Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud

RX J0046.5−7308 is a shell-type supernova remnant (SNR) in the Small Magellanic Cloud (SMC). We carried out new 12CO(J = 1-0, 3-2) observations toward the SNR using Mopra and the Atacama Submillimeter Telescope Experiment. We found eight molecular clouds (A-H) along the X-ray shell of the SNR. The t...

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Published inThe Astrophysical journal Vol. 881; no. 1; pp. 85 - 96
Main Authors Sano, H., Matsumura, H., Yamane, Y., Maggi, P., Fujii, K., Tsuge, K., Tokuda, K., Alsaberi, R. Z. E., Filipovi, M. D., Maxted, N., Rowell, G., Uchida, H., Tanaka, T., Muraoka, K., Takekoshi, T., Onishi, T., Kawamura, A., Minamidani, T., Mizuno, N., Yamamoto, H., Tachihara, K., Inoue, T., Inutsuka, S., Voisin, F., Tothill, N. F. H., Sasaki, M., McClure-Griffiths, N. M., Fukui, Y.
Format Journal Article
LanguageEnglish
Published Philadelphia The American Astronomical Society 10.08.2019
IOP Publishing
American Astronomical Society
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Abstract RX J0046.5−7308 is a shell-type supernova remnant (SNR) in the Small Magellanic Cloud (SMC). We carried out new 12CO(J = 1-0, 3-2) observations toward the SNR using Mopra and the Atacama Submillimeter Telescope Experiment. We found eight molecular clouds (A-H) along the X-ray shell of the SNR. The typical cloud size and mass are ∼10-15 pc and ∼1000-3000 M☉, 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 12CO(J = 3-2)/12CO(J = 1-0) > 1.2, which are not attributable to any identified internal infrared sources or high-mass stars. The H i 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, and G and H i clouds within the wind-blown cavity at VLSR = 117.1-122.5 km s−1 are associated with the SNR. The X-ray spectroscopy reveals the dynamical age of yr and the progenitor mass of 30 M☉, 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 data sets of the Atacama Large Millimeter/submillimeter Array; the kinematic temperature is K and the number density of molecular hydrogen is cm−3. The next generation of γ-ray observations will allow us to study the pion-decay γ-rays from the molecular clouds in the SMC SNR.
AbstractList 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 the Atacama Submillimeter Telescope Experiment. We found 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$1000-3000 $M_{\odot}$, 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) $> 1.2$, which are 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, and 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 $26000^{+1000}_{-2000}$ yr and the progenitor mass of $\gtrsim 30$ $M_{\odot}$, 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 the Atacama Large Millimeter/submillimeter Array; the kinematic temperature is $72^{+50}_{-37}$ K and the number density of molecular hydrogen is $1500^{+600}_{-300}$ cm$^{-3}$. The next generation of $\gamma$-ray observations will allow us to study the pion-decay $\gamma$-rays from the 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 12CO(J = 1-0, 3-2) observations toward the SNR using Mopra and the Atacama Submillimeter Telescope Experiment. We found eight molecular clouds (A-H) along the X-ray shell of the SNR. The typical cloud size and mass are ∼10-15 pc and ∼1000-3000 M☉, 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 12CO(J = 3-2)/12CO(J = 1-0) > 1.2, which are not attributable to any identified internal infrared sources or high-mass stars. The H i 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, and G and H i clouds within the wind-blown cavity at VLSR = 117.1-122.5 km s−1 are associated with the SNR. The X-ray spectroscopy reveals the dynamical age of yr and the progenitor mass of 30 M☉, 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 data sets of the Atacama Large Millimeter/submillimeter Array; the kinematic temperature is K and the number density of molecular hydrogen is cm−3. The next generation of γ-ray observations will allow us to study the pion-decay γ-rays from the 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 12CO(J = 1–0, 3–2) observations toward the SNR using Mopra and the Atacama Submillimeter Telescope Experiment. We found eight molecular clouds (A–H) along the X-ray shell of the SNR. The typical cloud size and mass are ∼10–15 pc and ∼1000–3000 M ☉, 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 12CO(J = 3–2)/12CO(J = 1–0) > 1.2, which are not attributable to any identified internal infrared sources or high-mass stars. The H i 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, and G and H i clouds within the wind-blown cavity at V LSR = 117.1–122.5 km s−1 are associated with the SNR. The X-ray spectroscopy reveals the dynamical age of \({26000}_{-2000}^{+1000}\) yr and the progenitor mass of ≳30 M ☉, 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 data sets of the Atacama Large Millimeter/submillimeter Array; the kinematic temperature is \({72}_{-37}^{+50}\) K and the number density of molecular hydrogen is \({1500}_{-300}^{+600}\) cm−3. The next generation of γ-ray observations will allow us to study the pion-decay γ-rays from the molecular clouds in the SMC SNR.
Abstract 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 the Atacama Submillimeter Telescope Experiment. We found eight molecular clouds (A–H) along the X-ray shell of the SNR. The typical cloud size and mass are ∼10–15 pc and ∼1000–3000  M ☉ , 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, which are not attributable to any identified internal infrared sources or high-mass stars. The H i 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, and G and H i clouds within the wind-blown cavity at V LSR  = 117.1–122.5 km s −1 are associated with the SNR. The X-ray spectroscopy reveals the dynamical age of yr and the progenitor mass of ≳30 M ☉ , 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 data sets of the Atacama Large Millimeter/submillimeter Array; the kinematic temperature is K and the number density of molecular hydrogen is cm −3 . The next generation of γ -ray observations will allow us to study the pion-decay γ -rays from the molecular clouds in the SMC SNR.
Author Fukui, Y.
Filipovi, M. D.
Tachihara, K.
Yamamoto, H.
Kawamura, A.
Inoue, T.
Takekoshi, T.
Maggi, P.
Fujii, K.
Tothill, N. F. H.
Uchida, H.
Tokuda, K.
Onishi, T.
Mizuno, N.
Minamidani, T.
Sasaki, M.
Muraoka, K.
Tanaka, T.
Rowell, G.
Alsaberi, R. Z. E.
Inutsuka, S.
Sano, H.
Voisin, F.
Tsuge, K.
Yamane, Y.
Maxted, N.
Matsumura, H.
McClure-Griffiths, N. M.
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Copyright 2019. The American Astronomical Society. All rights reserved.
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DocumentTitleAlternate Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud
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Notes AAS17154
Interstellar Matter and the Local Universe
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Snippet RX J0046.5−7308 is a shell-type supernova remnant (SNR) in the Small Magellanic Cloud (SMC). We carried out new 12CO(J = 1-0, 3-2) observations toward the SNR...
Abstract 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...
RX J0046.5−7308 is a shell-type supernova remnant (SNR) in the Small Magellanic Cloud (SMC). We carried out new 12CO(J = 1–0, 3–2) observations toward the 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...
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StartPage 85
SubjectTerms Astrophysics
Clouds
Hydrogen
Infrared sources (astronomy)
ISM: clouds
ISM: individual objects (RX J0046.5−7308, DEM S23)
ISM: supernova remnants
Magellanic Clouds
Massive stars
Molecular clouds
Physics
Pions
Radio telescopes
Spectroscopy
Stellar winds
Supernova
Supernova remnants
Velocity gradient
X-ray spectroscopy
Title Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud
URI https://iopscience.iop.org/article/10.3847/1538-4357/ab2ade
https://www.proquest.com/docview/2365773039/abstract/
https://hal.science/hal-02264951
Volume 881
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