FSVSCLUSTR - Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups
The FSVS Cluster Catalogue: galaxy clusters and groups in the Faint Sky Variability Survey Soechting I.K., Huber M.E., Clowes R.G., Howell S.B. <Monthly Notices of the Royal Astronomical Society 369, 1334 (2006)> =2006MNRAS.369.1334S
The number of the FSVS field in which the cluster was detected.
The identification of the cluster, formed from the survey name (FSVSCL) and the J2000 coordinates.
The Right Ascension of the cluster center in the selected equinox. This corresponds to the mean position of its members. The RA was given in J2000 coordinates to a precision of 1 second of time in the original table.
The Declination of the cluster center in the selected equinox. This corresponds to the mean position of its members. The declination was given in J2000 coordinates to a precision of 1 arcsecond in the original table.
The Galactic Longitude of the cluster center.
The Galactic Latitude of the cluster center.
The number of member galaxies, defined as the number of all objects found within the boundary of the cluster and falling within the color-magnitude filter in which the cluster has been detected.
The number of all objects contained within the cluster boundary.
The area occupied by the cluster, in arcmin2.
The projected number density of member galaxies, in arcmin-2.
The apparent I magnitude of the brightest cluster galaxy.
The apparent I magnitude of the third brightest member galaxy in the cluster, m3.
The maximum color of the color-magnitude filter in which the cluster has been detected.
The richness of the cluster, defined as the number of galaxies found within its spatial boundary, its color filter, and the magnitude range between m3 < I < m3 + 2, where m3 is the magnitude of the 3rd brightest cluster member.
This parameter is a flag which is set to 1 to indicate that the richness is underestimated because of a restricted magnitude range.
The estimated redshift of the cluster.
This parameter is a flag which is set to 1 to indicate that the cluster parameters may possibly have been influenced by the field boundary.
The minimized value of the chi-squared parameter defined by equation (10) in the published paper, the cluster red sequence (CRS) chi-squared parameter, ChiCRS2.
The CRS probability defined as P_CRS = Pr(Chi2 < ChiCRS2) for a chi-squared distribution with (n-3) degrees of freedom, where n is the number of cluster members.