The XMM-Newton serendipitous survey - IV. Optical identification of the XMM-Newton medium sensitivity survey (XMS)

X. Barcons; F. J. Carrera; M. T. Ceballos; M. J. Page; J. Bussons-Gordo; A. Corral; J. Ebrero; S. Mateos; J. A. Tedds; M. G. Watson; D. Baskill; M. Birkinshaw; T. Boller; N. Borisov; M. Bremer; G. E. Bromage; H. Brunner; A. Caccianiga; C. S. Crawford; M. S. Cropper; R. Della Ceca; P. Derry; A. C. Fabian; P. Guillout; Y. Hashimoto; G. Hasinger; B. J. M. Hassall; G. Lamer; N. S. Loaring; T. Maccacaro; K. O. Mason; R. G. McMahon; L. Mirioni; J. P. D. Mittaz; C. Motch; I. Negueruela; J. P. Osborne; F. Panessa; I. Perez-Fournon; J. P. Pye; T. P. Roberts; S. Rosen; N. Schartel; N. Schurch; A. Schwope; P. Severgnini; R. Sharp; G. C. Stewart; G. Szokoly; A. Ullan; M. J. Ward; R. S. Warwick; P. J. Wheatley; N. A. Webb; D. Worrall; W. Yuan; H. Ziaeepour

doi:10.1051/0004-6361:20077606

The XMM-Newton serendipitous survey - IV. Optical identification of the XMM-Newton medium sensitivity survey (XMS)

X. Barcons^*, F. J. Carrera, M. T. Ceballos, M. J. Page, J. Bussons-Gordo, A. Corral, J. Ebrero, S. Mateos, J. A. Tedds, M. G. Watson, D. Baskill, M. Birkinshaw, T. Boller, N. Borisov, M. Bremer, G. E. Bromage, H. Brunner, A. Caccianiga, C. S. Crawford, M. S. CropperR. Della Ceca, P. Derry, A. C. Fabian, P. Guillout, Y. Hashimoto, G. Hasinger, B. J. M. Hassall, G. Lamer, N. S. Loaring, T. Maccacaro, K. O. Mason, R. G. McMahon, L. Mirioni, J. P. D. Mittaz, C. Motch, I. Negueruela, J. P. Osborne, F. Panessa, I. Perez-Fournon, J. P. Pye, T. P. Roberts, S. Rosen, N. Schartel, N. Schurch, A. Schwope, P. Severgnini, R. Sharp, G. C. Stewart, G. Szokoly, A. Ullan, M. J. Ward, R. S. Warwick, P. J. Wheatley, N. A. Webb, D. Worrall, W. Yuan, H. Ziaeepour

^*Corresponding author for this work

School of Physics

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Abstract

Aims. X-ray sources at intermediate fluxes (a few x 10(-14) erg cm(-2) s(-1)) with a sky density of similar to 100 deg(-2) are responsible for a significant fraction of the cosmic X-ray background at various energies below 10 keV. The aim of this paper is to provide an unbiased and quantitative description of the X-ray source population at these fluxes and in various X-ray energy bands.

Methods. We present the XMM-Newton Medium sensitivity Survey (XMS), including a total of 318 X-ray sources found among the serendipitous content of 25 XMM-Newton target fields. The XMS comprises four largely overlapping source samples selected at soft (0.5-2 keV), intermediate (0.5-4.5 keV), hard (2-10 keV) and ultra-hard (4.5-7.5 keV) bands, the first three of them being flux-limited.

Results. We report on the optical identification of the XMS samples, complete to 85-95%. At the flux levels sampled by the XMS we find that the X-ray sky is largely dominated by Active Galactic Nuclei. The fraction of stars in soft X-ray selected samples is below 10%, and only a few per cent for hard selected samples. We find that the fraction of optically obscured objects in the AGN population stays constant at around 15-20% for soft and intermediate band selected X-ray sources, over 2 decades of flux. The fraction of obscured objects amongst the AGN population is larger (similar to 35-45%) in the hard or ultra-hard selected samples, and constant across a similarly wide flux range. The distribution in X-ray-to-optical flux ratio is a strong function of the selection band, with a larger fraction of sources with high values in hard selected samples. Sources with X-ray-to-optical flux ratios in excess of 10 are dominated by obscured AGN, but with a significant contribution from unobscured AGN.

Original language	English
Pages (from-to)	1191-U35
Number of pages	30
Journal	Astronomy and Astrophysics
Volume	476
Issue number	3
DOIs	https://doi.org/10.1051/0004-6361:20077606
Publication status	Published - Dec 2007

Keywords

X-rays : general
X-rays : galaxies
X-rays : stars
galaxies : active
ACTIVE GALACTIC NUCLEI
CHANDRA MULTIWAVELENGTH PROJECT
X-RAY SOURCES
DEEP ROSAT SURVEY
LOG S-RELATION
HELLAS2XMM SURVEY
SOURCE CATALOG
LOCKMAN HOLE
FOLLOW-UP
FIELD

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Barcons, X., Carrera, F. J., Ceballos, M. T., Page, M. J., Bussons-Gordo, J., Corral, A., Ebrero, J., Mateos, S., Tedds, J. A., Watson, M. G., Baskill, D., Birkinshaw, M., Boller, T., Borisov, N., Bremer, M., Bromage, G. E., Brunner, H., Caccianiga, A., Crawford, C. S., ... Ziaeepour, H. (2007). The XMM-Newton serendipitous survey - IV. Optical identification of the XMM-Newton medium sensitivity survey (XMS). Astronomy and Astrophysics, 476(3), 1191-U35. https://doi.org/10.1051/0004-6361:20077606

@article{5d712d31eb4e4e0db3afa58c07b4f568,

title = "The XMM-Newton serendipitous survey - IV. Optical identification of the XMM-Newton medium sensitivity survey (XMS)",

abstract = "Aims. X-ray sources at intermediate fluxes (a few x 10(-14) erg cm(-2) s(-1)) with a sky density of similar to 100 deg(-2) are responsible for a significant fraction of the cosmic X-ray background at various energies below 10 keV. The aim of this paper is to provide an unbiased and quantitative description of the X-ray source population at these fluxes and in various X-ray energy bands.Methods. We present the XMM-Newton Medium sensitivity Survey (XMS), including a total of 318 X-ray sources found among the serendipitous content of 25 XMM-Newton target fields. The XMS comprises four largely overlapping source samples selected at soft (0.5-2 keV), intermediate (0.5-4.5 keV), hard (2-10 keV) and ultra-hard (4.5-7.5 keV) bands, the first three of them being flux-limited.Results. We report on the optical identification of the XMS samples, complete to 85-95\%. At the flux levels sampled by the XMS we find that the X-ray sky is largely dominated by Active Galactic Nuclei. The fraction of stars in soft X-ray selected samples is below 10\%, and only a few per cent for hard selected samples. We find that the fraction of optically obscured objects in the AGN population stays constant at around 15-20\% for soft and intermediate band selected X-ray sources, over 2 decades of flux. The fraction of obscured objects amongst the AGN population is larger (similar to 35-45\%) in the hard or ultra-hard selected samples, and constant across a similarly wide flux range. The distribution in X-ray-to-optical flux ratio is a strong function of the selection band, with a larger fraction of sources with high values in hard selected samples. Sources with X-ray-to-optical flux ratios in excess of 10 are dominated by obscured AGN, but with a significant contribution from unobscured AGN.",

keywords = "X-rays : general, X-rays : galaxies, X-rays : stars, galaxies : active, ACTIVE GALACTIC NUCLEI, CHANDRA MULTIWAVELENGTH PROJECT, X-RAY SOURCES, DEEP ROSAT SURVEY, LOG S-RELATION, HELLAS2XMM SURVEY, SOURCE CATALOG, LOCKMAN HOLE, FOLLOW-UP, FIELD",

author = "X. Barcons and Carrera, \{F. J.\} and Ceballos, \{M. T.\} and Page, \{M. J.\} and J. Bussons-Gordo and A. Corral and J. Ebrero and S. Mateos and Tedds, \{J. A.\} and Watson, \{M. G.\} and D. Baskill and M. Birkinshaw and T. Boller and N. Borisov and M. Bremer and Bromage, \{G. E.\} and H. Brunner and A. Caccianiga and Crawford, \{C. S.\} and Cropper, \{M. S.\} and \{Della Ceca\}, R. and P. Derry and Fabian, \{A. C.\} and P. Guillout and Y. Hashimoto and G. Hasinger and Hassall, \{B. J. M.\} and G. Lamer and Loaring, \{N. S.\} and T. Maccacaro and Mason, \{K. O.\} and McMahon, \{R. G.\} and L. Mirioni and Mittaz, \{J. P. D.\} and C. Motch and I. Negueruela and Osborne, \{J. P.\} and F. Panessa and I. Perez-Fournon and Pye, \{J. P.\} and Roberts, \{T. P.\} and S. Rosen and N. Schartel and N. Schurch and A. Schwope and P. Severgnini and R. Sharp and Stewart, \{G. C.\} and G. Szokoly and A. Ullan and Ward, \{M. J.\} and Warwick, \{R. S.\} and Wheatley, \{P. J.\} and Webb, \{N. A.\} and D. Worrall and W. Yuan and H. Ziaeepour",

year = "2007",

month = dec,

doi = "10.1051/0004-6361:20077606",

language = "English",

volume = "476",

pages = "1191--U35",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

number = "3",

}

Barcons, X, Carrera, FJ, Ceballos, MT, Page, MJ, Bussons-Gordo, J, Corral, A, Ebrero, J, Mateos, S, Tedds, JA, Watson, MG, Baskill, D, Birkinshaw, M, Boller, T, Borisov, N, Bremer, M, Bromage, GE, Brunner, H, Caccianiga, A, Crawford, CS, Cropper, MS, Della Ceca, R, Derry, P, Fabian, AC, Guillout, P, Hashimoto, Y, Hasinger, G, Hassall, BJM, Lamer, G, Loaring, NS, Maccacaro, T, Mason, KO, McMahon, RG, Mirioni, L, Mittaz, JPD, Motch, C, Negueruela, I, Osborne, JP, Panessa, F, Perez-Fournon, I, Pye, JP, Roberts, TP, Rosen, S, Schartel, N, Schurch, N, Schwope, A, Severgnini, P, Sharp, R, Stewart, GC, Szokoly, G, Ullan, A, Ward, MJ, Warwick, RS, Wheatley, PJ, Webb, NA, Worrall, D, Yuan, W & Ziaeepour, H 2007, 'The XMM-Newton serendipitous survey - IV. Optical identification of the XMM-Newton medium sensitivity survey (XMS)', Astronomy and Astrophysics, vol. 476, no. 3, pp. 1191-U35. https://doi.org/10.1051/0004-6361:20077606

TY - JOUR

T1 - The XMM-Newton serendipitous survey - IV. Optical identification of the XMM-Newton medium sensitivity survey (XMS)

AU - Barcons, X.

AU - Carrera, F. J.

AU - Ceballos, M. T.

AU - Page, M. J.

AU - Bussons-Gordo, J.

AU - Corral, A.

AU - Ebrero, J.

AU - Mateos, S.

AU - Tedds, J. A.

AU - Watson, M. G.

AU - Baskill, D.

AU - Birkinshaw, M.

AU - Boller, T.

AU - Borisov, N.

AU - Bremer, M.

AU - Bromage, G. E.

AU - Brunner, H.

AU - Caccianiga, A.

AU - Crawford, C. S.

AU - Cropper, M. S.

AU - Della Ceca, R.

AU - Derry, P.

AU - Fabian, A. C.

AU - Guillout, P.

AU - Hashimoto, Y.

AU - Hasinger, G.

AU - Hassall, B. J. M.

AU - Lamer, G.

AU - Loaring, N. S.

AU - Maccacaro, T.

AU - Mason, K. O.

AU - McMahon, R. G.

AU - Mirioni, L.

AU - Mittaz, J. P. D.

AU - Motch, C.

AU - Negueruela, I.

AU - Osborne, J. P.

AU - Panessa, F.

AU - Perez-Fournon, I.

AU - Pye, J. P.

AU - Roberts, T. P.

AU - Rosen, S.

AU - Schartel, N.

AU - Schurch, N.

AU - Schwope, A.

AU - Severgnini, P.

AU - Sharp, R.

AU - Stewart, G. C.

AU - Szokoly, G.

AU - Ullan, A.

AU - Ward, M. J.

AU - Warwick, R. S.

AU - Wheatley, P. J.

AU - Webb, N. A.

AU - Worrall, D.

AU - Yuan, W.

AU - Ziaeepour, H.

PY - 2007/12

Y1 - 2007/12

N2 - Aims. X-ray sources at intermediate fluxes (a few x 10(-14) erg cm(-2) s(-1)) with a sky density of similar to 100 deg(-2) are responsible for a significant fraction of the cosmic X-ray background at various energies below 10 keV. The aim of this paper is to provide an unbiased and quantitative description of the X-ray source population at these fluxes and in various X-ray energy bands.Methods. We present the XMM-Newton Medium sensitivity Survey (XMS), including a total of 318 X-ray sources found among the serendipitous content of 25 XMM-Newton target fields. The XMS comprises four largely overlapping source samples selected at soft (0.5-2 keV), intermediate (0.5-4.5 keV), hard (2-10 keV) and ultra-hard (4.5-7.5 keV) bands, the first three of them being flux-limited.Results. We report on the optical identification of the XMS samples, complete to 85-95%. At the flux levels sampled by the XMS we find that the X-ray sky is largely dominated by Active Galactic Nuclei. The fraction of stars in soft X-ray selected samples is below 10%, and only a few per cent for hard selected samples. We find that the fraction of optically obscured objects in the AGN population stays constant at around 15-20% for soft and intermediate band selected X-ray sources, over 2 decades of flux. The fraction of obscured objects amongst the AGN population is larger (similar to 35-45%) in the hard or ultra-hard selected samples, and constant across a similarly wide flux range. The distribution in X-ray-to-optical flux ratio is a strong function of the selection band, with a larger fraction of sources with high values in hard selected samples. Sources with X-ray-to-optical flux ratios in excess of 10 are dominated by obscured AGN, but with a significant contribution from unobscured AGN.

AB - Aims. X-ray sources at intermediate fluxes (a few x 10(-14) erg cm(-2) s(-1)) with a sky density of similar to 100 deg(-2) are responsible for a significant fraction of the cosmic X-ray background at various energies below 10 keV. The aim of this paper is to provide an unbiased and quantitative description of the X-ray source population at these fluxes and in various X-ray energy bands.Methods. We present the XMM-Newton Medium sensitivity Survey (XMS), including a total of 318 X-ray sources found among the serendipitous content of 25 XMM-Newton target fields. The XMS comprises four largely overlapping source samples selected at soft (0.5-2 keV), intermediate (0.5-4.5 keV), hard (2-10 keV) and ultra-hard (4.5-7.5 keV) bands, the first three of them being flux-limited.Results. We report on the optical identification of the XMS samples, complete to 85-95%. At the flux levels sampled by the XMS we find that the X-ray sky is largely dominated by Active Galactic Nuclei. The fraction of stars in soft X-ray selected samples is below 10%, and only a few per cent for hard selected samples. We find that the fraction of optically obscured objects in the AGN population stays constant at around 15-20% for soft and intermediate band selected X-ray sources, over 2 decades of flux. The fraction of obscured objects amongst the AGN population is larger (similar to 35-45%) in the hard or ultra-hard selected samples, and constant across a similarly wide flux range. The distribution in X-ray-to-optical flux ratio is a strong function of the selection band, with a larger fraction of sources with high values in hard selected samples. Sources with X-ray-to-optical flux ratios in excess of 10 are dominated by obscured AGN, but with a significant contribution from unobscured AGN.

KW - X-rays : general

KW - X-rays : galaxies

KW - X-rays : stars

KW - galaxies : active

KW - ACTIVE GALACTIC NUCLEI

KW - CHANDRA MULTIWAVELENGTH PROJECT

KW - X-RAY SOURCES

KW - DEEP ROSAT SURVEY

KW - LOG S-RELATION

KW - HELLAS2XMM SURVEY

KW - SOURCE CATALOG

KW - LOCKMAN HOLE

KW - FOLLOW-UP

KW - FIELD

U2 - 10.1051/0004-6361:20077606

DO - 10.1051/0004-6361:20077606

M3 - Article (Academic Journal)

SN - 0004-6361

VL - 476

SP - 1191-U35

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 3

ER -

The XMM-Newton serendipitous survey - IV. Optical identification of the XMM-Newton medium sensitivity survey (XMS)

Abstract

Keywords

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