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Figure 9: Complement to Fig. 1. On-the-fly 1.3 mm continuum maps of Taurus embedded YSOs smoothed to a $13\hbox {$^{\prime \prime }$ }$ angular resolution. The positions of YSOs with weak emission are marked by star symbols. Contour levels and rms noise at map center are: a) 17 to 136 by 17 mJy/beam, $1\sigma \simeq 5$ mJy/beam; b) 20 40 mJy/beam, $1\sigma \simeq 6\$ mJy/beam; c) 25 to 100 by 25 mJy/beam, $1\sigma \simeq 6.5$ mJy/beam; d) 20 to 100 by 20 mJy/beam, $1\sigma \simeq 6.5$ mJy/beam

Figure 10: Complement to Fig. 2. On-the-fly 1.3 mm continuum maps of several isolated globules (a- d) and Perseus protostars (e- g) (all smoothed to a $13\hbox {$^{\prime \prime }$ }$ effective beam). Starless fragments are marked by cross symbols. Contour levels and rms noise at map center are: a) 40 to 160 by 40 mJy/beam, $1\sigma \simeq 11$ mJy/beam; b) 90, 180, 270 mJy/beam, $1\sigma \simeq 26$ mJy/beam; c) 75, 150, 225 mJy/beam, $1\sigma \simeq 22$ mJy/beam; d) 35 to 245 by 35 mJy/beam, $1\sigma \simeq 9.5$ mJy/beam; e) 75 to 600 by 75 mJy/beam and 700 to 1500 by 100 mJy/beam, $1\sigma \simeq 22$ mJy/beam; f) 75 to 300 by 75 mJy/beam and 450 600 by 750 mJy/beam, $1\sigma \simeq 21$ mJy/beam; g) 0.2 to 1 by 0.2 Jy/beam and 1.5, 2, 3, 4 Jy/beam, $1\sigma \simeq 55$ mJy/beam

Figure 11: Complement to Fig. 3. Radial intensity profiles of the environment of 12 Taurus embedded YSOs (a-l) and 4 starless cores (m-p). Column density estimates assuming $\k13=0.01\;\mbox{$\mbox{cm}^{2} \, \mbox{g}^{-1}$ }$ and $\mbox{$T_{\mbox{\tiny dust}}$ }=15\$K are shown on the right axis of each profile (in m-p: $\k13=0.005\;\mbox{$\mbox{cm}^{2} \, \mbox{g}^{-1}$ }$ and $\mbox{$T_{\mbox{\tiny dust}}$ }=10\$K). The observed profiles (solid curves) are compared with simulated model profiles (dotted curves) and with the 30 m beam (dashed curve). In b,c), e) and i), two source profiles are shown, before (upper solid curve) and after (lower solid curve) subtraction of the disk component observed by the IRAM Plateau de Bure interferometer at 1.4 mm (Motte et al. 2001); the latter should correspond to the profile of the envelope alone. The input models are all circularly symmetric with infinite power-law profiles, $I(\theta )\propto \theta ^{-m}$. Unlike YSO envelope profiles, the profiles of starless cores (in m-p) are not consistent with single power-law models

Figure 11: continued

Figure 12: Complement to Fig. 4. Radial intensity profiles of the environment of 3 isolated IRAS globules (a-c), 4 Perseus protostars (e-h), and 1 starless core (d). Column density estimates assume $\k13=0.01\;\mbox{$\mbox{cm}^{2} \, \mbox{g}^{-1}$ }$ and $\mbox{$T_{\mbox{\tiny dust}}$ }=20$K. In f-h), two source profiles are shown, before (upper solid curve) and after (lower solid curve) subtraction of the disk component observed by the IRAM PdBI interferometer at 1.4 mm (Motte et al. 2001). Unlike YSO envelope profiles, the profile of the starless core B361-NH3 (in d) is not consistent with a single power-law model