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09 October 2024 |
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Article overview
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Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A | | M. Aruga
; H. Sano
; Y. Fukui
; E. M. Reynoso
; G. Rowell
; K. Tachihara
; | | Date: |
1 Jun 2022 | | Abstract: | We have carried out a study of the interstellar medium (ISM) toward a
shell-like supernova remnant SNR Puppis A by using the NANTEN CO and ATCA HI
data. We synthesized a comprehensive picture of the SNR radiation by combining
the ISM data with the gamma ray and X-ray distributions. The ISM, both atomic
and molecular gas, is dense and highly clumpy, and is distributed along the
northeastern edge of the SNR shell. The CO distribution revealed an enhanced
line intensity ratio of CO($J$ = 2-1)/($J$ = 1-0) transitions as well as CO
line broadening, which indicate shock heating/acceleration. Further, the
velocity distribution of CO and HI shows signs of expansion at $sim$10 km
s$^{-1}$ in the receding part of the shell. The ISM interacting with the SNR
has large mass of $sim$10$^{4}$ $M_{odot}$ which is dominated by HI, showing
good spatial correspondence with the Fermi-LAT gamma ray image. This favors the
hadronic origin of the gamma rays, while additional contribution of the
leptonic component is not excluded. The distribution of the X-ray ionization
timescales within the shell suggests that the shock front ionized various parts
of the ISM at epochs ranging over a few to ten 1000 yr. We therefore suggest
that the age of the SNR is around 10$^{4}$ yr as given by the largest
ionization timescale. We estimate the total cosmic ray energy $W_{
m p}$ to be
10$^{47}$ erg, which is well placed in the cosmic ray escaping phase of an
age-$W_{
m p}$ plot including more than ten SNRs. | | Source: | arXiv, 2206.00211 | | Services: | Forum | Review | PDF | Favorites | |
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