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Ray TP, McCaughrean MJ, Caratti O Garatti A, Kavanagh PJ, Justtanont K, van Dishoeck EF, Reitsma M, Beuther H, Francis L, Gieser C, Klaassen P, Perotti G, Tychoniec L, van Gelder M, Colina L, Greve TR, Güdel M, Henning T, Lagage PO, Östlin G, Vandenbussche B, Waelkens C, Wright G. Author Correction: Outflows from the youngest stars are mostly molecular. Nature 2023; 623:E3. [PMID: 37845331 PMCID: PMC10620075 DOI: 10.1038/s41586-023-06744-8] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/18/2023]
Affiliation(s)
- T P Ray
- Dublin Institute for Advanced Studies, Dublin, Ireland.
- School of Physics, Trinity College Dublin, Dublin, Ireland.
| | | | | | - P J Kavanagh
- Dublin Institute for Advanced Studies, Dublin, Ireland
- Department of Experimental Physics, Maynooth University, Maynooth, Ireland
| | - K Justtanont
- Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, Onsala, Sweden
| | | | - M Reitsma
- European Space Agency, ESTEC, Noordwijk, the Netherlands
- Leiden Observatory, Leiden University, Leiden, the Netherlands
| | - H Beuther
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - L Francis
- Leiden Observatory, Leiden University, Leiden, the Netherlands
| | - C Gieser
- Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany
| | - P Klaassen
- UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK
| | - G Perotti
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - L Tychoniec
- European Southern Observatory, Garching, Germany
| | - M van Gelder
- Leiden Observatory, Leiden University, Leiden, the Netherlands
| | - L Colina
- Centro de Astrobiología (CAB, CSIC-INTA), Carretera de Ajalvir, Torrejón de Ardoz, Spain
| | - Th R Greve
- DTU Space, Technical University of Denmark, Kongens Lyngby, Denmark
| | - M Güdel
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
- Department of Astrophysics, University of Vienna, Vienna, Austria
- ETH Zürich, Institute for Particle Physics and Astrophysics, Zurich, Switzerland
| | - Th Henning
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - P O Lagage
- Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France
| | - G Östlin
- Department of Astronomy, Stockholm University, AlbaNova University Center, Stockholm, Sweden
| | | | - C Waelkens
- Institute of Astronomy, KU Leuven, Leuven, Belgium
| | - G Wright
- UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK
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Ray TP, McCaughrean MJ, Caratti O Garatti A, Kavanagh PJ, Justtanont K, van Dishoeck EF, Reitsma M, Beuther H, Francis L, Gieser C, Klaassen P, Perotti G, Tychoniec L, van Gelder M, Colina L, Greve TR, Güdel M, Henning T, Lagage PO, Östlin G, Vandenbussche B, Waelkens C, Wright G. Outflows from the youngest stars are mostly molecular. Nature 2023; 622:48-52. [PMID: 37619607 PMCID: PMC10550818 DOI: 10.1038/s41586-023-06551-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/03/2023] [Accepted: 08/17/2023] [Indexed: 08/26/2023]
Abstract
The formation of stars and planets is accompanied not only by the build-up of matter, namely accretion, but also by its expulsion in the form of highly supersonic jets that can stretch for several parsecs1,2. As accretion and jet activity are correlated and because young stars acquire most of their mass rapidly early on, the most powerful jets are associated with the youngest protostars3. This period, however, coincides with the time when the protostar and its surroundings are hidden behind many magnitudes of visual extinction. Millimetre interferometers can probe this stage but only for the coolest components3. No information is provided on the hottest (greater than 1,000 K) constituents of the jet, that is, the atomic, ionized and high-temperature molecular gases that are thought to make up the jet's backbone. Detecting such a spine relies on observing in the infrared that can penetrate through the shroud of dust. Here we report near-infrared observations of Herbig-Haro 211 from the James Webb Space Telescope, an outflow from an analogue of our Sun when it was, at most, a few times 104 years old. These observations reveal copious emission from hot molecules, explaining the origin of the 'green fuzzies'4-7 discovered nearly two decades ago by the Spitzer Space Telescope8. This outflow is found to be propagating slowly in comparison to its more evolved counterparts and, surprisingly, almost no trace of atomic or ionized emission is seen, suggesting its spine is almost purely molecular.
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Affiliation(s)
- T P Ray
- Dublin Institute for Advanced Studies, Dublin, Ireland.
- School of Physics, Trinity College Dublin, Dublin, Ireland.
| | | | | | - P J Kavanagh
- Dublin Institute for Advanced Studies, Dublin, Ireland
- Department of Experimental Physics, Maynooth University, Maynooth, Ireland
| | - K Justtanont
- Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, Onsala, Sweden
| | | | - M Reitsma
- European Space Agency, ESTEC, Noordwijk, the Netherlands
- Leiden Observatory, Leiden University, Leiden, the Netherlands
| | - H Beuther
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - L Francis
- Leiden Observatory, Leiden University, Leiden, the Netherlands
| | - C Gieser
- Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany
| | - P Klaassen
- UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK
| | - G Perotti
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - L Tychoniec
- European Southern Observatory, Garching, Germany
| | - M van Gelder
- Leiden Observatory, Leiden University, Leiden, the Netherlands
| | - L Colina
- Centro de Astrobiología (CAB, CSIC-INTA), Carretera de Ajalvir, Torrejón de Ardoz, Spain
| | - Th R Greve
- DTU Space, Technical University of Denmark, Kongens Lyngby, Denmark
| | - M Güdel
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
- Department of Astrophysics, University of Vienna, Vienna, Austria
- ETH Zürich, Institute for Particle Physics and Astrophysics, Zurich, Switzerland
| | - Th Henning
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - P O Lagage
- Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France
| | - G Östlin
- Department of Astronomy, Stockholm University, AlbaNova University Center, Stockholm, Sweden
| | | | - C Waelkens
- Institute of Astronomy, KU Leuven, Leuven, Belgium
| | - G Wright
- UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK
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Wallström SHJ, Lagadec E, Muller S, Black JH, Cox NLJ, Galván-Madrid R, Justtanont K, Longmore S, Olofsson H, Oudmaijer RD, Quintana-Lacaci G, Szczerba R, Vlemmings W, van Winckel H, Zijlstra A. ALMA Compact Array observations of the Fried Egg nebula: Evidence for large-scale asymmetric mass-loss from the yellow hypergiant IRAS 17163-3907. Astron Astrophys 2017; 597:A99. [PMID: 28190887 PMCID: PMC5300097 DOI: 10.1051/0004-6361/201628416] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
Yellow hypergiants are rare and represent a fast evolutionary stage of massive evolved stars. That evolutionary phase is characterised by a very intense mass loss, the understanding of which is still very limited. Here we report ALMA Compact Array observations of a 50″-mosaic toward the Fried Egg nebula, around one of the few Galactic yellow hypergiants IRAS 17163-3907. The emission from the 12CO J=2-1 line, H30α recombination line, and continuum is imaged at a resolution of ~8″, revealing the morphology of the molecular environment around the star. The continuum emission is unresolved and peaks at the position of the star. The radio recombination line H30α shows unresolved emission at the star, with an approximately gaussian spectrum centered on a velocity of 21±3 km s-1 with a width of 57±6 km s-1. In contrast, the CO 2-1 emission is complex and decomposes into several components beyond the contamination from interstellar gas in the line of sight. The CO spectrum toward the star is a broad plateau, centered at the systemic velocity of +18 km s-1 and with an expansion velocity of 100±10 km s-1. Assuming isotropic and constant mass-loss, we estimate a mass-loss rate of 8±1.5 ×10-5 M⊙ yr-1. At a radius of 25″ from the star, we detect CO emission associated with the dust ring previously imaged by Herschel. The kinematics of this ring, however, is not consistent with an expanding shell, but show a velocity gradient of vsys ±20 km s-1. In addition, we find a puzzling bright feature radially connecting the star to the CO ring, at a velocity of +40 km s-1 relative to the star. This spur feature may trace a unidirectional ejection event from the star. Our ACA observations reveal the complex morphology around IRAS 17163 and illustrate the breakthroughs that ALMA will bring to the field of massive stellar evolution.
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Affiliation(s)
- S H J Wallström
- Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439-92 Onsala, Sweden
| | - E Lagadec
- Laboratoire Lagrange, UMR7293, Université Côte d'Azur, CNRS, Observatoire de la Côte d'Azur, Boulevard de l'Observatoire, 06304 Nice Cedex 4, France
| | - S Muller
- Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439-92 Onsala, Sweden
| | - J H Black
- Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439-92 Onsala, Sweden
| | - N L J Cox
- Université de Toulouse, UPS-OMP, IRAP, 31028, Toulouse, France; CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse, France
| | - R Galván-Madrid
- Instituto de Radioastronomía y Astrofísica, UNAM, A.P. 3-72, Xangari, Morelia, 58089, Mexico
| | - K Justtanont
- Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439-92 Onsala, Sweden
| | - S Longmore
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool L3 5RF, UK
| | - H Olofsson
- Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439-92 Onsala, Sweden
| | - R D Oudmaijer
- School of Physics and Astronomy, The University of Leeds, Leeds, LS2 9JT, UK
| | - G Quintana-Lacaci
- Instituto de Ciencia de Materiales de Madrid, CSIC, C/Sor Juana Inés de la Cruz 3, E-28049 Cantoblanco, Spain
| | - R Szczerba
- Nicolaus Copernicus Astronomical Center, Rabianska 8, 87-100 Torun, Poland
| | - W Vlemmings
- Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439-92 Onsala, Sweden
| | - H van Winckel
- Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Heverlee, Belgium
| | - A Zijlstra
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, Manchester M13 9PL, UK
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Schmidt MR, He JH, Szczerba R, Bujarrabal V, Alcolea J, Cernicharo J, Decin L, Justtanont K, Teyssier D, Menten KM, Neufeld DA, Olofsson H, Planesas P, Marston AP, Sobolev AM, de Koter A, Schöier FL. Herschel/HIFI observations of the circumstellar ammonia lines in IRC+10216. Astron Astrophys 2016; 592:A131. [PMID: 28065983 PMCID: PMC5217166 DOI: 10.1051/0004-6361/201527290] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
CONTEXT A discrepancy exists between the abundance of ammonia (NH3) derived previously for the circumstellar envelope (CSE) of IRC+10216 from far-IR submillimeter rotational lines and that inferred from radio inversion or mid-infrared (MIR) absorption transitions. AIMS To address the discrepancy described above, new high-resolution far-infrared (FIR) observations of both ortho- and para-NH3 transitions toward IRC+10216 were obtained with Herschel, with the goal of determining the ammonia abundance and constraining the distribution of NH3 in the envelope of IRC+10216. METHODS We used the Heterodyne Instrument for the Far Infrared (HIFI) on board Herschel to observe all rotational transitions up to the J = 3 level (three ortho- and six para-NH3 lines). We conducted non-LTE multilevel radiative transfer modelling, including the effects of near-infrared (NIR) radiative pumping through vibrational transitions. The computed emission line profiles are compared with the new HIFI data, the radio inversion transitions, and the MIR absorption lines in the ν2 band taken from the literature. RESULTS We found that NIR pumping is of key importance for understanding the excitation of rotational levels of NH3. The derived NH3 abundances relative to molecular hydrogen were (2.8 ± 0.5) × 10-8 for ortho-NH3 and [Formula: see text] for para-NH3, consistent with an ortho/para ratio of 1. These values are in a rough agreement with abundances derived from the inversion transitions, as well as with the total abundance of NH3 inferred from the MIR absorption lines. To explain the observed rotational transitions, ammonia must be formed near to the central star at a radius close to the end of the wind acceleration region, but no larger than about 20 stellar radii (1σ confidence level).
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Affiliation(s)
- M. R. Schmidt
- N. Copernicus Astronomical Center, Rabiańska 8, 87-100 Toruń, Poland
| | - J. H. He
- Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming, Yunnan Province, China
| | - R. Szczerba
- N. Copernicus Astronomical Center, Rabiańska 8, 87-100 Toruń, Poland
| | - V. Bujarrabal
- Observatorio Astronómico Nacional. Ap 112, E-28803 Alcalá de Henares, Spain
| | - J. Alcolea
- Observatorio Astronómico Nacional (IGN), Alfonso XII N°3, E-28014 Madrid, Spain
| | - J. Cernicharo
- ICMM, CSIC, group of Molecular Astrophysics, C/Sor Juana Inés de la Cruz N3, 28049 Cantoblanco (Madrid), Spain
| | - L. Decin
- Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
- Sterrenkundig Instituut Anton Pannekoek, University of Amsterdam, Science Park 904, NL-1098 Amsterdam, The Netherlands
| | - K. Justtanont
- Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, S-439 92 Onsala, Sweden
| | - D. Teyssier
- European Space Astronomy Centre, ESA, P.O. Box 78, E-28691 Villanueva de la Cañada, Madrid, Spain
| | - K. M. Menten
- Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
| | | | - H. Olofsson
- Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, S-439 92 Onsala, Sweden
- Department of Astronomy, AlbaNova University Center, Stockholm University, SE–10691 Stockholm, Sweden
| | - P. Planesas
- Observatorio Astronómico Nacional (IGN), Alfonso XII N°3, E-28014 Madrid, Spain
| | - A. P. Marston
- European Space Astronomy Centre, ESA, P.O. Box 78, E-28691 Villanueva de la Cañada, Madrid, Spain
| | - A. M. Sobolev
- Ural Federal University, Astronomical Observatory, 620000 Ekaterinburg, Russian Federation
| | - A. de Koter
- Sterrenkundig Instituut Anton Pannekoek, University of Amsterdam, Science Park 904, NL-1098 Amsterdam, The Netherlands
| | - F. L. Schöier
- Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, S-439 92 Onsala, Sweden
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