Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasau..11q..84m&link_type=abstract
Astronomical Society of Australia, Proceedings, vol. 11, no. 1, p. 84
Astronomy and Astrophysics
Astronomy
Gamma Rays, Pulsars, Stellar Evolution, Supernova Remnants, Radio Astronomy, Radio Sources (Astronomy), Sky Surveys (Astronomy), Stellar Luminosity, Stellar Structure
Scientific paper
The Molonglo Observatory Synthesis Telescope discovered a faint supernova remnant associated with PSR 1706-44, one of only four gamma-ray pulsars. (Vela, the Crab and PSR 1509-58 also have an associated SNR.) The gamma-ray source was first discovered as 2CG342-02, the tenth strongest of 25 COS-B gamma-ray sources cataloged (Swanenburg et al., 1981, Astrophys. J. Lett. 243, L69). Low-resolution surveys show an extended (approximately 40 min x 25 min) source in the region with flux of approximately 25 Jy, suggesting a plerionic SNR (e.g. Jonas, de Jager and Baart, 1985, Astron. Astrophys. Suppl., 62, 105). A search for the gamma-ray source at 843 MHz with a resolution of 44 arcsec revealed a shell-type SNR--a half-ellipse with axes approximately 44 min x 32 min and low brightness of approximately 9 mJy per beam, giving Sigma843 = 3 x 10-21W m-2 Hz/sr (McAdam, Osborne and Parkinson, 1993, Nature, 361, 516). The Sigma-D relation suggests a diameter D approximately 34 pc at a distance of approximately 3 kpc in the Norma spiral arm of the Galaxy. It has a young (Sedov expansion) age of approximately 6000 years. The key linking the SNR and the gamma-ray source came (Kniffen et al., 1992, IAU Circ. 5485) when the Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory satellite detected pulsed gamma-radiation (Thompson et al., 1992, Nature, 359, 615) from the newly-discovered PSR 1706-44 (Johnston et al., 1992, Mon. Not. R. Astron. Soc. 255, 401). The pulsar position (epoch 1950) at RA = 17 hour 06 min 05.1 sec, delta = -44 deg 25 min 15.0 sec coincides in the MOST image with a 21 mJy source on the SE and of the SNR shell. The pulsar has a period of 102 ms and slows with characteristic age 17300 years. For it to move 18 min from centre to rim of the SNR shell in this time implies a proper motion of 0.06 sec/yr which is sufficiently large to check with VLBI astrometry. At the pusar dispersion distance (1.8 kpc), or the SNR distance of 3 kpc, the pulsar has apparently moved 10 or 16 pc at a transverse velocity of 540 or 900 km/s.
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