RT Journal Article
T1 X-ray luminosity functions of different morphological and X-ray type AGN populations
A1 Gallego Maestro, Jesús
AB Luminosity functions are one of the most important observational clues when studying galaxy evolution over cosmic time. In this paper we present the X-ray luminosity functions for X-ray detected AGN in the SXDS and GWS fields. The limiting fluxes of our samples are 9.0 ×10^(-15) and 4.8 ×10^(-16) erg cm^(-2) s^(-1) in the 0.5-7.0 keV band in the two fields, respectively. We carried out analysis in three X-ray bands and in two redshift intervals up to z≤1.4. Moreover, we derive the luminosity functions for different optical morphologies and X-ray types. We confirm strong luminosity evolution in all three bands, finding the most luminous objects at higher redshift. However, no signs of density evolution are found in any tested X-ray band. We obtain similar results for compact and early-type objects. Finally, we observe the “Steffen effect", where X-ray type-1 sources are more numerous at higher luminosities in comparison with type-2 sources.
PB Wiley-Vch Verlag gmbh
SN 0004-6337
YR 2013
FD 2013-03
LK https://hdl.handle.net/20.500.14352/34226
UL https://hdl.handle.net/20.500.14352/34226
LA eng
NO © 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. Artículo firmado por 15 autores. We thank Marc Huertas-Company for a number of valuable comments that improved the morphological classification of analysed sources. We also thank Jack Sulentic and the anonymous referee for all corrections and suggestions. We appreciate all comments from the XMM-Newton team during our SXDS X–ray data reduction, and we also thank the SXDS team for making their data available to the astronomical community. This research has been supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grant AYA2011- 29517-C03-01. MP, IM, and JM acknowledge Junta de Andalucía and MINECO through projects PO8-TIC-03531 and AYA2010- 15169. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). JIGS acknowledge financial support from the MINECO under project AYA2008-06311- C02-02 and AYA2011-29517-C03-02. JG acknowledges support from the MINECO through AYA2009-10368 project. The CEFCA is funded by the Fondo de Inversiones de Teruel, supported by both the Government of Spain (50%) and the regional Government of Aragón (50%). This work has been partially funded by the Spanish Ministerio de Ciencia e Innovación through the PNAYA, under grants AYA2006-14056 and through the ICTS 2009-14. This research has made use of software provided by the XMM-Newton Science Operations Centre and Chandra X–ray Center (CXC) in the application packages SAS and CIAO, respectively. IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. Virtual Observatory Tool for OPerations on Catalogues And Tables (TOPCAT) was used in this work.
NO Ministerio de Economía y Competitividad (MINECO)
NO Ministerio de Economía y Competitividad (MINECO)/Junta de Andalucía
NO Ministerio de Ciencia e Innovación (MICCIN)/PNAYA
NO Faculty of the European Space Astronomy Centre (ESAC)
NO Fondo de Inversiones de Teruel
DS Docta Complutense
RD 8 abr 2025