C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET21:47:46

2020A&A...641A.104A - Astronomy and Astrophysics, volume 641A, 104-104 (2020/9-1)

Studying star-forming processes at core and clump scales: the case of the young stellar object G29.862-0.0044.


Abstract (from CDS):

Aims. To advance our knowledge of star formation, in addition to statistical studies and large surveys of young stellar objects (YSOs), it is important to carry out detailed studies towards particular objects. Given that massive molecular clumps fragment into cores where star formation takes place, these kinds of studies should be done on different spatial scales. The aim of this work is to investigate the star-forming processes at core and clump scales.
Methods. Using near-infrared (NIR) data obtained with NIRI at the Gemini-North telescope, data of the complex molecular species CH3OCHO and CH3CN obtained from the Atacama Large Millimeter Array (ALMA) database, observations of HCN, HNC, HCO+, and C2H carried out with the Atacama Submillimeter Telescope Experiment (ASTE), and CO data from public surveys observed with the James Clerck Maxwell Telescope (JCMT), we perform a deep study of the YSO G29.862-0.0044 (YSO-G29) at core and clump spatial scales.
Results. The NIR emission shows that YSO-G29 is composed of two nebulosities separated by a dark lane, suggesting a scenario consistent with a typical disc plus jets system, albeit in this case highly asymmetric. The northern nebulosity is open, diffuse, and is divided into two branches, while the southern one is smaller and sharper. They are likely produced by the scattered light in cavities carved out by jets or winds on an infalling envelope of material, which also presents line emission of H2 S(1) 1-0 and 2-1, and [FeII]. The presence of the complex molecular species observed with ALMA confirms that we are mapping a hot molecular core. The CH3CN emission concentrates at the position of the dark lane and appears slightly elongated from southwest to northeast in agreement with the inclination of the system as observed in the NIR. The morphology of the CH3OCHO emission is more complex and extends along some filaments and concentrates in knots and clumps, mainly southwards of the dark lane, suggesting that the southern jet is encountering a dense region. The northern jet is able to flow more freely, generating the more extended features as seen in the NIR. This is in agreement with the redshifted molecular outflow traced by the 12CO J=3-2 line extending towards the northwest and the lack of a blueshifted outflow. This configuration can be explained by considering that G29-YSO is located at the furthest edge of the molecular clump along the line of sight, which is consistent with the position of the source in the cloud mapped in the C18O J=3-2 line. The detection of HCN, HNC, HCO+, and C2H allowed us to characterise the dense gas at clump scales, yielding results that are in agreement with the presence of a high-mass protostellar object.

Abstract Copyright: © ESO 2020

Journal keyword(s): stars: formation - stars: protostars - ISM: jets and outflows - ISM: molecules

Simbad objects: 10

goto Full paper

goto View the reference in ADS

Number of rows : 10

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
1 [RZP2014] JVLA 1 Y*O 03 43 51.02 +32 03 08.1           ~ 30 2
2 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2031 1
3 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1955 1
4 AGAL G029.862-00.044 Mas 18 45 59.437 -02 45 05.78           ~ 27 0
5 [WWS2012] G029.85-00.06 cor 18 46 00.9535 -02 46 14.756           ~ 2 0
6 NVSS J184601-024601 Rad 18 46 01.67 -02 46 01.6           ~ 3 0
7 NVSS J184603-024541 Rad 18 46 03.00 -02 45 41.0           ~ 2 0
8 GAL 029.96-00.02 Y*O 18 46 03.7 -02 39 21           ~ 334 1
9 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 448 0
10 IRAS 18449-0115 cor 18 47 34.4947 -01 12 40.269           ~ 316 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2020A&A...641A.104A and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact