Multiwavelength study of X-ray selected star-forming galaxies within the Chandra Deep Field-South |
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| Authors: | Daniel Rosa-González Denis Burgarella Kirpal Nandra Daniel Kunth Elena Terlevich † Roberto Terlevich † |
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| Institution: | INAOE, Luis Enrique Erro 1, Tonantzintla, Puebla 72840, México;Observatoire Astronomique Marseille Provence, Laboratoire d'Astrophysique de Marseille, 13376 Marseille Cedex 12, France;Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AW;Institut d'Astrophysique, Paris, 98 bis Boulevard Arago, F-75014 Paris, France |
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| Abstract: | We have combined multiwavelength observations of a selected sample of star-forming galaxies with galaxy evolution models in order to compare the results obtained for different star formation rate (SFR) tracers and to study the effect that the evolution of the star-forming regions has on them. We also aimed at obtaining a better understanding of the corrections due to extinction and nuclear activity on the derivation of the SFR. We selected the sample from Chandra data for the well studied region Chandra Deep Field -South (CDFS) and chose the objects that also have ultraviolet (UV) and infrared (IR) data from Galaxy Evolution Explorer ( GALEX ) and Great Observatories Origins Deep Survey (GOODS) Spitzer , respectively.
Our main finding is that there is good agreement between the extinction corrected SFR(UV) and the SFR(X), and we confirm the use of X-ray luminosities as a trustful tracer of recent star formation activity. Nevertheless, at SFR(UV) larger than about 5 M⊙ yr?1 there are several galaxies with an excess of SFR(X) suggesting the presence of an obscured active galactic nucleus (AGN) not detected in the optical spectra. We conclude that the IR luminosity is driven by recent star formation even in those galaxies where the SFR(X) is an order of magnitude higher than the SFR(UV) and therefore may harbour an AGN. One object shows SFR(X) much lower than expected based on the SFR(UV); this SFR(X) 'deficit' may be due to an early transient phase before most of the massive X-ray binaries were formed. An X-ray deficit could be used to select extremely young bursts in an early phase just after the explosion of the first supernovae associated with massive stars and before the onset of massive X-ray binaries. |
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| Keywords: | galaxies: fundamental parameters ultraviolet: galaxies X-rays: galaxies |
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