New VLA observations of the SNR Puppis A: the radio properties and the correlation with the X-ray emission

Abstract

Context. High-resolution, high-sensitivity multifrequency radio images of supernova remnants (SNRs) are essential in advancing the understanding of both the global SNR dynamics and particle acceleration mechanisms. Aims. In this paper we report on a new study of the SNR Puppis A based on VLA observations at 1425 MHz; the improvement represents a factor of two in angular resolution and almost ten times in sensitivity compared to the best previous image of Puppis A. This new image is used to compare with re-processed 327 MHz data and ROSAT and Chandra images to investigate morphological and spectral characteristics. Methods. The observations were carried out with the VLA in the DnC and CnB configurations in 2004. After combining with singledish data from Parkes, an angular resolution of 34 × 16 and an rms noise of 0.5 mJy beam −1 , were achieved. Archival VLA data at 327 MHz were also processed. The spectral index distribution was then determined by a direct comparison of the homogenized data at both 327 and 1425 MHz. In addition, to identify different spectral components, tomographic spectral analysis was performed. Results. The new 1425 MHz radio image reveals a highly structured border encircling a diffuse, featureless interior. In particular, the northern half of Puppis A displays a complex structure along the periphery, consisting of short arcs resembling "wave-like" features. These are oriented essentially perpendicular to the shock front on the NE side, but are tangential to the shock on the NW side. A remarkable correspondence between such "wave-like" features and spectral changes is observed. On the other hand, the brightest radio features (located to the E of the SNR and also detected in X-rays) have no counterpart in the spectral index distribution. Based on a uniform compilation of integrated flux densities between 19 and 8400 MHz, a global spectral index α = −0.52± 0.03 (S ∝ ν α ) has been determined. The new 1425 MHz image of Puppis A was compared with the ROSAT X-ray image of the entire SNR and with the resolved arcsec Chandra image of the bright E region. There is good overall agreement between the radio and high resolution X-ray images. At the arcsec level, however, the agreement of the radio and X-ray images is less striking. A noticeable similarity is found between Puppis A, with its E and W extensions, and analogous morphological features observed in the SNR W50. This suggests that Puppis A could be another case of a SNR shaped by the action of energetic jets.

The most complete and detailed X-ray view of the SNR Puppis A

“…Particularly all along the northwestern border it can be noticed that the "scalloped" view of the limb exactly corresponds with the "wave-like" structures revealed in radio with VLA observations at 1425 MHz (Castelletti et al 2006). Moreover a series of faint, curved filaments with a concave shape can be seen ahead of the main shock to the west side of Puppis A, near (α, δ) = 08 h 19 m 30 s , −42…”

“…These filaments appear as narrow fringes whose spectrum alternates between flat and steep. This pattern has been interpreted in Castelletti et al (2006) as a manifestation of Rayleigh-Taylor instabilities that distort the interface between ejecta and ambient gas, stretching and compressing the magnetic field and thus modifying the observed synchrotron emission.…”

“…In radio, Puppis A was observed using different facilities (Milne et al 1983;Dubner et al 1991;Castelletti et al 2006). One remarkable characteristic of Puppis A in this spectral range is the lack of neat edges.…”

High-resolution radio study of SNR IC 443 at low radio frequencies

“…Such faint emission is seen as a weak and irregular radio halo that in our 330 MHz image is notable at a mean level of ∼4σ extending up to 5 ahead of the bright sharp boundary. It is interesting to note that similar weak, diffuse emission upstream of the main shock is also observed in the cases of Puppis A and W44, along the sides where the expanding blast wave encountered molecular gas (Castelletti et al 2006, and. A series of small protrusions are also evident along most of the extension of the eastern rim.…”

The jet feedback mechanism (JFM) in stars, galaxies and clusters

“…Such is the structure of two opposite 'ears', as in the SNR Puppis A. Castelletti et al (2006) suggest that Puppis A was shaped by jets. Here I add that such jets might be the two opposite jets launched at the last jets-launching episode in the jittering jets model, after the core has been exploded.…”