Wind-swept clouds and possible triggered star formation associated with the supernova remnant G357.7+0.3

2009/07/07 by J. P. Phillips, G. Ramos-Larios, J. A. Perez-Grana · 12 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #Gamma-ray bursts and supernovae #Interstellar medium #Line (geometry) #Luminosity #Maser #Molecular cloud #Protostar #Star formation #Supernova #Supernova remnant #Young stellar object #astro-ph.GA

paper · pdf · doi:10.1111/j.1365-2966.2009.14988.x

published in Monthly Notices of the Royal Astronomical Society 397(3), 1215-1227 (Oxford University Press) · 13 pages, 9 figures, Publicated in MNRAS. 43 pages in arXiv

openalex publication_date 2009/07/07 · arxiv created 2009/09/10 · arxiv updated 2014/11/20 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

We present evidence for interaction between the supernova remnant (SNR) G357.7+0.3 and nearby molecular clouds, leading to the formation of wind-swept structures and bright emission rims. These features are not observed at visual wavelengths, but are clearly visible in mid-infrared mapping undertaken using the Spitzer Space Telescope. Analysis of one of these clouds, the bright cometary structure G357.46+0.60, suggests that it contains strong polycyclic aromatic hydrocarbon emission features in the 5.8 and 8.0 μm photometric bands, and that these are highly variable over relatively small spatial scales. The source is also associated with strong variations in electron density; a far-infrared continuum peak associated with dust temperatures of ∼30 K; and has previously been observed in the 1720 MHz maser transition of OH, known to be associated with SNR shock excitation of interstellar clouds. This source also appears to contain a young stellar object (YSO) within the bright rim structure, with a steeply rising spectrum between 1.25 and 24 μm. If the formation of this star has been triggered recently by the SNR, then YSO modelling suggests a stellar mass ∼5–10 M⊙, and luminosity LYSO∼102–2 × 103 L⊙. Finally, it is noted that a further, conical emission region appears to be associated with the Mira V1139 Sco, and it is suggested that this may represent the case of a Mira outflow interacting with a SNR. If this is the case, however, then the distance to the SNR must be ∼half of that determined from CS J= 2–1 and 3–2 line radial velocities.

Citations

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