2017A&A...606L...7B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST23:14:52

2017A&A...606L...7B - Astronomy and Astrophysics, volume 606, L7-7 (2017/10-1)

Deuterated methanol on a solar system scale around the HH212 protostar.

BIANCHI E., CODELLA C., CECCARELLI C., TAQUET V., CABRIT S., BACCIOTTI F., BACHILLER R., CHAPILLON E., GUETH F., GUSDORF A., LEFLOCH B., LEURINI S., PODIO L., RYGL K.L.J., TABONE B. and TAFALLA M.

Abstract (from CDS):

Context. Deuterium fractionation is a valuable tool for understanding the chemical evolution during the process that leads to the formation of a Sun-like planetary system.
Aims. Methanol is thought to be mainly formed during the prestellar phase, and its deuterated form keeps a memory of the conditions at that epoch. The unique combination of high angular resolution and sensitivity provided by ALMA enables us to measure methanol deuteration in the planet formation region around a Class 0 protostar and to understand its origin.
Methods. We mapped both the 13CH3OH and CH2DOH distribution in the inner regions (∼100au) of the HH212 system in Orion B. To this end, we used ALMA Cycle 1 and Cycle 4 observations in Band 7 with angular resolution down to ∼0.15.
Results. We detected 6 lines of 13CH3OH and 13 lines of CH2DOH with upper level energies of up to 438K in temperature units. We derived a rotational temperature of (171±52)K and column densities of 7x1016cm–2 (13CH3OH) and 1x1017cm–2 (CH2DOH), respectively. This yields a D/H ratio of (2.4±0.4)x10–2, which is lower by an order of magnitude than previously measured values using single-dish telescopes toward protostars located in Perseus. Our findings are consistent with the higher dust temperatures in Orion B with respect to the temperature derived for the Perseus cloud. The emission traces a rotating structure extending up to 45au from the jet axis, which is elongated by 90au along the jet axis. So far, the origin of the observed emission appears to be related with the accretion disc. Only higher spatial resolution measurements will be able to distinguish between different possible scenarios, however: disc wind, disc atmosphere, or accretion shocks.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: formation - ISM: molecules - ISM: individual objects: HH212 - ISM: abundances - ISM: abundances

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

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1061 0
2 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1053 3
3 LDN 1527 DNe 04 39 53 +25 45.0           ~ 495 0
4 QSO B0507+179 QSO 05 10 02.36912982 +18 00 41.5816534   20.0 19.0 19.09   ~ 313 1
5 QSO B0539-057 QSO 05 41 38.08338 -05 41 49.4284     20.4 20.70   ~ 210 2
6 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1164 0
7 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1071 1
8 [CCG2007] MM1 smm 05 43 51.4100 -01 02 53.160           ~ 15 1
9 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 280 1
10 ICRF J055250.1+031327 Bz? 05 52 50.10150010 +03 13 27.2431110       22.79   ~ 45 1
11 QSO B0605-0834 QSO 06 07 59.69923743 -08 34 49.9781718     18.5 17.70   ~ 394 1
12 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
13 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1035 1
14 NGC 7129 OpC 21 42 56 +66 06.2     11.5     ~ 233 0
15 NAME NGC 7129 FIR 2 IR 21 44 01.5 +66 03 40           ~ 84 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-23:14:52

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