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http://hdl.handle.net/20.500.12386/31252
Title: | FAUST I. The hot corino at the heart of the prototypical Class I protostar L1551 IRS5 | Authors: | Bianchi, E. Chandler, C. J. Ceccarelli, C. CODELLA, CLAUDIO Sakai, N. López-Sepulcre, A. Maud, L. T. Moellenbrock, G. Svoboda, B. Watanabe, Y. Sakai, T. Ménard, F. Aikawa, Y. Alves, F. Balucani, N. Bouvier, M. Caselli, P. Caux, E. Charnley, S. Choudhury, S. De Simone, M. Dulieu, F. Durán, A. Evans, L. Favre, C. FEDELE , DAVIDE Feng, S. FONTANI, FRANCESCO Francis, L. Hama, T. Hanawa, T. Herbst, E. Hirota, T. Imai, M. Isella, A. Jiménez-Serra, I. Johnstone, D. Kahane, C. Lefloch, B. Loinard, L. Maureira, M. J. MERCIMEK, SEYMA Miotello, A. Mori, S. Nakatani, R. Nomura, H. Oba, Y. Ohashi, S. Okoda, Y. Ospina-Zamudio, J. Oya, Y. Pineda, J. PODIO, LINDA Rimola, A. Cox, D. Segura Shirley, Y. TAQUET, VIANNEY DANIEL FRANCOIS TESTI, Leonardo Vastel, C. Viti, S. Watanabe, N. Witzel, A. Xue, C. Zhang, Y. Zhao, B. Yamamoto, S. |
Issue Date: | 2020 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. LETTERS | Number: | 498 | Issue: | 1 | First Page: | L87 | Abstract: | 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 Large Program FAUST. We detected several lines from methanol and its isopotologues (<SUP>13</SUP>CH<SUB>3</SUB>OH and CH<SUB>2</SUB>DOH), methyl formate and ethanol. Lines are bright toward 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 × 10<SUP>8</SUP> cm<SUP>-3</SUP>), and emitting size (˜10 au in radius). All CH<SUB>3</SUB>OH and <SUP>13</SUP>CH<SUB>3</SUB>OH 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 the present work, little chemical evolution from Class 0 to I hot corinos occurs. | URI: | http://hdl.handle.net/20.500.12386/31252 | URL: | https://academic.oup.com/mnrasl/article-abstract/498/1/L87/5874261?redirectedFrom=fulltext http://arxiv.org/abs/2007.10275v1 |
ISSN: | 1745-3925 | DOI: | 10.1093/mnrasl/slaa130 | Bibcode ADS: | 2020MNRAS.498L..87B | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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bianchi_2020_postprint.pdf | preprint | 352.23 kB | Adobe PDF | View/Open |
slaa130.pdf | PDF editoriale | 671.06 kB | Adobe PDF | View/Open |
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