2017A&A...603A.133A


C.D.S. - SIMBAD4 rel 1.7 - 2019.08.18CEST07:43:24

2017A&A...603A.133A - Astronomy and Astrophysics, volume 603A, 133-133 (2017/7-1)

Chemical segregation in hot cores with disk candidates. An investigation with ALMA.

ALLEN V., VAN DER TAK F.F.S., SANCHEZ-MONGE A., CESARONI R. and BELTRAN M.T.

Abstract (from CDS):

Context. In the study of high-mass star formation, hot cores are empirically defined stages where chemically rich emission is detected toward a massive YSO. It is unknown whether the physical origin of this emission is a disk, inner envelope, or outflow cavity wall and whether the hot core stage is common to all massive stars.
Aims. We investigate the chemical makeup of several hot molecular cores to determine physical and chemical structure. We use high spectral and spatial resolution submillimeter observations to determine how this stage fits into the formation sequence of a high-mass star.
Methods. The submillimeter interferometer ALMA (Atacama Large Millimeter Array) was used to observe the G35.20-0.74N and G35.03+0.35 hot cores at 350GHz in Cycle 0. We analyzed spectra and maps from four continuum peaks (A, B1, B2 and B3) in G35.20-0.74N, separated by 1000-2000 AU, and one continuum peak in G35.03+0.35. We made all possible line identifications across 8GHz of spectral windows of molecular emission lines down to a 3σ line flux of 0.5K and determined column densities and temperatures for as many as 35 species assuming local thermodynamic equilibrium (LTE).
Results. In comparing the spectra of the four continuum peaks, we find each has a distinct chemical composition expressed in over 400 different transitions. In G35.20, B1 and B2 contain oxygen- and sulfur-bearing organic and inorganic species but few nitrogen-bearing species whereas A and B3 are strong sources of O-, S-, and N-bearing organic and inorganic species (especially those with the CN bond). Column densities of vibrationally excited states are observed to be equal to or greater than the ground state for a number of species. Deuterated methyl cyanide is clearly detected in A and B3 with D/H ratios of 8 and 13%, respectively, but is much weaker at B1 and undetected at B2. No deuterated species are detected in G35.03, but similar molecular abundances to G35.20 were found in other species. We also find co-spatial emission of isocyanic acid (HNCO) and formamide (NH2CHO) in both sources indicating a strong chemical link between the two species.
Conclusions. The chemical segregation between N-bearing organic species and others in G35.20 suggests the presence of multiple protostars surrounded by a disk or torus.

Abstract Copyright: © ESO, 2017

Journal keyword(s): astrochemistry - stars: formation - stars: massive - ISM: individual objects: G35.20-0.74N - submillimeter: stars - ISM: individual objects: G35.03+0.35 - ISM: individual objects: G35.03+0.35

Nomenclature: Tables 1-3, Fig. 1: [AVS2017] G35.20AN (Nos A, B1-B3).

Simbad objects: 25

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Number of rows : 25

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 925 2
2 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 939 3
3 W 3(H2O) Mas 02 27 04.6 +61 52 25           ~ 112 0
4 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 640 0
5 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 1920 1
6 NAME Orion Core ? 05 35 14.5 -05 22 30           ~ 170 0
7 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 558 1
8 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 983 1
9 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 10884 0
10 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1832 1
11 GAL 029.96-00.02 Y*O 18 46 03.7 -02 39 21           ~ 325 1
12 [BSC2014] E cor 18 54 00.453 +02 01 17.54           ~ 2 0
13 [BSC2014] F cor 18 54 00.479 +02 01 17.06           ~ 2 0
14 [BSC2014] D cor 18 54 00.479 +02 01 18.90           ~ 2 0
15 [BSC2014] C cor 18 54 00.490 +02 01 20.26           ~ 2 0
16 [BSC2014] B cor 18 54 00.586 +02 01 19.78           ~ 2 0
17 [BSC2014] A cor 18 54 00.645 +02 01 19.23           ~ 4 0
18 GAL 035.03+00.35 HII 18 54 01.0 +02 01 32           ~ 34 0
19 [AVS2017] G35.20A cor 18 58 12.9480 +01 40 37.419           ~ 3 0
20 [AVS2017] G35.20B2 cor 18 58 13.0130 +01 40 36.649           ~ 2 0
21 [AVS2017] G35.20B1 cor 18 58 13.0300 +01 40 35.886           ~ 2 0
22 [DLW84] G35.2N HII 18 58 13.036 +01 40 36.00           ~ 88 0
23 [AVS2017] G35.20B3 cor 18 58 13.0570 +01 40 35.442           ~ 2 0
24 RAFGL 2591 Y*O 20 29 25.2650 +40 11 26.532   18       ~ 560 5
25 [WBN74] NGC 7538 IRS 9 Y*O 23 14 01.63 +61 27 20.2           ~ 335 0

    Equat.    Gal    SGal    Ecl

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2019.08.18-07:43:24

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