Multiband Observations of the Quasar PKS 2326–502 during Active and Quiescent Gamma-Ray States in 2010–2012

Journal Article · Wed Feb 01 00:00:00 EST 2017 · Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/835/2/182· OSTI ID:22663948

Dutka, Michael S. ^[1]; Carpenter, Bryce D.; Gehrels, Neil ^[2]; Ojha, Roopesh ^[3]; Finke, Justin D. ^[4]; D’Ammando, Filippo ^[5]; Kadler, Matthias ^[6]; Edwards, Philip G. ^[7]; Stevens, Jamie ^[8]; Torresi, Eleonora; Grandi, Paola ^[9]; Nesci, Roberto ^[10]; Krauß, Felicia ^[11]; Müller, Cornelia ^[12]; Wilms, Joern ^[13]

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1. The Catholic University of America, 620 Michigan Avenue, NE, Washington, DC 20064 (United States)
2. NASA Goddard Space Flight Center, Astrophysics Science Division, Code 661, Greenbelt, MD 20771 (United States)
3. UMBC/NASA Goddard Space Flight Center, Astrophysics Science Division, Code 661, Greenbelt, MD 20771 (United States)
4. Naval Research Laboratory, Space Science Division, Code 7653, 4555 Overlook Avenue, SW, Washington, DC 20375 (United States)
5. Università di Bologna Dipartimento di Fisica e Astronomia, INAF-IRA, Bologna (Italy)
6. Lehrstuhl für Astronomie, Universität Würzburg, Emil -Fischer-Straße 31, D-97074 Würzburg (Germany)
7. CSIRO Astronomy and Space Science, P.O. Box 76, Epping NSW 1710 (Australia)
8. CSIRO Astronomy and Space Science, 1828 Yarrie Lake Road, Narrabri NSW 2390 (Australia)
9. Istituto Nazionale di Astrofisica, (National Institute of Astrophysics) INAF-IASFBO, via Gobetti 101, I-40129 Bologna (Italy)
10. Istituto Nazionale di Astrofisica, (National Institute of Astrophysics) INAF-IAPS, via Fosso del Cavaliere 100, I-00133 Roma (Italy)
11. GRAPPA and Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam (Netherlands)
12. Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL, Nijmegen (Netherlands)
13. Remeis Observatory and ECAP, Sternwartstr. 7, D-96049 Bamberg (Germany)

Quasi-simultaneous observations of the Flat Spectrum Radio Quasar PKS 2326−502 were carried out in the γ -ray, X-ray, UV, optical, near-infrared, and radio bands. Using these observations, we are able to characterize the spectral energy distribution (SED) of the source during two flaring and one quiescent γ -ray states. These data were used to constrain one-zone leptonic models of the SEDs of each flare and investigate the physical conditions giving rise to them. While modeling one flare required only changes in the electron spectrum compared to the quiescent state, modeling the other flare required changes in both the electron spectrum and the size of the emitting region. These results are consistent with an emerging pattern of two broad classes of flaring states seen in blazars. Type 1 flares are explained by changes solely in the electron distribution, whereas type 2 flares require a change in an additional parameter. This suggests that different flares, even in the same source, may result from different physical conditions or different regions in the jet.

• OSTI ID: 22663948
• Journal Information: Astrophysical Journal, Vol. 835, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
COMPARATIVE EVALUATIONS
COSMIC RADIO SOURCES
DISTRIBUTION
ELECTRON SPECTRA
ENERGY SPECTRA
GALAXIES
GAMMA RADIATION
QUASARS
SIMULATION
ULTRAVIOLET RADIATION
X RADIATION