Mon. Not. R. Astron. Soc., 496, 1834-1844 (2020/August-1)
Atacama Compact Array observations of the pulsar-wind nebula of SNR 0540-69.3.
LUNDQVIST P., LUNDQVIST N., VLAHAKIS C., BJORNSSON C.-I., DICKEL J.R., MATSUURA M., SHIBANOV Y.A., ZYUZIN D.A. and OLOFSSON G.
Abstract (from CDS):
We present observations of the pulsar-wind nebula (PWN) region of SNR 0540-69.3. The observations were made with the Atacama Compact Array (ACA) in Bands 4 and 6. We also add radio observations from the Australia Compact Array at 3 cm. For 1.449-233.50 GHz, we obtain a synchrotron spectrum Fν ∝ναν, with the spectral index αν = 0.17 ± 0.02. To conclude how this joins the synchrotron spectrum at higher frequencies, we include hitherto unpublished AKARI mid-infrared data, and evaluate published data in the ultraviolet (UV), optical, and infrared (IR). In particular, some broad-band filter data in the optical must be discarded from our analysis due to contamination by spectral line emission. For the UV/IR part of the synchrotron spectrum, we arrive at αν = 0.87+0.08–0.10. There is room for 2.5 x 10–3 M☉ of dust with a temperature of ∼55 K if there are dual breaks in the synchrotron spectrum, one around ∼9 x 1010 Hz and another at ∼2 x 1013 Hz. The spectral index then changes at ∼9 x 1010 Hz from αν = 0.14 ± 0.07 in the radio to αν = 0.35–0.07+0.05 in the millimetre-to-far-IR range. The ACA Band 6 data marginally resolve the PWN. In particular, the strong emission ∼ 1".5 south-west of the pulsar, seen at other wavelengths, and resolved in the 3 cm data with its 0.''8 spatial resolution, is also strong in the millimetre range. The ACA data clearly reveal the supernova remnant shell ∼20-35 arcsec west of the pulsar, and for the shell we derive αν = 0.64 ± 0.05 for the range 8.6-145 GHz.
© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
pulsars: individual: PSR B0540-69.3 - supernovae: general - ISM: SNR 0540-69.3 - ISM: supernova remnants - Magellanic Clouds
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