2019A&A...628A..72U


Query : 2019A&A...628A..72U

2019A&A...628A..72U - Astronomy and Astrophysics, volume 628A, 72-72 (2019/8-1)

C2O and C3O in low-mass star-forming regions.

URSO R.G., PALUMBO M.E., CECCARELLI C., BALUCANI N., BOTTINELLI S., CODELLA C., FONTANI F., LETO P., TRIGILIO C., VASTEL C., BACHILLER R., BARATTA G.A., BUEMI C.S., CAUX E., JABER AL-EDHARI A., LEFLOCH B., LOPEZ-SEPULCRE A., UMANA G. and TESTI L.

Abstract (from CDS):


Context. C2O and C3O belong to the carbon chain oxides family. Both molecules have been detected in the gas phase towards several star-forming regions, and to explain the observed abundances, ion-molecule gas-phase reactions have been invoked. On the other hand, laboratory experiments have shown that carbon chain oxides are formed after energetic processing of CO-rich solid mixtures. Therefore, it has been proposed that they are formed in the solid phase in dense molecular clouds after cosmic ion irradiation of CO-rich icy grain mantles and released in the gas phase after their desorption.
Aims. In this work, we contribute to the understanding of the role of both gas-phase reactions and energetic processing in the formation of simple carbon chain oxides that have been searched for in various low-mass star-forming regions.
Methods. We present observations obtained with the Noto-32m and IRAM-30 m telescopes towards star-forming regions. We compare these with the results of a gas-phase model that simulates C2O and C3O formation and destruction, and laboratory experiments in which both molecules are produced after energetic processing (with 200 keV protons) of icy grain mantle analogues. Results. New detections of both molecules towards L1544, L1498, and Elias 18 are reported. The adopted gas phase model is not able to reproduce the observed C2O/C3O ratios, while laboratory experiments show that the ion bombardment of CO-rich mixtures produces C2O/C3O ratios that agree with the observed values.Conclusions. Based on the results obtained here, we conclude that the synthesis of both species is due to the energetic processing of CO-rich icy grain mantles. Their subsequent desorption because of non-thermal processes allows the detection in the gas-phase of young star-forming regions. In more evolved objects, the non-detection of both C2O and C3O is due to their fast destruction in the warm gas.

Abstract Copyright: © ESO 2019

Journal keyword(s): astrochemistry - ISM: molecules - ISM: abundances - methods: observational - methods: laboratory: solid state - techniques: spectroscopic

VizieR on-line data: <Available at CDS (J/A+A/628/A72): list.dat fits/* sp/*>

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 [SVS76] NGC 1333 13A smm 03 29 03.73 +31 16 03.8           ~ 67 0
2 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 339 0
3 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 641 1
4 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 473 0
5 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1282 1
6 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1155 0
7 LDN 1498 DNe 04 11.0 +24 58           ~ 259 0
8 IRAS 0437+257P08 TT? 04 39 55.7451364657 +25 45 01.943057594           B5 162 1
9 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1450 0
10 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 740 0
11 V* V2457 Ori Or* 05 35 26.97000 -05 09 54.4644         18.858 ~ 131 0
12 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2205 0
13 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1113 1
14 NAME IRAS 16293-2422B Y*O 16 32 22.63 -24 28 31.8           ~ 214 0
15 NAME IRAS 16293-2422A Y*O 16 32 22.869 -24 28 36.11           ~ 125 0
16 HH 375 Y*O 20 39 06.2 +68 02 15           ~ 170 0
17 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 516 0
18 [DE95] LDN 1157 B1 out 20 39 11 +68 01.3           ~ 205 0

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2021.09.27-17:34:16

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