All Tables

Table 1: Observational parameters used. The observations were made with the ISOCAM LW2 (5-8.5 $\mu$ m) and LW3 (12-18 $\mu$ m) filters at their respective reference wavelengths of 6.7 $\mu$ m and 14.3 $\mu$ m. On-chip integration time was always 5.04 seconds and the 3 $^{\prime \prime }$ per-pixel-field-of-view was used. M and N are the number of steps along each dimension of the raster, while dm and dn are the increments for a raster step. The sensitivity in $\mu$ Jy is given at the 5 $\sigma$ level. The table also includes the total area covered and the number of readouts per raster step. The rasters were repeated k times. Tot. t is the total time dedicated to each filter observation.
Table 2: The primary list of sources detected at 15 $\mu$ m. The columns are (from left to right): source identification number in order of increasing Right Ascension; source flux and precision before calibration (in ADUgs); source flux and precision after calibration (in mJy); Right Ascension and Declination of the infrared source (J2000); redshift and name of the optical counterpart, if known. The redshift of source ISO_Cl0024_02 was taken from Schmidt et al. (1986). All other redshifts are from Czoske et al. (2001) or provided by T. Treu (private communication). The names of the stars are from HEASARC.
Table 3: The supplementary list of 15 $\mu$ m sources. The meaning of the columns is the same as in Table 2.
Table 4: The list of 7 $\mu$ m sources with source flux exceeding 5 $\sigma$ of the local noise, and having 15 $\mu$ m counterparts. From left to right: 15 $\mu$ m source identification number as listed in Table 2; signal and precision of flux in ADU; flux and precision in mJy; Right Ascension, Declination; nature of the source; and finally the [7 $\mu$ m]/[15 $\mu$ m] colour ratio.
Table 5: References to ISOCAM sources in existing archives. The first column lists the source number from Tables 2 and 3. The key to the references in Cols. 2 to 8 is Dressler & Gunn (1992, DG), Czoske et al. (2001, CKS), Schneider et al. (1986, SDG), Smail et al. (1997, SDC), McLean & Teplitz (1996, MT), Butcher & Oemler (1978, BO), Soucail et al. (2000, S) and Pickles & van der Kruit (1991, P). The table does not include the four stars or the quasar PC 0023+1653.
Table 6: Results from model SEDs for known cluster galaxies in Cl 0024+1654. The columns list: LW3 identification number; best-fit SED model; number of data points in the observed SED; $\chi ^2$ of the fit; rejection probability of the fit; other acceptable models (rejection probability 95% or less); 15 $\mu$ m k-correction; luminosity at 15 $\mu$ m (h=0.7, $\Omega _{\rm m}=0.3$ , $\Omega _l=0.7$ ) using the transformation from Boselli et al. (1998), and k-corrected using best-fit SED; total infrared luminosity including the k-correction using the best-fit SED and computed using the transformation from Elbaz et al. (2002); SFR from total IR luminosity using the transformation of Kennicutt (1998); position in the V-I vs. I colour-magnitude diagram (Fig. 7) where "MS'' stands for "Main Sequence'', "BO'' for "Butcher-Oemler'', "U'' for "Unknown''; EW [O II] line from Czoske et al. (2001); SFR computed from the [O II] emission line using the transformation to the optical SFR; ratio infrared to optical SFR.
Table 7: Summary of ISOCAM observations and results at 15 $\mu$ m for five clusters of galaxies. The data was obtained from Metcalfe et al. (2003) for Abell 370, Abell 2218 and Abell 2390, Fadda et al. (2000) and Duc et al. (2002) for Abell 1689, and this paper for Cl 0024+1654. The content of the columns in the table are as follows: name and redshift of the cluster, total area scanned, sensitivity reported at the $5\sigma$ level, flux of the weakest reported source in $\mu$ Jy, total observation time, total number of sources detected including sources without redshifts and stars. Then number of cluster galaxies, virial radius, virial mass, number of sources with ${L_{\rm IR}>9\times10^{10}~L_{\odot}}$ detected and expected. The expected number of sources was obtained by comparison with Cl 0024+1654 as described in the text. Virial radii and masses are from Girardi & Mezzetti (2001) and King et al. (2002).