2018A&A...620A.158S


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.02CET03:28:07

2018A&A...620A.158S - Astronomy and Astrophysics, volume 620A, 158-158 (2018/12-1)

MALT90 molecular content on high-mass IR-dark clumps.

SARAL G., AUDARD M. and WANG Y.

Abstract (from CDS):


Context. High mass stars form in groups or clusters in dense molecular clumps with sizes of 1pc and masses of 200M. Infrared-dark clumps and the individual cores within them with sizes <0.1pc and masses <100M are important laboratories for high-mass star formation in order to study the initial conditions.
Aims. We investigate the physical and chemical properties of high-mass clumps in order to better understand the early evolutionary stages and find targets that show star formation signs such as infall motions or outflows.
Methods. We selected the high-mass clumps from ATLASGAL survey that were identified as dark at 8/24µm wavelengths. We used MALT90 Survey data which provides a molecular line set (HCO+, HNC, HCN, N2H+, H13CO+, HN13C, SiO) to investigate the physical and chemical conditions in early stages of star formation.
Results. Eleven sources have significant SiO detection (over 3σ) which usually indicates outflow activity. Thirteen sources are found with blue profiles in both or either HCO+ and/or HNC lines and clump mass infall rates are estimated to be in the range of 0.2x10–3M/yr-1.8x10–2M/yr. The excitation temperature is obtained as <24K for all sources. The column densities for optically thin lines of H13CO+ and HN13C are in the range of 0.4-8.8(x1012)cm–2, and 0.9-11.9(x1012)cm–2, respectively, while it is in the range of 0.1-7.5(x1014)cm–2 for HCO+ and HNC lines. The column densities for N2H+ were ranging between 4.4-275.7(x1012)cm–2 as expected from cold dense regions. Large line widths of N2H+ might indicate turbulence and large line widths of HCO+, HNC, and SiO indicate outflow activities. Mean optical depths are 20.32, and 23.19 for optically thick HCO+ and HCN lines, and 0.39 and 0.45 for their optically thin isotopologues H13CO+ and HN13C, respectively.
Conclusions. This study reveals the physical and chemical properties of 30 high-mass IR-dark clumps and the interesting targets among them based on their emission line morphology and kinematics.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: formation - stars: massive - ISM: lines and bands - ISM: abundances - ISM: molecules - submillimeter: ISM

VizieR on-line data: <Available at CDS (J/A+A/620/A158): clumps.dat list.dat fits/*>

Simbad objects: 38

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Number of rows : 38

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 1097 LIN 02 46 19.059 -30 16 29.68 10.46 9.97 9.48 8.72 9.8 ~ 1199 3
2 MMB G309.384-00.135 cor 13 47 23.98 -62 18 12.0           ~ 23 0
3 AGAL G317.867-00.151 Y*O 14 53 16 -59 26.5           ~ 18 0
4 AGAL G318.779-00.137 Y*O 14 59 33.06 -59 00 33.5           ~ 14 0
5 AGAL G320.881-00.397 Y*O 15 14 33.18 -58 11 28.5           ~ 13 0
6 MMB G326.986-00.031 Y*O 15 49 07.67 -54 23 04.5           ~ 14 0
7 AGAL G329.029-00.206 cor 16 00 32 -53 12.9           ~ 15 0
8 AGAL G331.709+00.582 Y*O 16 10 06.61 -50 50 29.0           ~ 22 0
9 AGAL G333.656+00.059 Y*O 16 21 11.61 -49 52 16.3           ~ 15 0
10 OH 335.79 +0.17 cor 16 29 47.3094168743 -48 15 52.204707131           ~ 54 0
11 MMB G336.957-00.225 cor 16 36 16.9344603433 -47 40 48.047756433           ~ 18 0
12 MMB G337.176-00.032 cor 16 36 18.82 -47 23 19.9           ~ 20 0
13 MMB G337.258-00.101 cor 16 36 56.32 -47 22 26.4           ~ 23 0
14 AGAL G338.786+00.476 Y*O 16 40 22.55 -45 51 04.1           ~ 15 0
15 MMB G340.785-00.096 cor 16 50 14.84 -44 42 26.3           ~ 47 0
16 MMB G342.484+00.183 cor 16 55 02.30 -43 12 59.8           ~ 22 0
17 MMB G343.756-00.163 cor 17 00 49.89 -42 26 08.2           ~ 20 0
18 AGAL G351.571+00.762 Y*O 17 20 51.00 -35 35 25.8           ~ 17 0
19 MMB G351.445+00.660 cor 17 20 54.61 -35 45 08.6           ~ 33 0
20 AGAL G353.066+00.452 Y*O 17 26 13.330 -34 31 53.52           ~ 17 0
21 AGAL G353.417-00.079 Y*O 17 29 18.94 -34 32 05.9           ~ 14 0
22 AGAL G354.944-00.537 cor 17 35 12.7753 -33 30 22.961           ~ 20 0
23 [BDS2003] 3 OpC 18 06 15 -21 37.5           ~ 7 0
24 MMB G008.683-00.368 cor 18 06 23.49 -21 37 10.2           ~ 26 0
25 AGAL G008.706-00.414 Y*O 18 06 37.2081 -21 37 06.564           ~ 28 0
26 MMB G010.444-00.018 cor 18 08 45.1076 -19 54 33.194           ~ 34 0
27 MMB G013.179+00.061 cor 18 14 00.96 -17 28 32.5           ~ 19 0
28 AGAL G014.194-00.194 Y*O 18 16 58.5794 -16 42 14.134           ~ 27 0
29 AGAL G014.492-00.139 Y*O 18 17 22.0275 -16 24 57.391           ~ 28 0
30 AGAL G014.114-00.574 Y*O 18 18 13.2635 -16 57 11.844           ~ 19 0
31 MMB G014.631-00.577 cor 18 19 15.21 -16 30 04.5           ~ 16 0
32 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1508 0
33 AGAL G018.876-00.489 Y*O 18 27 10 -12 42.7           ~ 9 0
34 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 457 0
35 GAL 034.3+00.1 SFR 18 53 22 +01 14.6           ~ 29 0
36 W 49 SFR 19 10 20 +09 07.7           ~ 521 1
37 W 51 SNR 19 23 50 +14 06.0           ~ 1174 1
38 GAL 010.62-00.39 ? ~ ~           ~ 2 0

    Equat.    Gal    SGal    Ecl

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2021.03.02-03:28:07

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