EDP Sciences
Free access
Volume 405, Number 2, July II 2003
Page(s) 591 - 596
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20030603

A&A 405, 591-596 (2003)
DOI: 10.1051/0004-6361:20030603

The faint supernova remnant G 34.7-0.4 (W44)

F. Mavromatakis1, P. Boumis2 and C. D. Goudis2, 3

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

(Received 11 March 2003 / 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 $\alpha+[$ $\ion{N}{ii}$ ] fluxes are ~8  $\times$ 10-17 erg s -1 cm -2 arcsec -2, while the [ $\ion{S}{ii}$ ] fluxes are lower around 4  $\times$ 10-17 erg s -1 cm -2 arcsec -2. Emission in the medium ionization line of [ $\ion{O}{iii}$ ] 5007 Å is not detected within our sensitivity limits, probably due to the heavy extinction towards the remnant. The long-slit spectra reveal strong [ $\ion{S}{ii}$ ] and [ $\ion{N}{ii}$ ] emission relative to H $\alpha$ and moderate [ $\ion{O}{i}$ ] 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

Offprint request: F. Mavromatakis, fotis@physics.uoc.gr

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