2015A&A...577A..49N


Query : 2015A&A...577A..49N

2015A&A...577A..49N - Astronomy and Astrophysics, volume 577A, 49-49 (2015/5-1)

Sulphur-bearing molecules in diffuse molecular clouds: new results from SOFIA/GREAT and the IRAM 30 m telescope.

NEUFELD D.A., GODARD B., GERIN M., PINEAU DES FORETS G., BERNIER C., FALGARONE E., GRAF U.U., GUESTEN R., HERBST E., LESAFFRE P., SCHILKE P., SONNENTRUCKER P. and WIESEMEYER H.

Abstract (from CDS):

We have observed five sulphur-bearing molecules in foreground diffuse molecular clouds lying along the sight-lines to five bright continuum sources. We have used the GREAT instrument on SOFIA to observe the SH 1383 GHz 2Π3/2 J=5/2←3/2 lambda doublet toward the star-forming regions W31C, G29.96-0.02, G34.3+0.1, W49N and W51, detecting foreground absorption towards all five sources; and the EMIR receivers on the IRAM 30 m telescope at Pico Veleta to detect the H2S 110-101 (169GHz), CS J=2-1 (98GHz) and SO 32-21 (99GHz) transitions. Upper limits on the H3S+ 10-00 (293GHz) transition were also obtained at the IRAM 30 m. In nine foreground absorption components detected towards these sources, the inferred column densities of the four detected molecules showed relatively constant ratios, with N(SH)/N(H2S) in the range 1.1-3.0, N(CS)/N(H2S) in the range 0.32-0.61, and N(SO)/N(H2S) in the range 0.08-0.30. The column densities of the sulphur-bearing molecules are very well correlated amongst themselves, moderately well correlated with CH (a surrogate tracer for H2), and poorly correlated with atomic hydrogen. The observed SH/H2 ratios - in the range 5 to 26x10–9 - indicate that SH (and other sulphur-bearing molecules) account for ≪1% of the gas-phase sulphur nuclei. The observed abundances of sulphur-bearing molecules, however, greatly exceed those predicted by standard models of cold diffuse molecular clouds, providing further evidence for the enhancement of endothermic reaction rates by elevated temperatures or ion-neutral drift. We have considered the observed abundance ratios in the context of shock and turbulent dissipation region (TDR) models. Using the TDR model, we find that the turbulent energy available at large scale in the diffuse ISM is sufficient to explain the observed column densities of SH and CS. Standard shock and TDR models, however, fail to reproduce the column densities of H2S and SO by a factor of about 10; more elaborate shock models - in which account is taken of the velocity drift, relative to H2, of SH molecules produced by the dissociative recombination of H3S+ - reduce this discrepancy to a factor ∼3.

Abstract Copyright:

Journal keyword(s): astrochemistry - ISM: molecules - submillimeter: ISM - molecular processes - ISM: clouds

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 3C 111 Sy1 04 18 21.2772425736 +38 01 35.801359968   19.75 18.05     ~ 894 1
2 W 31c HII 18 10 29.1 -19 56 05           ~ 321 0
3 GRS G018.85 +01.79 Rad 18 17.8 -11 54           ~ 25 1
4 CORNISH G029.9559-00.0168 Y*O 18 46 04.18 -02 39 21.3           ~ 351 0
5 OH 34.26 +0.15 SFR 18 53 18.54 +01 14 57.9           ~ 482 0
6 W 49n HII 19 10 13.2 +09 06 12           ~ 434 3
7 W 51 SNR 19 23 50 +14 06.0           ~ 1209 1

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2022.05.28-22:23:43

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