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.
Filter $\lambda_{\rm ref}$ n Steps dm dn Reads area Done k Sensitivity Tot. t

( $\mu$ m) M N ( $^{\prime \prime }$ ) ( $^{\prime \prime }$ ) per step $(\hbox{$^\prime$ }^2)$ times ( $\mu$ Jy) (sec)

LW2 6.7 6 6 45 45 14 28.6 1 400 3138

LW3 14.3 14 14 21 21 10 37.8 2 140 22 615

**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.
Filter	$\lambda_{\rm ref}$	n Steps	dm	dn	Reads	area	Done k	Sensitivity	Tot. t
	( $\mu$ m)	M	N	( $^{\prime \prime }$ )	( $^{\prime \prime }$ )	per step	$(\hbox{$^\prime$ }^2)$	times	( $\mu$ Jy)	(sec)
LW2	6.7	6	6	45	45	14	28.6	1	400	3138
LW3	14.3	14	14	21	21	10	37.8	2	140	22 615

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