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FAUST I. The hot corino at the heart of the prototypical Class I protostar L1551 IRS5 | | E. Bianchi
; C. J. Chandler
; C. Ceccarelli
; C. Codella
; N. Sakai
; A. López-Sepulcre
; L. T. Maud
; G. Moellenbrock
; B. Svoboda
; Y. Watanabe
; T. Sakai
; F. Ménard
; Y. Aikawa
; F. Alves
; N. Balucani
; M. Bouvier
; P. Caselli
; E. Caux
; S. Charnley
; S. Choudhury
; M. De Simone
; F. Dulieu
; A. Durán
; L. Evans
; C. Favre
; D. Fedele
; S. Feng
; F. Fontani
; L. Francis
; T. Hama
; T. Hanawa
; E. Herbst
; T. Hirota
; M. Imai
; A. Isella
; I. Jiménez-Serra
; D. Johnstone
; C. Kahane
; B. Lefloch
; L. Loinard
; M. J. Maureira
; S. Mercimek
; A. Miotello
; S. Mori
; R. Nakatani
; H. Nomura
; Y. Oba
; S. Ohashi
; Y. Okoda
; J. Ospina-Zamudio
; Y. Oya
; J. Pineda
; L. Podio
; A. Rimola
; D. Segura Cox
; Y. Shirley
; V. Taquet
; L. Testi
; C. Vastel
; S. Viti
; N. Watanabe
; A. Witzel
; C. Xue
; Y. Zhang
; B. Zhao
; S. Yamamoto
; | | Date: |
20 Jul 2020 | | 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 ($^{13}$CH$_{
m 3}$OH and CH$_{
m
2}$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 ($sim$100 K), density
($geq$1.5$ imes$10$^{8}$ cm$^{-3}$), and emitting size ($sim$10 au in
radius). All CH$_{
m 3}$OH and $^{13}$CH$_{
m 3}$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. | | Source: | arXiv, 2007.10275 | | Services: | Forum | Review | PDF | Favorites | |
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