The kinematics of the bi-lobal supernova remnant G 65.3+5.7 - Paper II

Details The kinematics of the bi-lobal supernova remnant G 65.3+5.7 - Paper II The kinematics of the bi-lobal supernova remnant G 65.3+5.7 - Paper II

2004-05-18

arxiv.org/abs/astro-ph/0405350v1

Astron.Astrophys. 424 (2004) 583-588

Astronomy and Astrophysics

Astrophysics

10 pages, 5 figures, accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20040410

Further deep, narrow-band images in the light of [O III] 5007 A have been added to the previous mosaic of the faint galactic supernova remnant G 65.3+5.7. Additionally longslit spatially resolved [O III] 5007 A line profiles have been obtained at sample positions using the Manchester Echelle Spectrometer at the San Pedro Martir observatory. The remnant is shown to be predominantly bi-lobal with an EW axis for this structure. However, a faint additional northern lobe has now been revealed. Splitting of the profiles along the slit lengths, when extrapolated to the remnant's centre, although uncertain suggests that the expansion velocity of this remnant is between 124 and 187 km/s ie much lower than the 400 km/s previously predicted for the forward shock velocity from the X-ray emission. An expansion proper motion measurement of 2.1+-0.4 arcsec in 48 years for the remnant's filamentary edge in the light of Halpha+[N II] has also been made. When combined with an expansion velocity of ~155 km/s, a distance of ~800 pc to G 65.3+5.7 is derived. Several possibilities are considered for the large difference in the expansion velocity measured here and the 400 km/s shock velocity required to generate the X-ray emission. It is also suggested that the morphology of the remnant may be created by a tilt in the galactic magnetic field in this vicinity.

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