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1. Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA

Author: Cordiner, M. A., Roth, N. X., Milam, S. N., Villanueva, G., Bockelee-Morvan, D., Remijan, A. J., Charnley, S. B., Biver, N., Lis, D. C., Qi, C., Bonev, B., Crovisier, J., and Boissier, J.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Astrophysics - Earth and Planetary Astrophysics
Abstract: Gas-phase molecules in cometary atmospheres (comae) originate primarily from (1) outgassing by the nucleus, (2) sublimation of icy grains in the near-nucleus coma, and (3) coma (photo-)chemical processes. However, the majority of cometary gases observed at radio wavelengths have yet to be mapped, so their production/release mechanisms remain uncertain. Here we present observations of six molecular species towards comet 46P/Wirtanen, obtained using the Atacama Large Millimeter/submillimeter Array (ALMA) during the comet's unusually close (~0.1 au) approach to Earth in December 2018. Interferometric maps of HCN, CH3OH, CH3CN, H2CO, CS and HNC were obtained at an unprecedented sky-projected spatial resolution of up to 25 km, enabling the nucleus and coma sources of these molecules to be accurately quantified. The HCN, CH3OH and CH3CN spatial distributions are consistent with production by direct outgassing from (or very near to) the nucleus, with a significant proportion of the observed CH3OH originating from sublimation of icy grains in the near-nucleus coma (at a scale-length $L_p=36\pm7$ km). On the other hand, H2CO, CS and HNC originate primarily from distributed coma sources (with $L_p$ values in the range 550-16,000 km), the identities of which remain to be established. The HCN, CH3OH and HNC abundances in 46P are consistent with the average values previously observed in comets, whereas the H2CO, CH3CN and CS abundances are relatively low., Comment: Accepted for publication in the Astrophysical Journal on 2023-06-17
Published: 2023
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2. Water, hydrogen cyanide, carbon monoxide, and dust production from distant comet 29P/Schwassmann-Wachmann 1

Author: Bockelée-Morvan, D., Biver, N., Schambeau, C. A., Crovisier, J., Opitom, C., Borro, M. de Val, Lellouch, E., Hartogh, P., Vandenbussche, B., Jehin, E., Kidger, M., Küppers, M., Lis, D. C., Moreno, R., Szutowicz, S., and Zakharov, V.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, planetary systems [Radio lines], astro-ph.EP, general [Comets], FOS: Physical sciences, Astronomy and Astrophysics, planetary systems [Infrared], individual: 29P/Schwassmann-Wachmann 1 [Comets], Astrophysics - Earth and Planetary Astrophysics
Abstract: 29P/Schwassmann-Wachmann 1 is a distant Centaur/comet, showing persistent CO-driven activity and frequent outbursts. We used the Herschel space observatory in 2010, 2011, and 2013 to observe H$_2$O and NH$_3$ and to image the dust coma. Observations with the IRAM 30 m were undertaken in 2007, 2010, 2011, and 2021 to monitor the CO production rate and to search for HCN. Modeling was performed to constrain the size of the sublimating icy grains and to derive the dust production rate. HCN is detected for the first time in comet 29P (at 5$\sigma$ in the line area). H$_2$O is detected as well, but not NH$_3$. H$_2$O and HCN line shapes differ strongly from the CO line shape, indicating that these two species are released from icy grains. CO production rates are in the range (2.9-5.6) $\times$ 10$^{28}$ s$^{-1}$ (1400--2600 kg s$^{-1}$). A correlation between the CO production rate and coma brightness is observed, as is a correlation between CO and H$_2$O production. The correlation obtained between the excess of CO production and excess of dust brightness with respect to the quiescent state is similar to that established for the continuous activity of comet Hale-Bopp. The measured $Q$(H$_2$O)/$Q$(CO) and $Q$(HCN)/$Q$(CO) production rate ratios are 10.0 $\pm$ 1.5 % and 0.12 $\pm$ 0.03 %, respectively, averaging the April-May 2010 measurements ($Q$(H$_2$O) = (4.1 $\pm$ 0.6) $\times$ 10$^{27}$ s$^{-1}$, $Q$(HCN) = (4.8 $\pm$ 1.1) $\times$ 10$^{25}$ s$^{-1}$). We derive three independent and similar values of the effective radius of the nucleus, $\sim$ 31 $\pm$ 3 km. The inferred dust mass-loss rates during quiescent phases are in the range 30-120 kg s$^{-1}$, indicating a dust-to-gas mass ratio $, Comment: 28 pages, 15 figures, A&A in press
Published: 2022
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3. Solar system science with the Orbiting Astronomical Satellite Investigating Stellar Systems (OASIS) observatory

Author: Anderson, C., Biver, N., Bjoraker, G., Cavalié, T., Chin, G., DiSanti, M., Hartogh, P., Tielens, A., and Walker, C.
Subjects: Space and Planetary Science, THz spectroscopy, Comets, Solar system science, Active icy moons, Astronomy and Astrophysics, Flight mission concept, Heterodyne spectral resolution, Planetary atmospheres
Abstract: The overarching theme of the Orbiting Astronomical Satellite for Investigating Stellar Systems (OASIS), an Astrophysics MIDEX-class mission concept, is Following water from galaxies, through protostellar systems, to Earth’s oceans. The OASIS science objectives address fundamental questions raised in “Pathways to Discovery in Astronomy and Astrophysics for the 2020s (National Academies of Sciences and Medicine, Pathways to Discovery in Astronomy and Astrophysics for the 2020s, 2021, https://doi.org/10.17226/26141, https://www.nap.edu/catalog/26141/pathways-to-discovery-in-astronomy-and-astrophysics-for-the-2020s)” and in “Enduring Quests and Daring Visions” (Kouveliotou et al. in Enduring quests-daring visions (NASA astrophysics in the next three decades), 2014, arXiv:1401.3741), in the areas of: 1) the Interstellar Medium and Planet Formation, 2) Exoplanets, Astrobiology, and the Solar System, and 3) Galaxies. The OASIS science objectives require space-borne observations of galaxies, molecular clouds, protoplanetary disks, and solar system objects utilizing a telescope with a collecting area that is only achievable by large apertures coupled with cryogenic heterodyne receivers. OASIS will deploy an innovative 14-meter inflatable reflector that enables >16× the sensitivity and >4× the angular resolution of Herschel, and complements the short wavelength capabilities of James Webb Space Telescope. The OASIS state-of-the-art cryogenic heterodyne receivers will enable high spectral resolution (resolving power $>10^{6}$ > 10 6 ) observations at terahertz (THz) frequencies. These frequencies encompass far-IR transitions of water and its isotopologues, HD, and other molecular species, from 660 to 63 μm that are otherwise obscured by Earth’s atmosphere. From observations of the ground state HD line, OASIS will directly measure gas mass in a wide variety of astrophysical objects. Over its one-year baseline mission, OASIS will find water sources as close as the Moon, to galaxies ∼4 billion light years away. This paper reviews the solar system science achievable and planned with OASIS.
Published: 2022

4. Orbiting Astronomical Satellite for Investigating Stellar Systems (OASIS): following the water trail from the interstellar medium to oceans

Author: Walker, C.K., Chin, G., Aalto, S., Anderson, C.M., Arenberg, J.W., Battersby, C., Bergin, E., Bergner, J., Biver, N., Bjoraker, G.L., Carr, J., Cavalié, T., De Beck, E., DiSanti, M.A., Hartogh, P., Hunt, L.K., Kim, D., Takashima, Y., Kulesa, C., Leisawitz, D., Najita, J., Rigopoulou, D., Schwarz, K., Shirly, Y., Stark, A.A., Tielens, X., Viti, S., Wilner, D., Wollack, E., Young, E., Hull, T.B., Hallibert, P., Keller, F., ASP 2021, 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 de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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 de Paris (UP), University of Arizona, NASA Goddard Space Flight Center (GSFC), Northrop Grumman Space Technology (Northrop Grumman Space Technology), Chemistry Technology Department, Tony B. Hull, Daewook Kim, Pascal Hallibert, and Fanny Keller
Subjects: HD, Solar System, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, moons, far-infrared spectroscopy, 7. Clean energy, 01 natural sciences, 010309 optics, proto-planetary disks, Spitzer Space Telescope, planets, Planet, 0103 physical sciences, galaxies, comets, Spectral resolution, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], James Webb Space Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, heterodyne spectroscopy, Astronomy, Water, 021001 nanoscience & nanotechnology, terahertz astronomy, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Interstellar medium, submillimeter spectroscopy, 13. Climate action, Satellite, Astrophysics::Earth and Planetary Astrophysics, 0210 nano-technology
Abstract: International audience; Orbiting Astronomical Satellite for Investigating Stellar Systems (OASIS) is a space-based, MIDEX-class mission concept that employs a 17-meter diameter inflatable aperture with cryogenic heterodyne receivers, enabling high sensitivity and high spectral resolution (resolving power ≥106) observations at terahertz frequencies. OASIS science is targeting submillimeter and far-infrared transitions of H2O and its isotopologues, as well as deuterated molecular hydrogen (HD) and other molecular species from 660 to 80 μm, which are inaccessible to ground-based telescopes due to the opacity of Earth’s atmosphere. OASIS will have
Published: 2021
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5. Deuterium in cometary water

Author: Bockelée-Morvan, Dominique, Lis, D.C., and Biver, N.
Abstract: Ground-based imaging spectroscopy of terrestrial planets is a powerful tool for monitoring the spatio-temporal variability of minor atmospheric species. Instantaneous mapping of planetary disks allows us to study transient phenomena and variations with local time and longitude, which are not easily observed by an orbiter in space. We have been using the TEXES (Texas Echelon Cross Echelle Spectrograph) imaging spectrometer at the NASA Infrared Telescope Facility (Maunakea Observatory, Hawaii) for two long-term observing campaigns: (1) monitoring of H2O2 and HDO on Mars (since 2001) and (2) monitoring of SO2 and HDO on Venus (since 2012). In both cases, HDO is used as a proxy of H2O. The Mars data have allowed us to study the seasonal variations of H2O2 on Mars (Encrenaz et al. A&A 627, A60, 2019). The Venus data have revealed that SO2 and H2O behave very differently at the cloudtop of Venus. Whereas H2O maps are globally uniform, SO2 shows strong spatial and short-term variations, with a time scale of a few hours (Encrenaz et al. A&A 623, A70, 2019 & EPSC 2019). These campaigns are performed in support to Mars Express and TGO on Mars, and Venus Express and Akatsuki on Venus.
Published: 2021
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6. 18-year long monitoring of the evolution of H2O vapor in the stratosphere of Jupiter with the Odin space telescope

Author: Benmahi, B., Cavalié, T., Dobrijevic, M., Biver, N., Bermudez-Diaz, K., Sandqvist, Aa., Lellouch, E., Moreno, R., Fouchet, T., Hue, V., Hartogh, P., Billebaud, F., Lecacheux, A., Hjalmarson, Å., Frisk, U., Olberg, M., and Team, andThe Odin
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Comet Shoemaker-Levy 9 impacted Jupiter in July 1994, leaving its stratosphere with several new species, among them water vapor (H2O). With the aid of a photochemical model H2O can be used as a dynamical tracer in the jovian stratosphere. In this paper, we aim at constraining vertical eddy diffusion (Kzz) at the levels where H2O resides. We monitored the H2O disk-averaged emission at 556.936 GHz with the Odin space telescope between 2002 and 2019, covering nearly two decades. We analyzed the data with a combination of 1D photochemical and radiative transfer models to constrain vertical eddy diffusion in the stratosphere of Jupiter. The Odin observations show us that the emission of H2O has an almost linear decrease of about 40% between 2002 and 2019.We can only reproduce our time series if we increase the magnitude of Kzz in the pressure range where H2O diffuses downward from 2002 to 2019, i.e. from ~0.2 mbar to ~5 mbar. However, this modified Kzz is incompatible with hydrocarbon observations. We find that, even if allowance is made for the initially large abundances of H2O and CO at the impact latitudes, the photochemical conversion of H2O to CO2 is not sufficient to explain the progressive decline of the H2O line emission, suggestive of additional loss mechanisms. The Kzz we derived from the Odin observations of H2O can only be viewed as an upper limit in the ~0.2 mbar to ~5 mbar pressure range. The incompatibility between the interpretations made from H2O and hydrocarbon observations probably results from 1D modeling limitations. Meridional variability of H2O, most probably at auroral latitudes, would need to be assessed and compared with that of hydrocarbons to quantify the role of auroral chemistry in the temporal evolution of the H2O abundance since the SL9 impacts. Modeling the temporal evolution of SL9 species with a 2D model would be the next natural step., Comment: 9 pages, 8 figures, accepted in Astronomy and Astrophysics
Published: 2020
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7. La première comète extrasolaire observée de l'histoire -2I/2019 Q4 (Borisov)

Author: Biver, N. and Biver, Nicolas
Subjects: [SDU] Sciences of the Universe [physics], [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract: Découverte de la première comète interstellaire : Le 30 aout 2019, l'astronome amateur Gennady Borisov découvre un nouvel objet de nature cométaire (dans le crépuscule du matin, avec son télescope de 65cm à F/D 1.5 (observatoire MARGO, en Crimée). C'est sa 8e découverte cométaire depuis 2013, même si ses précédentes ont peu fait parler d'elles, souvent découvertes vers la magnitude 17 et culminant au mieux vers la magnitude m 1 =10. D'abord temporairement nommé gb00234, il faudra attendre 12j avant que la découverte soit annoncée officiellement (circulaire MPEC 2019-R106 du 11 Septembre), car le calcul de son orbite a vite posé quelques soucis quand les écarts à une orbite parabolique (e=1.0), utilisée par défaut pour une première détermination d'orbite, sont devenus trop important. Il a donc fallu attendre de se rendre à l'évidence que l'excentricité était supérieure à 3 pour publier la première orbite ! Les conditions d'observations s'améliorant, l'intérêt de cet objet potentiellement extrasolaire grandissant, les mesures astrométriques arrivent en nombre et tous les 3j l'orbite se précise. De plus de 10% d'incertitude sur l'excentricité de l'orbite (e=3.2 à 3.7), on est désormais à e=3.33±0.02 après 4 semaines d'observations (> 500 observations, MPEC 2019-S120). Désormais l'origine extérieure au système solaire de cette comète (Figure 1) ne fait plus aucun doute. Après 3 semaines, la comète a été officiellement numéroté 2I/Borisov le 24 septembre par l'Union Astronomique Internationale [1], suite à la règle définie après la découverte de 1I/'Oumuamua (2017 U1), premier objet venant de l'extérieur du système solaire-mais dont l'aspect est resté purement astéroïdal durant ses 2 mois de visibilité fin 2017. Probabilité de voir une comète extrasolaire : Cette question s'est posée depuis longtemps. A la base (Glynn 1989), l'idée d'origine [2] est que depuis la découverte du Nuage de Oort (Oort 1950) on a estimé que ~45% des comètes arrivant du Nuage de Oort pour la première fois près du Soleil sont éjectées définitivement vers l'espace
Published: 2019

8. Masterreise der ETH-Geomatik-Absolventen

Author: Hübscher, F. and Biver, N.
Published: 2018
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9. Evolution of water production of 67P/Churyumov-Gerasimenko

Author: Hansen, Kenneth C., Altwegg, K., Berthelier, J. -J., Bieler, A., Biver, N., Bockelee-Morvan, D., Calmonte, U., Capaccioni, F., Combi, M. R., De Keyser, J., Fiethe, B., Fougere, N., Fuselier, S. A., Gasc, S., Gombosi, T. I., Huang, Z., Le Roy, L., Lee, S., Nilsson, H., Rubin, Martin, Shou, Y., Snodgrass, C., Tenishev, V., Tzou, C.-Y., Wedlund, C. Simon, Toth, Gabor, ROSINA Team, University of Michigan, Ann Arbor, University of Bern, Observatoire de Paris, Istituto Nazionale Astrofisica - Italy, Royal Belgian Institute for Space Aeronomy, TU Braunschweig, University of Texas at San Antonio, Jet Propulsion Laboratory, Swedish Institute of Space Physics, Open University, Department of Radio Science and Engineering, Aalto-yliopisto, and Aalto University
Subjects: individual: 67P/CG [comets], SIMULATION, DUST, CO2, PREPERIHELION, ROSINA, PERIHELION, miscellaneous [methods], ATMOSPHERE, ROSETTA ORBITER, TARGET COMET 67P/CHURYUMOV-GERASIMENKO, general [comets], HALE-BOPP
Abstract: We examine the evolution of the water production of comet 67P/Churyumov-Gerasimenko during the Rosetta mission (2014 June-2016 May) based on in situ and remote sensing measurements made by Rosetta instruments, Earth-based telescopes and through the development of an empirical coma model. The derivation of the empirical model is described and the model is then applied to detrend spacecraft position effects from the Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) data. The inter-comparison of the instrument data sets shows a high level of consistency and provides insights into the water and dust production. We examine different phases of the orbit, including the early mission (beyond 3.5 au) where the ROSINA water production does not show the expected increase with decreasing heliocentric distance. A second important phase is the period around the inbound equinox, where the peak water production makes a dramatic transition from northern to southern latitudes. During this transition, the waterdistribution is complex, but is driven by rotation and active areas in the north and south. Finally, we consider the perihelion period, where there may be evidence of time dependence in the water production rate. The peak water production, as measured by ROSINA, occurs 18-22 d after perihelion at 3.5 +/- 0.5 x 10(28) water molecules s(-1). We show that the water production is highly correlated with ground-based dust measurements, possibly indicating that several dust parameters are constant during the observed period. Using estimates of the dust/gas ratio, we use our measured water production rate to calculate a uniform surface loss of 2-4 m during the current perihelion passage.
Published: 2016

10. Isotopic ratios of H, C, N, O, and S in comets C/2012 F6 (Lemmon) and C/2014 Q2 (Lovejoy)

Author: Biver, N., Moreno, R., Bockelée-Morvan, D., Sandqvist, Aa., Colom, P., Crovisier, J., Lis, D. C., Boissier, J., Debout, V., Paubert, G., Milam, S., Hjalmarson, A., Lundin, S., Karlsson, T., Battelino, M., Frisk, U., Murtagh, D., team, the Odin, 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Swedish Space Corporation (SSC), Department of Radio and Space Science [Göteborg], Biologie et écologie tropicale et méditerranéenne [2007-2010] (BETM), Université de Perpignan Via Domitia (UPVD)-École pratique des hautes études (EPHE), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Solar System, 010504 meteorology & atmospheric sciences, Comet, FOS: Physical sciences, Astrophysics, 01 natural sciences, chemistry.chemical_compound, 0103 physical sciences, Isotopologue, 010303 astronomy & astrophysics, Chemical composition, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Line (formation), Physics, Heavy water, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Isotope, Astronomy and Astrophysics, Deuterium, chemistry, 13. Climate action, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: The apparition of bright comets C/2012 F6 (Lemmon) and C/2014 Q2 (Lovejoy) in March-April 2013 and January 2015, combined with the improved observational capabilities of submillimeter facilities, offered an opportunity to carry out sensitive compositional and isotopic studies of the volatiles in their coma. We observed comet Lovejoy with the IRAM 30m telescope between 13 and 26 January 2015, and with the Odin submillimeter space observatory on 29 January - 3 February 2015. We detected 22 molecules and several isotopologues. The H$_2^{16}$O and H$_2^{18}$O production rates measured with Odin follow a periodic pattern with a period of 0.94 days and an amplitude of ~25%. The inferred isotope ratios in comet Lovejoy are $^{16}$O/$^{18}$O = 499 $\pm$ 24 and D/H = 1.4 $\pm$ 0.4 $\times 10^{-4}$ in water, $^{32}$S/$^{34}$S = 24.7 $\pm$ 3.5 in CS, all compatible with terrestrial values. The ratio $^{12}$C/$^{13}$C = 109 $\pm$ 14 in HCN is marginally higher than terrestrial and $^{14}$N/$^{15}$N = 145 $\pm$ 12 in HCN is half the Earth ratio. Several upper limits for D/H or 12C/13C in other molecules are reported. From our observation of HDO in comet C/2014 Q2 (Lovejoy), we report the first D/H ratio in an Oort Cloud comet that is not larger than the terrestrial value. On the other hand, the observation of the same HDO line in the other Oort-cloud comet, C/2012 F6 (Lemmon), suggests a D/H value four times higher. Given the previous measurements of D/H in cometary water, this illustrates that a diversity in the D/H ratio and in the chemical composition, is present even within the same dynamical group of comets, suggesting that current dynamical groups contain comets formed at very different places or times in the early solar system., Accepted for publication in Astronomy and Astrophysics
Published: 2016
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11. Measuring the Distribution and Excitation of Cometary CH3OH Using ALMA

Author: Cordiner, M. A., Charnley, S. B., Mumma, M. J., Bockel��e-Morvan, D., Biver, N., Villanueva, G., Paganini, L., Milam, S. N., Remijan, A. J., Lis, D. C., Crovisier, J., Boissier, J., Kuan, Y. -J., and Coulson, I. M.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Atacama Large Millimeter/submillimeter Array (ALMA) was used to obtain measurements of spatially and spectrally resolved CH$_3$OH emission from comet C/2012 K1 (PanSTARRS) on 28-29 June 2014. Detection of 12-14 emission lines of CH$_3$OH on each day permitted the derivation of spatially-resolved rotational temperature profiles (averaged along the line of sight), for the innermost 5000 km of the coma. On each day, the CH$_3$OH distribution was centrally peaked and approximately consistent with spherically symmetric, uniform outflow. The azimuthally-averaged CH$_3$OH rotational temperature ($T_{rot}$) as a function of sky-projected nucleocentric distance ($\rho$), fell by about 40 K between $\rho=0$ and 2500 km on 28 June, whereas on 29 June, $T_{rot}$ fell by about 50 K between $\rho=$0 km and 1500 km. A remarkable ($\sim50$ K) rise in $T_{rot}$ at $\rho=$1500-2500 km on 29 June was not present on 28 June. The observed variations in CH$_3$OH rotational temperature are interpreted primarily as a result of variations in the coma kinetic temperature due to adiabatic cooling, and heating through Solar irradiation, but collisional and radiative non-LTE excitation processes also play a role., Comment: Submitted to Astronomy in Focus, Volume 1. Based on work presented at the XXIXth IAU General Assembly, August 2015
Published: 2016

12. Minor species from comet 67P as measured from the VIRTIS-H instrument aboard Rosetta

Author: Bockelee-Morvan, D., Encrenaz, T., Erard, S., Leyrat, C., Debout, V., Capaccioni, F., Filacchione, G., Drossart, P., Arnold, Gabriele, Biver, N, Crovisier, J., Schmitt, B., Fougere, N., Combi, M., 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), 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, and 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)
Subjects: 67P, minor species, Rosetta, Leitungsbereich PF, VIRTIS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Since July 2014, the Visual IR Thermal Imaging Spectrometer (VIRTIS) onboard the ESA’s Rosetta spacecraft has intensively observed comet 67P/ Churyumov-Gerasimenko (67P/C-G). First results were published in [3]. VIRTIS is composed of two channels, –M for mapping and –H for high resolution, working in the 0.25-5 μm and 2-5 μm wavelength domains, respectively. In addition to nucleus mapping observations, limb observations were carried out to obtain spectra of the coma, and to detect fluorescence emissions of gas phase species. H2O, CO2, CO and organics have strong vibrational bands in the 2.5-5 μm range. The ν3 vibrational bands of H2O and CO2 at 2.67 and 4.27 μm, respectively, were detected in mid-October 2014 using VIRTIS-H, and observed regularly since then. In this contribution, we will present observations of minor species, such as OCS, CO, CH4, NH3, CH3OH. These species have been detected in cometary atmospheres, some of them in comet 67P by other Rosetta instruments. Model simulations show that they should be detected with VIRTIS-H near perihelion. Observations with the VIRTIS instrument will allow us to investigate whether the outgassing distributions of the species and diurnal variations are related to their volatility. Data acquired in the November 2014 to January 2015 period indicate a very low CO abundance relative to water of less than 1.9% (3-sigma), and a CO/CO2 upper limit of 0.7 (3- sigma), which show that 67P/C-G is CO-poor, as measured for other Jupiter-family comets.
Published: 2015

13. Water Ortho-to-Para Ratio in Comet 67P/Churyumov-Gerasimenko from VIRTIS/Rosetta Observations

Author: Debout, V., Bockelee-Morvan, D., Erard, S., Leyrat, C., Capaccioni, F., Filacchione, G., Drossart, P., Arnold, Gabriele, Biver, N, Crovisier, J., Encrenaz, T., Quirico, E., Schmitt, B., 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), 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, and 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)
Subjects: 67P, Rosetta, Leitungsbereich PF, Water, Astrophysics::Earth and Planetary Astrophysics, VIRTIS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The ν3 vibrational band of H2O at 2.67 μm was observed with the high spectral-resolution channel of the Visible InfraRed Thermal Imaging Spectrometer (VIRTIS-H) onboard Rosetta. The spectral resolution is adequate to resolve the rovibrational structure of the band. High signal-to-noise ratios allow us to measure both the rotational temperature and the ortho-para ratio of water (OPR) in comet 67P/C-G. The measured OPR value will be presented and compared to measurements obtained in other comets from ground-based and space telescopes.
Published: 2015

14. The diurnal cycle of water ice on comet 67P/Churyumov-Gerasimenko

Author: DE SANCTIS, MARIA CRISTINA, CAPACCIONI, FABRIZIO, CIARNIELLO, Mauro, FILACCHIONE, GIANRICO, FORMISANO, Michelangelo, Mottola, S., RAPONI, Andrea, TOSI, Federico, Bockelée-Morvan, D., Erard, S., Leyrat, C., Schmitt, B., Ammannito, E., Arnold, G., Barucci, M. A., Combi, M., Capria, M. T., Cerroni, P., Ip, W. -H., Kuehrt, E., McCord, T. B., PALOMBA, Ernesto, Beck, P., Quirico, E., VIRTIS Team, PICCIONI, GIUSEPPE, BELLUCCI, Giancarlo, Fulchignoni, M., Jaumann, R., Stephan, K., Longobardo, A., MENNELLA, Vito, MIGLIORINI, Alessandra, Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M., Carlson, R., Carsenty, U., Colangeli, L., Combes, M., Crovisier, J., Drossart, P., Encrenaz, T., Federico, C., Fink, U., Fonti, S., Irwin, P., Langevin, Y., Magni, G., Moroz, L., Orofino, V., Schade, U., Taylor, F., Tiphene, D., Tozzi, G. P., Biver, N., Bonal, L., Combe, J. -Ph., Despan, D., Flamini, E., Fornasier, S., FRIGERI, ALESSANDRO, GRASSI, Davide, Gudipati, M. S., Mancarella, F., Markus, K., Merlin, F., OROSEI, ROBERTO, RINALDI, GIOVANNA, CARTACCI, MARCO, Cicchetti, A., GIUPPI, Stefano, Hello, Y., Henry, F., Jacquinod, S., Rees, J. M., NOSCHESE, RAFFAELLA, POLITI, ROMOLO, Peter, G., M. C., De Sancti, F., Capaccioni, M., Ciarniello, G., Filacchione, M., Formisano, S., Mottola, A., Raponi, F., Tosi, D., Bockele´e Morvan, S., Erard, C., Leyrat, B., Schmitt, E., Ammannito, G., Arnold, M. A., Barucci, M., Combi, M. T., Capria, P., Cerroni, W. H., Ip, E., Kuehrt, T. B., Mccord, E., Palomba, P., Beck, E., Quirico, G., Piccioni, G., Bellucci, M., Fulchignoni, R., Jaumann, K., Stephan, A., Longobardo, V., Mennella, A., Migliorini, J., Benkhoff, J. P., Bibring, Blanco, Armando, M., Blecka, R., Carlson, U., Carsenty, L., Colangeli, M., Combe, J., Crovisier, P., Drossart, T., Encrenaz, C., Federico, U., Fink, Fonti, Sergio, P., Irwin, Y., Langevin, G., Magni, L., Moroz, Orofino, Vincenzo, U., Schade, F., Taylor, D., Tiphene, G. P., Tozzi, N., Biver, L., Bonal, Combe, J. P. h., D., Despan, E., Flamini, S., Fornasier, A., Frigeri, D., Grassi, M. S., Gudipati, Mancarella, Francesca, K., Marku, F., Merlin, R., Orosei, G., Rinaldi, M., Cartacci, A., Cicchetti, S., Giuppi, Y., Hello, F., Henry, S., Jacquinod, J. M., Ree, R., Noschese, R., Politi, G., Peter, Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Department of Earth and Space Sciences [Seattle], University of Washington [Seattle], Laboratoire de Sciences de la Terre, ITA, USA, GBR, FRA, DEU, TWN, NLD, POL, and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)
Subjects: 67P/Churyumov-Gerasimenko, Time Factors, Extraterrestrial Environment, 010504 meteorology & atmospheric sciences, Comet, 01 natural sciences, water ice, Astrobiology, comet, Diurnal cycle, 0103 physical sciences, Sunrise, Water cycle, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Multidisciplinary, Meteoroid, Ice, Diurnal temperature variation, Temperature, food and beverages, Meteoroids, Environmental science, Volatilization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Surface water, cycle of water ice, Water vapor
Abstract: Observations of cometary nuclei have revealed a very limited amount of surface water ice, which is insufficient to explain the observed water outgassing. This was clearly demonstrated on comet 9P/Tempel 1, where the dust jets (driven by volatiles) were only partially correlated with the exposed ice regions. The observations of 67P/Churyumov-Gerasimenko have revealed that activity has a diurnal variation in intensity arising from changing insolation conditions. It was previously concluded that water vapour was generated in ice-rich subsurface layers with a transport mechanism linked to solar illumination, but that has not hitherto been observed. Periodic condensations of water vapour very close to, or on, the surface were suggested to explain short-lived outbursts seen near sunrise on comet 9P/Tempel 1. Here we report observations of water ice on the surface of comet 67P/Churyumov-Gerasimenko, appearing and disappearing in a cyclic pattern that follows local illumination conditions, providing a source of localized activity. This water cycle appears to be an important process in the evolution of the comet, leading to cyclical modification of the relative abundance of water ice on its surface.
Published: 2015
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15. Water D/H Ratio in Comet C/2009 P1 (Garradd) from Herschel

Author: Bockelée-Morvan, D., Swinyard, B., Biver, N., Hartogh, P., Miguel de Val-Borro, Szutowicz, S., Crovisier, J., Lis, D. C., Moreno, R., Lellouch, E., Bergin, E. A., Kueppers, M., Kidger, M., Emprechtinger, M., Courtin, R., Rengel, M., Blake, G., 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), 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, and 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)
Subjects: [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience
Published: 2012

16. Comet C/2011 L4 (Panstarrs)

Author: Biver, N., Bockelée-Morvan, D., Moreno, R., Crovisier, J., Hartogh, P., de Val-Borro, M., Kidger, M., Kueppers, M., Szutowicz, S., Lis, D., Blake, G., Gonzalez, J., Seargent, D., Mattiazzo, M., and Green, D.
Subjects: Planets and Comets, HIFI [HERSCHEL]
Published: 2012

17. Molecular abundances in comet 103P/Hartley 2 observed with the Arizona Radio Observatory

Author: Miguel de Val-Borro, Hartogh, P., Jarchow, C., Rengel, M., Biver, N., Bockelée-Morvan, D., Crovisier, J., Lis, D. C., Küppers, M., Szutowicz, S., 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), 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, and 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)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience
Published: 2011

18. Molecular composition and outgassing variability of 103P/Hartley 2 from mm and submm observations

Author: Biver, N., Bockel Ee-Morvan, D., Crovisier, J., Frisk, U., Sanqvist, A., Boissier, J., Colom, P., Miguel de Val-Borro, Dello Russo, N., Hartogh, P., Floren, H. G., Hjalmarson, A., Karlsson, T., Kawakita, H., Lecacheux, A., Lundin, S., Moreno, R., Nordh, H. L., Paubert, G., Vervack, R., Weaver, H., 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), 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, and 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)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience
Published: 2011

19. Observations of the Giant Planets with Herschel

Author: Lellouch, E., Hartogh, P., Feuchtgruber, H., Swinyard, B., Moreno, R., Cavalié, T., Orton, G., Bockelée-Morvan, D., Biver, N., Sagawa, H., Jarchow, C., 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, foreign laboratories (FL), CERN [Genève], sSE 2011, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-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)-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 de Bordeaux (UB), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)
Subjects: [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience; We describe the first results of the observations of the Giant Planets with Herschel.
Published: 2011

20. EPOXI: COMET 103P/HARTLEY 2 OBSERVATIONS FROM A WORLDWIDE CAMPAIGN

Author: Meech, KJ, A’Hearn, MF, Adams, JA, Bacci, P, Bai, J, Barrera, L, Battelino, M, Bauer, JM, Becklin, E, Bhatt, B, Biver, N, Bockelée-Morvan, D, Bodewits, D, Böhnhardt, H, Boissier, J, Bonev, BP, Borghini, W, Brucato, JR, Bryssinck, E, Buie, MW, Canovas, H, Castellano, D, Charnley, SB, Chen, WP, Chiang, P, Choi, Y-J, Christian, DJ, Chuang, Y-L, Cochran, AL, Colom, P, Combi, MR, Coulson, IM, Crovisier, J, Dello Russo, N, Dennerl, K, DeWahl, K, DiSanti, MA, Facchini, M, Farnham, TL, Fernández, Y, Florén, HG, Frisk, U, Fujiyoshi, T, Furusho, R, Fuse, T, Galli, G, García-Hernández, DA, Gersch, A, Getu, Z, Gibb, EL, Gillon, M, Guido, E, Guillermo, RA, Hadamcik, E, Hainaut, O, Hammel, HB, Harker, DE, Harmon, JK, Harris, WM, Hartogh, P, Hashimoto, M, Häusler, B, Herter, T, Hjalmarson, A, Holland, ST, Honda, M, Hosseini, S, Howell, ES, Howes, N, Hsieh, HH, Hsiao, H-Y, Hutsemékers, D, Immler, SM, Jackson, WM, Jeffers, SV, Jehin, E, Jones, TJ, de Juan Ovelar, M, Kaluna, HM, Karlsson, T, Kawakita, H, Keane, JV, Keller, LD, Kelley, MS, Kinoshita, D, Kiselev, NN, Kleyna, J, Knight, MM, Kobayashi, H, Kobulnicky, HA, Kolokolova, L, Kreiny, M, Kuan, Y-J, Küppers, M, Lacruz, JM, Landsman, WB, Lara, LM, Lecacheux, A, Levasseur-Regourd, AC, and Li, B
Subjects: individual [comets], Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: Earth- and space-based observations provide synergistic information for space mission encounters by providing data over longer timescales, at different wavelengths and using techniques that are impossible with an in situ flyby. We report here such observations in support of the EPOXI spacecraft flyby of comet 103P/Hartley 2. The nucleus is small and dark, and exhibited a very rapidly changing rotation period. Prior to the onset of activity, the period was 16.4hr. Starting in 2010 August the period changed from 16.6hr to near 19hr in December. With respect to dust composition, most volatiles and carbon and nitrogen isotope ratios, the comet is similar to other Jupiter-family comets. What is unusual is the dominance of CO 2 -driven activity near perihelion, which likely persists out to aphelion. Near perihelion the comet nucleus was surrounded by a large halo of water-ice grains that contributed significantly to the total water production. © 2011. The American Astronomical Society. All rights reserved..
Published: 2011

21. Detection of Enceladus Torus from Submillimeter Observations with Herschel/HIFI

Author: Lellouch, Emmanuel, Hartogh, P., Moreno, R., Bockelée-Morvan, D., Biver, N., Jarchow, C., Rengel, M., Cavalié, T., Helmich, F., Hsso Team, 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, 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), Observatoire aquitain des sciences de l'univers (OASU), 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), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Max Planck Institute for Solar System Research (MPS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université Sciences et Technologies - Bordeaux 1
Subjects: [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Physics::Space Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; The presence of water vapor in the stratospheres of the Giant Planets and Titan has been established from their emission in rotational lines longwards of 30 microns. Emission in the fundamental H2O line at 557 GHz has been spectrally resolved from heterodyne observations with SWAS at Jupiter and Saturn and ODIN at Jupiter, showing emission line-widths of about 20 km/s, due to planetary rotation. Initial observations of Saturn with the HIFI instrument on Herschel, performed in June 2009, revealed an additional 20 % deep, 5 km/s broad absorption superimposed to the emission, that was not seen in the SWAS observation performed in 1999 (Bergin et al. 2000). This absorption is certainly not due to water in Saturn itself, as the brightness temperature in the line core would indicate implausibly cold temperatures ( 95 K) in Saturn's upper atmosphere, and as the line-width is too narrow. Instead, we interpret it as water vapor absorption along the line-of-sight coming from the Enceladus H2O torus, the difference with the SWAS results being presumably related to the different viewing geometries. We developed an excitation model for water in Enceladus torus including excitation by solar and Saturn's radiation. Extended observations performed in June 2010, and covering the H2O 557, 987, 1113 and 1670 GHz (including a 5-point map at this frequency) confirm this interpretation, as does the fact that the 1097 GHz H2O line does not show absorption. An initial modelling of the data indicates line-of-sight water column densities of (1-3)x1013 cm-2. These observations provide a new method to study physical conditions in the Enceladus torus.
Published: 2010

22. First results of Herschel/PACS observations of Neptune

Author: Lellouch, E., Hartogh, P., Feuchtgruber, H., Vandenbussche, B., de Graauw, Th., Moreno, R., Jarchow, C., Cavalie, T., Orton, G., Banaszkiewicz, M., Blecka, M. I., Bockelee-Morvan, D., Crovisier, J., Encrenaz, T., Fulton, T., Kueppers, M., Lara, L. M., Lis, D. C., Medvedev, A. S., Rengel, M., Sagawa, H., Swinyard, B., Szutowicz, S., Bensch, F., Bergin, E., Billebaud, F., Biver, N., Blake, G. A., Blommaert, J. A. D. L., Cernicharo, J., Courtin, R., Davis, G. R., Decin, L., Encrenaz, P., Gonzalez, A., Jehin, E., Kidger, M., Naylor, D., Portyankina, G., Schieder, R., Sidher, S., Thomas, N., de Val-Borro, M., Verdugo, E., Waelkens, C., Aarts, H., Comito, C., Kawamura, J. H., Maestrini, A., Peacocke, T., Teipen, R., Tils, T., Wildeman, K., Walker, H., Blake, G.A., 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 Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, 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), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), California Institute of Technology (CALTECH), Center for Mathematics and Physics, University of Aizu, 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), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), 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), Departamento de Biologia Celular, Facultad de Biologia, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), European Southern Observatory (ESO), Centre Alexis Vautrin (CAV), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Nice Sophia Antipolis (1965 - 2019) (UNS), and Astronomy
Subjects: 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, Troposphere, Neptune, 0103 physical sciences, Mixing ratio, 010303 astronomy & astrophysics, Stratosphere, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, planets and satellites: composition, Astronomy and Astrophysics, planets and satellites: individual: Neptune, Deuterium, GIANT PLANETS, 13. Climate action, Space and Planetary Science, URANUS, Polar, Millimeter, ABUNDANCE, Earth and Planetary Astrophysics, ATMOSPHERES, techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report on the initial analysis of a Herschel/PACS full range spectrum of Neptune, covering the 51-220 micrometer range with a mean resolving power of ~ 3000, and complemented by a dedicated observation of CH4 at 120 micrometers. Numerous spectral features due to HD (R(0) and R(1)), H2O, CH4, and CO are present, but so far no new species have been found. Our results indicate that (i) Neptune's mean thermal profile is warmer by ~ 3 K than inferred from the Voyager radio-occultation; (ii) the D/H mixing ratio is (4.5+/-1) X 10**-5, confirming the enrichment of Neptune in deuterium over the protosolar value (~ 2.1 X 10**-5); (iii) the CH4 mixing ratio in the mid stratosphere is (1.5+/-0.2) X 10**-3, and CH4 appears to decrease in the lower stratosphere at a rate consistent with local saturation, in agreement with the scenario of CH4 stratospheric injection from Neptune's warm south polar region; (iv) the H2O stratospheric column is (2.1+/-0.5) X 10**14 cm-2 but its vertical distribution is still to be determined, so the H2O external flux remains uncertain by over an order of magnitude; and (v) the CO stratospheric abundance is about twice the tropospheric value, confirming the dual origin of CO suspected from ground-based millimeter/submillimeter observations., Accepted for publication in Astronomy & Astrophysics (special issue on Herschel first results)
Published: 2010
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23. Water and related chemistry in the Solar System. A Guaranteed Time Key Programme for Herschel

Author: Hartogh, P., Crovisier, J., Lellouch, E., Banaszkiewicz, M., Bensch, F., Bergin, E. A., Billebaud, F., Biver, N., Blake, G. A., Blommaert, J., Bockelée-Morvan, D., Cavalié, T., Cernicharo, J., Courtin, R., Davis, G., Decin, L., Encrenaz, P., Encrenaz, T., Graauw, T., Gonzáles, A., Hutsemékers, D., Jarchow, C., Jehin, E., Kidger, M., Küppers, M., Lange, A., Lara, L. -M, Lis, D. C., Lorente, R., Manfroid, J., Medvedev, A. S., Moreno, R., Naylor, D. A., Orton, G., Portyankina, G., Rengel, M., Sagawa, H., Sánchez-Portal, M., Schieder, R., Sidher, S., Stam, D., Swinyard, B., Szutowicz, S., Thomas, N., Thornhill, G., Bart Vandenbussche, Verdugo, E., Walker, H., 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), 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, and 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)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience
Published: 2009

24. Triple F--a comet nucleus sample return mission

Author: Küppers, Michael, Keller, H. U., Kührt, E., A'Hearn, M. F., Altwegg, K., Bertrand, R., Busemann, H., Capria, M. T., Colangeli, L., Davidsson, B., Ehrenfreund, P., Knollenberg, J., Mottola, S., Rathke, A., Weiss, P., Zolensky, M., Akim, E., Basilevsky, A., Galimov, E., Gerasimov, M., Korablev, O., Lomakin, I., Marov, M., Martynov, M., Nazarov, M., Zakharov, A., Zelenyi, L., Aronica, A., Ball, A. J., Barbieri, C., Bar-Nun, A., Benkhoff, J., Biele, J., Biver, N., Blum, J., Bockelée-Morvan, D., Botta, O., Bredehöft, J. H., Capaccioni, F., Charnley, S., Cloutis, E., Cottin, H., Cremonese, G., Crovisier, J., Crowther, S. A., Epifani, E. M., Esposito, F., Ferrari, A. C., Ferri, F., Fulle, M., Gilmour, J., Goesmann, F., Gortsas, N., Green, S. F., Groussin, O., Grün, E., Gutiérrez, P. J., Hartogh, P., Henkel, T., Hilchenbach, M., Ho, T. M., Horneck, G., Hviid, S. F., Ip, W. H., Jäckel, A., Jessberger, E., Kallenbach, R., Kargl, G., Kömle, N. I., Korth, A., Kossacki, K., Krause, C., Krüger, H., Li, Z. Y., Licandro, J., Lopez-Moreno, J. J., Lowry, S. C., Lyon, I., Magni, G., Mall, U., Mann, I., Markiewicz, W., Martins, Z., Maurette, M., Meierhenrich, U., Mennella, V., Ng, T. C., Nittler, L. R., Palumbo, P., Pätzold, M., Prialnik, D., Rengel, M., Rickman, H., Rodriguez, J., Roll, R., Rost, D., Rotundi, A., Sandford, S., Schönbächler, M., Sierks, H., Srama, R., Stroud, R. M., Szutowicz, S., Tornow, C., Ulamec, S., Wallis, M., Waniak, W., Weissman, P., Wieler, R., Wurz, P., Yung, K. L., Zarnecki, J. C., Schonbachler, Maria, Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), 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), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Solar System, Cosmic Vision, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], sample return, Sample return, space mission, 7. Clean energy, 01 natural sciences, Space mission, Astrobiology, Interplanetary dust cloud, Sample return mission, Comet nucleus, 0103 physical sciences, Comets, comets, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spacecraft, business.industry, Astronomy, Astronomy and Astrophysics, Cosmogony, 13. Climate action, Space and Planetary Science, cosmogony, Formation and evolution of the Solar System, business
Abstract: The Triple F (Fresh From the Fridge) mission, a Comet Nucleus Sample Return, has been proposed to ESA's Cosmic Vision program. A sample return from a comet enables us to reach the ultimate goal of cometary research. Since comets are the least processed bodies in the solar system, the proposal goes far beyond cometary science topics (like the explanation of cometary activity) and delivers invaluable information about the formation of the solar system and the interstellar molecular cloud from which it formed. The proposed mission would extract three sample cores of the upper 50cm from three locations on a cometary nucleus and return them cooled to Earth for analysis in the laboratory. The simple mission concept with a touch-and-go sampling by a single spacecraft was proposed as an M-class mission in collaboration with the Russian space agency ROSCOSMOS. © The Author(s) 2008.
Published: 2009
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25. The chemical diversity of comets

Author: Crovisier, J., Biver, N., Bockelée-Morvan, D., Boissier, J., Colom, P., and Lis, D. C.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics::Space Physics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: A fundamental question in cometary science is whether the different dynamical classes of comets have different chemical compositions, which would reflect different initial conditions. From the ground or Earth orbit, radio and infrared spectroscopic observations of a now significant sample of comets indeed reveal deep differences in the relative abundances of cometary ices. However, no obvious correlation with dynamical classes is found. Further results come, or are expected, from space exploration. Such investigations, by nature limited to a small number of objects, are unfortunately focussed on short-period comets (mainly Jupiter-family). But these in situ studies provide "ground truth" for remote sensing. We discuss the chemical differences in comets from our database of spectroscopic radio observations, which has been recently enriched by several Jupiter-family and Halley-type comets., Comment: In press in Earth, Moon and Planets (proceedings of the workshop "Future Ground-based Solar System Research: Synergies with Space Probes and Space Telescopes", Portoferraio, Isola d'Elba, Livorno (Italy), 8-12 September 2008). 6 pages with 2 figures
Published: 2009
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26. High-dispersion spectroscopic observations of 8P/Tuttle with VLT/CRIRES

Author: Kobayashi, Hitomi, Bockelee-Morvan, D., Dello Russo, N., Kawakita, H., Verback, R. J., Weaver, H., Jehin, E., Manfroid, J., Smette, A., Cochran, A., Hutsemekers, D., Schulz, R., Stuwe, J., Weiler, M., Zucconi, J., Arpigny, C., Biver, N., Crovisier, J., Magain, P., Rauer, H., Hugues Sana, 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), 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, and 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)
Subjects: organic molecules, spectroscopy, 8P/Tuttle, comets, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience
Published: 2008

27. A multi-wavelength simultaneous study of the composition of the Halley-family comet 8P/Tuttle at the VLT

Author: Bockelée-Morvan, D., Dello Russo, N., Jehin, E., Manfroid, J., Smette, A., Cochran, A., Hutsemékers, D., Kawakita, H., Kobayashi, H., Schulz, R., Weiler, M., Zucconi, J. M., Arpigny, C., Biver, N., Crovisier, J., Magain, P., Rauer, H., Hugues Sana, Vervack, R. J., Weaver, H., 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), 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, and 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)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience
Published: 2008

28. A multi-wavelength simultaneous study of the composition of the Halley family comet 8P/Tuttle at the VLT

Author: Bockelée-Morvan, D., Dello Russo, N., Jehin, E., Manfroid, J., Smette, A., Cochran, A., Hutsemékers, D., Kawakita, H., Kobayashi, H., Schulz, R., Weiler, M., Zucconi, J.-M., Arpigny, C., Biver, N., Crovisier, J., Magain, P., Rauer, Heike, Sana, H., Vervack, R. J., and Weaver, H.
Subjects: composition, 8P/Tuttle, high-resolution spectroscopy, comets
Published: 2008

29. Observation of water vapor in the stratosphere of Jupiter with the Odin Space Telescope

Author: CAVALIÉ, T., BILLEBAUD, F., BIVER, N., DOBRIJEVIC, M., LELLOUCH, E., BRILLET, J., LECACHEUX, J., HJALMARSON, A., SANDQVIST, A., FRISK, U., OLBERG, M., ODIN, Equipe, BERGIN, E. A., Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), 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), 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), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Stockholm Observatory Department of Astronomy, Stockholm University, Swedish Space Corporation (SSC), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Smithsonian Institution-Harvard University [Cambridge]
Subjects: spectroscopy, 010504 meteorology & atmospheric sciences, water, Odin space telescope, 01 natural sciences, Jupiter, Atmosphere, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spitzer Space Telescope, 0103 physical sciences, Spectral resolution, 010303 astronomy & astrophysics, Stratosphere, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, Line (formation), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, 13. Climate action, Space and Planetary Science, atmosphere, Satellite, Astrophysics::Earth and Planetary Astrophysics, Water vapor
Abstract: International audience; The water vapor line at 557 GHz has been observed with the Odin space telescope with a high signal-to-noise ratio and a high spectral resolution on November 8, 2002. The analysis of this observation as well as a re-analysis of previously published observations obtained with the SubmillimeterWavelength Astronomy Satellite seem to favor a cometary origin (Shoemaker-Levy 9) for water in the stratosphere of Jupiter, in agreement with the ISO observation results. Our model predicts that the water line should become fainter and broader from 2007. The observation of such a temporal variablity would be contradictory with an IDP steady flux, thussupporting the SL9 source hypothesis.
Published: 2008
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30. An investigation of the spin temperature of methanol in comet Hale-Bopp

Author: J. Bockelee-Morvan D. Biver N. Pardanaud C., Crovisier, Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Eds. J. Bouvier, A. Chalabaev, C. Charbonnel, Francois, Francoise, and Eds. J. Bouvier, A. Chalabaev, & C. Charbonnel
Subjects: [PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2007

31. 'An investigation of the spin temperature of methanol in comet Hale-Bopp.' – Affiche –

Author: C. Crovisier J. Bockelee-Morvan D. Biver N., Pardanaud, Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), and Francois, Francoise
Subjects: [PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Published: 2007

32. Detection of water vapor on Jupiter with the Odin space telescope

Author: CAVALIÉ, T., BILLEBAUD, F., LELLOUCH, E., BIVER, N., DOBRIJEVIC, M., BRILLET, J., LECACHEUX, A., HJALMARSON, A., SANDQVIST, A., FRISK, U., OLBERG, M., 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), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), 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), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Stockholm Observatory Department of Astronomy, Stockholm University, Swedish Space Corporation (SSC), Odin, and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract: The Infrared Space Observatory (ISO) has detected water vapor in the stratospheres of the giant planets and Titan and CO2 on Jupiter, Saturn and Neptune (Feuchtgruber et al. 1997, 1999, Lellouch et al. 1999). The presence of the atmospheric cold trap implies an external origin for H2O (interplanetary dust, sputtering from the satellites and /or rings, large meteoritic impacts). The H2O submillimeric line at 557 GHz was detected by the Submillimeter-Wave Astronomy Satellite (SWAS) in 1999 and 2001 (Bergin et al. 2000, Lellouch et al. 2002), but the vertical profile and the column density derived from the observations are different from the one obtained from ISO mesurements (Lellouch et al. 2002).The swedish sub-millimeter satellite Odin carries out a long lasting monitoring of Jupiter's H20 (110-101) 557 GHz line, since its launch in 2001. As an example, the high resolution H2O spectrum obtained on November 8th, 2002, will be presented and discussed here. Spectral analysis combined with the use of our photochemical model (Ollivier et al. 2000, adapted for Jupiter) provides new clues which help understanding the discrepancy between the ISO and SWAS results.
Published: 2007

33. Observations of Jupiter with SWAS and Odin: a cometary origin for water vapor in the stratosphere of Jupiter ?

Author: Cavalié, T., Billebaud, F., Lellouch, E., Biver, N., Dobrijevic, M., Brillet, J., Lecacheux, A., Hjalmarson, A., Sandqvist, A., Frisk, U., Olberg And The Odin Team, M., Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
Published: 2007

34. SMART-1 Impact Ground-based campaign

Author: Ehrenfreund, P., Foing, B. H., Veillet, C., Wooden, D., Gurvits, L., Cook, A. C., Koschny, D., Biver, N., Buckley, D., Ortiz, J. L., Di Martino, M., Dantowitz, R., Cooke, B., Reddy, V., Wood, M., Vennes, S., Albert, L., Sugita, S., Kasuga, T., Meech, K., Tokunaga, A., Lucey, P., Krots, A., Palle, E., Montanes, P., Trigo-Rodriguez, J., Cremonese, G., Barbieri, C., Ferri, F., Mangano, V., Bhandari, N., Chandrasekhar, T., Kawano, N., Matsumoto, K., Taylor, C., Hanslmeyer, A., Vaubaillon, J., Schultz, R., Erd, C., Gondoin, P., Levasseur-Regourd, A.-C., Khodachenko, M., Rucker, H., Burchell, M., Cole, M., Svedhem, H., Rossi, A., Colaprete, T., Goldstein, D., Schultz, P. H., Alkalai, L., Banerdt, B., Kato, M., Graham, F., Ball, A., Taylor, E., Baldwin, E., Berezhnoy, A., Lammer, H., Talevi, M., Landeau-Constantin, J., Weyhe, B. v., Ansari, S., Lawton, C., Lebreton, J. P., Friedman, L., Betts, B., Buoso, M., Williams, S., Cirou, A., David, L., Sanguy, O., Burke, J. D., Maley, P. D., de Morais, V. M., Marchis, F., Munoz, J. M. H., and Dighay, J.-L.
Abstract: Based on predictions of impact magnitude and cloud ejecta dynamics, we organized a SMART-1 ground-based observation campaign to perform coordinated measurements of the impact. Results from the coordinated multi-site campaign will be discussed.
Published: 2007

35. The Origin of Water Vapor in the Stratosphere of Jupiter: SWAS and Odin Observations

Author: Cavalié, T., Billebaud, F., Lellouch, E., Biver, N., Dobrijevic, M., Brillet, J., Lecacheux, A., Hjalmarson, A., Sandqvist, A., Frisk, U., Olberg, M., The Odin Team, Bergin, E. A., Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), 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), 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), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Stockholm Observatory Department of Astronomy, Stockholm University, Swedish Space Corporation (SSC), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-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 Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), and Pomies, Marie-Paule
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract: The Infrared Space Observatory (ISO) has detected water vapor in the stratospheres of the giant planets and Titan and CO2 on Jupiter, Saturn and Neptune (Feuchtgruber et al. 1997, 1999, Lellouch et al. 1997). The presence of the atmospheric cold trap implies an external origin for H2O (interplanetary dust (IDP), sputtering from the satellites and /or rings, large meteoritic impacts). In the case of Jupiter, the sources of water could either be IDP or the SL9 comet impacts (Moses et al. 2000, Lellouch et al. 2002). The H2O submillimetric line at 557 GHz on Jupiter was detected by the SWAS satellite in 1999 and 2001 (Bergin et al. 2000, Lellouch et al. 2002) and by the Odin space telescope in 2002 with a high signal to noise ratio. The vertical profile and the column density previously derived from the SWAS observations (Bergin et al. 2000) were different from the one obtained from ISO measurements (Lellouch et al. 2002). SWAS measurements favored an IDP source, whereas ISO observations favored a SL9 source. We have re-analyzed SWAS data with the same approach we had for Odin data (Cavalié et al. 2006). Both origins for water supply have been modeled with our time-dependant photochemical model (Ollivier et al. 2000, adapted for Jupiter). The origin of water vapor in the stratosphere of Jupiter as suggested by our results will be discussed. References : Feuchtgruber et al. (1997), Nature, 389, 159-162. Feuchtgruber et al. (1999), The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP, 427, 133. Lellouch et al. (1997), BAAS, 29, 992. Moses et al. (2000), Icarus, 145, 166-202. Lellouch et al. (2002), Icarus, 159, 112-131. Bergin et al. (2000), ApJ, 539, L147-L150. Ollivier et al. (2000), Plan. Space Sci., 48, 699-716. Cavalié et al. (2006), BAAS, 38, 497-498.
Published: 2007

36. Detection of water vapor on Jupiter with the Odin space telescope

Author: Cavalié, T., Billebaud, F., Lellouch, E., Biver, N., Dobrijevic, M., Brillet, J., Odin, Equipe, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), 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), 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), Stockholm Observatory Department of Astronomy, Stockholm University, and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Published: 2007

37. Contribution of the Odin space telescope to the understanding of the origin of water vapor in the atmosphere of Jupiter

Author: Cavalié, T., Billebaud, F., Lellouch, E., Biver, N., Dobrijevic, M., Brillet, J., Lecacheux, A., Hjalmarson, A., Sandqvist, A., Frisk, U., Olberg And The Odin Team., M., 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), 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'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), 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), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Stockholm Observatory Department of Astronomy, Stockholm University, Swedish Space Corporation (SSC), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract: International audience; The water vapor line at 557 GHz was observed on November 8, 2002, with the Odin space telescope. The analysis of this observation, characterized by a high signal-to-noise ratio and a high spectral resolution, seems to favor a cometary origin (Shoemaker-Levy 9) for water in the stratosphere of Jupiter, in agreement with the ISO observation results.
Published: 2007

38. 'Etude de l'effet en concentration sur la Conversion de Spin Nucléaire de la molécule d'eau piégée en matrices de gaz rare : un premier pas avant l'étude en glaces. Implications astrophysiques.' –Affiche –

Author: C. Crovisier J. Bockelee-Morvan D. Biver N., Pardanaud, Francois, Francoise, Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)
Published: 2007

39. Détection de la raie stratosphérique de l'eau à 557 GHz sur Jupiter avec le télescope spatial Odin

Author: Cavalié, T., Lellouch, E., Biver, N., Dobrijevic, M., Billebaud, F., Lecacheux, A., 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), Physique des plasmas, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), 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), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Le satellite ISO (Infrared Space Observatory) a détecté la présence de vapeur d'eau dans la stratosphère des planètes géantes et de Titan et du CO2 sur Jupiter, Saturne et Neptune ([1], [2], [3]). La présence de vapeur d'eau au-dessus de son niveau de condensation (piège froid troposphérique) dans les atmosphères des géantes implique la présence d'une source externe d'oxygène ([4], [5]). Plusieurs scénarios d'apport externe d'oxygène sont possibles : la chute de poussières interplanétaires, un flux provenant des anneaux ou des satellites ou encore la chute de comètes et d'astéroïdes. La densité de colonne d'eau déduite des observations est de 1.5x1015 cm-2 sur Jupiter. Le satellite SWAS (Submillimeter-Wave Astronomy Satellite) a détecté la transition fondamentale de l'eau à 557 GHz sur Jupiter [6]. Cette observation a permis de contraindre le niveau d'émission de la vapeur d'eau dans la stratosphère de la planète (5 mbar) et de donner une nouvelle valeur de la densité de colonne de vapeur d'eau présente (2.8 x1015 cm-2). Il existe donc une différence entre les interprétations des données ISO et SWAS en termes de quantité d'eau présente dans la stratosphère de Jupiter [5]. Dans la continuité de cette étude sur Jupiter, le télescope spatial ODIN a été employé pour observer la transition de l'eau à 557 GHz. L'analyse de ces nouvelles données et leur comparaison avec les résultats antérieurs devrait permettre, avec l'appui du modèle photochimique (développé pour Saturne et adapté à Jupiter) dont on dispose [7], de mieux contraindre la distribution verticale de la vapeur d'eau.
Published: 2006

40. Microwave Instrument for the Rosetta Orbiter (MIRO)

Author: Deschamps, A., Allen, M., Beaudin, G., Biver, N., Bockelee-Morvan, D., Crovisier, J., Despois, D., Encrenaz, P., Encrenaz, T., Frerking, M., Gulkis, S., Hartogh, P., Hofstadter, M., Ip, W., Janssen, M., Jarchow, C., Koch, T., Krieg, J., Lellouch, E., Mann, I., Muhleman, D., Rauer, H., Schloerb, P., Spilker, T., and Steinmetz, E.
Subjects: MIRO [ROSETTA]
Published: 2006

41. Detection Of Water Vapor In The Stratosphere Of Jupiter With The Odin Space Telescope

Author: Cavalié, T., Lellouch, E., Biver, N., Dobrijevic, M., Billebaud, F., Lecacheux, A., Hjalmarson, A., Sandqvist, A., Frisk, U., Olberg, M., Odin, Equipe, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2006

42. Chemical diversity of comets observed at radio wavelengths in 2003-2005

Author: CROVISIER, J., BIVER, N., BOCKELÉE-MORVAN, D., BOISSIER, J., COLOM, P., MORENO, R., LIS, D. C., PAUBERT, Gabriel, DESPOIS, D., GUNNARSSON, M., WEAVER, H. A., 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), California Institute of Technology (CALTECH), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), 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), Biologie et écologie tropicale et méditerranéenne [2007-2010] (BETM), Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Perpignan Via Domitia (UPVD), and Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience; In 2003-2005 seven comets were investigated at millimeter to submillimeter wavelengths using CSO and IRAM-30m facilities: C/2002 V1 (NEAT), C/2002 X5 (Kudo-Fujikawa), 2P/Encke, C/2002 T7 (LINEAR), C/2001 Q4 (NEAT), C/2004 Q2 (Machholz) and 9P/Tempel 1. With these observations, we can further extend our comparative study of the molecular composition of comets (Biver et al. 2002, EMP 90, 323) and improve our understanding on the evolution of molecular abundances with heliocentric distance (rh) (between rh = 0.1 and 2.8 AU from the Sun). The sample is also very diverse, with comets of the shortest (3.3 years) and long orbital period: 9000 to 30 million years. A total of 12 molecules: HCN, CH3OH, CS, CO, H2CO, H2S, HNC, CH3CN, SO, HNCO, HC3N and HCOOH were observed and detected in at least one comet, in some cases for the second time since their identification in comet Hale-Bopp in 1997. We present our main results, including the following findings: (1) The HNC/HCN production rate ratio appears to plateau at a maximum value around 0.2 for rh < 0.5 AU, after initially increasing with decreasing heliocentric distance; (2) The CH3OH/HCN ratio, on the other hand, seems to decrease towards the Sun, as observed in C/2002 X5 and C/2002 T7; (3) HDO was searched for in C/2004 Q2 (Machholz) and the upper limit obtained for the D/H ratio in water (< 0.00023; 3-σ ) is lower, though only marginally, than the value of 0.0003 measured in other long period comets; (4) Both comets 2P and C/2002 T7, the comets having the shortest and longest orbital periods among the sample, have a high methanol abundance (about 4% relative to water). The abundances of all molecules detected and searched for are presented and a comparison between comets, including comet Hale-Bopp, is shown.
Published: 2005

43. The composition of ices in comet C/1995 O1 (Hale-Bopp) from radio spectroscopy

Author: Crovisier, J., Bockelée-Morvan, D., Colom, P., Biver, N., Despois, D., and Lis, D. C.
Abstract: From radio spectroscopic observations of comets, more than 22 molecules, radicals and ions, plus several isotopologues, were detected, the majority of them being recently revealed in comets C/1996 B2 (Hyakutake) and C/1995 O1 (Hale-Bopp). Among them, 6 molecules were detected for the first time (Bockelée-Morvan et al. [CITE]) in the course of a spectral survey conducted at radio wavelengths in comet Hale-Bopp with the CSO, the IRAM 30-m telescope and Plateau de Bure interferometer. In addition, many species were searched for unsuccessfully, some of them with stringent upper limits. We present here a review of these observations and further analysis of their results. This include: (i) confirmed detection of acetaldehyde (CH_3CHO); (ii) limits on small molecules such as ketene (H_2CCO) or methanimine (CH_2NH); (iii) limits on the abundance ratios in homologous series such as HC_5N/HC_3N, ethanol/methanol, acetic acid/formic acid; (iv) searches for precursors of key cometary species such as atomic Na and HNC; (v) constraints on more exotic species ranging from water dimer (H_2O)_2 to glycine; (vi) detection of the H_2^(34)S isotopic species and independent observations of HDO and DCN; (vii) limits on several other deuterated species; (viii) limits on several radicals and ions and a tentative detection of the C_2H radical; (ix) the presence of unidentified lines. Typical abundance upper limits of 2–5 x 10^(-4) relative to water are achieved for many species. Better upper limits are obtained for some linear molecules with high dipole moments. But more complex molecules such as dimethyl ether or glycine are poorly constrained. These results should give important clues to the chemical composition of cometary ices, to the formation mechanisms of cometary material, and to the chemical processes which occur in the inner coma.
Published: 2004

44. A study of Trans-Neptunian Object 55636 (2002 TX300)

Author: Ortiz, J. L., Sota, A., Moreno, R., Lellouch, E., Biver, N., Doressoundiram, A., Rousselot, P., Gutiérrez, P.J., Márquez, I., Delgado, R.M. Gonzáles, Casanova, V., Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), 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), 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), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), PSL Research University (PSL), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), and 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)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
Published: 2004
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45. Molecular observations in comets: Constraints to planetary systems formation

Author: Crovisier, J., Biver, N., Bockelée-Morvan, D., Colom, P., Despois, D., Lis, D., Rauer, H., and The Team For Target-of-Opportunity Radio Observations of Comets
Published: 2000

46. Long-term evolution of the outgassing of comet Hale-Bopp from radio observations

Author: Biver, N., Bockelée-Morvan, D., Colom, P., Crovisier, J., Germain, B., Lellouch, E., Davies, J.K., Dent, W.R.F., Moreno, R., Paubert, G., Wink, J., Despois, D., Lis, D.C., Mehringer, D., Benford, D., Gardner, M., Phillips T.G., Gunnarsson, M., Rickman, H., Winnberg, A., Bergman, P., Johansson, L.E.B., and Rauer, H.
Published: 1999

47. New molecular species in comet C/1995 1 (Hale-Bopp) observed with the Caltech Submillimeter Observatory

Author: Lis, D.C., Mehringer, D.M., Benford, D., Gardner, M., Phillips, T.G., Bockelée-Morvan, D., Biver, N., Colom, P., Crovisier, J., Despois, D., and Rauer, H.
Published: 1999

48. Observations of the OH radical in comet C/1995 O1 (Hale-Bopp) with the Nançay Radio Telescope

Author: Colom, P., Gérard, E., Crovisier, J., Bockelée-Morvan, D., Biver, N., and Rauer, H.
Published: 1999

49. Spectroscopic Monitoring of Comet C/1996 B2 (Hyakutake) with the JCMT and IRAM Radio Telescopes

Author: Biver, N., Bockelée-Morvan, D., Crovisier, J., Davies, J.K., Matthews, H.E., Wink, J.E., Rauer, H., Colom, P., Dent, W.R.F., Despois, D., Moreno, R., Paubert, G., Jewitt, D., and Senay, M.
Subjects: Radio emission lines, Comets: Individual: Name: Hyakutake (C/1996 B2), Comets: General
Published: 1999

50. A molecular survey of comet C/1995 O1 (Hale-Bopp) at the IRAM telescopes

Author: Bockelée-Morvan, D., Wink, J., Despois, D., Colom, P., Biver, N. (IfA, University of Hawaii, USA), Crovisier, J., Gautier, D., Gérard, E., Lellouch, E., Moreno, R. (Observatoire de Paris-Meudon, France), Paubert, G., Rauer, H., Davies, J.K., and Dent, W.R.F.
Published: 1999

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