The corona of the broad-line radio galaxy 3C 390.3
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- Univ. of Cambridge, Cambridge (United Kingdom)
- California Inst. of Technology (CalTech), Pasadena, CA (United States)
- Univ. of Maryland, College Park, MD (United States); NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States)
- Caltech, Pasadena, CA (United States)
- Univ. of Michigan, Ann Arbor, MI (United States)
- Georgia Inst. of Technology, Atlanta, GA (United States)
- Univ. of California, Berkeley, CA (United States)
- Danish Technical Univ., Lyngby (Denmark)
- Univ. of California, Berkeley, CA (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
- Stanford Univ., Stanford, CA (United States)
- Univ. degli Studi Roma Tre, Roma (Italy)
- Univ. of Maryland, College Park, MD (United States)
- Univ. degli Studi Roma Tre, Roma (Italy); Univ. Grenoble Alpes, Grenoble (France)
- NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States)
We present the results from a joint Suzaku/NuSTAR broadband spectral analysis of 3C 390.3. The high quality data enables us to clearly separate the primary continuum from the reprocessed components allowing us to detect a high energy spectral cut-off ($${E}_{\mathrm{cut}}={117}_{-14}^{+18}$$ keV), and to place constraints on the Comptonization parameters of the primary continuum for the first time. The hard over soft compactness is $${69}_{-24}^{+124}$$ and the optical depth is $${4.1}_{-3.6}^{+0.5},$$ this leads to an electron temperature of $${30}_{-8}^{+32}$$ keV. Expanding our study of the Comptonization spectrum to the optical/UV by studying the simultaneous Swift-UVOT data, we find indications that the compactness of the corona allows only a small fraction of the total UV/optical flux to be Comptonized. Our analysis of the reprocessed emission show that 3C 390.3 only has a small amount of reflection (R ~ 0.3), and of that the vast majority is from distant neutral matter. Furthermore, we also discover a soft-X-ray excess in the source, which can be described by a weak ionized reflection component from the inner parts of the accretion disk. In addition to the backscattered emission, we also detect the highly ionized iron emission lines Fe xxv and Fe xxvi.
- Research Organization:
- SLAC National Accelerator Lab., Menlo Park, CA (United States)
- Sponsoring Organization:
- USDOE Office of Science (SC), High Energy Physics (HEP); National Aeronautics and Space Administration (NASA)
- Grant/Contract Number:
- AC02-76SF00515
- OSTI ID:
- 1313942
- Report Number(s):
- SLAC-PUB-16800; arXiv:1510.01333
- Journal Information:
- The Astrophysical Journal (Online), Vol. 814, Issue 1; ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)Copyright Statement
- Country of Publication:
- United States
- Language:
- English
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