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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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