Volume 584, December 2015
|Number of page(s)||9|
|Section||Interstellar and circumstellar matter|
|Published online||04 December 2015|
In this section, a comparison between the IRAM-PdBI CO(2−1) data presented in this paper and the large-scale emission is presented. In particular, VLA SiO emission data from Choi (2005) and single-dish CO data by Yıldız et al. (2012) are shown. The comparison shows the change of propagation direction from north-south to about 45° in the large-scale CO emission (see also Blake et al. 1995; Girart et al. 1999; Choi 2001, 2005), which also seems to be consistent with the large-scale SiO data. Our possible evidence of precession in the A2 jet on very small scales (Fig. 5) is consistent with the large-scale CO and SiO morphologies, confirming that the A2 jet dominates the large-scale emission. Moreover, the non-detection in the IRAM-PdBI data of CO(2−1) emission associated with the A2 jet at distances larger than about 3′′ from the source is possibly due to filtering of large-scale emission by the interferometer, suggesting that the CO emission associated with the A2 jet is quite extended.
Upper: the VLA SiO(1−0) map (red and blue contours) by Choi (2005) is shown in comparison with the proposed propagation directions of the A1 and A2 jets (green solid lines, see Fig. 5). The positions of IRAS4A1 and A2 (this work) and of IRAS4B (Looney et al. 2000) are marked with green triangles. Lower: the PdBI CO(2−1) map (grey scale and black contours) integrated over the whole velocity range of emission (−20, +55 km s-1) is compared with the JCMT CO(3−2) (red and blue contours) and APEX CO(6−5) (magenta and cyan contours) maps from Yıldız et al. (2012). CO(2−1) emission is only shown within the PdBI field of view of 20′′ at 230 GHz. The CO(3−2) and CO(6−5) maps are integrated in the velocity ranges between −20 km s-1 and 3 km s-1 for the blue-shifted emission and 12 km s-1 and 50 km s-1 for the red-shifted emission. The contour levels start at the 3σ level and increase in steps of 3σ for the CO(2−1) emission, from the 5σ level emission in steps of 10σ for the CO(3−2), and from the 5σ level emission in steps of 5σ for the CO(6−5).
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Figure B.1 shows the additional lines detected in the WideX spectra at the peak of the EHV gas that are analysed and discussed in the main text (see also Fig. 6 and Sect. 4.1). In particular, the CO(2−1), SO(65−54), H2CO(321−220), and H2CO(303−202) lines show a double-peaked profile with a velocity component peaking around the systemic velocity and a secondary velocity component around 50 km s-1; the SiO(5−4) line profile presents a broad wing emission that peaks at 50 km s-1 and extends down to the systemic velocity; finally, the 13CO(2−1), H2CO(322−221), CH3OH(422−312), and CH3OH(808−717) line profiles show a single emission peak around systemic velocity, possibly due to a lack of sensitivity.
Additional lines detected in the WideX spectra at the peak of the EHV gas.
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© ESO, 2015
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