FAUST I. The hot corino at the heart of the prototypical Class I protostar L1551 IRS5-Reference-Cited by-同舟云学术

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

Published:2020-07-21 Issue:1 Volume:498 Page:L87-L92
ISSN:1745-3925
Container-title:Monthly Notices of the Royal Astronomical Society: Letters
language:en
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Author:

Bianchi E¹^ORCID,Chandler C J²,Ceccarelli C¹^ORCID,Codella C¹³,Sakai N⁴^ORCID,López-Sepulcre A¹⁵,Maud L T⁶,Moellenbrock G²,Svoboda B²,Watanabe Y⁷^ORCID,Sakai T⁸,Ménard F¹,Aikawa Y⁹,Alves F¹⁰,Balucani N¹¹^ORCID,Bouvier M¹,Caselli P¹²,Caux E¹³,Charnley S¹⁴,Choudhury S¹⁰,De Simone M¹,Dulieu F¹⁵,Durán A¹⁶,Evans L³¹³,Favre C¹,Fedele D³,Feng S¹⁷¹⁸¹⁹,Fontani F³^ORCID,Francis L²⁰²¹,Hama T²²²³,Hanawa T²⁴,Herbst E²⁵,Hirota T¹⁸,Imai M²⁶,Isella A²⁷,Jiménez-Serra I²⁸,Johnstone D²⁰²¹,Kahane C¹,Lefloch B¹,Loinard L¹⁶²⁹,Maureira M J¹⁰,Mercimek S³³⁰,Miotello A⁶,Mori S⁹,Nakatani R⁴,Nomura H³¹,Oba Y³²,Ohashi S⁴,Okoda Y²⁶,Ospina-Zamudio J¹^ORCID,Oya Y²⁶,Pineda J¹⁰^ORCID,Podio L³^ORCID,Rimola A³²^ORCID,Segura Cox D¹²,Shirley Y³³,Taquet V³,Testi L⁶,Vastel C¹³,Viti S³⁴,Watanabe N³⁵,Witzel A¹,Xue C²⁵,Zhang Y⁴,Zhao B¹⁰^ORCID,Yamamoto S²⁶

Affiliation:

1. IPAG, Univ. Grenoble Alpes, CNRS, F-38000 Grenoble, France

2. National Radio Astronomy Observatory, PO Box O, Socorro, NM 87801, USA

3. INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy

4. RIKEN Cluster for Pioneering Research, 2-1, Hirosawa, Wako-shi, Saitama 351-0198, Japan

5. Institut de Radioastronomie Millimétrique, F-38406 Saint-Martin d’Hères, France

6. European Southern Observatory, Karl-Schwarzschild Str 2, D-85748 Garching bei München, Germany

7. Materials Science and Engineering, College of Engineering, Shibaura Institute of Technology, 3-7-5 Toyosu, Koto-ku, Tokyo 135-8548, Japan

8. Graduate School of Informatics and Engineering, The University of Electro-Communications, Chofu, Tokyo 182-8585, Japan

9. Department of Astronomy, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan

10. Max-Planck-Institut für extraterrestrische Physik (MPE), Gießenbachstr 1, D-85741 Garching, Germany

11. Department of Chemistry, Biology, and Biotechnology, The University of Perugia, Via Elce di Sotto 8, I-06123 Perugia, Italy

12. Center for Astrochemical Studies, Max-Planck-Institut für extraterrestrische Physik (MPE), Gießenbachstr 1, D-85741 Garching, Germany

13. IRAP, Université de Toulouse, CNRS, CNES, UPS, Toulouse 31400, France

14. Astrochemistry Laboratory, Code 691, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA

15. CY Cergy Paris Université, Sorbonne Université, Observatoire de Paris, PSL University, CNRS, LERMA, F-95000 Cergy, France

16. Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, A.P. 3-72 (Xangari), Morelia 8701, Mexico

17. CAS Key Laboratory of FAST, National Astronomical Observatory of China, Datun Road 20, Chaoyang, Beijing 100012, China

18. National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

19. Academia Sinica Institute of Astronomy and Astrophysics, No.1, Section 4, Roosevelt Rd, Taipei 10617, Taiwan

20. Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Elliot Building, Victoria, BC V8P 5C2, Canada

21. NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada

22. Komaba Institute for Science, The University of Tokyo, 3-8-1 Komaba, Meguro, Tokyo 153-8902, Japan

23. Department of Basic Science, The University of Tokyo, 3-8-1 Komaba, Meguro, Tokyo 153-8902, Japan

24. Center for Frontier Science, Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522, Japan

25. Department of Chemistry, University of Virginia, McCormick Road, PO Box 400319, Charlottesville, VA 22904, USA

26. Department of Physics, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan

27. Department of Physics and Astronomy, Rice University, 6100 Main Street, MS-108, Houston, TX 77005, USA

28. Centro de Astrobiologia (CSIC-INTA), Ctra. de Torrejon a Ajalvir, km 4, E-28850 Torrejon de Ardoz, Spain

29. Instituto de Astronomía, Universidad Nacional Autónoma de México, Ciudad Universitaria, A.P. 70-264, Cuidad de México 04510, Mexico

30. Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, via G. Sansone 1, I-50019 Sesto Fiorentino, Italy

31. Division of Science, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

32. Departament de Química, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain

33. Steward Observatory, 933 N Cherry Avenue, Tucson, AZ 85721, USA

34. Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

35. Institute of Low Temperature Science, Hokkaido University, N19W8, Kita-ku, Sapporo, Hokkaido 060-0819, Japan

Abstract

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 (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 × 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.

Funder

H2020 European Research Council

Japan Society for the Promotion of Science

Federación Española de Enfermedades Raras

Dirección General de Asuntos del Personal Académico, Universidad Nacional Autónoma de México

Consejo Nacional de Ciencia y Tecnología

Agence Nationale de la Recherche

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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