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Your search keyword '"Blue Sky Spectroscopy (BSS)"' showing total 3 results
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3 results on '"Blue Sky Spectroscopy (BSS)"'

1. PACS and SPIRE Spectroscopy of the Red Supergiant VY CMa

Author

Marvin L. Cohen, Helmut Feuchtgruber, Haley Louise Gomez, José Cernicharo, Bruce Swinyard, Pierre Royer, B. Vandenbussche, J. A. Yates, C. Waelkens, D. K. Witherick, Göran Olofsson, S. Regibo, F. Daniel, Edward Polehampton, Mikako Matsuura, Thomas Posch, Leen Decin, Peter Charles Hargrave, P. Imhof, M. J. Barlow, Rik Huygen, Roger Wesson, C. Jean, Rob Ivison, Martin Groenewegen, Robin Lombaert, Walter Kieran Gear, W. De Meester, Franz Kerschbaum, Pieter Degroote, Marcelino Agúndez, T. L. Lim, S. J. Leeks, Bruce Sibthorpe, Giorgio Savini, Joris Blommaert, Katrina Exter, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, University College of London [London] (UCL), Space Science and Technology Department, Rutherford Appleton Laboratory, Centro de Astrobiología, Consejo Superior de Investigaciones Científicas (CSIC)/Instituto Nacional de Técnica Aeroespacial (INTA) (CAB), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Molécules dans l'Univers, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Radio Astronomy Laboratory, University of California, Berkeley, Max-Planck-Institut für Extraterrestriche Physik (MPE), Cardiff University, Observatoire Royal de Belgique (ORB), Blue Sky Spectroscopy (BSS), UK Astronomy Technology Centre, Royal Observatory Edinburgh (UKATC), Institut für Astronomie, Universität Wien (IfA), and Department of Astronomy, Stockholm University, AlbaNova

Subjects
Physics, 010504 meteorology & atmospheric sciences, Wavelength range, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Luminosity, Spire, Supernova, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Isotopologue, Red supergiant, Spectroscopy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences
Abstract

International audience; With a luminosity >105 L&sun; and a mass-loss rate of ~2 × 10-4 M&sun; yr-1, the red supergiant VY CMa truly is a spectacular object. Because of its extreme evolutionary state, it could explode as supernova any time. Studying its circumstellar material, into which the supernova blast will run, provides interesting constraints on supernova explosions and on the rich chemistry taking place in such complex circumstellar envelopes. We have obtained spectroscopy of VY CMa over the full wavelength range offered by the PACS and SPIRE instruments of Herschel, i.e. 55-672 micron. The observations show the spectral fingerprints of more than 900 spectral lines, of which more than half belong to water. In total, we have identified 13 different molecules and some of their isotopologues. A first analysis shows that water is abundantly present, with an ortho-to-para ratio as low as ~1.3:1, and that chemical non-equilibrium processes determine the abundance fractions in the inner envelope.

Published
2010
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2. A study of the distant activity of comet C/2006 W3 (Christensen) using Herschel and ground-based radio telescopes

Author

L. M. Lara, Trevor Fulton, Miriam Rengel, M. R. Kidger, G. A. Blake, R. Moreno, Emmanuel Jehin, E. Lellouch, Michael Küppers, David A. Naylor, C. Waelkens, D. C. Lis, T. de Graauw, E. A. Bergin, Jean Manfroid, M. I. Blecka, T. Encrenaz, M. de Val-Borro, L. Decin, J. Crovisier, Slawomira Szutowicz, Christopher Jarchow, Bart Vandenbussche, José Cernicharo, J. A. D. L. Blommaert, Damien Hutsemekers, N. Thomas, Paul Hartogh, Dominique Bockelée-Morvan, Alexander S. Medvedev, Sarah Leeks, Marek Banaszkiewicz, Rudolf Schieder, P. J. Encrenaz, F. Bensch, B. M. Swinyard, N. Biver, Martin Emprechtinger, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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 Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Rutherford Appleton Laboratory, Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Institut d'Astrophysique, Géophysique et Océanographie, Université de Liège, European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Instituto de Astrofisica de Andalucia, CSIC (IAA), Space Research Centre, Polish Academy of Sciences (Wroclaw), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Blue Sky Spectroscopy (BSS), Herschel Science Center, ESAC/ESA, Astronomy Department, University of Michigan, Centro de Astrobiología, Consejo Superior de Investigaciones Científicas (CSIC)/Instituto Nacional de Técnica Aeroespacial (INTA) (CAB), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Instrumentation et télédétection, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Dynamique des milieux interstellaires et plasmas stellaires, SRON Netherlands Institute for Space Research, Department of Physics, University of Lethbridge, Lulea University of Technology (LTU), and University of Bern (UBERN)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Range (particle radiation), Continuum (design consultancy), Comet, FOS: Physical sciences, Astronomy and Astrophysics, Coma (optics), Astrophysics, Spectral line, Radio telescope, Spire, Space and Planetary Science, Spectral energy distribution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

Comet C/2006 W3 (Christensen) was observed in November 2009 at 3.3 AU from the Sun with Herschel. The PACS instrument acquired images of the dust coma in 70- and 160-micrometers filters, and spectra covering several H2O rotational lines. Spectra in the range 450-1550 GHz were acquired with SPIRE. The comet emission continuum from 70 to 672 micrometers was measured, but no lines were detected. The spectral energy distribution indicates thermal emission from large particles and provides a measure of the size distribution index and dust production rate. The upper limit to the water production rate is compared to the production rates of other species (CO, CH3OH, HCN, H2S, OH) measured with the IRAM 30-m and Nancay telescopes. The coma is found to be strongly enriched in species more volatile than water, in comparison to comets observed closer to the Sun. The CO to H2O production rate ratio exceeds 220%. The dust to gas production rate ratio is on the order of 1., Accepted for publication in Astronomy & Astrophysics (special issue on Herschel first results)

Published
2010
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3. Black hole accretion and star formation as drivers of gas excitation and chemistry in Markarian 231

Author

Axel Weiss, Fabian Walter, Marco Spaans, C. Kramer, S. D. Lord, Andrew I. Harris, Kalliopi Dasyra, V. Charmandaris, Thomas R. Greve, K. G. Isaak, Eduardo González-Alfonso, C. Vlahakis, Rolf Guesten, Howard A. Smith, Philippos Papadopoulos, L. Armus, A. Rykala, Frank P. Israel, Joseph M. Mazzarella, Yang Gao, Jesús Martín-Pintado, David A. Naylor, A. F. Loenen, Carsten Henkel, Aaron S. Evans, Rowin Meijerink, Luigi Spinoglio, P. van der Werf, Gordon J. Stacey, Susanne Aalto, E. M. Xilouris, Trevor Fulton, Sylvain Veilleux, Martina C. Wiedner, J. Fischer, D. B. Sanders, Giorgio Savini, Leiden Observatory, Cardiff University, Kapteyn Astronomical Institute, University of Groningen, Blue Sky Spectroscopy (BSS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Institut für Radioastronomie (MPIfR), Spitzer Science Center, California Institute of Technology (SSC), Remote Sensing Division, Naval Research laboratory, Naval Research Laboratory (NRL), Department of Astronomy, University of Maryland, University College of London [London] (UCL), Infrared Processing Analysis Center, California Institute of Technology (IPAC), Harvard-Smithsonian Center for Astrophysics, Departamente de Física, Universidad de Alcalá Henares, Department of Physics, University of Lethbridge, Department of Radio and Space Science, Chalmers University of Technology, Crete Center for Theoretical Physics, Department of Physics, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Astronomy Department, University of Virginia, Charlottesville, Purple Mountain Observatory, Instituto de Radio Astronomía Milimétrica (IRAM), Departamento de Astrofisica Molecular e Infrarroja-Instituto de Estructura de la Materia, Consejo Superior de Investigaciones Científica (CSIC), Rheinische Friedrich-Wilhelms-Universität Bonn, Institute for Astronomy, University of Hawaii, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Department of Astronomy, Cornell University, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Institute of Astronomy and Astrophysics, National Observatory of Athens, and Astronomy

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), GALAXY NUCLEI, Infrared, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, galaxies: starburst, LINES, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, DIAGNOSTICS, galaxies: individual: Mrk 231, infrared: galaxies, DENSE GAS, Astrophysics::Galaxy Astrophysics, Physics, Supermassive black hole, Star formation, Radiation field, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Galaxy, CO, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: nuclei, EMISSION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Excitation, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a full high resolution SPIRE FTS spectrum of the nearby ultraluminous infrared galaxy Mrk231. In total 25 lines are detected, including CO J=5-4 through J=13-12, 7 rotational lines of H2O, 3 of OH+ and one line each of H2O+, CH+, and HF. We find that the excitation of the CO rotational levels up to J=8 can be accounted for by UV radiation from star formation. However, the approximately flat luminosity distribution of the CO lines over the rotational ladder above J=8 requires the presence of a separate source of excitation for the highest CO lines. We explore X-ray heating by the accreting supermassive black hole in Mrk231 as a source of excitation for these lines, and find that it can reproduce the observed luminosities. We also consider a model with dense gas in a strong UV radiation field to produce the highest CO lines, but find that this model strongly overpredicts the hot dust mass in Mrk231. Our favoured model consists of a star forming disk of radius 560 pc, containing clumps of dense gas exposed to strong UV radiation, dominating the emission of CO lines up to J=8. X-rays from the accreting supermassive black hole in Mrk231 dominate the excitation and chemistry of the inner disk out to a radius of 160 pc, consistent with the X-ray power of the AGN in Mrk231. The extraordinary luminosity of the OH+ and H2O+ lines reveals the signature of X-ray driven excitation and chemistry in this region., 5 pages, 2 figures, accepted for publication in Astronomy & Astrophysics Special Issue on Herschel first results

Published
2010
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