2019A&A...632A..19T


Query : 2019A&A...632A..19T

2019A&A...632A..19T - Astronomy and Astrophysics, volume 632A, 19-19 (2019/12-0)

Interferometric observations of warm deuterated methanol in the inner regions of low-mass protostars.

TAQUET V., BIANCHI E., CODELLA C., PERSSON M.V., CECCARELLI C., CABRIT S., JORGENSEN J.K., KAHANE C., LOPEZ-SEPULCRE A. and NERI R.

Abstract (from CDS):

Methanol is a key species in astrochemistry because it is the most abundant organic molecule in the interstellar medium and is thought to be the mother molecule of many complex organic species. Estimating the deuteration of methanol around young protostars is of crucial importance because it highly depends on its formation mechanisms and the physical conditions during its moment of formation. We analyse several dozen transitions from deuterated methanol isotopologues coming from various existing observational datasets obtained with the IRAM-PdBI and ALMA sub-millimeter interferometers to estimate the methanol deuteration surrounding three low-mass protostars on Solar System scales. A population diagram analysis allows us to derive a [CH2DOH]/[CH3OH] abundance ratio of 3-6% and a [CH3OD]/[CH3OH] ratio of 0.4-1.6% in the warm inner (≤100-200AU) protostellar regions. These values are typically ten times lower than those derived with previous single-dish observations towards these sources, but they are one to two orders of magnitude higher than the methanol deuteration measured in massive hot cores. Dust temperature maps obtained from Herschel and Planck observations show that massive hot cores are located in warmer molecular clouds than low-mass sources, with temperature differences of ∼10K. The comparison of our measured values with the predictions of the gas-grain astrochemical model GRAINOBLE shows that such a temperature difference is sufficient to explain the different deuteration observed in low- to high-mass sources. This suggests that the physical conditions of the molecular cloud at the origin of the protostars mostly govern the present-day observed deuteration of methanol and therefore of more complex organic molecules. Finally, the methanol deuteration measured towards young solar-type protostars on Solar System scales seems to be higher by a factor of ∼5 than the upper limit in methanol deuteration estimated in comet Hale-Bopp. If this result is confirmed by subsequent observations of other comets, it would imply that an important reprocessing of the organic material likely occurred in the solar nebula during the formation of the Solar System.

Abstract Copyright: © ESO 2019

Journal keyword(s): astrochemistry - molecular processes - ISM: abundances - ISM: molecules - submillimeter: ISM - stars: formation

VizieR on-line data: <Available at CDS (J/A+A/632/A19): list.dat fits/*>

CDS comments: Calibrator J0541-0211 and J0552-3627 not identified.

Simbad objects: 31

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Number of rows : 31
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 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 431 3
2 [JCC87] IRAS 4A2 Y*O 03 29 10.413 +31 13 32.20           ~ 103 1
3 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 670 1
4 [JCC87] IRAS 4A1 Y*O 03 29 10.510 +31 13 31.01           ~ 91 1
5 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1331 1
6 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 583 0
7 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1217 0
8 QSO B0420-0127 QSO 04 23 15.8007747432 -01 20 33.063518580   17.50 17.00 16.28   ~ 1130 3
9 EM* LkCa 15 Or* 04 39 17.7911622816 +22 21 03.390090984   13.01 12.03 11.61   K5:Ve 614 1
10 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 459 0
11 QSO B0507+179 QSO 05 10 02.3689932504 +18 00 41.582562768   20.0 19.0 19.09   ~ 374 1
12 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2156 1
13 QSO B0539-057 QSO 05 41 38.0825893728 -05 41 49.441027200     20.4 20.70   ~ 229 2
14 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1272 0
15 [CAZ2013] HH 212 MMS Y*O 05 43 51.41 -01 02 53.2           ~ 8 0
16 [CCG2007] MM1 smm 05 43 51.4100 -01 02 53.160           ~ 16 1
17 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 335 1
18 ICRF J055250.1+031327 Bz? 05 52 50.1013410696 +03 13 27.242707260       22.79   ~ 52 1
19 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 960 1
20 QSO B0605-0834 BLL 06 07 59.6994046176 -08 34 49.980131256     18.5 17.70   ~ 422 1
21 THA 15-12 Or* 15 56 09.2066646912 -37 56 06.126118692   13.12 11.93 11.45   M0e 339 0
22 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3358 1
23 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1159 1
24 EM* AS 209 Or* 16 49 15.3034917000 -14 22 08.643317664   12.62 11.28     K4Ve 306 0
25 NGC 6334 HII 17 20 51 -36 06.9           ~ 639 0
26 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 2101 1
27 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 958 0
28 HD 319139 SB* 18 14 10.4818675368 -32 47 34.516836060   11.47 10.68   9.11 K5+K7 329 0
29 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 256 2
30 NGC 7129 OpC 21 42 58 +66 06.8     11.5     ~ 245 0
31 NAME NGC 7129 FIR 2 IR 21 44 01.5 +66 03 40           ~ 93 0

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2022.07.03-19:03:53

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