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Continuum Reverberation Mapping of the Accretion Disks in Two Seyfert 1 Galaxies

  • Author(s): Fausnaugh, MM
  • Starkey, DA
  • Horne, K
  • Kochanek, CS
  • Peterson, BM
  • Bentz, MC
  • Denney, KD
  • Grier, CJ
  • Grupe, D
  • Pogge, RW
  • De Rosa, G
  • Adams, SM
  • Barth, AJ
  • Beatty, TG
  • Bhattacharjee, A
  • Borman, GA
  • Boroson, TA
  • Bottorff, MC
  • Brown, JE
  • Brown, JS
  • Brotherton, MS
  • Coker, CT
  • Crawford, SM
  • Croxall, KV
  • Eftekharzadeh, S
  • Eracleous, M
  • Joner, MD
  • Henderson, CB
  • Holoien, TWS
  • Hutchison, T
  • Kaspi, S
  • Kim, S
  • King, AL
  • Li, M
  • Lochhaas, C
  • Ma, Z
  • Macinnis, F
  • Manne-Nicholas, ER
  • Mason, M
  • Montuori, C
  • Mosquera, A
  • Mudd, D
  • Musso, R
  • Nazarov, SV
  • Nguyen, ML
  • Okhmat, DN
  • Onken, CA
  • Ou-Yang, B
  • Pancoast, A
  • Pei, L
  • Penny, MT
  • Poleski, R
  • Rafter, S
  • Romero-Colmenero, E
  • Runnoe, J
  • Sand, DJ
  • Schimoia, JS
  • Sergeev, SG
  • Shappee, BJ
  • Simonian, GV
  • Somers, G
  • Spencer, M
  • Stevens, DJ
  • Tayar, J
  • Treu, T
  • Valenti, S
  • Van Saders, J
  • Villanueva, S
  • Villforth, C
  • Weiss, Y
  • Winkler, H
  • Zhu, W
  • et al.
Abstract

© 2018. The American Astronomical Society. All rights reserved.. We present optical continuum lags for two Seyfert 1 galaxies, MCG+08-11-011 and NGC 2617, using monitoring data from a reverberation mapping campaign carried out in 2014. Our light curves span the ugriz filters over four months, with median cadences of 1.0 and 0.6 days for MCG+08-11-011 and NGC 2617, respectively, combined with roughly daily X-ray and near-UV data from Swift for NGC 2617. We find lags consistent with geometrically thin accretion-disk models that predict a lag-wavelength relation of τ ∝ λ 4/3. However, the observed lags are larger than predictions based on standard thin-disk theory by factors of 3.3 for MCG+08-11-011 and 2.3 for NGC 2617. These differences can be explained if the mass accretion rates are larger than inferred from the optical luminosity by a factor of 4.3 in MCG+08-11-011 and a factor of 1.3 in NGC 2617, although uncertainty in the SMBH masses determines the significance of this result. While the X-ray variability in NGC 2617 precedes the UV/optical variability, the long (2.6 day) lag is problematic for coronal reprocessing models.

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