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).
Cluster z Area Sensitivity Faintest source Obs. t. Tot. n. Cluster ${R}_{\rm vir}$ ${M}_{\rm vir}$ $N_{\rm comp}$

$(\hbox{$^\prime$ }^2)$ (5 $\sigma$ ) ( $\mu$ Jy) (s) sources galaxies ( h^-1 Mpc) (h^-1 10¹⁴ ${M}_\odot$ ) Detected Expected

Cl 0024 0.39 37.8 140 141 22615 35 13 0.94 6.42 10 -

A 370 0.37 40.5 350 208 22688 20 1 0.91 5.53 1 8

A 1689 0.18 36.0 450 320 9500 18 11 1.1 5.7 0 1

A 2390 0.23 7.0 100 54 29300 28 4 1.62 20.35 0 1

A 2218 0.18 20.5 125 90 22000 46 6 1.63 18.27 0 1

**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).
Cluster	z	Area	Sensitivity	Faintest source	Obs. t.	Tot. n.	Cluster	${R}_{\rm vir}$	${M}_{\rm vir}$	$N_{\rm comp}$
		$(\hbox{$^\prime$ }^2)$	(5 $\sigma$ )	( $\mu$ Jy)	(s)	sources	galaxies	( h^-1 Mpc)	(h^-1 10¹⁴ ${M}_\odot$ )	Detected	Expected
Cl 0024	0.39	37.8	140	141	22615	35	13	0.94	6.42	10	-
A 370	0.37	40.5	350	208	22688	20	1	0.91	5.53	1	8
A 1689	0.18	36.0	450	320	9500	18	11	1.1	5.7	0	1
A 2390	0.23	7.0	100	54	29300	28	4	1.62	20.35	0	1
A 2218	0.18	20.5	125	90	22000	46	6	1.63	18.27	0	1

Source LaTeX | All tables | In the text

	1 Introduction
	2 The cluster
	3 Observations, data reduction and source detection
	4 Results
	5 Spatial, dynamical and colour properties of the 15 $\mu$ m cluster galaxies
	6 Comparison of Cl 0024+1654 with other clusters observed by ISO
	7 Conclusions
	Appendix A: Additional notes on some mid-infrared sources
	References