KEPLER OBSERVATIONS OF RAPID OPTICAL VARIABILITY IN THE BL LACERTAE OBJECT W2R1926+42

被引：61

作者：

Edelson, R. ^{[1
]}

Mushotzky, R. ^{[1
,2
]}

Vaughan, S. ^{[3
]}

Scargle, J. ^{[4
]}

Gandhi, P. ^{[5
]}

Malkan, M. ^{[6
]}

Baumgartner, W. ^{[2
]}

机构：

[1] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[2] NASA, High Energy Astrophys Lab, GSFC, Greenbelt, MD 20771 USA

[3] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England

[4] NASA, Astrobiol & Space Sci Div, Ames Res Ctr, Stanford, CA 94305 USA

[5] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan

[6] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 766卷 / 01期

关键词：

BL Lacertae objects: general; BL Lacertae objects: individual (W2R1926+42); galaxies: active; X-RAY BINARIES; ACTIVE GALACTIC NUCLEI; BLACK-HOLE; GALAXIES; JET; NOISE; CONNECTION; CATALOG; BLAZARS; LONG;

D O I：

10.1088/0004-637X/766/1/16

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the first Kepler monitoring of a strongly variable BL Lac, W2R1926+42. The light curve covers 181 days with similar to 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 nonlinearity 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 7 x 10(-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.

引用

页数：8

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