Issue |
A&A
Volume 415, Number 3, March I 2004
|
|
---|---|---|
Page(s) | 1051 - 1063 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20031694 | |
Published online | 13 February 2004 |
Multi-wavelength study of the G 82.2+5.3 supernova remnant
1
University of Crete, Physics Department, PO Box 2208, 710 03 Heraklion, Crete, Greece
2
Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
3
Foundation for Research and Technology-Hellas, PO Box 1527, 711 10 Heraklion, Crete, Greece
Corresponding author: F. Mavromatakis, fotis@physics.uoc.gr
Received:
8
August
2003
Accepted:
6
November
2003
We present the first CCD flux–calibrated images of the supernova remnant
G 82.2+5.3 in major optical emission lines. The medium ionization line of
[]5007 Å provides the first direct evidence of optical emission
originating from G 82.2+5.3.
Filamentary emission is detected in the west and east areas of the
remnant, roughly defining an ellipsoidal shell. The [
] emission is
rather well correlated with the radio emission suggesting their association,
while typical fluxes are found in the range of 20–30
10-17 erg s-1 cm-2 arcsec-2.
Deep long–slit spectra taken at specific positions of the remnant verify
that the detected filamentary emission originates from shock heated
gas, while the diffuse [
] emission in the south results from
photoionization processes. The spectra further suggest shock velocities
around 100 km s-1 and low electron densities. The X-ray surface brightness is
quite patchy,
missing obvious limb brightening and is dominated by a bright
bar–like emission region which is off-set from the geometric center
by ~9´.
The X-ray emission is thermal and requires two temperatures of 0.2 keV and
0.63 keV.
The bright bar region shows overabundant Mg, Si and Fe,
which might indicate still radiating ejecta matter.
The azimuthally averaged radial surface profile is consistent with the matter
density changing
with distance r from the center
e-r/r_0 with a characteristic
angular length of 36´, or, alternatively, with an r
density profile.
The matter inside the remnant is
quite likely structured like a porous cloudy medium. The average matter
density is ~0.04
with
the distance in units of 1.6 kpc. Because of the low density and
the long cooling times involved the remnant is more likely to be in the
adiabatic phase, which is consistent with the densities derived for the X-ray
plasma and the optical line emission, but it is not excluded that is has
reached the radiating phase. This, however, would imply a lower density, greater
age and much larger distance, at the edge of the upper limits obtained from N
and
.
Key words: ISM: general / ISM: supernova remnants / ISM: individual objects: G 82.2+5.3
© ESO, 2004
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