Molecular environments of the supernova remnant G359.1-0.5
| Autor: | Estela Marta Reynoso, L. K. Eppens, Jorge Ariel Combi, J. F. Albacete-Colombo, J. Lazendic-Galloway |
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| Jazyk: | angličtina |
| Rok vydání: | 2020 |
| Předmět: |
Ciencias Astronómicas
Ciencias Físicas Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences individual: (G359.1−0.5) [ISM] Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences INDIVIDUAL: (G359.1-0.5) [ISM] ISM: clouds purl.org/becyt/ford/1 [https] 0103 physical sciences Supernova remnant 010303 astronomy & astrophysics molecules [ISM] Astrophysics::Galaxy Astrophysics ISM: supernova remnant Physics 010308 nuclear & particles physics Astronomy and Astrophysics purl.org/becyt/ford/1.3 [https] Astrophysics - Astrophysics of Galaxies ISM: individual: (G359.1−0.5) ISM: molecules Astronomía CLOUDS [ISM] Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Humanities SUPERNOVA REMNANT [ISM] CIENCIAS NATURALES Y EXACTAS |
| Zdroj: | CONICET Digital (CONICET) Consejo Nacional de Investigaciones Científicas y Técnicas instacron:CONICET SEDICI (UNLP) Universidad Nacional de La Plata instacron:UNLP |
| Popis: | We report new CO observations and a detailed molecular-line study of the mixed morphology supernova remnant G359.1−0.5, which contains six OH (1720 MHz) masers along the radio shell, indicative of shock-cloud interaction. Observations of ¹²CO and ¹³CO J:1–0 lines were performed in a ∼38 × 38 arcmin area with the on-the-fly technique using the Kit Peak 12 Meter telescope. The molecular study has revealed the existence of a few clumps with densities ∼10³ cm⁻³ compatible in velocity and position with the OH (1720 MHz) masers. These clumps, in turn, appear to be part of a larger, elongated molecular structure ∼34 arcmin long extending between −12.48 and +1.83 km s⁻¹, adjacent to the western edge of the radio shell. According to the densities and relative position with respect to the masers, we conclude that the CO clouds depict unshocked gas, as observed in other remnants with OH (1720 MHz) masers. In addition, we investigated the distribution of the molecular gas towards the adjacent γ-ray source HESS J1745-303 (Aharonian et al. 2006) but could not find any morphological correlation between the γ-rays and the CO emission at any velocity in this region. Facultad de Ciencias Astronómicas y Geofísicas Instituto Argentino de Radioastronomía |
| Databáze: | OpenAIRE |
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