Abstract
G359.1-0.5 is a supernova remnant near the Galactic center region that
belongs to the mixed morphology type, showing a radio continuum shell
and diffuse thermal X-ray emission inside. Earlier molecular studies
around the location of G359.1-0.5 revealed an annular CO structure in
the velocity range from $-190$ to $-60~\rm{km} \rm{s}^{-1}$ with an
H{\sc i} counterpart, both concentric with the remnant. Six OH masers at
1720~MHz along the edge of the radio-continuum shell were detected at
velocities around $-5~\rm{km} \rm{s}^{-1}$, largely different from those
found in previous molecular studies.In this work, we identify a
molecular structure in the $^{12}$CO and $^{13}$CO J=1-0 lines between
the velocities $-12.48$ and $+1.83~\rm{km} \rm{s}^{-1}$ which contains
CO clumps apparently related to the OH masers. In addition, analyzing
XMM-Newton archival data, we found evidence that part of the interior
gas is not in ionization equilibrium. Finally, based on the collected
data, we suggest a likely astrophysical scenario for G359.5-0.1.
Original language | English |
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Pages (from-to) | 121-123 |
Journal | Boletín de la Asociación Argentina de Astronomía |
Volume | 61B |
Publication status | Published - 1 Jul 2020 |
Externally published | Yes |
Keywords
- ISM: clouds
- ISM: {individual objects (G359.1-0.5)}
- ISM: molecules
- {ISM: supernova remnants}
- X-rays: ISM
- {radiation} mechanisms: thermal