The Sloan Digital Sky Survey Reverberation Mapping Project: Initial C iv Lag Results from Four Years of Data

Grier, C. J.; Shen, Yue; Horne, K.; Brandt, W. N.; Trump, Jonathan R.; Hall, Patrick B.; Kinemuchi, Karen; Starkey, D.; Schneider, D.; Ho, Luis C.; Homayouni, Y.; Li, Jennifer I-Hsiu; McGreer, Ian D.; Peterson, Bradley M.; Bizyaev, Dmitry; Chen, Yuguang; Dawson, Kyle; Eftekharzadeh, Sarah; Guo, Yucheng; Jia, Siyao; Jiang, Linhua; Kneib, Jean-Paul; Li, Feng; Li, Zefeng; Nie, Jundan; Oravetz, Audrey; Oravetz, Daniel; Pan, Kaike; Petitjean, P.; Ponder, K. A.; Rogerson, Jesse; Vivek, M.; Zhang, Tianmen; Zou, Hu

doi:10.3847/1538-4357/ab4ea5

Cited by 101 publications

(126 citation statements)

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“…However, the RM technique requires long-term observational campaigns and is especially challenging at higher redshift (Kaspi et al 2000(Kaspi et al , 2007Peterson et al 2004;Bentz et al 2009;Denney et al 2010;Du et al 2014; Barth et al 2015;Shen et al 2015;Grier et al 2017Grier et al , 2019. A tight correlation between the BLR size (R) and the quasar continuum luminosity in optical bands has been revealed from the RM campaigns (Kaspi et al 2000(Kaspi et al , 2005Bentz et al 2013).…”

Section: Introductionmentioning

confidence: 99%

“…However, given the fact that before the Sloan Digital Sky Survey (SDSS) RM project (for a technical overview, see Shen et al 2015) the RM technique is mainly based on the Hβ emission line for the low-redshift AGN sample, the C IV emission line lacks direct calibrations from large samples. The most recently obtained C IV radius-luminosity relation based on the SDSS-RM project has raised the number of sources from ∼15 to ∼67 (Grier et al 2019). However, it is still controversial whether calibrations based on the overlap of the RM and the SE methods can reliably estimate the C IV-based BH masses for high-redshift luminous quasars (Shen et al 2008;Shen & Liu 2012;Park et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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C iv Emission-line Properties and Uncertainties in Black Hole Mass Estimates of z ∼ 3.5 Quasars

Zuo

Fan

et al. 2020

ApJ

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Using a high-luminosity (L bol ∼10 47.5-10 48.3 erg s −1), high-redshift (3.2<z<3.8) quasar sample of 19 quasars with optical and near-infrared spectroscopy, we investigate the reliability of the C IV-based black hole mass estimates (M BH). The median logarithm of the C IV-and Hβ-based M BH ratios is 0.110 dex, with a scatter of 0.647 dex. The C IV-to-Hβ BH mass differences are significantly correlated with the C IV FWHMs, blueshifts, and asymmetries. Corrections of the C IV FWHM using the blueshift and asymmetry reduce the scatter of the mass differences by ∼0.04-0.2 dex. Quasars in our sample accrete at the Eddington ratio R EDD >0.3 and cover a considerable range of blueshifts, with 18/19 of the quasars showing C IV blueshifts (with the median value of 1126 km s −1) and 14/19 of the quasars showing C IV blueshifts larger than 500 km s −1. It suggests that not all quasars with high Eddington ratios show large blueshifts. The Baldwin effect between the C IV rest-frame equivalent width (REW) and the continuum luminosity at 1350 Å is not seen, likely due to the limited luminosity range of our sample. We find a lack of flux in the red wing of the composite spectrum with larger C IV blueshift and detect a higher ratio of [O III] quasars with REW [O III] >5 Å in the subsample with lower C IV blueshift. It is more likely that they are caused by the combination of the Eddington ratio and the orientation effect.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

C iv Emission-line Properties and Uncertainties in Black Hole Mass Estimates of z ∼ 3.5 Quasars

Zuo

Fan

et al. 2020

ApJ

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“…There are many projects currently underway using these photometric data. The SDSS-RM team has been merging the Bok and CFHT data sets with the SDSS-BOSS spectra to analyze the various lags seen in the AGNs (see Grier et al 2017Grier et al , 2019. The photometry is also being used to measure interband continuum lags in quasars to learn about the accretion disk size (Homayouni et al 2019).…”

Section: Discussionmentioning

confidence: 99%

“…The SDSS-RM program has reported ∼100 additional broad-line lag measurements (Shen et al 2016b;Grier et al 2017Grier et al , 2019. In addition, the SDSS-RM collaboration has produced a wide variety of results using the first 1-4 yr of data, including studies of broad absorption-line variability, hostgalaxy properties, emission-line velocity shifts, and quasar variability (Grier et al 2015(Grier et al , 2017Matsuoka et al 2015;Shen et al 2015bShen et al , 2016aShen et al , 2016bSun et al 2015Sun et al , 2018Denney et al 2016aDenney et al , 2016bLi et al 2017;Yue et al 2018;Hemler et al 2019;Wang et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The Sloan Digital Sky Survey Reverberation Mapping Project: Photometric g and i Light Curves

Kinemuchi

McGreer

Kochanek

et al. 2020

ApJS

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The Sloan Digital Sky Survey (SDSS) Reverberation Mapping program monitors 849 active galactic nuclei (AGNs) both spectroscopically and photometrically. The photometric observations used in this work span over 4 yr and provide an excellent baseline for variability studies of these objects. We present the photometric light curves from 2014 to 2017 obtained by the Steward Observatory's Bok telescope and the Canada-France-Hawaii telescope with MegaCam. We provide details on the data acquisition and processing of the data from each telescope, the difference imaging photometry used to produce the light curves, and the calculation of a variability index to quantify each AGN's variability. We find that the Welch-Stetson J index provides a useful characterization of AGN variability and can be used to select AGNs for further study.

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“…From the relation between the radius of the BLR, RBLR, and the luminosity of the continuum at 5100Å given by McLure & Dunlop (2004), we can estimate that RBLR ∼ (2017) 800 light days at the distance where the H β is produced. If we use the relation between RBLR and the continuum luminosity at 1350Å given by Grier et al (2019), we obtain RBLR ∼ 700 light days for the C iv line. The large scatter affecting the above relations imply uncertainties of the order of a few hundred light days on RBLR.…”

Section: Blr Propertiesmentioning

confidence: 99%

Unveiling the monster heart: unbeamed properties of blazar 4C 71.07

Raiteri

Acosta–Pulido

Villata

et al. 2020

Monthly Notices of the Royal Astronomical Society

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4C 71.07 is a high-redshift blazar whose optical radiation is dominated by quasarlike nuclear emission. We here present the results of a spectroscopic monitoring of the source to study its unbeamed properties. We obtained 24 optical spectra at the Nordic Optical Telescope (NOT) and William Herschel Telescope (WHT) and 3 nearinfrared spectra at the Telescopio Nazionale Galileo (TNG). They show no evidence of narrow emission lines. The estimate of the systemic redshift from the H β and H α broad emission lines leads to z sys = 2.2130 ± 0.0004. Notwithstanding the nearly faceon orientation of the accretion disc, the high-ionization emission lines present large broadening as well as noticeable blueshifts, which increase with the ionizing energy of the corresponding species. This is a clear indication of strong ionized outflows. Line broadening and blueshift appear correlated. We applied scaling relationships to estimate the mass of the supermassive black hole from the Balmer and C iv lines, taking into account the prescriptions to correct for outflow. They give M BH ∼ 2 × 10 9 M ⊙ . We derived an Eddington luminosity L Edd ∼ 2.5 × 10 47 erg s −1 ∼ L disc , and a broad line region luminosity of L BLR ∼ 1.5 × 10 46 erg s −1 . The line fluxes do not show significant variability in time. In particular, there is no line reaction to the jet flaring activity detected in 2015 October-November. This implies that the jet gives no contribution to the photoionization of the broad line region in the considered period.

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The Sloan Digital Sky Survey Reverberation Mapping Project: Initial C iv Lag Results from Four Years of Data

Cited by 101 publications

References 120 publications

C iv Emission-line Properties and Uncertainties in Black Hole Mass Estimates of z ∼ 3.5 Quasars

C iv Emission-line Properties and Uncertainties in Black Hole Mass Estimates of z ∼ 3.5 Quasars

The Sloan Digital Sky Survey Reverberation Mapping Project: Photometric g and i Light Curves

Unveiling the monster heart: unbeamed properties of blazar 4C 71.07

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