2022A&A...662A..52E


Query : 2022A&A...662A..52E

2022A&A...662A..52E - Astronomy and Astrophysics, volume 662A52-52 (2022/6-1)

Gas phase Elemental abundances in Molecular cloudS (GEMS). VI. A sulphur journey across star-forming regions: study of thioformaldehyde emission.

ESPLUGUES G., FUENTE A., NAVARRO-ALMAIDA D., RODRIGUEZ-BARAS M., MAJUMDAR L., CASELLI P., WAKELAM V., ROUEFF E., BACHILLER R., SPEZZANO S., RIVIERE-MARICHALAR P., MARTIN-DOMENECH R. and MUNOZ CARO G.M.

Abstract (from CDS):


Context. In the context of the IRAM 30 m Large Program Gas phase Elemental abundances in Molecular CloudS (GEMS), we present a study of thioformaldehyde (H2CS) and its deuterated versions (HDCS and D2CS) in several starless cores located in a selected set of star-forming filaments of Taurus, Perseus, and Orion. These regions have different star formation activities and, therefore, distinct physical and chemical conditions.
Aims. Our goal is to investigate the influence of the environmental conditions on the abundances of these molecules in the cores, as well as the effect of time evolution.
Methods. We have modelled the observed lines of H2CS, HDCS, and D2CS using the radiative transfer code RADEX. We have also used the chemical code Nautilus to model the evolution of these species depending on the characteristics of the starless cores.
Results. We derive column densities and abundances for all the cores. We also derive deuterium fractionation ratios, Dfrac, which allow us to determine and compare the evolutionary stage between different parts of each star-forming region. Our results indicate that the north region of the B 213 filament in Taurus is more evolved than the south, while the north-eastern part of Perseus presents an earlier evolutionary stage than the south-western zone. Model results also show that Dfrac decreases with the cosmic-ray ionisation rate, while it increases with density and with the degree of sulphur depletion. In particular, we can only reproduce the observations when the initial sulphur depletion in the starless cores is at least one order of magnitude lower than the solar elemental sulphur abundance.
Conclusions. The progressive increase in HDCS/H2CS and D2CS/H2CS with time makes these ratios powerful tools for deriving the chemical evolutionary stage of starless cores. However, they cannot be used to derive the temperature of these regions, since both ratios present a similar evolution at two different temperature ranges (∼7-11 K and ∼ 15-19 K). Regarding chemistry, (deuterated) thioformaldehyde is mainly formed through gas-phase reactions (double-replacement and neutral-neutral displacement reactions), while surface chemistry plays an important role as a destruction mechanism.

Abstract Copyright: © ESO 2022

Journal keyword(s): astrochemistry - ISM: abundances - ISM: molecules - ISM: clouds - stars: formation

Simbad objects: 61

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Number of rows : 61
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 LDN 1448 DNe 03 22.5 +30 35           ~ 546 0
2 [KJT2007] SMM J032581+30423 cor 03 25 49.0 +30 42 25           ~ 17 1
3 LDN 1455 DNe 03 28 00.6480 +30 07 58.800           ~ 198 1
4 [HRF2005] 60 Y*O 03 28 39.3 +31 18 27           ~ 15 0
5 [HFR2007] 53 smm 03 29 04.75 +31 20 59.0           ~ 15 0
6 [EYG2006] Bolo 46 cor 03 29 08.90 +31 15 20.8           ~ 25 0
7 NGC 1333 OpC 03 29 09.2 +31 20 59           ~ 1575 1
8 [KJD2006] SMM J032917+31184 Y*O 03 29 11.3 +31 18 25           ~ 64 0
9 [KJD2006] SMM J032930+31251 cor 03 29 18.28 +31 25 06.3           ~ 21 0
10 [EYG2006] Bolo 58 cor 03 29 25.5 +31 28 18           ~ 68 0
11 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 350 0
12 JCMTSE J033317.8+310932 cor 03 33 17.85 +31 09 31.9           ~ 140 0
13 JCMTSE J033327.1+310701 cor 03 33 27.29 +31 07 10.2           ~ 55 0
14 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1553 0
15 IC 348 OpC 03 44 31.1 +32 10 02           ~ 1476 1
16 [KJT2007] SMM 3 smm 03 47 39.1 +32 52 18           ~ 14 0
17 LDN 1471 DNe 03 48.0 +32 54           ~ 349 0
18 Barnard 211 DNe 04 17 35 +27 43.1           ~ 141 0
19 HGBS J041741.9+280846 cor 04 17 41.8 +28 08 47           ~ 13 0
20 HGBS J041750.3+275604 cor 04 17 50.6 +27 56 01           ~ 11 0
21 HGBS J041803.8+282304 cor 04 18 03.8 +28 23 06           ~ 10 0
22 LDN 1495 DNe 04 18.1 +27 37           ~ 408 1
23 HGBS J041807.8+280506 cor 04 18 08.4 +28 05 12           ~ 15 0
24 [HTK2013] 7 cor 04 18 11.5 +27 35 15           ~ 12 0
25 LDN 1495A DNe 04 18.6 +28 25           ~ 39 0
26 HGBS J041937.7+271526 cor 04 19 37.6 +27 15 31           ~ 20 0
27 HGBS J041951.2+271138 cor 04 19 51.7 +27 11 33           ~ 9 0
28 Barnard 213 DNe 04 20 51 +27 16.3           ~ 249 0
29 [HTK2013] 16 cor 04 21 21.0 +27 00 09           ~ 11 0
30 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4971 0
31 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1872 0
32 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 965 0
33 LDN 1640 DNe 05 33 45 -05 41.0           ~ 33 0
34 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1249 2
35 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2421 1
36 M 42 HII 05 35 16.8 -05 23 15           ~ 4411 0
37 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 623 0
38 NAME Ori Complex Cld 05 35.3 -05 23           ~ 481 0
39 OMC 3 MoC 05 35 20.0 -05 01 00           ~ 301 1
40 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 1004 0
41 OMC 5 MoC 05 35.4 -05 55           ~ 28 0
42 OMC 2 MoC 05 35 27 -05 10.1           ~ 475 1
43 M 43 HII 05 35 31 -05 16.2           ~ 201 0
44 OMC 4 MoC 05 36 06 -05 35.7           ~ 80 0
45 NAME Ori A MoC 05 38 -07.1           ~ 3187 0
46 LDN 1641 MoC 05 39.0 -07 00           ~ 502 0
47 NAME Horsehead Nebula DNe 05 40 59.0 -02 27 30           ~ 555 0
48 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 657 1
49 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1498 0
50 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1198 1
51 LDN 1647 DNe 05 42.4 -09 58           ~ 46 0
52 LDN 1630 DNe 05 45.5 -00 59           ~ 392 0
53 M 78 RNe 05 46 45.8 +00 04 45   8.0       ~ 397 0
54 NGC 2071 RNe 05 47 10 +00 18.0           ~ 661 1
55 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1227 1
56 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 789 2
57 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 799 1
58 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1357 1
59 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 2443 1
60 LDN 483 DNe 18 17 35 -04 39.8           ~ 359 0
61 RAFGL 5541 Y*O 18 52 50.26 +00 55 29.6           ~ 122 1

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