The Lick Agn Monitoring Project 2011: Reverberation Mapping of Markarian 50

Barth, Aaron J.; Pancoast, Anna; Thorman, Shawn J.; Bennert, Vardha N.; Sand, David J.; Li, Weidong; Canalizo, Gabriela; Filippenko, A. V.; Gates, E. L.; Greene, Jenny E.; Malkan, Matthew A.; Stern, Daniel; Treu, Tommaso; Woo, J. H.; Assef, Roberto J.; Bae, Hyun‐Jin; Brewer, Brendon J.; Buehler, Tabitha; Cenko, S. Bradley; Clubb, K. I.; Cooper, Michael C.; Diamond‐Stanic, Aleksandar M.; Hiner, Kyle D.; Hönig, S. F.; Joner, M. D.; Kandrashoff, M. T.; Laney, C. D.; Lazarova, Mariana; Nierenberg, Anna; Park, Dawoo; Silverman, J. M.; Son, Donghoon; Sonnenfeld, Alessandro; Tollerud, Erik; Walsh, Jonelle L.; Walters, Richard; Silva, Robert L. da; Fumagalli, Michele; Gregg, Michael D.; Harris, Chelsea E.; Hsiao, E. Y.; Lee, Jeffrey; Lopez, Liliana; Rex, J.; Suzuki, N.; Trump, Jonathan R.; Tytler, David; Worseck, G.; Yesuf, Hassen M.

doi:10.1088/2041-8205/743/1/l4

Cited by 101 publications

(92 citation statements)

References 39 publications

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“…The average gas velocity is inferred from the emission-line width. The BLR size has been measured only for ∼50 active galaxies using reverberation mapping (e.g., Peterson et al 2004;Bentz et al 2009bBentz et al , 2013Denney et al 2010;Barth et al 2011), in which the time lag between continuum and BLR variability establishes a size scale for the BLR. In general, the geometry of the BLR (and the proportionality constant) is not known, and so the virial product alone (RΔV 2 /G) does not establish the absolute BH mass.…”

Section: Black Hole Massesmentioning

confidence: 99%

“…The virial BH mass measurements for the broad-line AGN candidates are obviously extremely indirect, and are subject to a number of systematic uncertainties. 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. Whether the geometry depends on fundamental parameters of the BH remains uncertain (Collin et al 2006).…”

Section: Black Hole Massesmentioning

confidence: 99%

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Dwarf Galaxies With Optical Signatures of Active Massive Black Holes

Reines

Greene

Geha

2013

ApJ

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498

829

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We present a sample of 151 dwarf galaxies (10 8.5 M 10 9.5 M ) that exhibit optical spectroscopic signatures of accreting massive black holes (BHs), increasing the number of known active galaxies in this stellar-mass range by more than an order of magnitude. Utilizing data from the Sloan Digital Sky Survey Data Release 8 and stellar masses from the NASA-Sloan Atlas, we have systematically searched for active BHs in ∼25,000 emission-line galaxies with stellar masses comparable to the Magellanic Clouds and redshifts z < 0.055. Using the narrow-line [O iii]/Hβ versus [N ii]/Hα diagnostic diagram, we find photoionization signatures of BH accretion in 136 galaxies, a small fraction of which also exhibit broad Hα emission. For these broad-line active galactic nucleus (AGN) candidates, we estimate BH masses using standard virial techniques and find a range of 10 5 M BH 10 6 M and a median of M BH ∼ 2 × 10 5 M . We also detect broad Hα in 15 galaxies that have narrow-line ratios consistent with star-forming galaxies. Follow-up observations are required to determine if these are true type 1 AGN or if the broad Hα is from stellar processes. The median absolute magnitude of the host galaxies in our active sample is M g = −18.1 mag, which is ∼1-2 mag fainter than previous samples of AGN hosts with low-mass BHs. This work constrains the smallest galaxies that can form a massive BH, with implications for BH feedback in low-mass galaxies and the origin of the first supermassive BH seeds.

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Section: Black Hole Massesmentioning

confidence: 99%

Section: Black Hole Massesmentioning

confidence: 99%

Dwarf Galaxies With Optical Signatures of Active Massive Black Holes

Reines

Greene

Geha

2013

ApJ

Self Cite

498

829

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“…However, several groups (e.g., Barth et al 2011b;Park et al 2012;Barth et al 2013;Hu et al 2015) have developed methods to isolate various components of the AGN spectrum, allowing for the disentanglement of various broad emission line features from the rest of the AGN, such as the host galaxy starlight, Fe ii features and various other species that often blend with the emission lines we are investigating. The recent success with isolating these different components of the AGN spectrum allows one to measure light curves for various AGN components despite strong starlight and blending (Barth et al 2011b;Barth et al 2013). As a result, the spectral decomposition methods have been continually improved and implemented in RM spectra (Park et al 2012;Barth et al 2015).…”

Section: Spectral Decompositonmentioning

confidence: 99%

“…However, with sufficiently high-quality RM data, we can actually resolve the time delays in velocity space and thus recover information about the possible phase space structure within the BLR. This velocityresolved analysis has been successfully done for several sets of data in recent years Denney et al 2010;Barth et al 2011b;Barth et al 2011a;Doroshenko et al 2012;Grier et al 2013b;De Rosa et al 2015;Du et al 2016;Pei et al 2017). In most cases, we see signatures of either gas in bound elliptical orbits or inflowing gas, although signatures of outflowing gas have also been seen (Denney et al 2009;Du et al 2016).…”

Section: Introductionmentioning

confidence: 99%

The Structure of the Broad-line Region in Active Galactic Nuclei. II. Dynamical Modeling of Data From the AGN10 Reverberation Mapping Campaign

Grier

Pancoast

Barth

et al. 2017

ApJ

138

171

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We present inferences on the geometry and kinematics of the broad-Hβ line-emitting region in four active galactic nuclei monitored as a part of the fall 2010 reverberation mapping campaign at MDM Observatory led by the Ohio State University. From modeling the continuum variability and response in emission-line profile changes as a function of time, we infer the geometry of the Hβ-emitting broad line regions to be thick disks that are close to face-on to the observer with kinematics that are well-described by either elliptical orbits or inflowing gas. We measure the black hole mass to be log 10 (M BH ) = 7.25 −0.23 for PG 2130+099. These black hole mass measurements are not based on a particular assumed value of the virial scale factor f , allowing us to compute individual f factors for each target. Our results nearly double the number of targets that have been modeled in this manner, and investigate the properties of a more diverse sample by including previously modeled objects. We measure an average scale factor f in the entire sample to be log 10f = 0.54 ± 0.17 when the line dispersion is used to characterize the line width, which is consistent with values derived using the normalization of the M BH -σ relation. We find that the scale factor f for individual targets is likely correlated with the black hole mass, inclination angle, and opening angle of the broad line region but we do not find any correlation with the luminosity.

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“…The new targets have been selected from recent RM programs. These include Arp 151, Mrk 1310, NGC 6814, and SBS 1116+583A from the Lick AGN Monitoring Project 2008 campaign (Bentz et al 2009b;Park et al 2012b), Mrk 50 from the Lick AGN Monitoring Project 2011 campaign (Barth et al 2011b), and the Kepler-field AGN Zw 229-015 (Barth et al 2011a). Table 1 summarizes the properties of the P13 AGN sample and the six new objects presented in this work.…”

Section: Sample Hst Observations and Data Reductionmentioning

confidence: 99%

Extending the Calibration of C iv-based Single-epoch Black Hole Mass Estimators for Active Galactic Nuclei*

Park

Barth

Woo

et al. 2017

ApJ

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We provide an updated calibration of C IV λ1549 broad emission line-based single-epoch (SE) black hole (BH) mass estimators for active galactic nuclei (AGNs) using new data for six reverberation-mapped AGNs at redshift z = 0.005 − 0.028 with BH masses (bolometric luminosities) in the range 10 6.5 -10 7.5 M (10 41.7 -10 43.8 erg s −1 ). New rest-frame UV-to-optical spectra covering 1150-5700 Å for the six AGNs were obtained with the Hubble Space Telescope (HST). Multi-component spectral decompositions of the HST spectra were used to measure SE emission-line widths for the C IV, Mg II, and Hβ lines as well as continuum luminosities in the spectral region around each line. We combine the new data with similar measurements for a previous archival sample of 25 AGNs to derive the most consistent and accurate calibrations of the C IV-based SE BH mass estimators against the Hβ reverberation-based masses, using three different measures of broad-line width: full-width at half maximum (FWHM), line dispersion (σ line ) and mean absolute deviation (MAD). The newly expanded sample at redshift z = 0.005 − 0.234 covers a dynamic range in BH mass (bolometric luminosity) of log M BH /M = 6.5 − 9.1 (log L bol /erg s −1 = 41.7 − 46.9), and we derive the new C IV-based mass estimators using a Bayesian linear regression analysis over this range. We generally recommend the use of σ line or MAD rather than FWHM to obtain a less biased velocity measurement of the C IV emission line, because its narrowline component contribution is difficult to decompose from the broad-line profile.

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The Lick Agn Monitoring Project 2011: Reverberation Mapping of Markarian 50

Cited by 101 publications

References 39 publications

Dwarf Galaxies With Optical Signatures of Active Massive Black Holes

Dwarf Galaxies With Optical Signatures of Active Massive Black Holes

The Structure of the Broad-line Region in Active Galactic Nuclei. II. Dynamical Modeling of Data From the AGN10 Reverberation Mapping Campaign

Extending the Calibration of C iv-based Single-epoch Black Hole Mass Estimators for Active Galactic Nuclei*

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