EDP Sciences
Free Access
Issue
A&A
Volume 563, March 2014
Article Number L3
Number of page(s) 7
Section Letters
DOI https://doi.org/10.1051/0004-6361/201323024
Published online 25 February 2014

Online material

Appendix A: The 3.2 mm continuum emission

Figure A.1 shows the emission map of the 3.2 mm continuum dust emission, which was produced as the 1.4 mm map using robust weighting, and restored with a clean beam of (PA = 38°). The 3.2 mm emission allows us to detect the MM1 (α(J2000): 03h 28m 5556, δ(J2000): +31° 14 3693) and MM2 (α(J2000): 03h 28m 5569, δ(J2000): +31° 14 3563) sources, consistent with what was found in the 1.4 mm image (see Table 1 and Fig. 1). The peak fluxes are 17 mJy beam-1 and 2 mJy beam-1 for MM1 and MM2, respectively. On the other hand, MM3 (revealed at 1.4 mm) is not detected at a 3σ sensitivity level of 0.75 mJy beam-1.

thumbnail Fig. A.1

Contour plots of the IRAS2A continuum emission at 3.2 mm. The ellipse shows the PdBI synthesised beam (HPBW): (PA = 38°). First contours and steps correspond to 5σ (1.3 mJy beam -1). Labels indicate the main source MM1 and the weaker source MM2. The black triangle stands for the position of MM3, revealed at 1.4 mm and not detected at 3.2 mm.

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Appendix B: SiO and SO channel maps

We show in Figs. A.1 and A.2 the channel maps of the SiO(5–4) and SO(65–54) blue- and redshifted (continuum subtracted) emissions towards IRAS2A. The images trace the clumps well at different velocities along the N-S jet driven by MM1 and also trace the redshifted E lobe associated with MM2. The grey lines show the deceleration of the highest velocity clumps.

Figure A.3 shows the SiO and SO PV diagrams along the E-W jet axis: as in the N-S case, the SiO emitting at the highest velocities is closely associated with the driving source MM2, confirming that SiO is a powerful tracer of the jet launching region.

thumbnail Fig. B.1

Channel maps of the SiO(5–4) blue- and redshifted (continuum subtracted) emissions towards IRAS2A. Each panel shows the emission integrated over a velocity interval of 2.5 km s-1 centred at the value given in the upper-right corner. The thick box and the magenta contours indicate the range associated with the systemic velocity. Thick contours correspond to the 5σ emission of the 1.4 mm continuum map shown in Fig. 1 and indicate the position of the MM1, MM2, and MM3 continuum sources. The ellipse in the top-left panel shows the PdBI synthesised beam (HPBW): (PA = 33°). First contours and steps correspond to 5σ (15 mJy beam -1 km s-1) and 10σ, respectively. Grey lines indicate the slowing down of the highest velocity SiO clumps (see text).

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thumbnail Fig. B.2

Channels map of the SO(65–54) blue- and redshifted (continuum subtracted) emissions towards IRAS2A. Each panel shows the emission integrated over a velocity interval of 2.7 km s-1 centred at the value given in the upper-right corner. Symbols are drawn as in Fig. 2. The ellipse in the top-left panel shows the PdBI synthesised beam (HPBW): (PA = 33°). First contours and steps correspond to 5σ (15 mJy beam-1 km s-1) and 10σ, respectively. Grey lines indicate the slowing down of the highest velocity SO clump (see text).

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thumbnail Fig. B.3

Position-velocity cut of SiO(5–4) (grey scale and black contours) and SO(65–54) (magenta contours) along the whole E-W jet (PA = 105°, see the grey line in Fig. 1). First contours and steps correspond to 5σ (2.5 K for SiO and 4.0 K for SO) and 3σ, respectively. Dashed lines mark the positions of MM2 and the protostellar envelope VLSR (+6.5 km s-1). We note that the SiO and SO emission at negative angular offsets traces the N-S outflow driven by MM1 (see Fig. 1).

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© ESO, 2014

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