Context. The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z less than or similar to 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z approximate to 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. Aims. We want to collect X-ray data in a field where it exists an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. Methods. We observed a field of 0.2 deg(2) in the Selected Area 57, for 67 ks with XMM-Newton. We detected X-ray sources, and we correlated the list with a photographic survey of SA 57, complete to B-J similar to 23 and with available spectroscopic data. Results. We obtained a catalogue of 140 X-ray sources to limiting fluxes 5 x 10(-16), 2 x 10(-15) erg cm(-2) s(-1) in the 0.5 - 2 keV and 2 - 10 keV respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O < 0.1.

Trevese, D., Vagnetti, F., Puccetti, S., Fiore, F., Tomei, M., & Bershady, M.A. (2007). An X-ray survey in SA 57 with XMM-Newton. ASTRONOMY & ASTROPHYSICS, 469(3), 1211-1219 [10.1051/0004-6361:20077359].

An X-ray survey in SA 57 with XMM-Newton

VAGNETTI, FAUSTO;
2007

Abstract

Context. The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z less than or similar to 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z approximate to 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. Aims. We want to collect X-ray data in a field where it exists an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. Methods. We observed a field of 0.2 deg(2) in the Selected Area 57, for 67 ks with XMM-Newton. We detected X-ray sources, and we correlated the list with a photographic survey of SA 57, complete to B-J similar to 23 and with available spectroscopic data. Results. We obtained a catalogue of 140 X-ray sources to limiting fluxes 5 x 10(-16), 2 x 10(-15) erg cm(-2) s(-1) in the 0.5 - 2 keV and 2 - 10 keV respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O < 0.1.
Pubblicato
Rilevanza internazionale
Articolo
Sì, ma tipo non specificato
Settore FIS/05 - Astronomia e Astrofisica
English
Con Impact Factor ISI
Galaxies: active; Galaxies: quasars: general; Surveys; X-rays: galaxies
Trevese, D., Vagnetti, F., Puccetti, S., Fiore, F., Tomei, M., & Bershady, M.A. (2007). An X-ray survey in SA 57 with XMM-Newton. ASTRONOMY & ASTROPHYSICS, 469(3), 1211-1219 [10.1051/0004-6361:20077359].
Trevese, D; Vagnetti, F; Puccetti, S; Fiore, F; Tomei, M; Bershady, M
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2108/31358
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