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Open Access Publications from the University of California

Reverberation mapping of the kepler field agn KA1858+4850

  • Author(s): Pei, L
  • Barth, AJ
  • Aldering, GS
  • Briley, MM
  • Carroll, CJ
  • Carson, DJ
  • Cenko, SB
  • Clubb, KI
  • Cohen, DP
  • Cucchiara, A
  • Desjardins, TD
  • Edelson, R
  • Fang, JJ
  • Fedrow, JM
  • Filippenko, AV
  • Fox, OD
  • Furniss, A
  • Gates, EL
  • Gregg, M
  • Gustafson, S
  • Horst, JC
  • Joner, MD
  • Kelly, PL
  • Lacy, M
  • Laney, CD
  • Leonard, DC
  • Li, W
  • Malkan, MA
  • Margon, B
  • Neeleman, M
  • Nguyen, ML
  • Prochaska, JX
  • Ross, NR
  • Sand, DJ
  • Searcy, KJ
  • Shivvers, IS
  • Silverman, JM
  • Smith, GH
  • Suzuki, N
  • Smith, KL
  • Tytler, D
  • Werk, JK
  • Worseck, G
  • et al.

© 2014. The American Astronomical Society. All rights reserved.. KA1858+4850 is a narrow-line Seyfert 1 galaxy at redshift 0.078 and is among the brightest active galaxies monitored by the Kepler mission. We have carried out a reverberation mapping campaign designed to measure the broad-line region size and estimate the mass of the black hole in this galaxy. We obtained 74 epochs of spectroscopic data using the Kast Spectrograph at the Lick 3 m telescope from 2012 February to November, and obtained complementary V-band images from five other ground-based telescopes. We measured the Hβ light curve lag with respect to the V-band continuum light curve using both cross-correlation techniques (CCF) and continuum light curve variability modeling with the JAVELIN method and found rest-frame lags of days and τJAVELINdays. The Hβ rms line profile has a width of σline = 770 ± 49 km s-1. Combining these two results and assuming a virial scale factor of f = 5.13, we obtained a virial estimate of for the mass of the central black hole and an Eddington ratio of L/L Edd 0.2. We also obtained consistent but slightly shorter emission-line lags with respect to the Kepler light curve. Thanks to the Kepler mission, the light curve of KA1858+4850 has among the highest cadences and signal-to-noise ratios ever measured for an active galactic nucleus; thus, our black hole mass measurement will serve as a reference point for relations between black hole mass and continuum variability characteristics in active galactic nuclei.

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