| Issue |
A&A
Volume 557, September 2013
|
|
|---|---|---|
| Article Number | A98 | |
| Number of page(s) | 25 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201321204 | |
| Published online | 10 September 2013 | |
Online material
Mopra centroid velocities toward the central position, P1.
CS 5−4 and H13CO+ 4−3 centroid velocities (APEX) at positions perpendicular to the filament.
H13CO+ 3−2 centroid velocities (APEX) at positions parallel and perpendicular to the filament.
C17O 2−1 and C18O 2−1 centroid velocities (APEX) at positions perpendicular to the filament.
Observed linewidth, thermal, and non-thermal velocity dispersions toward the central position.
 |
Fig. 2
Transitions observed with Mopra towards the central position of Cha-MMS1, in main-beam brightness temperature scale. The dotted line shows the systemic velocity of Cha-MMS1, derived from a seven component hyperfine fit to the N2H+ 1−0 multiplet. |
| Open with DEXTER | |
 |
Fig. 3
Transitions observed with APEX towards the central position of Cha-MMS1, in main-beam brightness temperature scale. The dotted line shows the systemic velocity of Cha-MMS1, derived from a seven component hyperfine fit to the N2H+ 1−0 multiplet observed with Mopra without correcting for the +0.1 km s-1 velocity shift (see Sect. 3.2.1). |
| Open with DEXTER | |
 |
Fig. 12
Transition opacities for the best fit model “MCS”. The dotted line shows the systemic velocity of Cha-MMS1. For the APEX spectra, a correction of 0.1 km s-1 was added (see Sect. 3.2.1). |
| Open with DEXTER | |
 |
Fig. 13
Kinetic (black) and excitation temperature (colour) for all the transitions of the best fit model “MCS”. |
| Open with DEXTER | |
 |
Fig. 15
Transition opacities for the best fit model “MHCOP”. The dotted line shows the systemic velocity of Cha-MMS1. For the APEX spectra, a correction of 0.1 km s-1 was added (see Sect. 3.2.1). |
| Open with DEXTER | |
 |
Fig. 16
Same as Fig. 13 for the best fit model “MHCOP”. |
| Open with DEXTER | |
 |
Fig. 18
Transition opacities for the best fit model “MCO”. The dotted line shows the systemic velocity of Cha-MMS1. For the APEX spectra, a correction of 0.1 km s-1 was added (see Sect. 3.2.1). |
| Open with DEXTER | |
© ESO, 2013
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