Water cooling of shocks in protostellar outflows: Herschel-PACS map of L1157
| Autor: | Christophe Risacher, Per Bjerkeli, Doug Johnstone, Bengt Larsson, M. Benedettini, Javier R. Goicoechea, J. Santiago, R. Visser, Fabien Daniel, Carsten Dominik, S. Bruderer, Paola Caselli, O. A. Benz, C. Codella, J. Braine, J. A. Stern, L. Kirstensen, Gary J. Melnick, John E. Pearson, Michel Fich, N. Whyborn, Rafael Bachiller, P. J. Encrenaz, Steven D. Doty, Berengere Parise, David A. Neufeld, Michael Olberg, R. Shipman, M. Marseille, Jes K. Jørgensen, Michael J. Kaufman, Fabrice Herpin, Brunella Nisini, J. Desbat, Geoffrey A. Blake, C. McCoey, P. Saraceno, R. Plime, Dariusz C. Lis, G. J. Herczeg, E. A. Bergin, Michiel R. Hogerheijde, José Cernicharo, Susanne F. Wampfler, D. Teyssier, T. A. van Kempen, A. Baaudry, Teresa Giannini, Frank Helmich, Th. de Graaw, Bertrand Delforge, A. M. di Giorgio, Friedrich Wyrowski, Sylvain Bontemps, T. Jacq, Umut A. Yildiz, F. F. S. van der Tak, Asunción Fuente, Mario Tafalla, Serena Viti, René Liseau, W. A. Hatch, E. F. van Dishoeck, Rudolf Schieder, I. Peron |
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| Přispěvatelé: | Low Energy Astrophysics (API, FNWI), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), INAF - Osservatorio Astrofisico di Arcetri (OAA), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], SRON Netherlands Institute for Space Research (SRON), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, ESO, European Southern Observatory (ESO), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Radioastronomie (MPIFR), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), European Space Agency (ESA)-European Space Agency (ESA), ITA, USA, GBR, FRA, ESP, NLD, Astronomy, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), École normale supérieure - Paris (ENS-PSL), Universiteit Leiden, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA) |
| Předmět: |
ARRAY CAMERA
Astronomy FOS: Physical sciences DUST Astrophysics 01 natural sciences 0103 physical sciences PROGRAM Water cooling Solar and Stellar Astrophysics Total energy 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) QB Line (formation) Physics stars: formation Shock (fluid dynamics) Research Programm of Institute for Mathematics Astrophysics and Particle Physics [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] 010308 nuclear & particles physics SWAS ICE CLASS-0 SOURCES Astronomy and Astrophysics REGIONS [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] Astrophysics - Astrophysics of Galaxies ISM: molecules CHESS SPECTRAL SURVEY Stars ISM: jets and outflows Astrophysics - Solar and Stellar Astrophysics GAS 13. Climate action Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Excited state ComputingMethodologies_DOCUMENTANDTEXTPROCESSING Outflow EMISSION Intensity (heat transfer) Galaxy Astrophysics |
| Zdroj: | Scopus-Elsevier Astronomy & Astrophysics, 518. EDP Sciences Astronomy and Astrophysics-A&A Astronomy and Astrophysics-A&A, EDP Sciences, 2010, 518, pp.L120. ⟨10.1051/0004-6361/201014603⟩ Astronomy & astrophysics, 518:L120. EDP Sciences Astronomy & Astrophysics, 518, L120 Astronomy and Astrophysics-A&A, 2010, 518, pp.L120. ⟨10.1051/0004-6361/201014603⟩ Astronomy & Astrophysics, 518, pp. L120 |
| ISSN: | 0004-6361 |
| DOI: | 10.1051/0004-6361/201014603⟩ |
| Popis: | In the framework of the Water in Star-forming regions with Herschel (WISH) key program, maps in water lines of several outflows from young stars are being obtained, to study the water production in shocks and its role in the outflow cooling. This paper reports the first results of this program, presenting a PACS map of the o-H2O 179 um transition obtained toward the young outflow L1157. The 179 um map is compared with those of other important shock tracers, and with previous single-pointing ISO, SWAS, and Odin water observations of the same source that allow us to constrain the water abundance and total cooling. Strong H2O peaks are localized on both shocked emission knots and the central source position. The H2O 179 um emission is spatially correlated with emission from H2 rotational lines, excited in shocks leading to a significant enhancement of the water abundance. Water emission peaks along the outflow also correlate with peaks of other shock-produced molecular species, such as SiO and NH3. A strong H2O peak is also observed at the location of the proto-star, where none of the other molecules have significant emission. The absolute 179 um intensity and its intensity ratio to the H2O 557 GHz line previously observed with Odin/SWAS indicate that the water emission originates in warm compact clumps, spatially unresolved by PACS, having a H2O abundance of the order of 10^-4. This testifies that the clumps have been heated for a time long enough to allow the conversion of almost all the available gas-phase oxygen into water. The total water cooling is ~10^-1 Lo, about 40% of the cooling due to H2 and 23% of the total energy released in shocks along the L1157 outflow. Comment: Accepted for publication in Astronomy and Astrophysics (Herschel special issue) |
| Databáze: | OpenAIRE |
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