Discovery of Shocked Molecular Clouds Associated with the Shell-Type Supernova Remnant RX J0046.5$-$7308 in the Small Magellanic Cloud. (arXiv:1904.04836v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sano_H/0/1/0/all/0/1">H. Sano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsumura_H/0/1/0/all/0/1">H. Matsumura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamane_Y/0/1/0/all/0/1">Y. Yamane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maggi_P/0/1/0/all/0/1">P. Maggi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fujii_K/0/1/0/all/0/1">K. Fujii</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tsuge_K/0/1/0/all/0/1">K. Tsuge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tokuda_K/0/1/0/all/0/1">K. Tokuda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alsaberi_R/0/1/0/all/0/1">R. Z. E. Alsaberi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Filipovic_M/0/1/0/all/0/1">M. D. Filipovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maxted_N/0/1/0/all/0/1">N. Maxted</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rowell_G/0/1/0/all/0/1">G. Rowell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Uchida_H/0/1/0/all/0/1">H. Uchida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tanaka_T/0/1/0/all/0/1">T. Tanaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muraoka_K/0/1/0/all/0/1">K. Muraoka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takekoshi_T/0/1/0/all/0/1">T. Takekoshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onishi_T/0/1/0/all/0/1">T. Onishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawamura_A/0/1/0/all/0/1">A. Kawamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Minamidani_T/0/1/0/all/0/1">T. Minamidani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mizuno_N/0/1/0/all/0/1">N. Mizuno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamamoto_H/0/1/0/all/0/1">H. Yamamoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tachihara_K/0/1/0/all/0/1">K. Tachihara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inoue_T/0/1/0/all/0/1">T. Inoue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inutsuka_S/0/1/0/all/0/1">S. Inutsuka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Voisin_F/0/1/0/all/0/1">F. Voisin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tothill_N/0/1/0/all/0/1">N. F. H. Tothill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sasaki_M/0/1/0/all/0/1">M. Sasaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McClure_Griffiths_N/0/1/0/all/0/1">N. M. McClure-Griffiths</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukui_Y/0/1/0/all/0/1">Y. Fukui</a>
RX J0046.5$-$7308 is a shell-type supernova remnant (SNR) in the Small
Magellanic Cloud (SMC). We carried out new $^{12}$CO($J$ = 1-0, 3-2)
observations toward the SNR using Mopra and ASTE. We reveled eight molecular
clouds (A-H) along the X-ray shell of the SNR. The typical cloud size and mass
are $sim$10-15 pc and $sim$2000-5000 $M_{odot}$, respectively. The X-ray
shell is slightly deformed and has the brightest peak in the southwestern shell
where two molecular clouds A and B are located. The four molecular clouds A, B,
F, and G have high-intensity ratios of $^{12}$CO($J$ = 3-2) / $^{12}$CO($J$ =
1-0) $> 1.2$, not attributable to any identified internal infrared sources or
high-mass stars. The HI cavity and its expanding motion are found toward the
SNR, which are likely created by strong stellar winds from a massive
progenitor. We suggest that the molecular clouds A-D, F, G, and HI clouds
within the wind-blown cavity at $V_mathrm{LSR} = 117.1$-122.5 km s$^{-1}$ are
to be associated with the SNR. The X-ray spectroscopy reveals the dynamical age
of $25000^{+2000}_{-1000}$ yr and the progenitor mass of $sim$20 $M_{odot}$,
which is also consistent with the proposed scenario. We determine physical
conditions of the giant molecular cloud LIRS 36A using the large velocity
gradient analysis with archival datasets of ALMA; the kinematic temperature is
$72^{+50}_{-37}$ K and the number density of molecular hydrogen is
$1500^{+600}_{-300}$ cm$^{-3}$. Next generation of $gamma$-ray observations
will allow us to study the pion-decay $gamma$-rays from the GMC and molecular
clouds in the SMC SNR.
RX J0046.5$-$7308 is a shell-type supernova remnant (SNR) in the Small
Magellanic Cloud (SMC). We carried out new $^{12}$CO($J$ = 1-0, 3-2)
observations toward the SNR using Mopra and ASTE. We reveled eight molecular
clouds (A-H) along the X-ray shell of the SNR. The typical cloud size and mass
are $sim$10-15 pc and $sim$2000-5000 $M_{odot}$, respectively. The X-ray
shell is slightly deformed and has the brightest peak in the southwestern shell
where two molecular clouds A and B are located. The four molecular clouds A, B,
F, and G have high-intensity ratios of $^{12}$CO($J$ = 3-2) / $^{12}$CO($J$ =
1-0) $> 1.2$, not attributable to any identified internal infrared sources or
high-mass stars. The HI cavity and its expanding motion are found toward the
SNR, which are likely created by strong stellar winds from a massive
progenitor. We suggest that the molecular clouds A-D, F, G, and HI clouds
within the wind-blown cavity at $V_mathrm{LSR} = 117.1$-122.5 km s$^{-1}$ are
to be associated with the SNR. The X-ray spectroscopy reveals the dynamical age
of $25000^{+2000}_{-1000}$ yr and the progenitor mass of $sim$20 $M_{odot}$,
which is also consistent with the proposed scenario. We determine physical
conditions of the giant molecular cloud LIRS 36A using the large velocity
gradient analysis with archival datasets of ALMA; the kinematic temperature is
$72^{+50}_{-37}$ K and the number density of molecular hydrogen is
$1500^{+600}_{-300}$ cm$^{-3}$. Next generation of $gamma$-ray observations
will allow us to study the pion-decay $gamma$-rays from the GMC and molecular
clouds in the SMC SNR.
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