A 408‐MHz aperture synthesis radio telescope

Veidt, B.; Landecker, T. L.; Vaneldik, J. F.; Dewdney, P. E.; Routledge, D.

doi:10.1029/rs020i005p01118

Cited by 28 publications

(20 citation statements)

References 13 publications

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“…The 1420 MHz continuum sensitivity has been increased by a factor of 3 and the angular resolution by a factor of 2 and a 408 MHz continuum channel has been added (Veidt et al 1985). Polarimetry at 1420 MHz has recently been added, and the observations reported here were made as the Ðrst test of the new facility.…”

Section: Radio Observationsmentioning

confidence: 99%

DA 530: A Supernova Remnant in a Stellar Wind Bubble

Landecker

Routledge

Reynolds

et al. 1999

ApJ

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The high-latitude supernova remnant (SNR) DA 530 (G93.3]6.9), apparently a typical shell remnant, has highly polarized radio continuum emission and a very uniform circumferential magnetic Ðeld. We present new radio continuum (408 and 1420 MHz) and H I line observations, made with the Dominion Radio Astrophysical Observatory Synthesis Telescope, and we have made the Ðrst detection of X-ray emission from the SNR, using the ROSAT Position-Sensitive Proportional Counter. The SNR lies within a shell of H I, possibly created by an earlier stellar wind, whose kinematic distance is nominally 2.5 kpc but whose actual distance may be larger. The X-ray emission is extremely faint. A Raymond-Smith ionization-equilibrium model Ðts the data and suggests a very low density, D0.05 cm~3, consistent with the occurrence of the supernova in a stellar wind cavity, but this model yields an explosion energy 100 times lower than the accepted value. A nonequilibrium shock model, incorporating a range of ionization timescales, is able to give more realistic physical parameters for the supernova remnant. On the balance of the evidence, we place DA 530 at a distance of 3.5 kpc, the largest distance permitted by the H I observations, where it lies 420 pc above the Galactic plane. The explosion, probably a Type Ia supernova, in a low-density cavity has resulted in weak X-ray emission and slow evolution. The explosion energy was 3.9 ] 1050 ergs and the age is D5000 years. The remnant, having swept up 3.9in an M _ ambient density of D0.01 cm~3, is only now in the adiabatic phase, and this explains the absence of detected optical emission. Despite the low ambient density the efficiency of generation of synchrotron radio emission is D0.4%, higher than in some historical SNRs. The ratio of radio to X-ray Ñux is about 100 times that for the remnant of SN 1006, which has comparable radio continuum properties. The very uniform magnetic Ðeld is not explained. DA 530 joins a small group of remnants at high Galactic latitude with unusual features, perhaps resulting from low ambient densities. Inhomogeneous nonequilibrium ionization models may be required for the interpretation of the X-ray emission from many other older SNRs.

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Section: Radio Observationsmentioning

confidence: 99%

DA 530: A Supernova Remnant in a Stellar Wind Bubble

Landecker

Routledge

Reynolds

et al. 1999

ApJ

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“…The continuum radio emission from the IC 443/G189.6+ 3.3/S249 region was mapped at 408 and 1420 MHz with the Synthesis Telescope at the DRAO (Roger et al 1973;Veidt et al 1985). The synthesized beam at 1420 MHz is 2 0 32B00 (north-south) by 0 0 57B35 (east-west), and at 408 MHz is 8 0 42B63 (north-south) by 3 0 19B57 (east-west).…”

Section: Observations and Analysismentioning

confidence: 99%

1420 and 408 MHz Continuum Observations of the IC 443/G189.6+3.3 Region

Leahy¹

2004

Astron J

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Observations at 1420 and 408 MHz were made with the Dominion Radio Astrophysical Observatory Synthesis Telescope of the region including IC 443 and G189.6+3.3. A spectral index map is computed: the bright northeast part of IC 443 has 408-1420 MHz spectral index ¼ 0:43 AE 0:02, the southwest part has ¼ 0:2 0:6, and G189.6+3.3 has ¼ 0:1 0:7. The radio images are compared with optical, infrared, molecular line, and X-ray images. The appearance of IC 443 as two half-shells is due to the ring of shocked molecular gas that sits at the join of the half-shells. G189.6+3.3 has nonthermal radio emission and is confirmed as a separate supernova remnant. The pulsar wind nebula found by Chandra likely originates in G189.6+3.3 rather than in IC 443.

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“…3C 400.2 was observed in the λ 21-cm HI line using the Synthesis Telescope at the Dominion Radio Astrophysical Observatory (DRAO) (Roger et al 1973;Veidt et al 1985) in June 1995. The field of view is 2.…”

Section: Observationsmentioning

confidence: 99%

The structure of atomic gas around the supernova remnant 3C 400.2

Giacani¹,

Dubner²,

Cappa

et al. 1998

Astron. Astrophys. Suppl. Ser.

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Abstract. The interaction of the SNR 3C 400.2 with the interstellar medium is investigated on the basis of the HI observations using the Synthesis Radio Telescope at the Dominion Radio Astrophysical Observatory (DRAO). These new data show the existence of a dense atomic cloud associated with 3C 400.2 in the velocity range +14 to +42 km s −1 , and high velocity clouds probably accelerated by the supernova blast wave at v = −49.5 km s −1 and +69 km s −1 . We propose that the complex remnant 3C 400.2 is the result of a supernova explosion in a region of the interstellar medium containing a density discontinuity. A breakout phenomenon may explain the observed morphology in the different spectral regimes.

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A 408‐MHz aperture synthesis radio telescope

Cited by 28 publications

References 13 publications

DA 530: A Supernova Remnant in a Stellar Wind Bubble

DA 530: A Supernova Remnant in a Stellar Wind Bubble

1420 and 408 MHz Continuum Observations of the IC 443/G189.6+3.3 Region

The structure of atomic gas around the supernova remnant 3C 400.2

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