TY - JOUR
T1 - Associated molecular and atomic clouds with x-ray shell of superbubble 30 Doradus C in the LMC
AU - Yamane, Y.
AU - Sano, H.
AU - Filipović, M. D.
AU - Tokuda, K.
AU - Fujii, K.
AU - Babazaki, Y.
AU - Mitsuishi, I.
AU - Inoue, T.
AU - Aharonian, F.
AU - Inaba, T.
AU - Inutsuka, S.
AU - Maxted, N.
AU - Mizuno, N.
AU - Onishi, T.
AU - Rowell, G.
AU - Tsuge, K.
AU - Voisin, F.
AU - Yoshiike, S.
AU - Fukuda, T.
AU - Kawamura, A.
AU - Bamba, A.
AU - Tachihara, K.
AU - Fukui, Y.
PY - 2021
Y1 - 2021
N2 - 30 Doradus C is a superbubble that emits the brightest non-thermal X- and TeV gamma-rays in the Local Group. To explore the detailed connection between the high-energy radiation and the interstellar medium, we have carried out new CO and Hi observations using the Atacama Large Millimeter/Submillimeter Array (ALMA), Atacama Submillimeter Telescope Experiment, and the Australia Telescope Compact Array with resolutions of up to 3 pc. The ALMA data of 12CO(J = 1-0) emission revealed 23 molecular clouds, with typical diameters of ∼6-12 pc and masses of ∼600-10,000 M o˙. A comparison with the X-rays of XMM-Newton at ∼3 pc resolution shows that X-rays are enhanced toward these clouds. The CO data were combined with the Hi to estimate the total interstellar protons. A comparison of the interstellar proton column density and the X-rays revealed that the X-rays are enhanced with the total proton column density. These are most likely to be caused by the shock-cloud interaction, which is modeled by magnetohydrodynamical simulations (Inoue et al. 2012). We also note a trend for the X-ray photon index to vary with distance from the center of the high-mass star cluster. This suggests that the cosmic-ray electrons are accelerated by one or multiple supernovae in the cluster. Based on these results, we discuss the role of the interstellar medium in cosmic-ray particle acceleration.
AB - 30 Doradus C is a superbubble that emits the brightest non-thermal X- and TeV gamma-rays in the Local Group. To explore the detailed connection between the high-energy radiation and the interstellar medium, we have carried out new CO and Hi observations using the Atacama Large Millimeter/Submillimeter Array (ALMA), Atacama Submillimeter Telescope Experiment, and the Australia Telescope Compact Array with resolutions of up to 3 pc. The ALMA data of 12CO(J = 1-0) emission revealed 23 molecular clouds, with typical diameters of ∼6-12 pc and masses of ∼600-10,000 M o˙. A comparison with the X-rays of XMM-Newton at ∼3 pc resolution shows that X-rays are enhanced toward these clouds. The CO data were combined with the Hi to estimate the total interstellar protons. A comparison of the interstellar proton column density and the X-rays revealed that the X-rays are enhanced with the total proton column density. These are most likely to be caused by the shock-cloud interaction, which is modeled by magnetohydrodynamical simulations (Inoue et al. 2012). We also note a trend for the X-ray photon index to vary with distance from the center of the high-mass star cluster. This suggests that the cosmic-ray electrons are accelerated by one or multiple supernovae in the cluster. Based on these results, we discuss the role of the interstellar medium in cosmic-ray particle acceleration.
UR - https://hdl.handle.net/1959.7/uws:65589
U2 - 10.3847/1538-4357/ac0adb
DO - 10.3847/1538-4357/ac0adb
M3 - Article
SN - 0004-637X
VL - 918
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 36
ER -