2018A&A...617A..10C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:11:42

2018A&A...617A..10C - Astronomy and Astrophysics, volume 617A, 10-10 (2018/9-1)

Water and interstellar complex organics associated with the HH 212 protostellar disc. On disc atmospheres, disc winds, and accretion shocks.

CODELLA C., BIANCHI E., TABONE B., LEE C.-F., CABRIT S., CECCARELLI C., PODIO L., BACCIOTTI F., BACHILLER R., CHAPILLON E., GUETH F., GUSDORF A., LEFLOCH B., LEURINI S., PINEAU DES FORETS G., RYGL K.L.J. and TAFALLA M.

Abstract (from CDS):


Context. The unprecedented combination of high-sensitivity and high angular resolution provided by the ALMA interferometer allows us to shed light on the processes leading to the formation of the jet-disc system associated with a Sun-like mass protostar.
Aims. We investigate the physical and chemical properties of the gas associated with water and interstellar complex organic molecules around a protostar on solar system scales.
Methods. The HH 212 protostellar system, in Orion B, has been mapped, thanks to ALMA-Band 7 Cycle 1 and Cycle 4 observations of dueterated water (HDO) and acetaldehyde (CH3CHO) emission with an angular resolution down to ∼0.15" (60au).
Results. Many emission lines due to 14 CH3CHO and 1 HDO transitions at high excitation (Eu between 163 and 335K) have been imaged in the inner ∼70au region. The local thermal equilibrium analysis of the CH3CHO emission leads to a temperature of 78±14K and a column density of 7.6±3.2x1015cm–2, which, when NH2 of 1024cm–2 is assumed, leads to an abundance of XCH3CHO~=8x10–9. The large velocity gradient analysis of the HDO emission also places severe constraints on the volume density, nH2~=108cm–3. The line profiles are 5-7km/s wide, and CH3CHO and HDO both show a ±2km/s velocity gradient over a size of ∼70au (blue-shifted emission towards the north-west and red-shifted emission towards the south-east) along the disc equatorial plane, in agreement with what was found so far using other molecular tracers.
Conclusions. The kinematics of CH3CHO and HDO are consistent with the occurrence of a centrifugal barrier, that is, the infalling envelope-rotating disc ring, which is chemically enriched through low-velocity accretion shocks. The emission radius is ∼60au, in good agreement with what was found before for another interstellar complex organic molecule such as NH2CHO. We support a vertical structure for the centrifugal barrier, suggesting the occurrence of two outflowing, expanding, and rotating rings above and below (of about 40-45au) the optically thick equatorial disc plane. It is tempting to speculate that these rings could probe the basis of a wind launched from this region.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: formation - ISM: jets and outflows - ISM: molecules - ISM: individual objects: HH212

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

Simbad objects: 13

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Number of rows : 13

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 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1053 3
2 LDN 1527 DNe 04 39 53 +25 45.0           ~ 495 0
3 QSO B0507+179 QSO 05 10 02.36912982 +18 00 41.5816534   20.0 19.0 19.09   ~ 313 1
4 QSO B0539-057 QSO 05 41 38.08338 -05 41 49.4284     20.4 20.70   ~ 210 2
5 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1164 0
6 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1071 1
7 [CCG2007] MM1 smm 05 43 51.4100 -01 02 53.160           ~ 15 1
8 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 280 1
9 LDN 1630 DNe 05 45.5 -00 59           ~ 350 0
10 M 78 RNe 05 46 45.8 +00 04 45   8.0       ~ 342 0
11 ICRF J055250.1+031327 Bz? 05 52 50.10150010 +03 13 27.2431110       22.79   ~ 45 1
12 QSO B0605-0834 QSO 06 07 59.69923743 -08 34 49.9781718     18.5 17.70   ~ 394 1
13 LDN 663 DNe 19 36 55 +07 34.4           ~ 555 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-03:11:42

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