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| G359.1-0.2 | |
|---|---|
| Name | G359.1-0.2 |
| Type | Supernova remnant |
| Epoch | J2000 |
| Constellation | Sagittarius |
| Distance | ~8 kpc (Galactic Center) |
| Size | ~20 arcmin |
| Coordinates | 17h45m, −29° (approx.) |
G359.1-0.2 is a Galactic supernova remnant located near the center of the Milky Way. It has been studied in multiple wavebands including radio and X-ray, and is notable for its association with molecular clouds and shock interaction in the inner Sagittarius A region. Observations tie it into broader investigations of high-energy phenomena near Sgr A*, the Central Molecular Zone, and stellar populations related to Arches Cluster and Quintuplet Cluster.
G359.1-0.2 was first identified in radio surveys that included instruments associated with Very Large Array and later imaged with telescopes such as the Australia Telescope Compact Array and the Molonglo Observatory Synthesis Telescope, appearing in catalogs alongside remnants like SNR G359.0-0.9 and Sgr A East. Subsequent X-ray detections used observatories including ASCA, Chandra X-ray Observatory, and XMM-Newton, placing it in the context of high-energy studies like those examining the Galactic Center X-ray Emission. Infrared and molecular-line follow-ups employed facilities such as Atacama Large Millimeter/submillimeter Array and the James Clerk Maxwell Telescope to probe associations similar to research on Sgr B2 and M-0.13-0.08.
G359.1-0.2 lies projected within the central few hundred parsecs of the Milky Way, near landmarks including Sgr A East and the Sgr A complex, and projected close to the Radio Arc. Its angular extent, measured in surveys coordinated with Green Bank Telescope and Effelsberg 100-m Radio Telescope, implies a physical diameter comparable to other Galactic Center remnants such as G0.9+0.1 when placed at distances used for Galactic Center objects. The remnant displays a shell-like morphology in radio maps similar to classical examples like Cassiopeia A and Tycho's Supernova. Spectral-line studies of molecular species including CO and OH—conducted in campaigns similar to those focusing on Sgr C and Sgr D—reveal dense cloud structures in its vicinity.
In the radio band, G359.1-0.2 exhibits nonthermal synchrotron emission with a spectral index derived from multi-frequency measurements using arrays such as the VLA and ATCA, comparable to remnants studied in surveys like the Galactic Plane Survey (GPS). Polarization studies reference techniques used for 3C 391 and W44, indicating magnetic-field-ordered regions where compression by shocks aligns fields, akin to features seen toward SNR IC 443. X-ray observations report thermal and possibly nonthermal components; analyses using instruments from ASCA and Chandra employ plasma models similar to those applied to SNR G359.0-0.9 and to studies of diffuse emission around Sgr A*.
Positioned within the Central Molecular Zone, G359.1-0.2 interacts with structures including the CND (Circumnuclear Disk) and dense clouds like M-0.02-0.07, placing it among objects that shape the energetic landscape near Sgr A*. Its environment features high cosmic-ray densities and strong magnetic fields, comparable to conditions inferred near Arches Cluster winds and Quintuplet Cluster outflows. Studies link energetic feedback from remnants like G359.1-0.2 to processes investigated in research on Fermi Bubbles and the origin of Galactic Center TeV emission observed with the High Energy Stereoscopic System.
Molecular-line detections of OH masers and broadened CO profiles—techniques also used to study interactions in W28 and IC 443—indicate that the shock front from G359.1-0.2 is impacting adjacent molecular clouds, triggering shocked-gas chemistry analogous to that in Sgr B2(N). Observations of HI and H2 emission using methodologies similar to surveys of Molecular Ring regions reveal kinematic signatures of cloud acceleration and compression. The interaction likely enhances local densities and magnetic-field amplification in a manner comparable to interactions seen in 3C 391 and W44, potentially influencing star formation traced by surveys of Infrared Dark Clouds and young stellar objects cataloged in Spitzer Space Telescope studies.
Distance estimates place G359.1-0.2 near the nominal distance to the Galactic Center (~8 kpc), using kinematic arguments analogous to those applied to Sgr A East and Sgr B2, and by association with molecular cloud velocities measured in CO surveys conducted by teams using Nobeyama Radio Observatory and IRAM. Age constraints, inferred from shock velocities and X-ray plasma parameters similar to analyses for remnants like W28 and Kes 73, suggest a middle-aged supernova remnant, potentially several 10^4 years old, in a radiative or transition phase. Its evolutionary status is influenced by the high-density, high-pressure Central Molecular Zone environment, paralleling evolutionary scenarios developed for other Galactic Center remnants in comparative studies involving SNR G0.9+0.1 and Sgr A East.
Category:Supernova remnants