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Figure 1:
Composite colour image of Sh2-212 in the optical.
North is up and east is left. The size of the field is
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Figure 2:
Composite colour image of Sh2-212 in the optical and the mid-IR.
Red corresponds to the MSX emission at 8.3 ![]() |
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Figure 3:
Sh2-212. Composite colour image of Sh2-212 in the near-IR (J is
blue, H is green, K is red). The colours of the stars are mainly
determined by extinction.
North is up and east is left. The size of the field is
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Figure 4: K versus J-K diagram. The main sequence is drawn for a visual extinction of zero (full line) and 3 mag (dotted line). The reddening lines, corresponding to a visual extinction of 30 mag, are issued from O3V and B2V stars. A few stars are identified, according to Fig. 6. Moffat et al.'s (1979) stars are identified by their number according to these authors. The asterisks are for 2MASS measurements. The connected full circles are for the star No. 228 (the YSO) and its associated nebulosity. |
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Figure 5:
J-H versus H-K diagram for stars with ![]() |
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Figure 6:
Identification of a few objects discussed in the text. The underlying
image is a colour composite of the [S II] frame (blue) and of the K frame
(orange). The lines indicate the limits of our ![]() |
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Figure 7:
Channel maps of the 12CO
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Figure 8:
Top left: condensation C1, showing the 13CO(2-1) emission integrated
between
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Figure 9: Molecular lines observed towards the molecular fragments C1 to C4. |
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Figure 10:
Radio continuum emission (contours)
superimposed on the H image (grey scale). Star No. 228 is indicated by an arrow.
The contours show 1.3 cm continuum emission from the UC H II region
coinciding in direction with the
MSX point source and the star. The angular resolution of the radio image
is
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Figure 11:
H I emission associated with Sh2-212, integrated between
-40 km s-1 and -48 km s-1. The radio angular
resolution (
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Figure 12: Spectral energy distribution of star No. 228, a massive YSO. Filled circles are the fluxes listed in Table 6. The five best fitting models obtained using the web-based tool of Robitaille et al. (2007) are presented. |
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Figure 13: Morphology of the Sh2-212 complex. |
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Figure 14: Confrontation of observations and simulations. Left: 12CO emission, integrated over the velocity. Right: simulation of a turbulent cloud illuminated by the UV radiation of a massive star (Dale et al. 2005, their Fig. 16). |
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