EDP Sciences
Free Access
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

Table 6

Mopra centroid velocities toward the central position, P1.

Table 7

CS 5−4 and H13CO+ 4−3 centroid velocities (APEX) at positions perpendicular to the filament.

Table 8

H13CO+ 3−2 centroid velocities (APEX) at positions parallel and perpendicular to the filament.

Table 9

C17O 2−1 and C18O 2−1 centroid velocities (APEX) at positions perpendicular to the filament.

Table 11

Observed linewidth, thermal, and non-thermal velocity dispersions toward the central position.

thumbnail 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.

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thumbnail 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

thumbnail 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).

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thumbnail Fig. 13

Kinetic (black) and excitation temperature (colour) for all the transitions of the best fit model “MCS”.

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thumbnail 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

thumbnail Fig. 16

Same as Fig. 13 for the best fit model “MHCOP”.

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thumbnail 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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