WARPS - Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)
The WARPS survey. VI. Galaxy cluster and source identifications from phase I. Perlman E.S., Horner D.J., Jones L.R., Scharf C.A., Ebeling H., Wegner G., Malkan M. <Astrophys. J. Suppl. Ser. 140, 265 (2002)> =2002ApJS..140..265P
The assigned source name. The prefix used for the names of sources is WARPS (rather than WARP as in the published version), as recommended by the Dictionary of Astronomical Nomenclature.
The ROSAT pointing which contains the source.
The Right Ascension of the X-ray source in the selected equinox. The typical positional error is 15 arcseconds. The RA was listed in J2000 coordinates and to a precision of 0.1 seconds of time in the original published tables.
The Declination of the X-ray source in the selected equinox. The typical positional error is 15 arcseconds. The Declination was listed in J2000 coordinates and to a precision of 1 arcsecond in the original published tables.
The Galactic Longitude of the X-ray source.
The Galactic Latitude of the X-ray source.
The raw count rate obtained from the Voronoi Tessellation and Percolation (VTP) detection algorithm, in counts per second.
The corrected (i.e., total) count rate as obtained from the Voronoi Tessellation and Percolation (VTP) detection algorithm, in counts per second.
The Galactic Hydrogen column density from Dickey & Lockman (1990, ARAA, 28, 215), in units of H atoms cm-2.
The unabsorbed X-ray flux in the 0.5 - 2.0 keV band, in units of erg/cm2/s. For clusters of galaxies, the flux was calculated using the same iterative method which was used by Ebeling et al. (1998, MNRAS, 301, 881). For some clusters, this flux may include a component from contaminating sources (e.g., AGNs): see Section 4.4 of the published paper for details for each cluster. The authors assumed a Raymond-Smith spectrum with a redshift appropriate for each cluster and a metal abundance of 0.3 solar. The temperature of the model was derived iteratively by constraining the cluster to obey the observed L-T relation (White, Jones, & Forman 1997, MNRAS, 292, 419). Fluxes were obtained for AGNs and unidentified sources assuming a power-law spectrum with Fnu ~ nu-1, where nu is frequency. The fluxes for sources identified as stars were calculated assuming a Raymond-Smith model with a temperature of 2 x 106 K and with no correction for Galactic hydrogen column density.
The logarithm of the rest-frame source luminosity in the 0.5-2.0 keV band, in units of erg/s, derived in the same manner as the flux. Values of q0 = 0.5 and H0 = 50 km s-1 Mpc-1 were assumed.
The core radius of the cluster, in arcseconds. Note that this is very crude as it is based on ROSAT data which in most cases barely resolve the cluster.
The source extent parameter, defined as the ratio SKing/Spoint as discussed in Section 2.1 of the published paper.
The imaging status of the source. The letters indicates the band of the optical image(s) obtained, B, I or R.
The status of the spectroscopic follow-up, where a "Y" indicates that spectra were taken for this source. Note that the HEASARC has set values of this parameter which were "..." in the original published Tables 2 and 3 to "N"; also that for sources which were in Table 5 of the published paper but which were not listed in either Tables 2 or 3, the HEASARC has left the value blank.
The identification of the source (e.g., cluster, AGN, star). Identifications in lower case were identified based on the literature (primarily using NED and SIMBAD), while upper case IDs are based on WARPS optical follow-up observations. Sources listed as blends are briefly discussed in the notes parameter.
The redshift of the source, if known,
This parameter is a flag which is set to ":" to indicate that the redshift value is uncertain or to "]" if the redshift was estimated photometrically. Such individual cases are discussed in Section 4.4 of the published paper.
The number of galaxy redshifts used to derive the cluster redshift.
The spectral type, given for sources that have been identified as stars.
This parameter contains some additional flags, as follows: a "c" indicates that the cluster is contaminated or possibly contaminated by other sources; a "<" indicates that the cluster flux falls below the limit for inclusion in the statistically complete, flux-limited sample; a "?" indicates a possible cluster or group for which optical follow-up was not completed, usually because it was below the flux limit; an "8" indicates that the cluster was found in a field targeted at another cluster; a "b" indicates that this field was dropped due to high background. See the notes in Section 4.4 of the published paper for more details on the flagged sources.
This parameter contains alternate names and other notes. Sources listed as SHARC appear in the SHARC Bright Survey catalog (Romer et al. 2000, ApJS, 126, 209). Sources listed as VMF correspond to sources in the CfA 160 square degree survey of Vikhlinin et al. (1998, ApJ, 498, 21). Sources listed as RIXOS correspond to sources in the RIXOS survey catalog (Mason et al. 2000, MNRAS, 311, 456). NVSS (Condon et al. 1998, AJ, 115, 1693) and FIRST (e.g., White et al. 1997, ApJ, 475, 479) radio sources are also indicated.
The HEASARC created this new parameter in order to indicate from which table a particular entry originates: it is set to 2 for sources listed in Table 2 of the published paper, the WARPS-I Source Catalog, to 3 for sources listed in Table 3 of the published paper, the "Other Sources", and to 5 for sources listed in Table 5 of the published paper, the WARPS-I Additional Clusters and Candidates, which were not present in either Tables 2 or 3.
The HEASARC created this new parameter in order to indicate whether or not a source is part of the WARPS-I statistically complete, flux-limited sample, i.e., is listed in Table 4 of the published paper.
The HEASARC Browse object classification, based on the source_type and spect_type parameter values, if available.