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19 April 2024

» arxiv » 1005.2562

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Star formation in AGN hosts in GOODS-N
L. Shao ; D. Lutz ; R. Nordon ; R. Maiolino ; D.M. Alexander ; B. Altieri ; P. Andreani ; H. Aussel ; F.E. Bauer ; S. Berta ; A. Bongiovanni ; W.N. Brandt ; M. Brusa ; A. Cava ; J. Cepa ; A. Cimatti ; E. Daddi ; H. Dominguez-Sanchez ; D. Elbaz ; N.M. Forster Schreiber ; N. Geis ; R. Genzel ; A. Grazian ; C. Gruppioni ; G. Magdis ; B. Magnelli ; V. Mainieri ; A.M. Perez Garcia ; A. Poglitsch ; P. Popesso ; F. Pozzi ; L. Riguccini ; G. Rodighiero ; E. Rovilos ; A. Saintonge ; M. Salvato ; M. Sanchez Portal ; P. Santini ; E. Sturm ; L.J. Tacconi ; I. Valtchanov ; M. Wetzstein ; E. Wieprecht ;
Date:	14 May 2010
Abstract:	Sensitive Herschel far-infrared observations can break degeneracies that were inherent to previous studies of star formation in high-z AGN hosts. Combining PACS 100 and 160um observations of the GOODS-N field with 2Msec Chandra data, we detect ~20% of X-ray AGN individually at >3sig. The host far-infrared luminosity of AGN with L2-10~10^43erg/s increases with redshift by an order of magnitude from z=0 to z~1. In contrast, there is little dependence of far-infrared luminosity on AGN luminosity, for L2-10<~10^44erg/s AGN at z>~1. We do not find a dependence of far-infrared luminosity on X-ray obscuring column, for our sample which is dominated by L2-10<10^44erg/s AGN. In conjunction with properties of local and luminous high-z AGN, we interpret these results as reflecting the interplay between two paths of AGN/host coevolution. A correlation of AGN luminosity and host star formation is traced locally over a wide range of luminosities and also extends to luminous high z AGN. This correlation reflects an evolutionary connection, likely via merging. For lower AGN luminosities, star formation is similar to that in non-active massive galaxies and shows little dependence on AGN luminosity. The level of this secular, non-merger driven star formation increasingly dominates over the correlation at increasing redshift.
Source:	arXiv, 1005.2562
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