All Tables

Table 1: Summary of the imaging data. The magnitude limits are $5\sigma$ limits in 2 $^{\prime \prime }$ diameter apertures.
Table 2: Spectroscopic catalog. The columns show object ID, coordinates in J2000, redshift, confidence flag (0 and 1 mean secure and possible redshifts, respectively), and aperture magnitudes within 2 $^{\prime \prime }$ apertures and their errors. The systematic zero point errors are not included here. The redshift error does not include wavelength calibration error, which is typically $0.3~\rm\AA$ . Full Table 2 is available in electronic form.
Table 3: X-ray properties of the four clumps (see Fig. 4 for the definition of the clumps). Clump 3 is not detected in the X-ray data, and the numbers quoted below are $3\sigma$ limits. The coordinates correspond to the peak of the X-ray emission. The L_X luminosity is based on the extrapolation of the detected flux to R₅₀₀, described in Finoguenov et al. (2007). The total mass is computed using the scaling relations (L_X-M) with the weak lensing calibration for mass from COSMOS, achieved at a similar redshift ( $z\sim 0.9$ ) and luminosity range (Leauthaud et al. in prep.). The newly discovered clumps are assumed to lie at the same redshift as the RDCSJ0910 cluster (i.e., clump 1).
Table 4: Intrinsic $i-K_{\rm s}$ color scatter around the red sequence as a function of $K_{\rm s}$ band magnitude.
Full version
Table 2: Spectroscopic catalog. The columns show object ID, coordinates in J2000, redshift, confidence flag (0 and 1 mean secure and possible redshifts, respectively), and aperture magnitudes within 2 $^{\prime \prime }$ apertures and their errors. The systematic zero point errors are not included here. The redshift error does not include wavelength calibration error which is typically $0.3~\rm\AA$ .