Browsing by Author "Yamamoto, S."

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    HCN emission from translucent gas and UV-illuminated cloud edges revealed by wide-field IRAM 30 m maps of the Orion B GMC
    (2023) Santa-Maria, M. G.; Goicoechea, J. R.; Pety, J.; Gerin, M.; Orkisz, J. H.; Le Petit, F.; Einig, L.; Palud, P.; Magalhaes, V. de Souza; Beslic, I.; Segal, L.; Bardeau, S.; Bron, E.; Chainais, P.; Chanussot, J.; Gratier, P.; Guzman, V. V.; Hughes, A.; Languignon, D.; Levrier, F.; Lis, D. C.; Liszt, H. S.; Le Bourlot, J.; Oya, Y.; Oberg, K.; Peretto, N.; Roueff, E.; Roueff, A.; Sievers, A.; Thouvenin, P. -A.; Yamamoto, S.
    Context. Massive stars form within dense clumps inside giant molecular clouds (GMCs). Finding appropriate chemical tracers of the dense gas (n(H-2) > several 10(4) cm(-)3 or A(V) > 8 mag) and linking their line luminosity with the star formation rate is of critical importance.
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    Physical properties of accretion shocks toward the Class I protostellar system Oph-IRS 44
    (2022) de la Villarmois, E. Artur; Guzman, V. V.; Jorgensen, J. K.; Kristensen, L. E.; Bergin, E. A.; Harsono, D.; Sakai, N.; van Dishoeck, E. F.; Yamamoto, S.
    Context. The final outcome and chemical composition of a planetary system depend on its formation history: the physical processes that were involved and the molecular species available at different stages. Physical processes such as accretion shocks are thought to be common in the protostellar phase, where the envelope component is still present, and they can release molecules from the dust to the gas phase, altering the original chemical composition of the disk. Consequently, the study of accretion shocks is essential for a better understanding of the physical processes at disk scales and their chemical output.