Figure 3 from SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. III. OPTICAL CONTINUUM EMISSION AND BROADBAND TIME DELAYS IN NGC 5548

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SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. III. OPTICAL CONTINUUM EMISSION AND BROADBAND TIME DELAYS IN NGC 5548

Authors: M. M. Fausnaugh, K. D. Denney, A. J. Barth, M. C. Bentz, M. C. Bottorff, M. T. Carini, K. V. Croxall, G. De Rosa, M. R. Goad, Keith Horne, M. D. Joner, S. Kaspi, M. Kim, S. A. Klimanov, C. S. Kochanek, D. C. Leonard, H. Netzer, B. M. Peterson, K. Schnülle, S. G. Sergeev, M. Vestergaard, W.-K. Zheng, Y. Zu, M. D. Anderson, P. Arévalo, C. Bazhaw, G. A. Borman, T. A. Boroson, W. N. Brandt, A. A. Breeveld, B. J. Brewer, E. M. Cackett, D. M. Crenshaw, E. Dalla Bontà, A. De Lorenzo-Cáceres, M. Dietrich, R. Edelson, N. V. Efimova, J. Ely, P. A. Evans, A. V. Filippenko, K. Flatland, N. Gehrels, S. Geier, J. M. Gelbord, L. Gonzalez, V. Gorjian, C. J. Grier, D. Grupe, P. B. Hall, S. Hicks, D. Horenstein, T. Hutchison, M. Im, J. J. Jensen, J. Jones, J. Kaastra, B. C. Kelly, J. A. Kennea, S. C. Kim, K. T. Korista, G. A. Kriss, J. C. Lee, P. Lira, F. MacInnis, E. R. Manne-Nicholas, S. Mathur, I. M. McHardy, C. Montouri, R. Musso, S. V. Nazarov, R. P. Norris, J. A. Nousek, D. N. Okhmat, A. Pancoast, I. Papadakis, J. R. Parks, L. Pei, R. W. Pogge, J.-U. Pott, S. E. Rafter, H.-W. Rix, D. A. Saylor, J. S. Schimoia, M. Siegel, M. Spencer, D. Starkey, H.-I. Sung, K. G. Teems, T. Treu, C. S. Turner, P. Uttley, C. Villforth, Y. Weiss, J.-H. Woo, H. Yan, and S. Young

2016 The Astrophysical Journal 821 56.

Provider: AAS Journals

Caption: Figure 3.

Top panel: mean SED of NGC 5548 from far-UV to optical wavelengths, corrected for Galactic extinction. The vertical error bars represent the AGN in the maximum and minimum states of the campaign. The horizontal error bars represent the rms width of the filter transmission curves. See Section 4 for a discussion of the host-galaxy estimate. Middle panel: variable SED component, calculated from the difference in flux between the minimum and maximum states, which more cleanly identifies the accretion-disk spectrum. The dashed red line is the predicted spectrum for a standard thin disk—discrepancies at short wavelengths may be due to extinction internal to the AGN or the inner edge of the disk. Bottom panel: fractional variability ﹩{F}_{{\rm{var}}}﹩ as a function of wavelength. ﹩{\sigma }_{{\rm{DRW}}}﹩ is the DRW amplitude from the JAVELIN fits. For clarity, a small shift in wavelength to the ﹩{F}_{{\rm{var}}}﹩ points has been applied.

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