson et al. 2004; Bentz et al. 2009; Denney et al. 2010).”
COMPARING SINGLE-EPOCH VIRIAL BLACK HOLE MASS ESTIMATORS FOR LUMINOUS QUASARS (2012, methodology): “Over the past several decades, reverberation mapping (RM, e.g., Bahcall et al. 1972; Blandford & McKee 1982; Peterson 1993) has proven to be a viable technique to measure (broad-line) AGN BH mass by providing an estimate of the broad line region (BLR) sizeR (e.g., Peterson et al. 2004), combined…”
THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: TECHNICAL OVERVIEW (2014, methodology): “Reverberation mapping (RM) is a technique for studying the structure and kinematics of the broad-line regions (BLRs) of active galactic nuclei (AGNs) and quasars (e.g., Blandford & McKee 1982; Peterson 1993, 2014).”
Modelling reverberation mapping data – II. Dynamical modelling of the Lick AGN Monitoring Project 2008 data set (2013, methodology): “The geometry and dynamics of the BLR can be further constrained by reverberation mapping measurements, where changes in the AGN continuum emission are monitored alongside the echo of these same changes in the BLR emission lines (Blandford & McKee 1982; Peterson 1993; Peterson et al. 2004).”
Broad Emission-Line Shifts in Quasars: An Orientation Measure for Radio-Quiet Quasars? (2002, background): “…1) that the BELR region is stratified in ionization, specifically that the low-ionization region is located farther from the continuum source than the high-ionization region (Peterson 1993), but see O’Brien et al. (1998); and 2) that an optically thick accretion disk is interior to both regions.”
Simultaneous X-ray/optical/UV snapshots of active galactic nuclei from XMM–Newton: spectral energy distributions for the reverberation mapped sample (2008, methodology): “The foundations and assumptions behind the technique are discussed in detail in the review of Peterson & Horne (2004), but the essence of the approach involves monitoring the response of optical broad line fluxes from the BLR to variations in the underlying (UV) continuum flux.”
Active Galactic Nucleus Black Hole Masses and Bolometric Luminosities (2002, methodology): “The reverberation mapping technique utilizes the time lag between continuum and emission lines to derive the distance of the BLR from the black hole (Blandford & McKee 1982; Peterson 1993).”
AN ALTERNATIVE APPROACH TO MEASURING REVERBERATION LAGS IN ACTIVE GALACTIC NUCLEI (2010, background): “Three outliers from the CCF RBLR–”
THE LICK AGN MONITORING PROJECT: BROAD-LINE REGION RADII AND BLACK HOLE MASSES FROM REVERBERATION MAPPING OF Hβ (2009, methodology): “…is used as a reliable method for detecting AGNs in surveys (e.g., van den Bergh et al. 1973; Heckman 1976; Véron & Hawkins 1995), and it is the fundamental basis upon which rests the technique of measuring black hole masses known as reverberation mapping (Blandford & McKee 1982; Peterson 1993).”
THE STRUCTURE OF THE BROAD-LINE REGION IN ACTIVE GALACTIC NUCLEI. I. RECONSTRUCTED VELOCITY-DELAY MAPS (2012, methodology): “Reverberation techniques use the time variability observed in the AGN continuum emission and the subsequent response of the gas in the BLR (Blandford & McKee 1982; Peterson 1993).”
REVERBERATION MAPPING MEASUREMENTS OF BLACK HOLE MASSES IN SIX LOCAL SEYFERT GALAXIES (2010, methodology): “The technique of reverberation mapping (Blandford & McKee 1982; Peterson 1993) has been used to directly measure black hole masses in relatively local broad-line (Type 1) AGNs for over two decades (see compilation by Peterson et al. 2004).”
Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research (2004, methodology): “In its current application, reverberation mapping (§ 8.3) targets the Broad Line Region (BLR) of Type 1 AGNs (Blandford & McKee 1982; Peterson 1993; Peterson 2002).”
A systematic search for changing-look quasars in SDSS (2015, background): “…Schmidt et al. 2012; Ruan et al. 2014), the broad emission lines (BELs) seen in quasar spectra are usually less variable and lagged with respect to the continuum, as seen in reverberation mapping studies (e.g., Clavel et al. 1991; Peterson 1993; Grier et al. 2012; Peterson 2014; Shen et al. 2015).”
REVERBERATION MAPPING RESULTS FOR FIVE SEYFERT 1 GALAXIES (2012, methodology): “…BH sphere of influence is much too small to be resolvable – 3 – in any but the nearest galaxies, the only direct method of measuring MBH in distant galaxies is reverberation mapping (Blandford & McKee 1982; Peterson 1993), which is applicable to Type 1, or broad-line, active galactic nuclei (AGNs).”
Metallicities and Abundance Ratios from Quasar Broad Emission Lines (2001, background): “However, more recent line variability studies (Peterson 1993, Goad, O’Brien & Gondhalekar 1993, Ferland et al. 1992, Reichert et al. 1994, Korista et al. 1995, Peterson & Wandel 1999, Kaspi & Netzer 1999) indicate that the BELR is spatially stratified with, quite likely, a wide range of densities.”