2014A&A...563A..95D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST02:24:58

2014A&A...563A..95D - Astronomy and Astrophysics, volume 563A, 95-95 (2014/3-1)

Simultaneous XMM-Newton and HST-COS observation of 1H 0419-577. II. Broadband spectral modeling of a variable Seyfert galaxy.

DI GESU L., COSTANTINI E., PICONCELLI E., EBRERO J., MEHDIPOUR M. and KAASTRA J.S.

Abstract (from CDS):

In this paper, we present the longest exposed (97 ks) XMM-Newton EPIC-pn spectrum ever obtained for the Seyfert 1.5 galaxy 1H 0419-577. With the aim of explaining the broadband emission of this source, we took advantage of the simultaneous coverage in the optical/UV that was provided in the present case by the XMM-Newton Optical Monitor and by a HST-COS observation. Archival FUSE flux measurements in the far-ultraviolet were also used for the present analysis. We successfully modeled the X-ray spectrum and the optical/UV fluxes data points using a Comptonization model. We found that a blackbody temperature of T∼56eV accounts for the optical/UV emission originating in the accretion disk. This temperature serves as an input for the Comptonized components that model the X-ray continuum. Both a warm (Twc∼0.7keV, τwc∼7) and a hot corona (Thc∼160keV, τhc∼0.5) intervene to upscatter the disk photons to X-ray wavelengths. With the addition of a partially covering (Cv∼50%) cold absorber with a variable opacity ( NH~[1019-1022]cm–2), this model can also explain the historical spectral variability of this source, with the present dataset presenting the lowest one ( NH∼1019cm–2). We discuss a scenario where the variable absorber becomes less opaque in the highest flux states because it gets ionized in response to the variations of the X-ray continuum. The lower limit for the absorber density derived in this scenario is typical for the broad line region clouds. We infer that 1H 0419-577 may be viewed from an intermediate inclination angle i≥54°, and, on this basis, we speculate that the X-ray obscuration may be associated with the innermost dust-free region of the obscuring torus. Finally, we critically compare this scenario with all the different models (e.g., disk reflection) that have been used in the past to explain the variability of this source.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: individual: 1H0419-577 - X-rays: galaxies

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 863 Sy1 02 14 33.5610949475 -00 46 00.180128181   14.48 13.81 17.9   ~ 571 0
2 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1523 2
3 LB 1727 Sy1 04 26 00.7188445954 -57 12 01.772037544 13.68 14.58 14.37 14.8   ~ 235 0
4 2MASX J05580206-3820043 Sy1 05 58 02.0566732230 -38 20 04.453517461   16.05 14.98 11.6   ~ 202 1
5 QSO B0558-5026 BLL 05 59 47.3917733375 -50 26 52.026945176   15.18 14.97     ~ 243 1
6 IC 450 Sy1 06 52 12.32333 +74 25 37.2376   15.16 14.19     ~ 498 1
7 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3379 2
8 NGC 4388 Sy2 12 25 46.820 +12 39 43.45 11.91 11.76 11.02     ~ 1183 2
9 ESO 383-35 Sy1 13 35 53.7686909139 -34 17 44.139127597   13.89 13.61 8.9   ~ 1378 0
10 Mrk 509 Sy1 20 44 09.7504131334 -10 43 24.724854084   13.35 13.12 10.7   ~ 1128 0
11 IRAS 21262+5643 Sy1 21 27 45.3943647524 +56 56 34.913660916       16.6   ~ 128 0
12 NGC 7582 GiP 23 18 23.621 -42 22 14.06 11.62 10.92 10.62     ~ 796 2

    Equat.    Gal    SGal    Ecl

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2020.07.08-02:24:58

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