Volume 405, Number 2, July II 2003
|Page(s)||591 - 596|
|Section||Interstellar and circumstellar matter|
|Published online||19 June 2003|
The faint supernova remnant G 34.7-0.4 (W44)
University of Crete, Physics Department, PO Box 2208, 710 03 Heraklion, Crete, Greece
2 Institute of Astronomy & Astrophysics, National Observatory of Athens, I. Metaxa and V. Pavlou, P. Penteli, 15236 Athens, Greece
3 Astronomical Laboratory, Department of Physics, University of Patras, 26500 Rio–Patras, Greece
Corresponding author: F. Mavromatakis, email@example.com
Accepted: 18 April 2003
Flux calibrated images of the known supernova remnant G 34.7-0.4 in basic optical emission lines are presented. The low ionization images show a relatively flat flux distribution. The diffuse and patchy morphology of the detected optical emission may indicate the presence of turbulent magnetic fields. Typical observed H] fluxes are ~8 10-17 erg s-1 cm-2 arcsec-2, while the  fluxes are lower around 4 10-17 erg s-1 cm-2 arcsec-2. Emission in the medium ionization line of  5007 Å is not detected within our sensitivity limits, probably due to the heavy extinction towards the remnant. The long-slit spectra reveal strong  and  emission relative to Hα and moderate  6300 Å emission. Shock velocities in the range of 110–150 km s-1 and low electron densities are estimated. Archival MSX infrared data show emission in the south and west areas of the remnant matching rather well the optical and radio emission.
Key words: ISM: general / ISM: supernova remnants / ISM: individual objects: G 34.7-0.4
© ESO, 2003
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