Table 2: MIR fluxes for the Spitzer-IRAC sources towards the mm core.

ID		 Position $F_{\nu}(3.6)$ $F_{\nu}(4.5)$ $F_{\nu}(5.8)$ $F_{\nu}(8.0)$
  $\alpha(2000)$ $\delta(2000)$ (mJy) (mJy) (mJy) (mJy)

1		 $\rm05^{h}40^{m}54.2^{s}$ $35\degr41\hbox{$^\prime$ }59\hbox{$^{\prime\prime}$ }$ $8.6 \pm 0.8$ $7.0 \pm 0.8$ <12 <39
2 $\rm05^{h}40^{m}53.7^{s}$ $35\degr41\hbox{$^\prime$ }56\hbox{$^{\prime\prime}$ }$ $7.8 \pm 0.9$ $4.7 \pm 1.2$ <11 <19
3 $\rm05^{h}40^{m}53.5^{s}$ $35\degr41\hbox{$^\prime$ }53\hbox{$^{\prime\prime}$ }$ $17.2 \pm 0.3$ $21.2 \pm 0.6$ $29 \pm 1$ $43 \pm 4$
4 $\rm05^{h}40^{m}53.7^{s}$ $35\degr41\hbox{$^\prime$ }47\hbox{$^{\prime\prime}$ }$ $1.9 \pm 0.2$ $2.9 \pm 0.4$ <3 <5
5 (M 1) $\rm05^{h}40^{m}53.6^{s}$ $35\degr41\hbox{$^\prime$ }43\hbox{$^{\prime\prime}$ }$ $8.6 \pm 0.1$ $15.0 \pm 0.1$ $16 \pm 1$ $13 \pm 1$
6 $\rm05^{h}40^{m}54.0^{s}$ $35\degr41\hbox{$^\prime$ }41\hbox{$^{\prime\prime}$ }$ $2.1 \pm 0.1$ $4.8 \pm 0.1$ $9 \pm 1$ $9 \pm 1$
7 $\rm05^{h}40^{m}54.4^{s}$ $35\degr41\hbox{$^\prime$ }29\hbox{$^{\prime\prime}$ }$ $5.9 \pm 0.1$ $7.5 \pm 0.1$ $9 \pm 1$ $10 \pm 1$
8 $\rm05^{h}40^{m}53.8^{s}$ $35\degr41\hbox{$^\prime$ }27\hbox{$^{\prime\prime}$ }$ $33.6 \pm 0.1$ $33.1 \pm 0.1$ $36 \pm 1$ $54 \pm 1$
9a $\rm05^{h}40^{m}52.2^{s}$ $35\degr41\hbox{$^\prime$ }41\hbox{$^{\prime\prime}$ }$ $5.0 \pm 0.3$ $4.7 \pm 0.2$ <5 <24
10 $\rm05^{h}40^{m}52.7^{s}$ $35\degr41\hbox{$^\prime$ }45\hbox{$^{\prime\prime}$ }$ $8.5 \pm 0.2$ $7.6 \pm 0.2$ $9 \pm 1$ $18 \pm 7$
11 $\rm05^{h}40^{m}52.2^{s}$ $35\degr41\hbox{$^\prime$ }55\hbox{$^{\prime\prime}$ }$ $5.4 \pm 0.8$ $2.9 \pm 0.7$ <17 <95
12 $\rm05^{h}40^{m}51.7^{s}$ $35\degr41\hbox{$^\prime$ }57\hbox{$^{\prime\prime}$ }$ $3.5 \pm 0.8$ $2.7 \pm 0.6$ <20 <59
13 (S235AB-MIR) $0\rm 5^{h}40^{m}53.4^{s}$ $35\degr41\hbox{$^\prime$ }49\hbox{$^{\prime\prime}$ }$ <0.6 $5.0 \pm 0.3$ $14 \pm 1$ $28 \pm 2$
14 $\rm05^{h}40^{m}53.0^{s}$ $35\degr41\hbox{$^\prime$ }53\hbox{$^{\prime\prime}$ }$ $1.7 \pm 0.9$ $3.7 \pm 1.0$ $3 \pm 4$ <35
15 $\rm05^{h}40^{m}52.7^{s}$ $35\degr41\hbox{$^\prime$ }52\hbox{$^{\prime\prime}$ }$ $2.4 \pm 1.1$ $1.2 \pm 0.9$ <9 <22

a N-E of a close by source only visible in the 5.8 $\mu $m band.

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