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J/A+A/548/A99       XMM-Newton Slew Survey in 2-10keV        (Warwick+, 2012)

The XMM-Newton Slew Survey in the 2-10 keV band. Warwick R.S., Saxton R.D., Read A.M. <Astron. Astrophys. 548, A99 (2012)> =2012A&A...548A..99W
ADC_Keywords: Surveys ; Galaxy catalogs ; Active gal. nuclei ; X-ray sources Keywords: surveys - X-rays: general - galaxies: active Abstract: The on-going XMM-Newton Slew Survey (XSS) provides coverage of a significant fraction of the sky in a broad X-ray bandpass. Although shallow by contemporary standards, in the "classical" 2-10keV band of X-ray astronomy, the XSS provides significantly better sensitivity than any currently available all-sky survey. We investigate the source content of the XSS, focussing on detections in the hard 2-10keV band down to a very low threshold (≥4counts net of background). At the faint end, the survey reaches a flux sensitivity of roughly 3x10-12erg/cm2/s (2-10keV). Our starting point was a sample of 487 sources detected in the XSS (up to and including release XMMSL1d2) at high galactic latitude in the hard band. Through cross-correlation with published source catalogues from surveys spanning the electromagnetic spectrum from radio through to gamma-rays, we find that 45% of the sources have likely identifications with normal/active galaxies. A further 18% are associated with other classes of X-ray object (nearby coronally active stars, accreting binaries, clusters of galaxies), leaving 37% of the XSS sources with no current identification. We go on to define an XSS extragalactic sample comprised of 219 galaxies and active galaxies selected in the XSS hard band. We investigate the properties of this extragalactic sample including its X-ray logN-logS distribution. We find that in the low-count limit, the XSS is, as expected, strongly affected by Eddington bias. There is also a very strong bias in the XSS against the detection of extended sources, most notably clusters of galaxies. A significant fraction of the detections at and around the low-count limit may be spurious. Nevertheless, it is possible to use the XSS to extract a reasonably robust sample of extragalactic sources, excluding galaxy clusters. The differential logN-logS relation of these extragalactic sources matches very well to the HEAO-1 A2 all-sky survey measurements at bright fluxes and to the 2XMM source counts at the faint end. The substantial sky coverage afforded by the XSS makes this survey a valuable resource for studying X-ray bright source samples, including those selected specifically in the hard 2-10keV band. Description: Details of the sources which comprise the hard-band selected XSS extragalactic sample are given in the Table. The table provides the following information for each source: the XSS name; whether the source was also detected in the XSS soft band (1=yes, 0=no); the XSS hard band (2-10keV) flux and error on the flux (in units of 10-11ergs/cm2/s) ; the RA and Dec of the proposed counterpart; the name of the counterpart; the type of the counterpart; the redshift (if known). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 126 219 XSS extragalactic sample parameters
See also: B/xmm : XMM-Newton Observation Log (XMM-Newton SOC, 2012) J/A+A/480/611 : XMM-Newton Slew Survey catalogue, XMMSL1 (Saxton+, 2008) J/MNRAS/412/1853 : XMM Slew Survey unidentified X-ray sources (Starling+, 2011) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 6 A6 --- --- [XMMSL1] 8- 23 A16 --- XMMSL1 SLEW XSS identifier (JHHMMSS.s+DDMMSS) 25 I1 --- Soft [0/1] Detected in soft band? (1=yes, 0=no) 27- 45 F19.17 10-14W/m2 Flux Flux in 2-10keV bands (10-11erg/cm2/s) 47- 65 F19.17 10-14W/m2 e_Flux Error on Flux 67- 75 F9.5 deg RAdeg Right ascension of counterpart (J2000) 77- 85 F9.5 deg DEdeg Declination of counterpart (J2000) 87-110 A24 --- ID Name of counterpart 112-116 A5 --- Type Type of counterpart (1) 119-126 F8.5 --- z ?=-9 Redshift of counterpart
Note (1): Classes(population) are: BLLac(28), Galaxy(38), LINER(2), QSO(35), RG(5), Sy1(60), Sy1.2(8), Sy1.5(11), Sy1.9(3), Sy2(11), UVX(18). "RG" are red galaxies/QSOs, and "UVX" are sources initially categorized as Galaxies which ere switched to AGN on the basis of their UV to near-IR colour.
Acknowledgements: A.M. Read, amr30(at)
(End) Patricia Vannier [CDS] 19-Oct-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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