Issue |
A&A
Volume 398, Number 1, January IV 2003
|
|
---|---|---|
Page(s) | 153 - 158 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20021635 | |
Published online | 14 January 2003 |
Optical line emission from the supernova remnant G 73.9+0.9
University of Crete, Physics Department, PO Box 2208, 710 03 Heraklion, Crete, Greece
Corresponding author: fotis@physics.uoc.gr
Received:
12
August
2002
Accepted:
25
October
2002
Flux calibrated images of the field around the known supernova
remnant G 73.9+0.9 in the H
], [
], [
], and [
] emission
lines are presented.
The low ionization images are characterized by diffuse emission both within
and outside the extent of the remnant. The flux calibrated images revealed
a few small scale structures in the east areas of G 73.9+0.9.
The long–slit spectra identify
the emission from one of them as emission from shock heated gas.
This patchy structure is ~3´ long and emits Hα flux at a level
of ~33
10-17 erg s-1 cm-2 arcsec-2.
The bright diffuse arc–like structure in the center of the field seems
to be associated to G 73.9+0.9 given its spectral signature and positional
relation with the non–thermal radio emission.
A ~8´ long filamentary
structure with an absolute Hα flux of ~9
10-17 erg s-1 cm-2 arcsec-2 is detected
in the [
] emission line to the south of G 73.9+0.9 but is probably
unrelated. The deep long–slit spectra suggest complete
recombination zones, shock velocities below 90 km s-1, low electron
densities (<50 cm-3) and non–negligible magnetic field strengths.
Key words: ISM: general / ISM: supernova remnants / ISM: individual objects: G 73.9+0.9
© ESO, 2003
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