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|Title:||Chandra X-ray observations of the hyper-luminous infrared galaxy IRAS F15307+3252|
Hogan, M. T.
Edge, A. C.
Fabian, A. C.
Russell, H. R.
Astronomia de raigs X
|Publisher:||Royal Astronomical Society|
|Abstract:||Hyper-luminous infrared galaxies (HyLIRGs) lie at the extreme luminosity end of the IR galaxy population with LIR > 1013 L.. They are thought to be closer counterparts of the more distant sub-millimeter galaxies, and should therefore be optimal targets to study the most massive systems in formation.We present deep Chandra observations of IRAS F15307+3252 (100 ks), a classical HyLIRG located at z=0.93 and hosting a radio-loudAGN(L1.4 GHz ∼3.5×1025WHz−1). The Chandra images reveal the presence of extended (r=160 kpc), asymmetric X-ray emission in the soft 0.3-2.0 keV band that has no radio counterpart.We therefore argue that the emission is of thermal origin originating from a hot intragroup or intracluster medium virializing in the potential. We find that the temperature (∼2 keV) and bolometric X-ray luminosity (∼3 × 1043 erg s−1) of the gas follow the expected LX-ray-T correlation for groups and clusters, and that the gas has a remarkably short cooling time of 1.2 Gyr. In addition, VLA radio observations reveal that the galaxy hosts an unresolved compact steep-spectrum (CSS)source, most likely indicating the presence of a young radio source similar to 3C186. We also confirm that the nucleus is dominated by a redshifted 6.4 keV Fe Kα line, strongly suggesting that the AGN is Compton-thick. Finally, Hubble images reveal an overdensity of galaxies and sub-structure in the galaxy that correlates with soft X-ray emission. This could be a snapshot view of on-going groupings expected in a growing cluster environment. IRAS F15307+3252 might therefore be a rare example of a group in the process of transforming into a cluster.|
|Note:||Reproducció del document publicat a: https://doi.org/10.1093/mnras/stw2468|
|It is part of:||Monthly Notices of the Royal Astronomical Society, 2016, vol. 464, p. 2223-2233|
|Appears in Collections:||Articles publicats en revistes (Institut de Ciències del Cosmos (ICCUB))|
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