Table 1: Photometry of sources in the field.

Source		   $\alpha$(J2000) $\delta$(J2000) $F_{\rm B}$ $F_{\rm R}$ $F_{\rm J}$ $F_{\rm H}$ $F_{K_{\rm s}}$ $F_{6.75~\mu{\rm m}}^{a}$ $F_{15~\mu{\rm m}}^{a}$ $F_{24~\mu{\rm m}}$ $F_{70~\mu{\rm m}}$ $F_{850~\mu{\rm m}}$
        mJy mJy mJy mJy mJy Jy Jy Jy Jy Jy
A   23:40:54.65 +61:10:27.6 - - - - - - - 0.14 65 2.2
B   23:40:50.42 +61:10:37.4 - - 0.8 1.5 1.7 0.2 0.14 0.16 <25 <0.3
C   23:40:50.25 +61:10:27.6 - - 1.5 6.1 10.6 <0.02 0.6 0.6 <25 <0.3
D   23:40:57.11 +61:10:41.0 - - 0.07 0.35 0.7 0.2 0.1 0.3 <25 <0.4
E   23:40:56.35 +61:10:30.0 - - 0.07 0.16 0.6 0.3 0.2 1.0 <35 <0.8
F   23:40:55.50 +61:10:49.0 - - - - - 0.26 0.2 0.5 12 <0.5
G   23:40:52.62 +61:11:09.2 - - 0.1 0.06 0.2 -e -e 0.13 <30 <0.5
       1 23:40:58.97 +61:10:27.9 0.1 0.4 0.07 0.5 0.5          
Hb      2 23:40:59.04 +61:10:33.3 0.05 0.2 0.07 0.1 0.1 <0.01 <0.15 0.14 <20 <0.2
       3 23:40:59.11 +61:10:43.8 - - 0.8 0.8 0.6          
I   23:40:57.62 +61:11:08.0 0.2 0.7 6.4 6.6 5.1 0.24 0.1 0.08 -c <0.2
L   23:40:49.23 +61:11:23.9 - - 0.64 2.0 5.5 -e -e 0.3 -c <0.1
M   23:40:47.45 +61:10:57.6 - - - - - 0.04 0.01 0.33 <15 <0.2
N   23:40:41.44 +61:10:28.1 - - 0.5 1.5 2.4 -e -e 0.4 -c -d
P   23:40:49.23 +61:10:11.6 - - 0.4 1.7 4.9 0.02 0.03 0.1 <15 <0.4
R   23:40:48.55 +61:10:15.9 - - 1.0 1.3 2.1 -e -e 0.08 <15 <0.4
a From ISOCAM images (Molinari et al. 1998b).
b Although the positional association of other $K_{\rm s}$ sources to the 24 $\mu $m peaks is very good (see Fig. 1b), it seems likely that source H, since it is much shallower than the other 24 $\mu $m peaks, could be associated to one of the three nearest $K_{\rm s}$ sources visible in its close proximity.
c This source is not covered by the 70 $\mu $m image.
d This source is not covered by the 850 $\mu $m image.
e This source is not covered by the ISOCAM images.


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