JOYS

Autor(en): C. Gieser, H. Beuther, E. F. Van Dishoeck, L. Francis, M. L. Van Gelder, L. Tychoniec, P. J. Kavanagh, G. Perotti, A. Caratti O Garatti, T. P. Ray, P. Klaassen, K. Justtanont, H. Linnartz, W. R.M. Rocha, K. Slavicinska, L. Colina, M. Güdel, Th Henning, P. O. Lagage, G. A Stlin, B. Vandenbussche, C. Waelkens, G. Wright
Abstrakt: Context. High-mass star formation occurs in a clustered mode where fragmentation is observed from an early stage onward. Young protostars can now be studied in great detail with the recently launched James Webb Space Telescope (JWST). Aims. We study and compare the warm (>100 K) and cold (<100 K) material toward the high-mass star-forming region (HMSFR) IRAS 23385+6053 (IRAS 23385 hereafter) combining high-angular-resolution observations in the mid-infrared (MIR) with the JWST Observations of Young protoStars (JOYS) project and with the NOrthern Extended Millimeter Array (NOEMA) at millimeter (mm) wavelengths at angular resolutions of 0.a2 1.a0. Methods. We investigated the spatial morphology of atomic and molecular species using line-integrated intensity maps. We estimated the temperature and column density of different gas components using H₂ transitions (warm and hot component) and a series of CH₃CN transitions as well as 3 mm continuum emission (cold component). Results. Toward the central dense core of IRAS 23385, the material consists of relatively cold gas and dust ( 50 K), while multiple outflows create heated and/or shocked H₂ and show enhanced temperatures ( 400 K) along the outflow structures. An energetic outflow with enhanced emission knots of [FeII] and [NiII] suggests J-type shocks, while two other outflows have enhanced emission of only H₂ and [SI] caused by C-type shocks. The latter two outflows are also more prominent in molecular line emission at mm wavelengths (e.g., SiO, SO, H₂CO, and CH₃OH). Data of even higher angular resolution are needed to unambiguously identify the outflow-driving sources given the clustered nature of IRAS 23385. While most of the forbidden fine structure transitions are blueshifted, [NeII] and [NeIII] peak at the source velocity toward the MIR source A/mmA2 suggesting that the emission is originating from closer to the protostar. Conclusions. The warm and cold gas traced by MIR and mm observations, respectively, are strongly linked in IRAS 23385. The outflows traced by MIR H₂ lines have molecular counterparts in the mm regime. Despite the presence of multiple powerful outflows that cause dense and hot shocks, a cold dense envelope still allows star formation to further proceed. To study and fully understand the spatially resolved MIR properties, a representative sample of low- and high-mass protostars has to be probed using JWST.
Organisation(en): Institut für Astrophysik
Externe Organisation(en): Max-Planck-Institut für extraterrestrische Physik, Max-Planck-Institut für Astronomie, Leiden University, European Southern Observatory (Germany), National University of Ireland, Maynooth, INAF-Osservatorio Astronomico di Capodimonte, Dublin Institute for Advanced Studies, The Royal Observatory, Edinburgh, Chalmers University of Technology, Eidgenössische Technische Hochschule Zürich, Université Paris Saclay, Oskar Klein Centre, Katholieke Universiteit Leuven, Centro de Astrobiología (CSIC-INTA)
Journal: Astronomy and Astrophysics
Band: 679
Anzahl der Seiten: 17
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/202347060
Publikationsdatum: 11-2023
Peer-reviewed: Ja
ÖFOS 2012: 103003 Astronomie, 103004 Astrophysik
Schlagwörter
ASJC Scopus Sachgebiete: Astronomy and Astrophysics, Space and Planetary Science
Link zum Portal: https://ucrisportal.univie.ac.at/de/publications/1c6c7e3d-2eae-4b5a-a96b-64a4b1bc66bf

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