Статья

<i>KEPLER</i>OBSERVATIONS OF RAPID OPTICAL VARIABILITY IN THE BL LACERTAE OBJECT W2R1926+42

R. EdelsonDepartment of Astronomy, University of Maryland, College Park, MD 20742-2421, USA; [email protected]R. MushotzkyDepartment of Astronomy, University of Maryland, College Park, MD 20742-2421, USA; [email protected]S. VaughanX-ray and Observational Astronomy Group, Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UKJ. ScargleAstrobiology and Space Science Division, NASA Ames Research Center, Moffet Field, CA 94035, USAP. GandhiInstitute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, chuo-ku, Sagamihara, Kanagawa 252-5210, JapanM. MalkanDepartment of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095-1547, USAW. BaumgartnerLaboratory for High Energy Astrophysics, NASA/GSFC, Code 662, Greenbelt, MD 20771, USA

2013en

ABI

Аннотация

We present the first Kepler monitoring of a strongly variable BL Lac, W2R1926+42. The light curve covers 181 days with ~0.2% errors, 30 minute sampling and >90% duty cycle, showing numerous delta I/I > 25% flares over timescales as short as a day. The flux distribution is highly skewed and non-Gaussian. The variability shows a strong rms-flux correlation with the clearest evidence to date for non-linearity in this relation. We introduce a method to measure periodograms from the discrete autocorrelation function, an approach that may be well-suited to a wide range of Kepler data. The periodogram is not consistent with a simple power-law, but shows a flattening at frequencies below 7x10-5 Hz. Simple models of the power spectrum, such as a broken power law, do not produce acceptable fits, indicating that the Kepler blazar light curve requires more sophisticated mathematical and physical descriptions than currently in use.

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Идентификаторы

DOI: 10.1088/0004-637x/766/1/16

Цитирования и источники

Цитирований: 2Использованных источников: 0

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