The hard X-ray emission of luminous infrared galaxies

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dc.creatorRisaliti, G.
dc.creatorGilli, R.
dc.creatorMaiolino, R.
dc.creatorSalvati, M.
dc.date2000-02-24
dc.date.accessioned2026-07-07T01:52:28Z
dc.date.available2026-07-07T01:52:28Z
dc.descriptionWe present a study of the hard X-ray properties of a sample that includes all the Luminous Infrared Galaxies (LIGs, L_IR > 10^11 L_sun) observed in the 2-10 keV energy band (new and archival data). We find that a significant fraction of the sources optically classified as AGNs do not show any indication of nuclear activity in the X rays, thus suggesting heavy absorption along our line of sight. The absence of strong emission in the 20-200 keV band in a subsample of LIGs observed with BeppoSAX suggests that in many cases these sources are completely Compton thick (N_H > 10^25 cm^(-2)). From a comparison between the infrared and the X-ray emission we deduce that the mid-IR emission is absorbed by a lower column density than the X-ray emission or, alternatively, that the dust-to-gas ratio is lower than Galactic. We describe a simple model that reproduces the IR-X correlation by means of mixed AGN and starburst contributions and we compare the predictions of this model with the observational data at X-ray and optical wavelengths. Finally, we discuss the biases that affect the currently available samples of LIGs and briefly analyze a small unbiased sample, finding that at least 50% of the sources host a (weak) AGN.
dc.description12 LaTeX pages including 6 postscript figures. Accepted for publication in A&A
dc.identifierhttps://arxiv.org/abs/astro-ph/0002460
dc.identifierhttp://arxiv.org/abs/astro-ph/0002460
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/634
dc.subjectAstrophysics
dc.titleThe hard X-ray emission of luminous infrared galaxies
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