The faint supernova remnant G 34.7-0.4 (W44)

¹ 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, fotis@physics.uoc.gr

Received: 11 March 2003
Accepted: 18 April 2003

Abstract

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.