2010A&A...521L..13M


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.19CEST15:30:27

2010A&A...521L..13M - Astronomy and Astrophysics, volume 521, L13-13 (2010/10-1)

Excitation and abundance of C3 in star forming cores. Herschel/HIFI observations of the sight-lines to W31C and W49N.

MOOKERJEA B., GIESEN T., STUTZKI J., CERNICHARO J., GOICOECHEA J.R., DE LUCA M., BELL T.A., GUPTA H., GERIN M., PERSSON C.M., SONNENTRUCKER P., MAKAI Z., BLACK J., BOULANGER F., COUTENS A., DARTOIS E., ENCRENAZ P., FALGARONE E., GEBALLE T., GODARD B., GOLDSMITH P.F., GRY C., HENNEBELLE P., HERBST E., HILY-BLANT P., JOBLIN C., KAZMIERCZAK M., KOLOS R., KRELOWSKI J., LIS D.C., MARTIN-PINTADO J., MENTEN K.M., MONJE R., PEARSON J.C., PERAULT M., PHILLIPS T.G., PLUME R., SALEZ M., SCHLEMMER S., SCHMIDT M., TEYSSIER D., VASTEL C., YU S., DIELEMAN P., GUESTEN R., HONINGH C.E., MORRIS P., ROELFSEMA P., SCHIEDER R., TIELENS A.G.G.M. and ZMUIDZINAS J.

Abstract (from CDS):

We present spectrally resolved observations of triatomic carbon (C3) in several ro-vibrational transitions between the vibrational ground state and the low-energy ν2 bending mode at frequencies between 1654-1897GHz along the sight-lines to the submillimeter continuum sources W31C and W49N, using Herschel's HIFI instrument. We detect C3 in absorption arising from the warm envelope surrounding the hot core, as indicated by the velocity peak position and shape of the line profile. The sensitivity does not allow to detect C3 absorption due to diffuse foreground clouds. From the column densities of the rotational levels in the vibrational ground state probed by the absorption we derive a rotation temperature (Trot) of ∼50-70K, which is a good measure of the kinetic temperature of the absorbing gas, as radiative transitions within the vibrational ground state are forbidden. It is also in good agreement with the dust temperatures for W31C and W49N. Applying the partition function correction based on the derived Trot, we get column densities N(C3)∼7-9x1014cm–2 and abundance x(C3)∼10–8 with respect to H2. For W31C, using a radiative transfer model including far-infrared pumping by the dust continuum and a temperature gradient within the source along the line of sight we find that a model with x(C3)=10–8, Tkin=30-50K, N(C3)=1.5x1015cm–2 fits the observations reasonably well and provides parameters in very good agreement with the simple excitation analysis.

Abstract Copyright:

Journal keyword(s): ISM: lines and bands - ISM: molecules - radiative transfer - ISM: individual objects: W49N - ISM: individual objects: W31C

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 IRC +10216 C* 09 47 57.406 +13 16 43.56     10.96     C9,5e 2102 0
2 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1851 1
3 W 31 SFR 18 10 28.6 -19 55 51           ~ 240 0
4 W 31c HII 18 10 29.1 -19 56 05           ~ 298 0
5 W 49n HII 19 10 13.2 +09 06 12           ~ 403 3
6 W 49a SFR 19 10 15.7 +09 06 05           ~ 255 2

    Equat.    Gal    SGal    Ecl

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2019.10.19-15:30:27

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