2022A&A...657A..78C


Query : 2022A&A...657A..78C

2022A&A...657A..78C - Astronomy and Astrophysics, volume 657A, 78-78 (2022/1-1)

Organic chemistry in the protosolar analogue HOPS-108: Environment matters.

CHAHINE L., LOPEZ-SEPULCRE A., NERI R., CECCARELLI C., MERCIMEK S., CODELLA C., BOUVIER M., BIANCHI E., FAVRE C., PODIO L., ALVES F.O., SAKAI N. and YAMAMOTO S.

Abstract (from CDS):


Context. Hot corinos are compact regions around solar-mass protostellar objects that are very rich in interstellar Complex Organic Molecules (iCOMs). How the abundance of these molecules is affected by the environmental physical conditions is still an open question. More specifically, addressing this point is key to understand our own chemical origins since the Solar System formed in a large cluster of low- to high-mass stars and was therefore subject to external heating and ultraviolet irradiation which may have shaped the chemistry of its early formation stages.
Aims. The goal of this high resolution study is to determine the abundance ratios of iCOMs in HOPS-108, which is a Class 0 protostar and a hot corino candidate located in the nearest Solar System analogue, the protostellar cluster OMC-2 FIR 4, in Orion. We aim to compare the abundance ratios to those found in other hot corinos, which are all located in less crowded environments, in order to understand the impact of environmental conditions on hot corinos' chemistry.
Methods. We observed the OMC-2 FIR 4 proto-cluster using the Band 6 of the Atacama Large (sub-)Millimetre Array in Cycle 4 with an angular resolution of ∼0.''28 (110 au). We determined the abundances and temperature of the species using local thermodynamic equilibrium (LTE) and non-LTE analysis.
Results. Our results reveal a rich organic chemistry towards HOPS-108, asserting that it is a hot corino where the following iCOMs are detected: CH3OH, HCOOCH3, CH3OCH3, CH318OH_, CH2DOH, CH3COCH3, CH3CHO, CH3CN, 13CH3CN, C2H5CN, and NH2CHO. Remarkably, we find a possible enhancement in the HCOOCH3 abundance with respect to other known hot corinos. Indeed, the [CH3OCH3]/[HCOOCH3] abundance ratio in this source is ∼0.2 and, within the uncertainties, it deviates from the known correlation marginally where [CH3OCH3]/[HCOOCH3] ∼1. A relatively low [CH2DOH]/[CH3OH] abundance ratio of ∼0.02 is also obtained, which is in agreement with that found in another Orion source, HH212, suggesting a higher gas temperature during the early phases of ice mantle formation.
Conclusions. The [CH3OCH3]/[HCOOCH3] and [CH2DOH]/[CH3OH] abundance ratios in HOPS-108 might result from different physical conditions in the Orion molecular complex compared to other regions. The former ratio cannot be reproduced with current chemical models, highlighting the importance of improving the chemical networks with theoretical calculations. More hot corinos located in heavily clustered regions such as Orion should be targeted in order to measure these ratios and evaluate whether they are an environmental product or whether HOPS-108 is an exceptional hot corino overall.

Abstract Copyright: © L. Chahine et al. 2022

Journal keyword(s): astrochemistry - ISM: individual objects: OMC-2 FIR 4 - ISM: molecules - stars: formation

Simbad objects: 59

goto Full paper

goto View the references in ADS

Number of rows : 59
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 LDN 1448 DNe 03 22.5 +30 35           ~ 502 0
2 [TLL2016] Per-emb-22-B Rad 03 25 22.3520 +30 45 13.151           ~ 7 0
3 [TLL2016] Per-emb-22-A Rad 03 25 22.4100 +30 45 13.254           ~ 9 0
4 LDN 1448NW Y*O 03 25 35.66 +30 45 34.2           ~ 68 0
5 [TTK2018] Per-emb-33-A cm 03 25 36.3120 +30 45 15.153           ~ 6 0
6 LDN 1448NA smm 03 25 36.49 +30 45 22.2           ~ 180 1
7 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 250 1
8 SSTc2d J032539.1+304358 Y*? 03 25 39.12 +30 43 58.2           ~ 43 1
9 NAME LDN 1455 IRS 4 cor 03 27 43.23 +30 12 28.9           ~ 70 0
10 [TLL2016] Per-emb-35-A Rad 03 28 37.0910 +31 13 30.788           ~ 7 0
11 [TLL2016] Per-emb-35-B Rad 03 28 37.2190 +31 13 31.751           ~ 6 0
12 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 439 3
13 NAME HH 7-11 MMS 2 smm 03 29 03.056 +31 15 51.67           ~ 79 0
14 [SVS76] NGC 1333 13A2 IR 03 29 03.374 +31 16 01.87           ~ 15 0
15 V* V512 Per Or* 03 29 03.7578170808 +31 16 03.947525688           ~ 371 0
16 [JCC87] IRAS 4A2 Y*O 03 29 10.413 +31 13 32.20           ~ 110 1
17 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 684 1
18 [JJK2007] 23 Y*O 03 29 10.68 +31 18 20.6           ~ 38 1
19 ASR 32 Y*O 03 29 11.25 +31 18 31.7           ~ 47 1
20 NAME IRAS 4B1 South Y*O 03 29 12.06 +31 13 01.7           ~ 32 1
21 IRAS 03282+3035 cor 03 31 20.98 +30 45 30.1           ~ 168 0
22 IRAS 03292+3039 cor 03 32 17.96 +30 49 47.5           ~ 75 0
23 [EES2009] Per-emb 10 Y*O 03 33 16.45 +31 06 52.5           ~ 16 1
24 JCMTSE J033317.8+310932 cor 03 33 17.85 +31 09 31.9           ~ 100 0
25 [KJD2006] SMM J033335+31075 PoC 03 33 21.3 +31 07 28           ~ 96 0
26 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1266 0
27 HH 211 Y*O 03 43 56.52 +32 00 52.8           ~ 343 0
28 [TLL2016] Per-emb-11-A Rad 03 43 57.0650 +32 03 04.788           ~ 6 0
29 [TLL2016] Per-emb-11-C Rad 03 43 57.6880 +32 03 09.975           ~ 6 0
30 IRAS 03445+3242 Y*O 03 47 41.603 +32 51 43.79           ~ 192 0
31 LDN 1551 DNe 04 31 30.0 +18 12 30           ~ 794 1
32 4C -02.19 QSO 05 01 12.80988538 -01 59 14.2564557   19.1 18.4 19.04   ~ 555 1
33 QSO B0507+179 QSO 05 10 02.36912937 +18 00 41.5815635   20.0 19.0 19.09   ~ 387 1
34 QSO B0521-365 BLL 05 22 57.98464178 -36 27 30.8512953   15.26 14.62 14.48   ~ 792 2
35 NAME Ori Trapezium OpC 05 35 16.5 -05 23 14           ~ 1568 1
36 M 42 OpC 05 35 17 -05 23.4           ~ 3970 0
37 NAME Ori Complex Cld 05 35.3 -05 23           ~ 405 0
38 GBS-VLA J053525.96-050543.3 Rad 05 35 25.96 -05 05 43.3           ~ 7 0
39 [TMV2019] OMC-2 FIR4 ALMA1 mm 05 35 26.785 -05 10 08.83           ~ 3 0
40 V* V2457 Ori Or* 05 35 26.97000 -05 09 54.4644         18.858 ~ 143 0
41 OMC 2 MoC 05 35 27 -05 10.1           ~ 434 1
42 HOPS 108 Y*O 05 35 27.07 -05 10 00.4           ~ 25 0
43 JW 808 Y*O 05 35 27.4713701592 -05 09 44.128270008         14.407 M2e 28 0
44 2MASS J05352762-0509337 Y*O 05 35 27.622 -05 09 33.78           ~ 90 0
45 TKK 870 Y*O 05 35 28.19 -05 03 41.2           ~ 45 0
46 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 358 1
47 QSO B0605-0834 BLL 06 07 59.69924014 -08 34 49.9783246     18.5 17.70   ~ 429 1
48 BHR 71 MoC 12 01 36.810 -65 08 49.22           ~ 145 0
49 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3446 1
50 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1193 1
51 NAME IRAS 16293-2422B Y*O 16 32 22.63 -24 28 31.8           ~ 251 0
52 NAME IRAS 16293-2422A Y*O 16 32 22.869 -24 28 36.11           ~ 154 0
53 LDN 483 DNe 18 17 35 -04 39.8           ~ 276 0
54 [HMH2007] 67 Y*O 18 29 06.20 +00 30 43.3           ~ 21 1
55 SSTc2d J182909.0+003132 cor 18 29 09.07 +00 31 32.4           ~ 24 0
56 SH 2-68 N Y*O 18 29 48.09 +01 16 45.0           ~ 130 1
57 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1049 2
58 LDN 663 DNe 19 36 55 +07 34.4           ~ 612 0
59 V* V1142 Aql Mi* 19 37 10.6584483696 +07 36 27.145824048       13.56   ~ 19 0

To bookmark this query, right click on this link: simbad:objects in 2022A&A...657A..78C and select 'bookmark this link' or equivalent in the popup menu


2023.01.31-01:07:26

© Université de Strasbourg/CNRS

    • Contact