Open AccessShocked molecular gas towards the supernova remnant G359.1–0.5 and the Snake
Author(s) -
Lazendic J. S.,
Wardle M.,
Burton M. G.,
YusefZadeh F.,
Whiteoak J. B.,
Green A. J.,
Ashley M. C. B.
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05227.x
Subject(s) - physics , supernova remnant , maser , astrophysics , supernova , molecular cloud , line (geometry) , shock (circulatory) , protein filament , shock wave , spectral line , bar (unit) , hydrogen line , atomic physics , astronomy , stars , geometry , thermodynamics , medicine , mathematics , biology , meteorology , genetics
We have found a bar of shocked molecular hydrogen (H 2 ) towards the OH(1720 MHz) maser located at the projected intersection of supernova remnant (SNR) G359.1–0.5 and the non‐thermal radio filament known as the Snake. The H 2 bar is well aligned with the SNR shell and almost perpendicular to the Snake. The OH(1720 MHz) maser is located inside the sharp western edge of the H 2 emission, which is consistent with the scenario in which the SNR drives a shock into a molecular cloud at that location. The spectral line profiles of 12 CO, HCO + and CS towards the maser show broad‐line absorption, which is absent in the 13 CO spectra and most probably originates from the pre‐shock gas. A density gradient is present across the region and is consistent with the passage of the SNR shock, while the H 2 filament is located at the boundary between the pre‐shock and post‐shock regions.