A high-resolution H i study towards the supernova remnant Puppis A and its environments

Abstract

We observed the supernova remnant (SNR) Puppis A in the 21 cm line with the Australia Telescope Compact Array with the aim of determining the systemic velocity and, hence, the corresponding kinematic distance. For the compact, background sources in the field, we obtain absorption spectra by applying two methods: (a) subtracting profiles on-and off-source towards continuum emission, and (b) filtering short spacial frequencies in the Fourier plane to remove large scale emission. One of the brightest features to the East of the shell of Puppis A was found to be a background source, probably extragalactic. Removing the contribution from this and the previously known unrelated sources, the systemic velocity of Puppis A turns out to be limited between 8 and 12 km s −1 , which places this source at a distance of 1.3 ± 0.3 kpc. From the combined images that include both single dish and interferometric data, we analyze the distribution of the interstellar hydrogen. We suggest that an ellipsoidal ring at v ∼ +8 km s −1 could be the relic of a bubble blown by the progenitor of Puppis A, provided the distance is 1.2 kpc. The main consequences of the new systemic velocity and distance as compared with previous publications (v = +16 km s −1 and d = 2.2 kpc) are the absence of a dense interacting cloud to the East to explain the morphology, and the decrease of the shell size and the neutron star velocity, which are now in better agreement with statistical values.

Intermediate-mass Elements in Young Supernova Remnants Reveal Neutron Star Kicks by Asymmetric Explosions

“…Note-a Since no direct measurement exists, we inferred the values from an evolutionary model by Chevalier & Oishi (2003) with an assumption of the ejecta mass of 5 M ⊙ , a mass-loss rate of 2×10 −5 M yr −1 , and a stellar wind speed of 10 km s −1 . References are as follows: [1] Reed et al (1995) [2] Fesen et al (2006) [3] Gotthelf et al (2001) [4] Tananbaum (1999) [5] Gaensler & Wallace (2003) [6] Winkler et al (2009) [7] Bhalerao et al (2015) [8] Hughes et al (2003) [9] Reynoso et al (1995) [10] Reynoso et al (2017) [11] Becker et al (2012) [12] Gotthelf & Halpern (2009) [13] Gotthelf et al (2013) [14] Winkler et al (1988) [15] Tian & Leahy (2008) [16] Wachter et al (2004) [17] Vasisht & Gotthelf (1997) [18] Paron et al (2006) [19] Carter et al (1997) [20] Garmire et al (2000) [21] De Luca et al (2006) [22] Esposito et al (2011) [23] Feast (1999) [24] Park et al (2012) [25] Kulkarni et al (2003). Note-The region names in the first row correspond to those in Fig.…”

New perspectives on the supernova remnant Puppis A based on a radio polarization study

“…The ATCA configurations were EW 352 and 750A for the first and second 13hr runs respectively, so that the visibilities correspond to baselines between 31 and 735 m excluding the 6th, fixed antenna. A thorough analysis of the continuum data was published in Reynoso & Walsh (2015), while the Hi 21 cm line study was reported in Reynoso et al (2017). The primary flux and bandpass calibrator was PKS 1934-638, while PKS 0823-500 was used for phase and polarization calibration.…”

“…The data reduction was carried out with the miriad software package (Sault et al 1995). The observations in the EW 352 array were affected by a bug which was fixed as described in Reynoso et al (2017). The uv data were split in eleven bands of 128 MHz, centered at frequencies from 1302 to 2582 MHz.…”

Core collapse supernova remnants with ears

“…The image displays the radio continuum emission produced at 1.4 GHz. It was published by Reynoso & Walsh (2015), and reproduced by Reynoso et al (2017). Right: A full view of Puppis A in X-ray, where red, green, and blue correspond to the 0.3-0.7, 0.7-1.0, and 1.0-8.0 keV bands, respectively (from Dubner et al 2013).…”