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| Title: | Simultaneous X-ray and infrared variability in the quasar 3C273 - II. Confirmation of the correlation and X-ray lag | |
| Authors: | McHardy, Ian; Lawson, Anthony; Newsam, Andrew; Marscher, Alan P.; Sokolov, Andrei S.; Urry, C. Megan; Wehrle, Ann E. | |
| Affiliation: | AA(School of Physics and Astronomy, University of Southampton SO17 1BJ), AB(School of Physics and Astronomy, University of Southampton SO17 1BJ), AC(School of Physics and Astronomy, University of Southampton SO17 1BJ; Liverpool John Moores University, Astrophysics Research Institute, Birkenhead CH41 1LD), AD(Institute for Astrophysical Research, 725 Commonwealth Avenue, Boston University, Boston, MA 02215, USA), AE(Institute for Astrophysical Research, 725 Commonwealth Avenue, Boston University, Boston, MA 02215, USA), AF(Department of Physics, Yale University, PO Box 208121, New Haven, CT 06520-8121, USA), AG(IPAC, Jet Propoulsion Laboratory and California Institute of Technology, Pasadena, CA 91125, USA) | |
| Publication: | Monthly Notices of the Royal Astronomical Society, Volume 375, Issue 4, pp. 1521-1527. (MNRAS Homepage) | |
| Publication Date: | 03/2007 | |
| Origin: | MNRAS | |
| MNRAS Keywords: | galaxies: active , quasars: individual: 3C273 , X-rays: galaxies | |
| Abstract Copyright: | (c) 2007 The Authors. Journal compilation © 2007 RAS | |
| DOI: | 10.1111/j.1365-2966.2006.11420.x | |
| Bibliographic Code: | 2007MNRAS.375.1521M |
The previous correlation was based on one moderately well-sampled flare and another poorly sampled flare, so the possibility of chance correlated variability exists. Here, we report on further X-ray and IR observations of 3C273 which confirm the behaviour seen in Paper I. During a 2-week period of observations, we see a flare of amplitude ~25per cent, lasting for ~5 d, showing a high correlation between IR and X-ray variations, with the X-rays lagging by ~1.45 +/- 0.15 d. These observations were not scheduled at any special time, implying that the same mechanism - almost certainly SSC - dominates the X-ray emission on most occasions and that the structure of the emission region is similar in most small flares.
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