C.D.S. - SIMBAD4 rel 1.7 - 2020.06.03CEST06:23:34

2016A&A...595A..88L - Astronomy and Astrophysics, volume 595A, 88-88 (2016/11-1)

G345.45+1.50: an expanding ring-like structure with massive star formation.


Abstract (from CDS):

Context. Ring-like structures in the interstellar medium (ISM) are commonly associated with high-mass stars. Kinematic studies of large structures in giant molecular clouds (GMCs) toward these ring-like structures may help us to understand how massive stars form.
Aims. The origin and properties of the ring-like structure G345.45+1.50 is investigated through observations of the 13CO(3-2) line. The aim of the observations is to determine the kinematics in the region and to compare physical characteristics estimated from gas emission with those previously determined using dust continuum emission. This area in the sky is well suited for studies like this because the ring is located 1.5° above the Galactic plane at 1.8kpc from the Sun, thus molecular structures are rarely superposed on our line of sight, which minimizes confusion effects that might hinder identifying of individual molecular condensations.
Methods. The 13CO(3-2) line was mapped toward the whole ring using the Atacama Pathfinder Experiment (APEX) telescope. The observations cover 17'x20' in the sky with a spatial resolution of 0.2pc and an rms of ∼1K at a spectral resolution of 0.1km/s.
Results. The ring is found to be expanding with a velocity of 1.0km/s, containing a total mass of 6.9x103M, which agrees well with that determined using 1.2mm dust continuum emission. An expansion timescale of ∼3x106yr and a total energy of ∼7x1046erg are estimated. The origin of the ring might have been a supernova explosion, since a 35.5cm source, J165920-400424, is located at the center of the ring without an infrared counterpart. The ring is fragmented, and 104 clumps were identified with diameters of between 0.3 and 1.6pc, masses of between 2.3 and 7.5x102M, and densities of between ∼102 and ∼104cm–3. At least 18% of the clumps are forming stars, as is shown in infrared images. Assuming that the clumps can be modeled as Bonnor-Ebert spheres, 13 clumps are collapsing, and the rest of them are in hydrostatic equilibrium with an external pressure with a median value of 4x104K/cm3. In the region, the molecular outflow IRAS 16562-3959 is identified, with a velocity range of 38.4km/s, total mass of 13M, and kinematic energy of 7x1045erg. Finally, five filamentary structures were found at the edge of the ring with an average size of 3pc, a width of 0.6pc, a mass of 2x102M, and a column density of 6x1021cm–2.

Abstract Copyright: © ESO 2016

Journal keyword(s): ISM: clouds - stars: massive - stars: formation - dust, extinction - ISM: kinematics and dynamics - ISM: molecules

VizieR on-line data: <Available at CDS (J/A+A/595/A88): tablef1.dat>

Status at CDS:  

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 MGPS J165920-400424 Rad 16 59 29.0 -40 04 23           ~ 2 0
2 GAL 345.5+01.5 MoC 17 00 -40.0           ~ 3 0
3 IRAS 16562-3959 SFR 16 59 42.257 -40 03 45.17           ~ 43 0
4 GAL 345.5+01.0 MoC 17 02 -40.3           ~ 7 0

    Equat.    Gal    SGal    Ecl

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