A new candidate supernova remnant G 70.5+1.9
F. Mavromatakis (1), P. Boumis (2), J. Meaburn (3), A. Caulet (4) ((1), Technological Education Institute of Crete, Department of Sciences,, Heraklion, Crete, Greece, (2) Institute of Astronomy & Astrophysics, National, Observatory of Athens, Greece
TL;DR
This paper presents optical observations and spectroscopic analysis of a compact filament complex in the galactic plane, proposing it as a new supernova remnant candidate based on emission features and kinematic data.
Contribution
It introduces a newly identified supernova remnant candidate, G 70.5+1.9, supported by optical emission line diagnostics and kinematic evidence, despite lacking non-thermal radio and X-ray detection.
Findings
Optical emission line diagnostics suggest a supernova origin.
Kinematic data supports the supernova remnant hypothesis.
The object lacks detected non-thermal radio and X-ray emissions.
Abstract
A compact complex of line emission filaments in the galactic plane has the appearance of those expected of an evolved supernova remnant though non-thermal radio and X-ray emission have not yet been detected. This optical emission line region has now been observed with deep imagery and both low and high-dispersion spectroscopy. Diagnostic diagrams of the line intensities from the present spectra and the new kinematical observations both point to a supernova origin. However, several features of the nebular complex still require an explanation within this interpretation.
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