WARPS2 - Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog
The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.
The WARPS survey. VII. The WARPS-II cluster catalog. Horner D.J., Perlman E.S., Ebeling H., Jones L.R., Scharf C.A., Wegner G., Malkan M., Maughan B. <Astrophys. J. Suppl. Ser., 176, 374-413 (2008)> =2008ApJS..176..374H 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 cluster name, of the J2000.0-based form 'WARPS JHHMM.m+DDMMA' recommended by the Dictionary of Nomenclature of Celestial Objects (superceding the form 'WARP JHHMM.m+DDMMA' used in the paper itself), where 'A' is used to differentiate a few spatially close clusters and can be either 'E' or 'W'. Many WARPS-II clusters have been previously identified, mostly by other serendipitous cluster surveys similar to WARPS (see Section 4 of the reference paper). The known aliases for WARPS-II clusters (usually listed as they appear in NED) are given in the alt_names parameter.
The Right Ascension of the WARPS-II cluster in the selected equinox. This was given in J2000.0 decimal degrees to a precision of 10-4 degrees in the original table.
The Declination of the WARPS-II cluster in the selected equinox. This was given in J2000.0 decimal degrees to a precision of 10-4 degrees in the original table.
The Galactic Longitude of the WARPS-II cluster.
The Galactic Latitude of the WARPS-II cluster.
The Galactic hydrogen column density in the direction of the WARPS-II cluster, in cm-2, taken from Dickey & Lockman, (1990, ARA&A, 28, 215).
The unabsorbed source flux in the 0.5-2.0 keV energy band, in erg cm-2 s-1. The authors calculated the final flux from the total count rate using the same iterative method as Ebeling et al. (1998, MNRAS, 301, 881). They assume a Raymond-Smith spectrum with the measured cluster redshift (see Section 2.3 of the reference paper), a metal abundance of 0.3 solar, and the hydrogen column density for the cluster coordinates from Dickey & Lockman (1990, ARAA, 28, 215). The temperature of the model was derived iteratively by constraining the cluster to obey the L - T relation, TX in keV = 2.76 Lbol0.33 (White et al. 1997, MNRAS, 292, 419).
The logarithm of the rest-frame source luminosity of the cluster in the 0.5-2.0 keV band derived in the same manner as the flux, in erg s-1. This was derived assuming a cosmology in which q = 0.5 and H0 = 50 km s-1 Mpc-1.
The logarithm of the rest-frame source luminosity of the cluster in the 0.5-2.0 keV band derived in the same manner as the flux, in erg s-1. This was derived assuming a cosmology in which H0= 70 km s-1 Mpc-1, OmegaM=0.3 and OmegaLambda=0.7.
The redshift of the cluster.
The number of galaxy redshifts used to derive the cluster redshift.
This flag parameter is set to '?' to indicate that there is uncertainty in the number of valid galaxy redshifts used to derive the cluster redshift, or to '.5' in one case (WARPS J1117.5+0746) so as to indicate that, in addition to one good-quality galaxy redshift which was used (indicated by a num_redshifts value of 1), one low-quaility galaxy redshift was also used to calculate the cluster redshift (a value of 1.5 is given for the number of redshifts for this cluster in the published paper).
The estimated core radius of the cluster, in arcseconds, assuming a King profile with beta = 2/3. Note that these should be interpreted with caution given the size of the ROSAT PSF. Clusters that the authors split on the basis of redshift or other information do not have measured core radii.
Notes or comments (if any) about the source. See Section 3.2 of the published paper for more details about many of these sources.
The known aliases for the WARPS-II cluster (usually listed as they appear in NED).
This parameter was added by the HEASARC in order to allow users to easily identify from which of the samples discussed in the reference paper a given source was taken. Sources which were in Table 2, the WARPS-II statistically complete, flux-limited sample, have been given source_sample values of 'Main', while those in Table 3, the WARPS-II additional clusters and candidates, have been given source_sample values of 'Other'.