SIMBAD references

2020MNRAS.498L..87B - Mon. Not. R. Astron. Soc., 498, L87-L92 (2020/October-2)

FAUST I. The hot corino at the heart of the prototypical Class I protostar L1551 IRS5.

BIANCHI E., CHANDLER C.J., CECCARELLI C., CODELLA C., SAKAI N., LOPEZ-SEPULCRE A., MAUD L.T., MOELLENBROCK G., SVOBODA B., WATANABE Y., SAKAI T., MENARD F., AIKAWA Y., ALVES F., BALUCANI N., BOUVIER M., CASELLI P., CAUX E., CHARNLEY S., CHOUDHURY S., DE SIMONE M., DULIEU F., DURAN A., EVANS L., FAVRE C., FEDELE D., FENG S., FONTANI F., FRANCIS L., HAMA T., HANAWA T., HERBST E., HIROTA T., IMAI M., ISELLA A., JIMENEZ-SERRA I., JOHNSTONE D., KAHANE C., LEFLOCH B., LOINARD L., MAUREIRA M.J., MERCIMEK S., MIOTELLO A., MORI S., NAKATANI R., NOMURA H., OBA Y., OHASHI S., OKODA Y., OSPINA-ZAMUDIO J., OYA Y., PINEDA J., PODIO L., RIMOLA A., SEGURA-COX D., SHIRLEY Y., TAQUET V., TESTI L., VASTEL C., VITI S., WATANABE N., WITZEL A., XUE C., ZHANG Y., ZHAO B. and YAMAMOTO S.

Abstract (from CDS):

The study of hot corinos in solar-like protostars has been so far mostly limited to the Class 0 phase, hampering our understanding of their origin and evolution. In addition, recent evidence suggests that planet formation starts already during Class I phase, which therefore represents a crucial step in the future planetary system chemical composition. Hence, the study of hot corinos in Class I protostars has become of paramount importance. Here, we report the discovery of a hot corino towards the prototypical Class I protostar L1551 IRS5, obtained within the ALMA (Atacama Large Millimeter/submillimeter Array) Large Program FAUST (Fifty AU STudy of the chemistry in the disc/envelope system of solar-like protostars). We detected several lines from methanol and its isotopologues (13CH3OH and CH2DOH), methyl formate, and ethanol. Lines are bright towards the north component of the IRS5 binary system, and a possible second hot corino may be associated with the south component. The methanol lines' non-LTE analysis constrains the gas temperature (∼100 K), density (>=1.5 x 108 cm–3), and emitting size (∼10 au in radius). All CH3OH and 13CH3OH lines are optically thick, preventing a reliable measure of the deuteration. The methyl formate and ethanol relative abundances are compatible with those measured in Class 0 hot corinos. Thus, based on this work, little chemical evolution from Class 0 to I hot corinos occurs.

Abstract Copyright: © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): astrochemistry - stars: formation - ISM: molecules

Simbad objects: 12

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2021.07.31-19:00:31

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