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We carried out new CO($J$ = 2-1) observations toward the mixed-morphologysupernova remnant (SNR) W49B with the Atacama Large Millimeter/submillimeterArray (ALMA). We found that CO clouds at $\sim$10 km s$^{-1}$ show a goodspatial correspondence with synchrotron radio continuum as well as an X-raydeformed shell. The bulk mass of molecular clouds accounts for the western partof the shell, not for the eastern shell where near-infrared H$_2$ emission isdetected. The molecular clouds at $\sim$10 km s$^{-1}$ show higher kinetictemperature of $\sim$20-60 K, suggesting that modest shock-heating occurred.The expanding motion of the clouds with $\Delta V \sim$6 km s$^{-1}$ was formedby strong winds from the progenitor system. We argue that the barrel-likestructure of Fe rich ejecta was possibly formed not only by an asymmetricexplosion, but also by interactions with dense molecular clouds. We also founda negative correlation between the CO intensity and the electron temperature ofrecombining plasma, implying that the origin of the high-temperaturerecombining plasma in W49B can be understood as the thermal conduction model.The total energy of accelerated cosmic-ray protons $W_\mathrm{p}$ is estimatedto be $\sim$$2\times 10^{49}$ erg by adopting an averaged gas density of$\sim$$650\pm200$ cm$^{-3}$. The SNR age-$W_\mathrm{p}$ diagram indicates thatW49B shows one of the highest in-situ values of $W_\mathrm{p}$ in the gamma-raybright SNRs.

astrophysical journal/the astrophysical journal

ALMA CO Observations of the Mixed-Morphology Supernova Remnant W49B:  Efficient Production of Recombining Plasma and Hadronic Gamma-rays via  Shock-Cloud Interactions