2017A&A...606A.117I


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST18:46:40

2017A&A...606A.117I - Astronomy and Astrophysics, volume 606A, 117-117 (2017/10-1)

The active nucleus of the ULIRG IRAS F00183-7111 viewed by NuSTAR.

IWASAWA K., SPOON H.W.W., COMASTRI A., GILLI R., LANZUISI G., PICONCELLI E., VIGNALI C., BRUSA M. and PUCCETTI S.

Abstract (from CDS):

We present an X-ray study of the ultra-luminous infrared galaxy IRAS F00183-7111 (z=0.327), using data obtained from NuSTAR, Chandra X-ray Observatory, Suzaku and XMM-Newton. The Chandra imaging shows that a point-like X-ray source is located at the nucleus of the galaxy at energies above 2keV. However, the point source resolves into diffuse emission at lower energies, extending to the east, where the extranuclear [OIII]λ5007 emission, presumably induced by a galactic-scale outflow, is present. The nuclear source is detected by NuSTAR up to the rest-frame 30keV. The strong, high-ionization Fe K line, first seen by XMM-Newton, and subsequently by Suzaku and Chandra, is not detected in the NuSTAR data. The line flux appears to have been declining continuously between 2003 and 2016, while the continuum emission remained stable to within 30%. Further observations are needed to confirm this. The X-ray continuum below 10keV is characterised by a hard spectrum caused by cold absorption of NH∼1x1023cm–2, compatible to that of the silicate absorption at 9.7µm, and a broad absorption feature around 8keV which we attribute to a high-ionization Fe K absorption edge. The latter is best described by a blueshifted, high-ionization (logξ∼3) absorber with a column density of NH∼1x1024cm–2, similar to the X-ray high-velocity outflows observed in a number of active nuclei. No extra hard component, which would arise from a strongly absorbed (i.e. Compton-thick) source, is seen in the NuSTAR data. While a pure reflection scenario (with a totally hidden central source) is viable, direct emission from the central source of L2–10keV~=2x1044erg/s, behind layers of cold and hot absorbing gas may be an alternative explanation. In this case, the relative X-ray quietness (Lx/Lbol,AGN≥6x10–3), the high-ionization Fe line, strong outflows inferred from various observations, and other similarities to the well-studied ULIRG/QSO Mrk 231 point that the central source in this ULIRG might be accreting close to the Eddington limit.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: active - galaxies: individual: IRAS F00183-7111 - X-rays: galaxies - X-rays: galaxies

Simbad objects: 10

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Number of rows : 10

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 IRAS F00183-7111 Sy2 00 20 34.7 -70 55 27     20.6     ~ 121 0
2 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4093 2
3 Mrk 1506 Sy1 04 33 11.0958197353 +05 21 15.617543663   15.72 15.05 10.08   ~ 1841 2
4 2MASX J05210136-2521450 Sy2 05 21 01.3987198411 -25 21 45.269338983   15.47 14.75     ~ 427 0
5 NAME IRAS F08572+3915 NW LIN 09 00 25.364 +39 03 54.23     16.66     ~ 364 1
6 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 2069 0
7 NGC 4355 Sy2 12 26 54.628 -00 52 39.51   14.21 13.37     ~ 405 2
8 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1781 3
9 NGC 4945 Sy2 13 05 27.279 -49 28 04.44   9.31 14.40 7.55   ~ 1265 2
10 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2683 4

    Equat.    Gal    SGal    Ecl

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2020.07.14-18:46:40

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