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9 results on '"Sara Faggi"'

1. No evidence of phosphine in the atmosphere of Venus from independent analyses

Author

Bryan J. Butler, Paul Hartogh, Nicolas Biver, Colin Wilson, Statia Luszcz-Cook, Sara Faggi, Richard Cosentino, Geronimo L. Villanueva, Imke de Pater, Avi Mandell, Mark Gurwell, Ravi Kumar Kopparapu, Manuela Lippi, Conor A. Nixon, Katherine de Kleer, Vincent Kofman, Stefanie N. Milam, S. B. Charnley, Patrick G. J. Irwin, Ann Carine Vandaele, Alexander E. Thelen, Martin A. Cordiner, Arielle Moullet, Thomas Fauchez, Edward Molter, Giuliano Liuzzi, Giada Arney, NASA Goddard Space Flight Center (GSFC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Venus, Astrophysics, 01 natural sciences, Submillimeter Array, Spectral line, Atmosphere of Venus, Atmosphere, 0103 physical sciences, Radiative transfer, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, James Clerk Maxwell Telescope, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Line (formation), Earth and Planetary Astrophysics (astro-ph.EP), Physics, biology, Astronomy and Astrophysics, biology.organism_classification, 13. Climate action, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The detection of phosphine (PH3) in the atmosphere of Venus has been recently reported based on millimeter-wave radio observations (Greaves et al. 2020), and its re-analyses (Greaves et al. 2021a/b). In this Matters Arising we perform an independent reanalysis, identifying several issues in the interpretation of the spectroscopic data. As a result, we determine sensitive upper-limits for PH3 in Venus' atmosphere (>75 km, above the cloud decks) that are discrepant with the findings in G2020 and G2021a/b. The measurements target the fundamental first rotational transition of PH3 (J=1-0) at 266.944513 GHz, which was observed with the James Clerk Maxwell Telescope (JCMT) in June 2017 and with the Atacama Large Millimeter/submillimeter Array (ALMA) in March 2019. This line's center is near the SO2 (J=309,21-318,24) transition at 266.943329 GHz (only 1.3 km/s away from the PH3 line) which represents a potential source of contamination. The JCMT and ALMA data, as presented in G2020, are at spectral resolutions comparable to the frequency separation of the two lines. Moreover, the spectral features identified are several km/s in width, and therefore do not permit distinct spectroscopic separation of the candidate spectral lines of PH3 and SO2. We present the radiative transfer modelling we have performed and then discuss the ALMA and JCMT analyses in turn.

Published
2021
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2. Probing the Atmospheric Cl Isotopic Ratio on Mars: Implications for Planetary Evolution and Atmospheric Chemistry

Author

Frank Daerden, Bojan Ristic, Sara Faggi, Manish R. Patel, Shohei Aoki, Joanna Gurgurewicz, Ann Carine Vandaele, Giuliano Liuzzi, Sébastien Viscardy, Vincent Kofman, P. A. Tesson, Giancarlo Bellucci, Michael J. Mumma, Daniel Mège, Loïc Trompet, Ian Thomas, Elise W. Knutsen, Lori Neary, Justin Erwin, Geronimo L. Villanueva, Séverine Robert, Frédéric Schmidt, Michael D. Smith, Jose-Juan Lopez-Moreno, Matteo Crismani, NASA Goddard Space Flight Center (GSFC), Department of Physics [Washington], American University Washington D.C. (AU), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), California State University [San Bernardino] (CSUSB), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Géosciences Paris Saclay (GEOPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de la matière condensée et des nanosciences / Institute of Condensed Matter and Nanosciences (IMCN), Université Catholique de Louvain = Catholic University of Louvain (UCL), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Belgian Science Policy Office, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), UK Space Agency, National Aeronautics and Space Administration (US), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Agenzia Spaziale Italiana, and European Space Agency

Subjects
010504 meteorology & atmospheric sciences, Mars Exploration Program, Atmosphere of Mars, 010502 geochemistry & geophysics, 01 natural sciences, 7. Clean energy, Occultation, Trace gas, Astrobiology, law.invention, Orbiter, Geophysics, 13. Climate action, law, [SDU]Sciences of the Universe [physics], Atmospheric chemistry, Nadir, General Earth and Planetary Sciences, Environmental science, Formation and evolution of the Solar System, 0105 earth and related environmental sciences
Abstract

Following the recent detection of HCl in the atmosphere of Mars by ExoMars/Trace Gas Orbiter, we present here the first measurement of the 37Cl/35Cl isotopic ratio in the Martian atmosphere using a set of Nadir Occultation for MArs Discovery (NOMAD) observations. We determine an isotopic anomaly of −6 ± 78‰ compared to Earth standard, consistent with the −51‰–−1‰ measured on Mars’ surface by Curiosity. The measured isotopic ratio is also consistent with surface measurements, and suggests that Cl reservoirs may have undergone limited processing since formation in the Solar Nebula. The examination of possible sources and sinks of HCl shows only limited pathways to short-term efficient Cl fractionation and many plausible reservoirs of “light” Cl. © 2021. American Geophysical Union., ExoMars is a space mission of the European Space Agency (ESA) and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by the Spanish MICINN through its Plan Nacional and by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), as well as by UK Space Agency through grants ST/V002295/1, ST/V005332/1 and ST/S00145X/1 and Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709), and the CBK PAN team from the EXOMHYDR project, carried out within the TEAM program of the Foundation for Polish Science cofinanced by the European Union under the European Regional Development Fund (TEAM/2016-3/20). This work was supported by NASA's Mars Program Office under WBS 604796, "Participation in the TGO/NOMAD Investigation of Trace Gases on Mars" and by NASA's SEEC initiative under Grant Number NNX17AH81A, "Remote sensing of Planetary Atmospheres in the Solar System and Beyond." U.S. investigators were supported by the National Aeronautics and Space Administration. S. Viscardy acknowledges support from the Belgian Fonds de la Recherche Scientifique-FNRS under grant numbers 30442502 (ET_HOME) and Belgian Science Policy Office BrainBe MICROBE Projects. S. Aoki is "Charge de Recherches" at the F.R.S-FNRS. F. Schmidt acknowledges support from the "Institut National des Sciences de l'Univers" (INSU), the "Center National de la Recherche Scientifique" (CNRS) and "Center National d'Etudes Spatiales" (CNES) through the "Program National de Planetologie". S. Robert thanks BELSPO for the FED-tWIN funding (Prf-2019-077-RT-MOLEXO).

Published
2021
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3. Planetary Spectrum Generator: an accurate online radiative transfer suite for atmospheres, comets, small bodies and exoplanets

Author

Geronimo L. Villanueva, Sara Faggi, S. Protopapa, M. D. Smith, and Avi Mandell

Subjects
Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, 01 natural sciences, law.invention, Telescope, Orbiter, Planet, law, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Spectroscopy, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Radiation, Spacecraft, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Atomic and Molecular Physics, and Optics, Exoplanet, Asteroid, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Earth and Planetary Astrophysics
Abstract

We have developed an online radiative-transfer suite (https://psg.gsfc.nasa.gov) applicable to a broad range of planetary objects (e.g., planets, moons, comets, asteroids, TNOs, KBOs, exoplanets). The Planetary Spectrum Generator (PSG) can synthesize planetary spectra (atmospheres and surfaces) for a broad range of wavelengths (UV/Vis/near-IR/IR/far-IR/THz/sub-mm/Radio) from any observatory (e.g., JWST, ALMA, Keck, SOFIA), any orbiter (e.g., ExoMars, Juno), or any lander (e.g., MSL). This is achieved by combining several state-of-the-art radiative transfer models, spectroscopic databases and planetary databases (i.e., climatological and orbital). PSG has a 3D (three-dimensional) orbital calculator for most bodies in the solar system, and all confirmed exoplanets, while the radiative-transfer models can ingest billions of spectral signatures for hundreds of species from several spectroscopic repositories. It integrates the latest radiative-transfer and scattering methods in order to compute high resolution spectra via line-by-line calculations, and utilizes the efficient correlated-k method at moderate resolutions, while for computing cometary spectra, PSG handles non-LTE and LTE excitation processes. PSG includes a realistic noise calculator that integrates several telescope / instrument configurations (e.g., interferometry, coronagraphs) and detector technologies (e.g., CCD, heterodyne detectors, bolometers). Such an integration of advanced spectroscopic methods into an online tool can greatly serve the planetary community, ultimately enabling the retrieval of planetary parameters from remote sensing data, efficient mission planning strategies, interpretation of current and future planetary data, calibration of spectroscopic data, and development of new instrument/spacecraft concepts., Journal of Quantitative Spectroscopy and Radiative Transfer, submitted

Published
2018

4. Ground-based monitoring of comet 67P/Churyumov-Gerasimenko gas activity throughout the Rosetta mission

Author

Sara Faggi, Alan Fitzsimmons, Cyrielle Opitom, Emmanuel Jehin, Jean Manfroid, Michaël Gillon, G. P. Tozzi, and Colin Snodgrass

Subjects
Physics, 010504 meteorology & atmospheric sciences, Low resolution, Comet, Astronomy, Astronomy and Astrophysics, Coma (optics), Optically active, 01 natural sciences, 13. Climate action, Space and Planetary Science, Comet nucleus, 0103 physical sciences, TRAPPIST, 010303 astronomy & astrophysics, Spectrograph, individual: 67P/Churyumov-Gerasimenko [comets], 0105 earth and related environmental sciences
Abstract

Simultaneously to the ESA Rosetta mission, a world-wide ground-based campaign provided measurements of the large scale activity of comet 67P/Churyumov-Gerasimenko through measurement of optically active gas species and imaging of the overall dust coma. We present more than two years of observations performed with the FORS2 low resolution spectrograph at the VLT, TRAPPIST, and ACAM at the WHT. We focus on the evolution of the CN production, as a tracer of the comet activity. We find that it is asymmetric with respect to perihelion and different from that of the dust. The CN emission is detected for the first time at 1.34 au pre-perihelion and production rates then increase steeply to peak about two weeks after perihelion at (1.00±0.10) ×1025 molecules s−1, while the post-perihelion decrease is more shallow. The evolution of the comet activity is strongly influenced by seasonal effects, with enhanced CN production when the Southern hemisphere is illuminated.

Published
2017
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5. The 67P/Churyumov-Gerasimenko observation campaign in support of the Rosetta mission

Author

Benoit Carry, M. F. A'Hearn, Sebastien Besse, Michaël Gillon, M. J. Mumma, Galin Borisov, B. Rajkumar, Janet E. Drew, Olga Muñoz, Viktor Afanasiev, Tarik Zegmott, Lucas Paganini, D. Bodewits, Rita Schulz, Emily Kramer, Adam J. McKay, Diane H. Wooden, J. de León, Michael Schmidt, Geraint H. Jones, S. Haque, Andrew McNeill, Fernando Moreno, Sara Faggi, P. J. Gutiérrez, Jérémie Lasue, Aurélie Guilbert-Lepoutre, J. M. Sunshine, Javier Licandro, Zhong-Yi Lin, Pedro Lacerda, Philippe Rousselot, Jose Luis Ortiz, Nicolas Biver, Marco Micheli, J. J. López-Moreno, Matthew M. Knight, Jon Marchant, Detlef Koschny, Dominik R. G. Schleicher, F. Aceituno, Michael S. P. Kelley, Colin Snodgrass, G. P. Tozzi, Michael A. DiSanti, Karen J. Meech, Olivier Hainaut, Alfredo Sota, Niklas J. T. Edberg, Edith Hadamcik, Rene Duffard, Rosita Kokotanekova, Erika L. Gibb, Damien Hutsemekers, E. Ramos, Y. Ramanjooloo, A. Guijarro, Ulrich Hopp, Luisa Lara, Stephen C. Lowry, Tim Lister, Anita L. Cochran, V. Casanova, Pablo Santos-Sanz, J. Kleyna, R. Hedrosa, M. Pajuelo, A. K. Sen, Cyrielle Opitom, Emmanuel Jehin, A. Thompson, Alan Fitzsimmons, Geronimo L. Villanueva, E. J. W. de Mooij, Stefano Bagnulo, C. Ries, Boncho P. Bonev, O. Ivanova, Amy Mainzer, John K. Davies, Blair C. Conn, Anny Chantal Levasseur-Regourd, P. Nikolov, Auni Somero, Nikolai Kiselev, Lori M. Feaga, Maria Monguió, Francisco J. Pozuelos, A. Stinson, M. Delacruz, Björn Davidsson, Jacqueline V. Keane, M. Kluge, Dean C. Hines, Simon F. Green, Jean Manfroid, James Bauer, Silvia Protopapa, M. de Val-Borro, T. Pursimo, Xiaobin Wang, Cecilia Tubiana, Hermann Boehnhardt, Masafumi Yagi, I. Mohammed, Vera Rosenbush, F. Hoyo, Harry Lehto, G. Bergond, B. Yang, Méabh Hyland, Arno Riffeser, Hideaki Fujiwara, Erin L. Ryan, B. Zaprudin, School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] ( OU ), Department of Astronomy [College Park], University of Maryland [College Park], Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Special Astrophysical Observatory of the Russian Academy of Sciences ( SAO ), Russian Academy of Sciences [Moscow] ( RAS ), Armagh Observatory [Armagh], Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Centro Astronómico Hispano Alemán, European Space Astronomy Center ( ESAC ), European Space Agency ( ESA ), 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 Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Department of Physics [Washington], American University Washington D.C. ( AU ), Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), McDonald Observatory, University of Texas at Austin [Austin], Research School of Astronomy and Astrophysics [Canberra] ( RSAA ), Australian National University ( ANU ), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy ( AURA ), UK Astronomy Technology Centre ( UK ATC ), Science and Technology Facilities Council ( STFC ), Universidad de La Laguna ( ULL ), Instituto de Astrofisica de Canarias ( IAC ), Astrophysics Research Centre [Belfast] ( ARC ), Queen's University [Belfast] ( QUB ), Catholic University of America, Astrochemistry Laboratory [Greenbelt], NASA Goddard Space Flight Center ( GSFC ), Department of Astrophysical Sciences [Princeton], Princeton University, Institute for Astronomy [Honolulu], University of Hawaii at Manoa ( UHM ), School of Physics, Astronomy and Mathematics [Hatfield], University of Hertfordshire [Hatfield] ( UH ), Swedish Institute of Space Physics [Uppsala] ( IRF ), National Astronomical Observatory of Japan ( NAOJ ), Department of Physics and Astronomy [Columbia], University of Missouri-Columbia, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), European Southern Observatory ( ESO ), Department of Physics [Trinidad], The University of the West Indies, Space Telescope Science Institute ( STSci ), Ludwig-Maximilians University [Munich] ( LMU ), Astronomical Institute of the Slovak Academy of Sciences, Slovak Academy of Science [Bratislava] ( SAS ), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Centre for Planetary Sciences [UCL/Birkbeck] ( CPS ), Main Astronomical Observatory of NAS of Ukraine ( MAO ), National Academy of Sciences of Ukraine ( NASU ), Research and Scientific Support Department, ESTEC ( RSSD ), European Space Research and Technology Centre ( ESTEC ), European Space Agency ( ESA ) -European Space Agency ( ESA ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Tuorla Observatory, University of Turku, Institute of Astronomy [Taiwan] ( IANCU ), National Central University [Taiwan] ( NCU ), Las Cumbres Observatory ( LCO ), Centre for Astrophysics and Planetary Science [Canterbury] ( CAPS ), University of Kent [Canterbury], Astrophysics Research Institute [Liverpool] ( ARI ), Liverpool John Moores University ( LJMU ), ESA SSA-NEO Coordination Centre, Caribbean Institute of Astronomy ( CARINA ), Pontificia Universidad Católica del Perú ( PUCP ), Nordic Optical Telescope ( NOT ), SETI Institute, Lowell Observatory [Flagstaff], European Space Agency, Scientific Support Office, Assam University, INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Istituto Nazionale di Astrofisica ( INAF ), Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences [Beijing] ( CAS ), Yunnan Observatories, Chinese Academy of Sciences [Changchun Branch] ( CAS ), NASA Ames Research Center ( ARC ), Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), University of Maryland System-University of Maryland System, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Special Astrophysical Observatory of the Russian Academy of Sciences (SAO), Russian Academy of Sciences [Moscow] (RAS), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Centro Astronómico Hispano Alemán, Observatorio de Calar Alto (CAHA), European Space Astronomy Centre (ESAC), European Space Agency (ESA), 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 (MPS), Max-Planck-Gesellschaft, American University Washington D.C. (AU), Institute of Astronomy of the Bulgarian Academy of Sciences, Bulgarian Academy of Sciences (BAS), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Research School of Astronomy and Astrophysics [Canberra] (RSAA), Australian National University (ANU), Association of Universities for Research in Astronomy (AURA), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Universidad de La Laguna [Tenerife - SP] (ULL), Instituto de Astrofisica de Canarias (IAC), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), NASA Goddard Space Flight Center (GSFC), University of Hawai‘i [Mānoa] (UHM), University of Hertfordshire [Hatfield] (UH), Swedish Institute of Space Physics [Uppsala] (IRF), National Astronomical Observatory of Japan (NAOJ), Department of Physics and Astronomy [Columbia] (Mizzou Physics), University of Missouri [Columbia] (Mizzou), University of Missouri System-University of Missouri System, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Space Telescope Science Institute (STSci), Ludwig-Maximilians-Universität München (LMU), Slovak Academy of Science [Bratislava] (SAS), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Las Cumbres Observatory (LCO), Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Caribbean Institute of Astronomy (CARINA), Pontificia Universidad Católica del Perú (PUCP), Nordic Optical Telescope (NOT), ESA Scientific Support Office, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Chinese Academy of Sciences [Beijing] (CAS), Chinese Academy of Sciences [Changchun Branch] (CAS), NASA Ames Research Center (ARC), NASA-California Institute of Technology (CALTECH), Agence Spatiale Européenne = European Space Agency (ESA), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), 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), and Pontificia Universidad Católica del Perú = Pontifical Catholic University of Peru (PUCP)

Subjects
Future studies, History, 010504 meteorology & atmospheric sciences, General Mathematics, Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], General Physics and Astronomy, FOS: Physical sciences, Context (language use), 01 natural sciences, Astrobiology, Jupiter, 0103 physical sciences, 010303 astronomy & astrophysics, QC, 0105 earth and related environmental sciences, QB, Earth and Planetary Astrophysics (astro-ph.EP), comet 67P/Churyumov?Gerasimenko, Rosetta, solar system, observational astronomy, ta115, Spacecraft, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], General Engineering, Articles, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Early results, business, [ SDU.ASTR.SR ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a summary of the campaign of remote observations that supported the European Space Agency's Rosetta mission. Telescopes across the globe (and in space) followed comet 67P/Churyumov-Gerasimenko from before Rosetta's arrival until nearly the end of mission in September 2016. These provided essential data for mission planning, large-scale context information for the coma and tails beyond the spacecraft, and a way to directly compare 67P with other comets. The observations revealed 67P to be a relatively `well behaved' comet, typical of Jupiter family comets and with activity patterns that repeat from orbit-to-orbit. Comparison between this large collection of telescopic observations and the in situ results from Rosetta will allow us to better understand comet coma chemistry and structure. This work is just beginning as the mission ends -- in this paper we present a summary of the ground-based observations and early results, and point to many questions that will be addressed in future studies., Comment: Author prepared version; final published version available at journal. 22 pages

Published
2017
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6. The dust environment of comet 67P/Churyumov-Gerasimenko from Rosetta OSIRIS/GIADA and VLT observations in the 4.5 to 2.9 AU heliocentric distance range inbound

Author

M. F. A'Hearn, Sebastien Besse, Horst Uwe Keller, M. De Cecco, Alan Fitzsimmons, Emmanuel Jehin, Stefano Debei, Giampiero Naletto, Olivier Hainaut, R. Rodrigo, Francesco Marzari, Carsten Guettler, Géza Kovács, Dennis Bodewits, Olivier Groussin, J. Agarwal, Wing-Huen Ip, Laurent Jorda, Hans Rickman, Detlef Koschny, G. P. Tozzi, N. Oklay, L. M. Lara, V. Della Corte, Colin Snodgrass, F. Moreno, Nicolas Thomas, Jörg Knollenberg, Maurizio Pajola, P. Gutiérrez Marqués, Stubbe F. Hviid, G. Cremonese, Sara Faggi, J. J. Lopez Moreno, Francesca Ferri, B. J. R. Davidsson, E. Kuehrt, J. L. Bertaux, V. Da Deppo, Stefano Mottola, S. Fornasier, J.-R. Kramm, Holger Sierks, J. B. Vincent, Cecilia Tubiana, Monica Lazzarin, Ivano Bertini, P. L. Lamy, Marco Fulle, Cesare Barbieri, P. J. Gutierrez, Michael Kueppers, C. Opitom, M. A. Barucci, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), European Southern Observatory (ESO), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), International Space Science Institute [Bern] (ISSI), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Department of Physics and Astronomy [Uppsala], Uppsala University, Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Gauss Professor Akademie der Wissenschaften zu Göttingen, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), CNR Institute for Photonics and Nanotechnologies (IFN), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Department of Industrial Engineering [Padova], University of Trento [Trento], INAF - Osservatorio Astronomico di Trieste (OAT), DLR Institute of Planetary Research, German Aerospace Center (DLR), Institute of Space Science, National Central University, Operations Department (ESAC), European Space Astronomy Centre (ESAC), Department of Information Engineering [Padova] (DEI), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), INAF - Osservatorio Astrofisico di Arcetri (OAA), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, ITA, USA, GBR, FRA, DEU, Max-Planck-Institut für Sonnensystemforschung (MPS), Universita degli Studi di Padova, European Space Agency (ESA)-European Space Agency (ESA), Universität Bern [Bern], Consiglio Nazionale delle Ricerche [Roma] (CNR), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)

Subjects
67P/Churyumov-Gerasimenko, 010504 meteorology & atmospheric sciences, Monte Carlo method, Comet, Data analysis, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Coma (optics), Astrophysics, 01 natural sciences, Photometry, Methods: data analysis, 0103 physical sciences, Range (statistics), Comets, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Comets: individual: 67P/Churyumov-Gerasimenko, Physics, comets: individual: 67P/Churyumov-Gerasimenko / methods: data analysis / techniques: photometric, Very Large Telescope, Spacecraft, biology, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Mass ratio, biology.organism_classification, 13. Climate action, Space and Planetary Science, astro-ph.EP, Techniques: photometric, Osiris, business, Astrophysics - Earth and Planetary Astrophysics
Abstract

The ESA Rosetta spacecraft, currently orbiting around comet 67P, has already provided in situ measurements of the dust grain properties from several instruments, particularly OSIRIS and GIADA. We propose adding value to those measurements by combining them with ground-based observations of the dust tail to monitor the overall, time-dependent dust-production rate and size distribution. To constrain the dust grain properties, we take Rosetta OSIRIS and GIADA results into account, and combine OSIRIS data during the approach phase (from late April to early June 2014) with a large data set of ground-based images that were acquired with the ESO Very Large Telescope (VLT) from February to November 2014. A Monte Carlo dust tail code has been applied to retrieve the dust parameters. Key properties of the grains (density, velocity, and size distribution) were obtained from Rosetta observations: these parameters were used as input of the code to considerably reduce the number of free parameters. In this way, the overall dust mass-loss rate and its dependence on the heliocentric distance could be obtained accurately. The dust parameters derived from the inner coma measurements by OSIRIS and GIADA and from distant imaging using VLT data are consistent, except for the power index of the size-distribution function, which is $\alpha$=--3, instead of $\alpha$=--2, for grains smaller than 1 mm. This is possibly linked to the presence of fluffy aggregates in the coma. The onset of cometary activity occurs at approximately 4.3 au, with a dust production rate of 0.5 kg/s, increasing up to 15 kg/s at 2.9 au. This implies a dust-to-gas mass ratio varying between 3.8 and 6.5 for the best-fit model when combined with water-production rates from the MIRO experiment., Comment: Accepted by Astronomy and Astrophysics (January 17th, 2016)

Published
2016
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7. Detailed Analysis of Near-IR Water (H2O) Emission in Comet C/2014 Q2 (Lovejoy) with the GIANO/TNG Spectrograph

Author

M. J. Mumma, F. Massi, G. P. Tozzi, Sara Faggi, Geronimo Villanueva, John Robert Brucato, A. Tozzi, Nicoletta Sanna, Ernesto Oliva, ITA, and USA

Subjects
Physics, 010504 meteorology & atmospheric sciences, Comet, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Water production, Spectral line, law.invention, Telescope, Resonance fluorescence, Space and Planetary Science, law, 0103 physical sciences, Critical test, 010303 astronomy & astrophysics, Spectrograph, 0105 earth and related environmental sciences, Line (formation)
Abstract

We observed the Oort cloud comet C/2014 Q2 (Lovejoy) on 2015 January 31 and February 1 and 2 at a heliocentric distance of 1.3 au and geocentric distance of 0.8 au during its approach to the Sun. Comet Lovejoy was observed with GIANO, the near-infrared high-resolution spectrograph mounted at the Nasmyth-A focus of the TNG (Telescopio Nazionale Galileo) telescope in La Palma, Canary Islands, Spain. We detected strong emissions of radical CN and water, along with many emission features of unidentified origin, across the 1-2.5 μm region. Spectral lines from eight ro-vibrational bands of H2O were detected, six of them for the first time. We quantified the water production rate [Q(H2O), (3.11 ± 0.14) × 1029 s-1] by comparing the calibrated line fluxes with the Goddard full non-resonance cascade fluorescence model for H2O. The production rates of ortho-water [Q(H2O)ORTHO, (2.33 ± 0.11) × 1029 s-1] and para-water [Q(H2O)PARA, (0.87 ± 0.21) × 1029 s-1] provide a measure of the ortho-to-para ratio (2.70 ± 0.76)). The confidence limits are not small enough to provide a critical test of the nuclear spin temperature.

Published
2016

8. The Volatile Composition of Comet C/2017 E4 (Lovejoy) before its Disruption, as Revealed by High-resolution Infrared Spectroscopy with iSHELL at the NASA/IRTF

Author

Geronimo Villanueva, Lucas Paganini, M. J. Mumma, and Sara Faggi

Subjects
Physics, 010504 meteorology & atmospheric sciences, Infrared, Comet, Analytical chemistry, Infrared spectroscopy, Astronomy and Astrophysics, Planetary system, 01 natural sciences, Spectral line, Space and Planetary Science, Abundance (ecology), 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Spectrograph, 0105 earth and related environmental sciences
Abstract

In 2017 April, we acquired comprehensive high-resolution spectra of newly discovered comet C/2017 E4 (Lovejoy) as it approached perihelion, and before its disintegration. We detected many cometary emission lines in the range (2.8-5.3) μm, in four customized instrument settings (L1-c, L3, Lp1-c, and M1) of iSHELL-the new near-IR high-resolution immersion echelle spectrograph at NASA/IRTF (Maunakea, Hawaii). We identified 12 molecular species: nine primary volatiles (H2O, HCN, NH3, CO, C2H2, C2H6, CH4, CH3OH, H2CO) and three product species (CN, NH2, OH). We detected 85 H2O emission lines from 12 water vibrational bands across L1-c and M1 settings. The many detected water emission lines enabled retrieval of accurate measures for ortho- and para-H2O independently, thereby reducing systematic uncertainty in the derived ortho-para ratio and nuclear spin temperature. Excitation analyses and emission profile analyses were performed for all species, and molecular abundance ratios relative to water are compared with values found for other Oort Cloud comets in our infrared database. Abundance ratios are consistent for most species, with the exception of underabundant methanol and overabundant ammonia in E4.

Published
2018
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9. Distant activity of 67P/Churyumov-Gerasimenko in 2014: Ground-based results during the Rosetta pre-landing phase

Author

Matthew M. Knight, Cyrielle Opitom, Emmanuel Jehin, Sara Faggi, Tim Lister, Gian Paolo Tozzi, Olivier Hainaut, Blair C. Conn, Bin Yang, Jean Manfroid, Alan Fitzsimmons, Aurélie Guilbert-Lepoutre, Agata Rozek, D. M. Bramich, Cecilia Tubiana, Colin Snodgrass, Stephen C. Lowry, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Brightness, 010504 meteorology & atmospheric sciences, Comet, Phase (waves), FOS: Physical sciences, comets, individual, 67P/Churyumov-Gerasimenko, Astronomy, Astronomy and Astrophysics, Context (language use), Coma (optics), 01 natural sciences, Photometry (optics), [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, 0103 physical sciences, Orbit (dynamics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

As the ESA Rosetta mission approached, orbited, and sent a lander to comet 67P/Churyumov-Gerasimenko in 2014, a large campaign of ground-based observations also followed the comet. We constrain the total activity level of the comet by photometry and spectroscopy to place Rosetta results in context and to understand the large-scale structure of the comet's coma pre-perihelion. We performed observations using a number of telescopes, but concentrate on results from the 8m VLT and Gemini South telescopes in Chile. We use R-band imaging to measure the dust coma contribution to the comet's brightness and UV-visible spectroscopy to search for gas emissions, primarily using VLT/FORS. In addition we imaged the comet in near-infrared wavelengths (JHK) in late 2014 with Gemini-S/Flamingos 2. We find that the comet was already active in early 2014 at heliocentric distances beyond 4 au. The evolution of the total activity (measured by dust) followed previous predictions. No gas emissions were detected despite sensitive searches. The comet maintains a similar level of activity from orbit to orbit, and is in that sense predictable, meaning that Rosetta results correspond to typical behaviour for this comet. The gas production (for CN at least) is highly asymmetric with respect to perihelion, as our upper limits are below the measured production rates for similar distances post-perihelion in previous orbits., 12 pages, accepted in A&A

Published
2016
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