Measuring the Variability in K2 Optical Light Curves of 3C 273 and Other Fermi Active Galactic Nuclei in 2015-2017

被引：5
作者：
Carini, Michael [1 ]
Wehrle, Ann E. [2 ]
Wiita, Paul J. [3 ]
Ward, Zoe [4 ]
Pendleton, Kennedy [4 ]
机构：
[1] Western Kentucky Univ, Dept Phys & Astron, 1906 Coll Hts Blvd, Bowling Green, KY 42101 USA
[2] Space Sci Inst, 4765 Walnut St,Suite B, Boulder, CO 80301 USA
[3] Coll New Jersey, Dept Phys, POB 7718, Ewing, NJ 08628 USA
[4] Western Kentucky Univ, Carol Martin Gatton Acad Math & Sci Kentucky, 1906 Coll Hts Blvd, Bowling Green, KY 42101 USA
来源：
ASTROPHYSICAL JOURNAL | 2020年 / 903卷 / 02期
基金：
美国国家航空航天局; 瑞典研究理事会;
关键词：
Active galactic nuclei; Active galaxies; Jets; MAGNETICALLY ARRESTED ACCRETION; POWER SPECTRA; JETS; CATALOG; RADIO; MICROVARIABILITY; BLAZARS; OBJECTS; POLARIZATION; PHOTOMETRY;
D O I：
10.3847/1538-4357/abbb92
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We characterize the variability in nearly continuous optical observations of the bright radio-loud quasar 3C 273 and nine additional active galactic nuclei detected with the Fermi Gamma-ray Space Telescope Large Area Telescope (Fermi-LAT). Optical observations were obtained during the K2 mission with the Kepler spacecraft for periods of 49 to 83 days conducted with 1 minute (short) or 30 minutes (long) cadences in 2015-2017. 3C 273 was quiescent during the course of the observations, varying by only a factor of 1.02. Three objects, PKS 0047+023, PKS 1216-10, and PKS B2320-035, were active, varying by factors of 1.8-3.4. Six other objects were comparatively quiet, varying by factors of less than 1.4. Power spectral densities (PSDs) were calculated for each object. Overall, the slopes of most PSDs, as well as those we reported in an earlier paper, were in the range -2.0 to -2.7 and are consistent with those produced by turbulence in the relativistic jet, and not by "hot spots" in the disk emission. Mechanisms operating in the jet other than turbulence, such as "mini-jets" or "jet-in-jets", may also produce the observed range of PSD slopes. Both accretion disk and jet models are plausible origins for the 3C 273 optical variability during the K2 observations.
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页数：15
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