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153. The HP³ Radiometer on InSight

Author

Mueller, N., Grott, M., Piqueux, S., Spohn, T., Smrekar, S.E., Knollenberg, J., Hudson, T.L., Spiga, A., Forget, F., Millour, E., Lemmon, M.T., Maki, J., Golombek, M., and Banerdt, W.B.

Subjects
Asteroiden und Kometen, Planetenphysik, Leitungsbereich PF, Astrophysics::Solar and Stellar Astrophysics, Mars, Messung, Astrophysics::Earth and Planetary Astrophysics, Oberflächentemperatur, Astrophysics::Galaxy Astrophysics, Physics::Atmospheric and Oceanic Physics, Physics::Geophysics
Abstract

The Heat Flow and Physical Properties Package (HP³) includes an infrared Radiometer attached to the deck of the InSight lander. The radiometer will observe the seasonal temperature variation over the course of the mission. Fitting of diurnal temperature curves and of the response to eclipses provides an estimate of thermophysical properties of the near surface, and possibly constrains atmospheric variables such as the ratio of visible to infrared dust opacity.

Published
2019

154. The methane cycles on Pluto over seasonal and astronomical timescales

Author

Bertrand, Tanguy, Forget, F., Umurhan, O.M., Moore, J.M., Young, L.A., Protopapa, S., Grundy, W.M., Schmitt, B., Dhingra, R.D., Binzel, R.P., Earle, A.M., Cruikshank, D.P., Stern, S.A., Weaver, H.A., Ennico, K., Olkin, C.B., Beyer, David, O'Brien, Paul, Withers, Gwen, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), NASA, Southwest Research Institute [Boulder] (SwRI), Lowell Observatory [Flagstaff], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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 Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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 Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), NASA Ames Research Center (ARC), Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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]), and Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL)

Subjects
Brightness, glacier, 010504 meteorology & atmospheric sciences, Thermodynamic equilibrium, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, volatile transport, 01 natural sciences, Mantle (geology), Latitude, Astrobiology, paleoclimate, 0103 physical sciences, Paleoclimatology, Thermal, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), geography, geography.geographical_feature_category, Pluto, Modeling, Astronomy and Astrophysics, Glacier, CH4 ice, GCM, 13. Climate action, Space and Planetary Science, atmosphere, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

New Horizons observations suggest that CH4 on Pluto has a complex history, involving reservoirs of different composition, thickness and stability controlled by volatile processes occurring on different timescales. In order to interpret these observations, we use a Pluto volatile transport model able to simulate the cycles of N2 and CH4 ices over millions of years. By assuming fixed solid mixing ratios, we explore how changes in surface albedos, emissivities and thermal inertias impact volatile transport. This work is therefore a direct and natural continuation of the work by Bertrand et al. (2018), which only explored the N2 cycles. Results show that bright CH4 deposits can create cold traps for N2 ice outside Sputnik Planitia, leading to a strong coupling between the N2 and CH4 cycles. Depending on the assumed albedo for CH4 ice, the model predicts CH4 ice accumulation (1) at the same equatorial latitudes where the Bladed Terrain Deposits are observed, supporting the idea that these CH4-rich deposits are massive and perennial, or (2) at mid-latitudes (25{\deg}N-70{\deg}N), forming a thick mantle which is consistent with New Horizons observations. In our simulations, both CH4 ice reservoirs are not in an equilibrium state and either one can dominate the other over long timescales, depending on the assumptions made for the CH4 albedo. This suggests that long-term volatile transport exists between the observed reservoirs. The model also reproduces the formation of N2 deposits at mid-latitudes and in the equatorial depressions surrounding the Bladed Terrain, as observed by New Horizons. At the poles, only seasonal CH4 and N2 deposits are obtained in Pluto's current orbital configuration. Finally, we show that Pluto's atmosphere always contained, over the last astronomical cycles, enough gaseous CH4 to absorb most of the incoming Lyman-flux., Comment: Accepted in Icarus

Published
2019

155. The HP3 Radiometer on InSight

Author

Müller, Nils, Grott, Matthias, Piqueux, S., Spohn, Tilman, Smrekar, S., Knollenberg, Jörg, Hudson, T.L., Spiga, Aymeric, Forget, F., Millour, Ehouarn, Lemmon, M. T., Maki, J., Golombek, M., and Banerdt, W.B.

Subjects
Asteroiden und Kometen, Planetenphysik, Institutsplanung / Zentrale Aufgaben PF, Mars, Messung, Oberflächentemperatur
Abstract

Introduction: The Heat Flow and Physical Properties Package (HP³) includes an infrared Radiometer attached to the deck of the InSight lander. The main objective of this part of the instrument is to con-strain the surface thermal boundary condition for the heat flow derivation by the instrumented tether de-ployed into the subsurface. The heat flow in the subsurface can be affected by seasonal and diurnal temperature variations, by radiation from the lander, its shadow, and the change in surface albedo caused by dust removal during landing and later deposition. The radiometer will observe the seasonal variation over the course of the mission. Fitting of diurnal temperature curves provides an estimate of albedo and other thermophysical properties of the near surface.

Published
2019

156. One Year of ACS/TGO Observations of the Mars Atmosphere

Author

Korablev, O. I., Montmessin, Franck, Fedorova, A. A., Trokhimovskiy, Alexander, Luginin, M., Ignatiev, N. I., Lefèvre, Franck, Shakun, A., Patrakeev, A., Belyaev, D. A., Bertaux, Jean-Loup, Olsen, Kevin, Baggio, Lucio, Alday, J., Wilson, C. F., Guerlet, S., Young, R. M. B., Millour, E., Forget, F., Grigoriev, A. V., Maslov, I., Patsaev, D., Arnold, G., Grassi, Davide, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and Cardon, Catherine

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics]
Abstract

International audience; ACS onboard the ExoMars TGO) observes the martian atmosphere, using solar occultations and nadir. Status update of the ACS results obtained during one year of observations with the emphasis on trace gases, and the major dust event will be given.

Published
2019

158. Exploring Mars' Planetary Boundary Layer with InSight

Author

Spiga, Aymeric, Banfield, D., Pla-Garcia, J., Newman, C., Murdoch, N., Lorenz, R.D., Lemmon, Mark T., Lognonne, P., Kenda, B., Garcia, R., Forget, F., Millour, E., Mueller, N., Navarro, S., Rodriguez, S., Perrin, C., and Banerdt, W.B.

Subjects
Planetenphysik, Oberfläche, Mars, Meteorologie
Abstract

How InSight is helping to understand the martian atmosphere and weather close to the surface.

Published
2019

159. Mars Atmospheric Science from NASA's InSight Lander

Author

Banfield, D., Spiga, Aymeric, Newman, C., Lorenz, R.D., Forget, F., Lemmon, M. T., Viudez-Moreira, D., Pla-Garcia, J., Teanby, N., Murdoch, N., Garcia, R., Lognonne, P., Kenda, B., Perrin, C., Rodriguez, S., Lucas, A., Kawamura, T., Mimoun, D., Karatekin, O., Lewis, S., Pike, W.T., McClean, J., Charalambous, C., Mueller, N., Millour, E., Mora-Sotomayor, L., Navarro, S., Rodriguez-Manfredi, J. -A., Torres, J., Maki, J., Smrekar, S., and Banerdt, W.B.

Subjects
Physics::Fluid Dynamics, Planetenphysik, Mars, Astrophysics::Earth and Planetary Astrophysics, Meteorologie, Astrophysics::Galaxy Astrophysics, Physics::Atmospheric and Oceanic Physics, Physics::Geophysics
Abstract

InSight carries a sophisticated Meteorological Station and has observed a dust storm, baroclinic waves, thermal tides, gravity waves, undular bores, convective vortices (with dust cleaning), infrasound, clouds and aeolian change. We report on these.

Published
2019

160. Pluto's lower atmosphere and pressure evolution from ground-based stellar occultations, 1988-2016

Author

Meza, E, Sicardy, B, Assafin, M, Ortiz, JL, Bertrand, T, Lellouch, E, Desmars, J, Forget, F, Bérard, D, Doressoundiram, A, Lecacheux, J, Oliveira, JM, Roques, F, Widemann, T, Colas, F, Vachier, F, Renner, S, Leiva, R, Braga-Ribas, F, Benedetti-Rossi, G, Camargo, JIB, Dias-Oliveira, A, Morgado, B, Gomes-Júnior, AR, Vieira-Martins, R, Behrend, R, Tirado, AC, Duffard, R, Morales, N, Santos-Sanz, P, Jelínek, M, Cunniffe, R, Querel, R, Harnisch, M, Jansen, R, Pennell, A, Todd, S, Ivanov, VD, Opitom, C, Gillon, M, Jehin, E, Manfroid, J, Pollock, J, Reichart, DE, Haislip, JB, Ivarsen, KM, LaCluyze, AP, Maury, A, Gil-Hutton, R, Dhillon, V, Littlefair, S, Marsh, T, Veillet, C, Bath, K-L, Beisker, W, Bode, H-J, Kretlow, M, Herald, D, Gault, D, Kerr, S, Pavlov, H, Faragó, O, Klös, O, Frappa, E, Lavayssière, M, Cole, AA, Giles, AB, Greenhill, JG, Hill, KM, Buie, MW, Olkin, CB, Young, EF, Young, LA, Wasserman, LH, Devogèle, M, French, RG, Bianco, FB, Marchis, F, Brosch, N, Kaspi, S, Polishook, D, Manulis, I, Larbi, MAM, Benkhaldoun, Z, Daassou, A, Azhari, YE, Moulane, Y, Broughton, J, Milner, J, Dobosz, T, Bolt, G, Lade, B, Gilmore, A, Kilmartin, P, Allen, WH, Graham, PB, Loader, B, McKay, G, Talbot, J, Parker, S, Abe, L, Bendjoya, P, Rivet, J-P, Vernet, D, Fabrizio, LD, Lorenzi, V, Magazzù, A, Molinari, E, Gazeas, K, Tzouganatos, L, Carbognani, A, Bonnoli, G, Marchini, A, Leto, G, Sanchez, RZ, Mancini, L, Kattentidt, B, Dohrmann, M, Guhl, K, Rothe, W, Walzel, K, Wortmann, G, Eberle, A, Hampf, D, Ohlert, J, Krannich, G, Murawsky, G, Gährken, B, Gloistein, D, Alonso, S, Román, A, Communal, J-E, Jabet, F, Visscher, SD, Sérot, J, Janik, T, Moravec, Z, Machado, P, Selva, A, Perelló, C, Rovira, J, Conti, M, Papini, R, Salvaggio, F, Noschese, A, Tsamis, V, Tigani, K, Barroy, P, Irzyk, M, Neel, D, Godard, JP, Lanoiselée, D, Sogorb, P, Vérilhac, D, Bretton, M, Signoret, F, Ciabattari, F, Naves, R, Boutet, M, Queiroz, JD, Lindner, P, Lindner, K, Enskonatus, P, Dangl, G, Tordai, T, Eichler, H, Hattenbach, J, Peterson, C, Molnar, LA, and Howell, RR

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Pluto's tenuous nitrogen (N2) atmosphere undergoes strong seasonal effects due to high obliquity and orbital eccentricity, and has been recently (July 2015) observed by the New Horizons spacecraft. Goals are (i) construct a well calibrated record of the seasonal evolution of surface pressure on Pluto and (ii) constrain the structure of the lower atmosphere using a central flash observed in 2015. Method: eleven stellar occultations by Pluto observed between 2002 and 2016 are used to retrieve atmospheric profiles (density, pressure, temperature) between $\sim$5 km and $\sim$380 km altitude levels (i.e. pressures from about 10 microbar to 10 nanobar). Results: (i) Pressure has suffered a monotonic increase from 1988 to 2016, that is compared to a seasonal volatile transport model, from which tight constraints on a combination of albedo and emissivity of N2 ice are derived; (ii) A central flash observed on 2015 June 29 is consistent with New Horizons REX profiles, provided that (a) large diurnal temperature variations (not expected by current models) occur over Sputnik Planitia and/or (b) hazes with tangential optical depth of about 0.3 are present at 4-7 km altitude levels and/or (c) the nominal REX density values are overestimated by an implausibly large factor of about 20% and/or (d) higher terrains block part of the flash in the Charon facing hemisphere., 21 pages, 11 figures

Published
2019

161. HP³ Radiometer Measurements from the Mars Mission InSight

Author

Mueller, N., Grott, M., Piqueux, S., Kopp, Emanuel, Spohn, T., Smrekar, S.E., Knollenberg, J., Hudson, T.L., Krause, C., Plesa, A.-C., Siegler, M.A., Spiga, Aymeric, Forget, F., Millour, E., Morgan, P., Golombek, M., and Banerdt, W.B.

Subjects
Asteroiden und Kometen, Weltrauminstrumente, Planetenphysik, Leitungsbereich PF, Mars, Messung, Oberflächentemperatur, Nutzerzentrum für Weltraumexperimente (MUSC)
Published
2019

162. Trebananib or placebo plus carboplatin and paclitaxel as first-line treatment for advanced ovarian cancer (TRINOVA-3/ENGOT-ov2/GOG-3001): a randomised, double-blind, phase 3 trial

Author

Vergote, I. Scambia, G. O'Malley, D.M. Van Calster, B. Park, S.-Y. del Campo, J.M. Meier, W. Bamias, A. Colombo, N. Wenham, R.M. Covens, A. Marth, C. Raza Mirza, M. Kroep, J.R. Ma, H. Pickett, C.A. Monk, B.J. Park, S.Y. Song, Y.S. Makarova, Y. Trinidad, J. Ngan, H.Y.S. Aravantinos, G. Nam, J.-H. Gorbunova, V. Krikunova, L. Bae, D.-S. Arija, J.A.A. Mirza, M.R. Zamagni, C. Papandreou, C. Raspagliesi, F. Lisyanskaya, A. Benzaquen, A.O. Tognon, G. Ortega, E. Herraez, A.C. Buscema, J. Green, A. Burger, R. Sakaeva, D. Sanchez, A.R. Ghamande, S. King, L. Petru, E. Peen, U. Takeuchi, S. Ushijima, K. Martin, A.G. Kamelle, S. Carney, M. Forget, F. Bentley, J. Sehouli, J. Zola, P. Kato, H. Fadeeva, N. Gotovkin, E. Vladimirov, V. Marin, M.R. Alia, E.G. Shahin, M. Bhoola, S. Tewari, K. Anderson, D. Honhon, B. Pelgrims, J.G. Oza, A. Jimenez, J.G.-D. Hansen, V. Benjamin, I. Renard, V. Van den Bulck, H. Haenle, C. Koumakis, G. Yokota, H. Popov, V. Bradley, W. Wenham, R. Reid, R. McNamara, D. Friedman, R. Barlin, J. Spirtos, N. Chapman, J. Sevelda, P. Huizing, M. Lamot, C. Goffin, F. Hondt, L.D. Covens, A. Spadafora, S. Rautenberg, B. Reimer, T. Möbus, V. Hilpert, F. Gropp-Meier, M. Savarese, A. Pignata, S. Verderame, F. Mizuno, M. Takano, H. Ottevanger, P. Velasco, A.P. Palacio-Vazquez, I. Law, A. McIntyre, K. Teneriello, M. Fields, A. Lentz, S. Street, D. Schwartz, B. Mannel, R. Lim, P. Pulaski, H. Janni, W. Zorr, A. Karck, U. Cheng, A.C.K. Sorio, R. Gridelli, C. Aoki, D. Oishi, T. Hirashima, Y. Boere, I. Ferrer, E.F. Braly, P. Wilks, S. Lee, C. Schilder, J. Veljovich, D. Secord, A. Davis, K. Rojas-Espaillat, L. Lele, S. DePasquale, S. Squatrito, R. Schauer, C. Dirix, L. Vuylsteke, P. Joosens, E. Provencher, D. Lueck, H.-J. Hein, A. Burges, A. Canzler, U. Park-Simon, T.-W. Griesinger, F. Gadducci, A. Alabiso, O. Okamoto, A. Sawasaki, T. Saito, T. Ibañez, A.H. Calomeni, C. Spillman, M. Choksi, J. Taylor, N. Muller, C. Moore, D. DiSilvestro, P. Cunningham, M. Rose, P. Oppelt, P. Verhoeven, D. Graas, M.-P. Ghatage, P. Tonkin, K. Kurzeder, C. Schnappauf, B. Müller, V. Schmalzrie, H. Kalofonos, H. Bruzzone, M. Kroep, J. Diaz, C.C. Garcia, J.M. Polo, S.H. Garrison, M. Rocconi, R. Andrews, S. Bristow, R. McHale, M. Basil, J. Houck III, W. Bell, M. Cosin, J. Modesitt, S. Kendrick, J. Wade III, J. Wong, C. Evans, A. Buekers, T. Vanderkwaak, T. Ferriss, J. Darus, C. DAndre, S. Higgins, R. Monk, B. Bakkum-Gamez, J. DeMars, L. Van Le, L. Puls, L. Trehan, S. LaPolla, J. Michelson, E.D. Merchant, J. Peterson, C. Reid, G. Seago, D. Zweizig, S. Gajewski, W. Panwalkar, A. Leikermoser, R. Bogner, G. Debruyne, P. D'hondt, R. Berteloot, P. Kerger, J. Biagi, J. Castonguay, V. Welch, S. Muhic, A. Heubner, M. Grischke, E.-M. Rack, B. Fleisch, M. Lordick, F. Pectasides, D. Ho, W.M. Selvaggi, L. Vasquez, F.M. Villanueva, W.O.B. Alavez, A.M. Kessels, L. Bertran, A.S. Fernandez, C.M. Fabregat, M.B. Del Prete, S. Elkas, J. Cecchi, G. Kumar, P. Huh, W. Messing, M. Karimi, M. Kelley, A. Edraki, B. Mutch, D. Leiserowitz, G. Anderson, J. Lentz, S. Chambers, S. Morris, R. Waggoner, S. Gordon, A. Method, M. Johnson, P. Lord, R. Drake, J. Sivarajan, K. Midathada, M. Rice, K. Wadsworth, T. Pavelka, J. Edwards, R. Miller, D.S. Ford, P.L. Hurteau, J. Bender, D. Schimp, V. Creasman, W. Lerner, R. Chamberlain, D. Kueck, A. McDonald, J. Malad, S. Robinson-Bennett, B. Davidson, S. Krivak, T. Lestingi, T. Arango, H. Berard, P. Finkelstein, K. Gaur, R. Krasner, C. Ueland, F. Talmage, L. Yamada, S. Sutton, G. Potkul, R. Prasad-Hayes, M. Osborne, J. Celano, P. Thigpen, J. Sharma, S. Schilder, R. Tammela, J. Kemeny, M. Brown, A. Eisenhauer, E. Williams, J. Rowland, K. Nahum, K. Burke, J. Dar, Z. Fleming, N. Gibb, R. Guirguis, A. Herzog, T. John, V. Kumar, S. Kamat, A. Kassar, M. Leitao, M. Levine, L. Mendez, L. Patel, D. Berry, E. Warshal, D. Wolf, J. Zarwan, C. Collins, Y. Spitzer, G. Miller, B. Einstein, M. TRINOVA-3/ENGOT-ov2/GOG-3001 investigators

Abstract

Background: Angiopoietin 1 and 2 regulate angiogenesis and vascular remodelling by interacting with the tyrosine kinase receptor Tie2, and inhibition of angiogenesis has shown promise in the treatment of ovarian cancer. We aimed to assess whether trebananib, a peptibody that inhibits binding of angiopoietin 1 and 2 to Tie2, improved progression-free survival when added to carboplatin and paclitaxel as first-line therapy in advanced epithelial ovarian, primary fallopian tube, or peritoneal cancer in a phase 3 clinical trial. Methods: TRINOVA-3, a multicentre, multinational, phase 3, double-blind study, was done at 206 investigational sites (hospitals and cancer centres)in 14 countries. Eligible patients were aged 18 years or older with biopsy-confirmed International Federation of Gynecology and Obstetrics (FIGO)stage III to IV epithelial ovarian, primary peritoneal, or fallopian tube cancers, and an ECOG performance status of 0 or 1. Eligible patients were randomly assigned (2:1)using a permuted block method (block size of six patients)to receive six cycles of paclitaxel (175 mg/m2)and carboplatin (area under the serum concentration-time curve 5 or 6)every 3 weeks, plus weekly intravenous trebananib 15 mg/kg or placebo. Maintenance therapy with trebananib or placebo continued for up to 18 additional months. The primary endpoint was progression-free survival, as assessed by the investigators, in the intention-to-treat population. Safety analyses included patients who received at least one dose of study treatment. This trial is registered with ClinicalTrials.gov, number NCT01493505, and is complete. Findings: Between Jan 30, 2012, and Feb 25, 2014, 1164 patients were screened and 1015 eligible patients were randomly allocated to treatment (678 to trebananib and 337 to placebo). After a median follow-up of 27·4 months (IQR 17·7–34·2), 626 patients had progression-free survival events (405 [60%]of 678 in the trebananib group and 221 [66%]of 337 in the placebo group). Median progression-free survival did not differ between the trebananib group (15·9 months [15·0–17·6])and the placebo group (15·0 months [12·6–16·1])groups (hazard ratio 0·93 [95% CI 0·79–1·09]; p=0·36). 512 (76%)of 675 patients in the trebananib group and 237 (71%)of 336 in the placebo group had grade 3 or worse treatment-emergent adverse events; of which the most common events were neutropenia (trebananib 238 [35%]vs placebo 126 [38%])anaemia (76 [11%]vs 40 [12%]), and leucopenia (81 [12%]vs 35 [10%]). 269 (40%)patients in the trebananib group and 104 (31%)in the placebo group had serious adverse events. Two fatal adverse events in the trebananib group were considered related to trebananib, paclitaxel, and carboplatin (lung infection and neutropenic colitis); two were considered to be related to paclitaxel and carboplatin (general physical health deterioration and platelet count decreased). No treatment-related fatal adverse events occurred in the placebo group. Interpretation: Trebananib plus carboplatin and paclitaxel did not improve progression-free survival as first-line treatment for advanced ovarian cancer. The combination of trebananib plus carboplatin and paclitaxel did not produce new safety signals. These results show that trebananib in combination with carboplatin and paclitaxel is minimally effective in this patient population. Funding: Amgen. © 2019 Elsevier Ltd

Published
2019

163. The Latest Mars Climate Database (Version 6.0)

Author

Millour, E., Forget, F., Spiga, A., Vals, M., Zakharov, V., Montabone, L., Lefèvre, F., Montmessin, Franck, Chaufray, Jean-Yves, López-Valverde, M. A., González-Galindo, F., Lewis, S. R., Read, P., Desjean, M. -C., and Cipriani, F.

Abstract

Ninth International Conference on Mars, held 22-25 July, 2019 in Pasadena, California. LPI Contribution No. 2089, id.6171, The Mars Climate Database (MCD) is a database of meteorological fields derived from General Circulation Model (GCM) numerical simulations of the martian atmosphere and validated using available observational data.

Published
2019

164. Lower atmosphere and pressure evolution on Pluto from ground-based stellar occultations, 1988-2016

Author

Meza, E. Sicardy, B. Assafin, M. Ortiz, J.L. Bertrand, T. Lellouch, E. Desmars, J. Forget, F. Bérard, D. Doressoundiram, A. Lecacheux, J. Marques Oliveira, J. Roques, F. Widemann, T. Colas, F. Vachier, F. Renner, S. Leiva, R. Braga-Ribas, F. Benedetti-Rossi, G. Camargo, J.I.B. Dias-Oliveira, A. Morgado, B. Gomes-Júnior, A.R. Vieira-Martins, R. Behrend, R. Castro Tirado, A. Duffard, R. Morales, N. Santos-Sanz, P. Jelínek, M. Cunniffe, R. Querel, R. Harnisch, M. Jansen, R. Pennell, A. Todd, S. Ivanov, V.D. Opitom, C. Gillon, M. Jehin, E. Manfroid, J. Pollock, J. Reichart, D.E. Haislip, J.B. Ivarsen, K.M. LaCluyze, A.P. Maury, A. Gil-Hutton, R. Dhillon, V. Littlefair, S. Marsh, T. Veillet, C. Bath, K.-L. Beisker, W. Bode, H.-J. Kretlow, M. Herald, D. Gault, D. Kerr, S. Pavlov, H. Faragó, O. Klös, O. Frappa, E. Lavayssière, M. Cole, A.A. Giles, A.B. Greenhill, J.G. Hill, K.M. Buie, M.W. Olkin, C.B. Young, E.F. Young, L.A. Wasserman, L.H. Devogèle, M. French, R.G. Bianco, F.B. Marchis, F. Brosch, N. Kaspi, S. Polishook, D. Manulis, I. Ait Moulay Larbi, M. Benkhaldoun, Z. Daassou, A. El Azhari, Y. Moulane, Y. Broughton, J. Milner, J. Dobosz, T. Bolt, G. Lade, B. Gilmore, A. Kilmartin, P. Allen, W.H. Graham, P.B. Loader, B. McKay, G. Talbot, J. Parker, S. Abe, L. Bendjoya, P. Rivet, J.-P. Vernet, D. Di Fabrizio, L. Lorenzi, V. Magazzú, A. Molinari, E. Gazeas, K. Tzouganatos, L. Carbognani, A. Bonnoli, G. Marchini, A. Leto, G. Zanmar Sanchez, R. Mancini, L. Kattentidt, B. Dohrmann, M. Guhl, K. Rothe, W. Walzel, K. Wortmann, G. Eberle, A. Hampf, D. Ohlert, J. Krannich, G. Murawsky, G. Gährken, B. Gloistein, D. Alonso, S. Román, A. Communal, J.-E. Jabet, F. DeVisscher, S. Sérot, J. Janik, T. Moravec, Z. MacHado, P. Selva, A. Perelló, C. Rovira, J. Conti, M. Papini, R. Salvaggio, F. Noschese, A. Tsamis, V. Tigani, K. Barroy, P. Irzyk, M. Neel, D. Godard, J.P. Lanoiselée, D. Sogorb, P. Vérilhac, D. Bretton, M. Signoret, F. Ciabattari, F. Naves, R. Boutet, M. De Queiroz, J. Lindner, P. Lindner, K. Enskonatus, P. Dangl, G. Tordai, T. Eichler, H. Hattenbach, J. Peterson, C. Molnar, L.A. Howell, R.R.

Abstract

Context. The tenuous nitrogen (N2) atmosphere on Pluto undergoes strong seasonal effects due to high obliquity and orbital eccentricity, and has recently (July 2015) been observed by the New Horizons spacecraft. Aims. The main goals of this study are (i) to construct a well calibrated record of the seasonal evolution of surface pressure on Pluto and (ii) to constrain the structure of the lower atmosphere using a central flash observed in 2015. Methods. Eleven stellar occultations by Pluto observed between 2002 and 2016 are used to retrieve atmospheric profiles (density, pressure, temperature) between altitude levels of ∼5 and ∼380 km (i.e. pressures from ∼10 μbar to 10 nbar). Results. (i) Pressure has suffered a monotonic increase from 1988 to 2016, that is compared to a seasonal volatile transport model, from which tight constraints on a combination of albedo and emissivity of N2 ice are derived. (ii) A central flash observed on 2015 June 29 is consistent with New Horizons REX profiles, provided that (a) large diurnal temperature variations (not expected by current models) occur over Sputnik Planitia; and/or (b) hazes with tangential optical depth of ∼0.3 are present at 4-7 km altitude levels; and/or (c) the nominal REX density values are overestimated by an implausibly large factor of ∼20%; and/or (d) higher terrains block part of the flash in the Charon facing hemisphere. © E. Meza et al. 2019.

Published
2019

167. 220P Elacestrant vs fulvestrant or aromatase inhibitor (AI) in phase III trial evaluating elacestrant, an oral selective estrogen receptor degrader (SERD), vs standard of care (SOC) endocrine monotherapy for ER+/HER2- advanced/metastatic breast cancer (mBC): Subgroup analysis from EMERALD

Author

Aftimos, P.G., Cortés, J., Bidard, F.C., V. Kaklamani, Bardia, A., Neven, P., Streich, G., Montero, A., Forget, F., Mouret Reynier, M.A., Sohn, J., Taylor, D., Harnden, K., Khong, H., Kocsis, J., Dalenc, F., Dillon, P., Tonini, G., Grzegorzewski, K.J., and Lu, J.

Published
2022
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168. DYNAMO: a Mars upper atmosphere package for investigating solar wind interaction and escape processes, and mapping Martian fields

Author

Chassefière, E., Nagy, A., Mandea, M., Primdahl, F., Rème, H., Sauvaud, J.-A., Lin, R., Barabash, S., Mitchell, D., Zurbuchen, T., Leblanc, F., Berthelier, J.-J., Waite, H., Young, D.T., Clarke, J., Parrot, M., Trotignon, J.-G., Bertaux, J.-L., Quèmerais, E., Barlier, F., Szegö, K., Szalaı̈, S., Bougher, S., Forget, F., Lilensten, J., Barriot, J.-P., Chanteur, G., Luhmann, J., Hulot, G., Purucker, M., Breuer, D., Smrekar, S., Jakosky, B., Menvielle, M., Sasaki, S., Acuna, M., Keating, G., Touboul, P., Gérard, J.-C., Rochus, P., Orsini, S., Cerutti-Maori, G., Porteneuve, J., Meftah, M., and Malique, Ch.

Published
2004
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169. Antibacterial and antifungal activity of defensins from the Australian paralysis tick, Ixodes holocyclus

Author

Cabezas-Cruz, A., Tonk, M., Bleackley, M.R., Valdés, J.J, Barrero, R.A., Hernández-Jarguín, A., Moutailler, S., Vilcinskas, A., Richard-Forget, F., Anderson, M.A., Rodriguez-Valle, M., Cabezas-Cruz, A., Tonk, M., Bleackley, M.R., Valdés, J.J, Barrero, R.A., Hernández-Jarguín, A., Moutailler, S., Vilcinskas, A., Richard-Forget, F., Anderson, M.A., and Rodriguez-Valle, M.

Abstract

Tick innate immunity involves humoral and cellular responses. Among the humoral effector molecules in ticks are the defensins which are a family of small peptides with a conserved γ-core motif that is crucial for their antimicrobial activity. Defensin families have been identified in several hard and soft tick species. However, little is known about the presence and antimicrobial activity of defensins from the Australian paralysis tick Ixodes holocyclus. In this study the I. holocyclus transcriptome was searched for the presence of defensins. Unique and non-redundant defensin sequences were identified and designated as holosins 1 – 5. The antimicrobial activity of holosins 2 and 3 and of the predicted γ-cores of holosins 1–4 (HoloTickCores 1–4), was assessed using Gram-negative and Gram-positive bacteria as well as the fungus Fusarium graminearum and the yeast Candida albicans. All holosins had molecular features that are conserved in other tick defensins. Furthermore holosins 2 and 3 were very active against the Gram-positive bacteria Staphylococcus aureus and Listeria grayi. Holosins 2 and 3 were also active against F. graminearum and C. albicans and 5 μM of peptide abrogate the growth of these microorganisms. The activity of the synthetic γ-cores was lower than that of the mature defensins apart from HoloTickCore 2 which had activity comparable to mature holosin 2 against the Gram-negative bacterium Escherichia coli. This study reveals the presence of a multigene defensin family in I. holocyclus with wide antimicrobial activity.

Published
2019

170. Global spatial risk assessment of sharks under the footprint of fisheries

Author

Queiroz, N., Humphries, N.E., Couto, A., Vedor, M., da Costa, I., Sequeira, A.M.M., Mucientes, G., Santos, A.M., Abascal, F.J., Abercrombie, D.L., Abrantes, K., Acuña-Marrero, D., Afonso, A.S., Afonso, P., Anders, D., Araujo, G., Arauz, R., Bach, P., Barnett, A., Bernal, D., Berumen, M.L., Bessudo Lion, S., Bezerra, N.P.A., Blaison, A.V., Block, B.A., Bond, M.E., Bonfil, R., Bradford, R.W., Braun, C.D., Brooks, E.J., Brooks, A., Brown, J., Bruce, B.D., Byrne, M.E., Campana, S.E., Carlisle, A.B., Chapman, D.D., Chapple, T.K., Chisholm, J., Clarke, C.R., Clua, E.G., Cochran, J.E.M., Crochelet, E.C., Dagorn, L., Daly, R., Cortés, D.D., Doyle, T.K., Drew, M., Duffy, C.A.J., Erikson, T., Espinoza, E., Ferreira, L.C., Ferretti, F., Filmalter, J.D., Fischer, G.C., Fitzpatrick, R., Fontes, J., Forget, F., Fowler, M., Francis, M.P., Gallagher, A.J., Gennari, E., Goldsworthy, S.D., Gollock, M.J., Green, J.R., Gustafson, J.A., Guttridge, T.L., Guzman, H.M., Hammerschlag, N., Harman, L., Hazin, F.H.V., Heard, M., Hearn, A.R., Holdsworth, J.C., Holmes, B.J., Howey, L.A., Hoyos, M., Hueter, R.E., Hussey, N.E., Huveneers, C., Irion, D.T., Jacoby, D.M.P., Jewell, O.J.D., Johnson, R., Jordan, L.K.B., Jorgensen, S.J., Joyce, W., Keating Daly, C.A., Ketchum, J.T., Klimley, A.P., Kock, A.A., Koen, P., Ladino, F., Lana, F.O., Lea, J.S.E., Llewellyn, F., Lyon, W.S., MacDonnell, A., Macena, B.C.L., Marshall, H., McAllister, J.D., McAuley, R., Meÿer, M.A., Morris, J.J., Nelson, E.R., Papastamatiou, Y.P., Patterson, T.A., Peñaherrera-Palma, C., Pepperell, J.G., Pierce, S.J., Poisson, F., Quintero, L.M., Richardson, A.J., Rogers, P.J., Rohner, C.A., Rowat, D.R.L., Samoilys, M., Semmens, J.M., Sheaves, M., Shillinger, G., Shivji, M., Singh, S., Skomal, G.B., Smale, M.J., Snyders, L.B., Soler, G., Soria, M., Stehfest, K.M., Stevens, J.D., Thorrold, S.R., Tolotti, M.T., Towner, A., Travassos, P., Tyminski, J.P., Vandeperre, F., Vaudo, J.J., Watanabe, Y.Y., Weber, S.B., Wetherbee, B.M., White, T.D., Williams, S., Zárate, P.M., Harcourt, R., Hays, G.C., Meekan, M.G., Thums, M., Irigoien, X., Eguíluz, V.M., Duarte, C.M., Sousa, L.L., Simpson, S.J., Southall, E.J., Sims, D.W., Queiroz, N., Humphries, N.E., Couto, A., Vedor, M., da Costa, I., Sequeira, A.M.M., Mucientes, G., Santos, A.M., Abascal, F.J., Abercrombie, D.L., Abrantes, K., Acuña-Marrero, D., Afonso, A.S., Afonso, P., Anders, D., Araujo, G., Arauz, R., Bach, P., Barnett, A., Bernal, D., Berumen, M.L., Bessudo Lion, S., Bezerra, N.P.A., Blaison, A.V., Block, B.A., Bond, M.E., Bonfil, R., Bradford, R.W., Braun, C.D., Brooks, E.J., Brooks, A., Brown, J., Bruce, B.D., Byrne, M.E., Campana, S.E., Carlisle, A.B., Chapman, D.D., Chapple, T.K., Chisholm, J., Clarke, C.R., Clua, E.G., Cochran, J.E.M., Crochelet, E.C., Dagorn, L., Daly, R., Cortés, D.D., Doyle, T.K., Drew, M., Duffy, C.A.J., Erikson, T., Espinoza, E., Ferreira, L.C., Ferretti, F., Filmalter, J.D., Fischer, G.C., Fitzpatrick, R., Fontes, J., Forget, F., Fowler, M., Francis, M.P., Gallagher, A.J., Gennari, E., Goldsworthy, S.D., Gollock, M.J., Green, J.R., Gustafson, J.A., Guttridge, T.L., Guzman, H.M., Hammerschlag, N., Harman, L., Hazin, F.H.V., Heard, M., Hearn, A.R., Holdsworth, J.C., Holmes, B.J., Howey, L.A., Hoyos, M., Hueter, R.E., Hussey, N.E., Huveneers, C., Irion, D.T., Jacoby, D.M.P., Jewell, O.J.D., Johnson, R., Jordan, L.K.B., Jorgensen, S.J., Joyce, W., Keating Daly, C.A., Ketchum, J.T., Klimley, A.P., Kock, A.A., Koen, P., Ladino, F., Lana, F.O., Lea, J.S.E., Llewellyn, F., Lyon, W.S., MacDonnell, A., Macena, B.C.L., Marshall, H., McAllister, J.D., McAuley, R., Meÿer, M.A., Morris, J.J., Nelson, E.R., Papastamatiou, Y.P., Patterson, T.A., Peñaherrera-Palma, C., Pepperell, J.G., Pierce, S.J., Poisson, F., Quintero, L.M., Richardson, A.J., Rogers, P.J., Rohner, C.A., Rowat, D.R.L., Samoilys, M., Semmens, J.M., Sheaves, M., Shillinger, G., Shivji, M., Singh, S., Skomal, G.B., Smale, M.J., Snyders, L.B., Soler, G., Soria, M., Stehfest, K.M., Stevens, J.D., Thorrold, S.R., Tolotti, M.T., Towner, A., Travassos, P., Tyminski, J.P., Vandeperre, F., Vaudo, J.J., Watanabe, Y.Y., Weber, S.B., Wetherbee, B.M., White, T.D., Williams, S., Zárate, P.M., Harcourt, R., Hays, G.C., Meekan, M.G., Thums, M., Irigoien, X., Eguíluz, V.M., Duarte, C.M., Sousa, L.L., Simpson, S.J., Southall, E.J., and Sims, D.W.

Abstract

Brucellosis is a highly contagious zoonosis affecting humans and a wide range of domesticated and wild animal species. An important element for effective disease containment is to improve knowledge, attitudes and practices (KAP) of afflicted communities. This study aimed to assess the KAP related to brucellosis at the human–animal interface in an endemic area of Egypt and to identify the risk factors for human infection. A matched case–control study was conducted at the central fever hospitals located in six governorates in northern Egypt. Face‐to‐face interviews with cases and controls were conducted using a structured questionnaire. In total, 40.7% of the participants owned farm animals in their households. The overall mean practice score regarding animal husbandry, processing and consumption of milk and dairy products were significantly lower among cases compared with controls (−12.7 ± 18.1 vs. 0.68 ± 14.2, respectively; p < .001). Perceived barriers for notification of animal infection/abortion were predominate among cases and positively correlated with participants’ education. The predictors of having brucellosis infection were consumption of unpasteurized milk or raw dairy products and practicing animal husbandry. Applying protective measures against infection significantly reduced its risk. A model predicting risk factors for brucellosis among those who own animal showed that frequent abortions per animal increased the chance for brucellosis infection among human cases by 50‐fold (95% CI: 8.8–276.9), whereas the use of protective measures in animal care reduced the odds (OR = 0.11 [95% CI: 0.03–0.45]). In conclusion, consumption of unprocessed dairy products was equally important as contact with infected/aborted animals as major risk factors for Brucella spp. infection among humans in Egypt. There is poor knowledge, negative attitudes and risky behaviours among villagers which can perpetuate the risk of brucellosis transmission at the human–animal interface.

Published
2019

171. Modeling wind-driven ionospheric dynamo currents at Mars: expectations for insight magnetic field measurements

Author

National Aeronautics and Space Administration (US), Consejo Superior de Investigaciones Científicas (España), Ministerio de Ciencia, Innovación y Universidades (España), Centre National de la Recherche Scientifique (France), Lillis, R.J., Fillingim, M.O., Ma, Y., González-Galindo, F., Forget, F., Johnson, C.L., Mittelholz, A., Russell, C.T., Andersson, L., Fowler, C.M., National Aeronautics and Space Administration (US), Consejo Superior de Investigaciones Científicas (España), Ministerio de Ciencia, Innovación y Universidades (España), Centre National de la Recherche Scientifique (France), Lillis, R.J., Fillingim, M.O., Ma, Y., González-Galindo, F., Forget, F., Johnson, C.L., Mittelholz, A., Russell, C.T., Andersson, L., and Fowler, C.M.

Abstract

We model expected dynamo currents above, and resulting magnetic field profiles at, InSight's landing site on Mars, including for the first time the effect of electron-ion collisions. We calculate their diurnal and seasonal variability using inputs from global models of the Martian thermosphere, ionosphere, and magnetosphere. Modeled currents primarily depend on plasma densities and the strength of the neutral wind component perpendicular to the combined crustal and draped magnetic fields that thread the ionosphere. Negligible at night, currents are the strongest in the late morning and near solstices due to stronger winds and near perihelion due to both stronger winds and higher plasma densities from solar EUV photoionization. Resulting surface magnetic fields of tens of nanotesla and occasionally >100 nT may be expected at the InSight landing site. We expect currents and surface fields to vary significantly with changes in the draped magnetic field caused by Mars' dynamic solar wind environment. ©2019. American Geophysical Union. All Rights Reserved.

Published
2019

172. Mars' Background Free Oscillations

Author

Schimmel, Martin [0000-0003-2601-4462], Nishikawa, J., Lognonné, P., Kawamura, T., Spiga, A., Stutzmann, E., Schimmel, Martin, Bertrand, T., Forget, F., Kurita, K., Schimmel, Martin [0000-0003-2601-4462], Nishikawa, J., Lognonné, P., Kawamura, T., Spiga, A., Stutzmann, E., Schimmel, Martin, Bertrand, T., Forget, F., and Kurita, K.

Abstract

Observations and inversion of the eigenfrequencies of free oscillations constitute powerful tools to investigate the internal structure of a planet. On Mars, such free oscillations can be excited by atmospheric pressure and wind stresses from the Martian atmosphere, analogous to what occurs on Earth. Over long periods and on a global scale, this phenomenon may continuously excite Mars' background free oscillations (MBFs), which constitute the so-called Martian hum. However, the source exciting MBFs is related both to the global-scale atmospheric circulation on Mars and to the variations in pressure and wind at the planetary boundary layer, for which no data are available.To overcome this drawback, we focus herein on a global-scale source and use results of simulations based on General Circular Models (GCMs). GCMs can predict and reproduce long-term, global-scale Martian pressure and wind variations and suggest that, contrary to what happens on Earth, daily correlations in the Martian hum might be generated by the solar-driven GCM. After recalling the excitation terms, we calculate MBFs by using GCM computations and estimate the contribution to the hum made by the global atmospheric circulation. Although we work at the lower limit of MBF signals, the results indicate that the signal is likely to be periodic, which would allow us to use more efficient stacking theories than can be applied to Earth's hum. We conclude by discussing the perspectives for the InSight SEIS instrument to detect the Martian hum. The amplitude of the MBF signal is on the order of nanogals and is therefore hidden by instrumental and thermal noise, which implies that, provided the predicted daily coherence in hum excitation is present, the InSight SEIS seismometer should be capable of detecting the Martian hum after monthly to yearly stacks.

Published
2019

173. ExoMars Atmospheric Mars Entry and Landing Investigations and Analysis (AMELIA)

Author

Ferri, F., Karatekin, Ö., Lewis, S., Forget, F., Aboudan, A., Colombatti, G., Bettanini, C., Debei, S., Van Hove, B., Dehant, V., Harri, A., Leese, M., Mäkinen, T., Millour, E., Muller-Wodarg, I., Ori, G., Pacifici, A., Paris, S., Patel, M., Schoenenberger, M., Herath, J., Siili, T., Spiga, A., Tokano, T., Towner, Martin, Withers, P., Asmar, S., Plettemeier, D., Ferri, F., Karatekin, Ö., Lewis, S., Forget, F., Aboudan, A., Colombatti, G., Bettanini, C., Debei, S., Van Hove, B., Dehant, V., Harri, A., Leese, M., Mäkinen, T., Millour, E., Muller-Wodarg, I., Ori, G., Pacifici, A., Paris, S., Patel, M., Schoenenberger, M., Herath, J., Siili, T., Spiga, A., Tokano, T., Towner, Martin, Withers, P., Asmar, S., and Plettemeier, D.

Abstract

The entry, descent and landing of Schiaparelli, the ExoMars Entry, descent and landing Demonstrator Module (EDM), offered a rare (once-per-mission) opportunity for in situ investigations of the martian environment over a wide altitude range. The aim of the ExoMars AMELIA experiment was to exploit the Entry, Descent and Landing System (EDLS) engineering measurements for scientific investigations of Mars’ atmosphere and surface. Here we present the simulations, modelling and the planned investigations prior to the Entry, Descent and Landing (EDL) event that took place on 19th October 2016. Despite the unfortunate conclusion of the Schiaparelli mission, flight data recorded during the entry and the descent until the loss of signal, have been recovered. These flight data, although limited and affected by transmission interruptions and malfunctions, are essential for investigating the anomaly and validating the EDL operation, but can also contribute towards the partial achievement of AMELIA science objectives.

Published
2019

174. Near Surface Properties of Martian Regolith Derived From InSight HP3‐RAD Temperature Observations During Phobos Transits.

Author

Mueller, N., Piqueux, S., Lemmon, M., Maki, J., Lorenz, R. D., Grott, M., Spohn, T., Smrekar, S. E., Knollenberg, J., Hudson, T. L., Krause, C., Millour, E., Forget, F., Golombek, M., Hagermann, A., Attree, N., Siegler, M., and Banerdt, W. B.

Subjects
MARTIAN surface, SURFACE properties, REGOLITH, THERMAL conductivity, SURFACE temperature, THERMAL properties
Abstract

We use the Martian surface temperature response to Phobos transits observed next to the InSight lander in Elysium Planitia to constrain the thermal properties of the uppermost layer of regolith. Modeled transit lightcurves validated by solar panel current measurements are used to modify the boundary conditions of a 1D heat conduction model. We test several model parameter sets, varying the thickness and thermal conductivity of the top layer to explore the range of parameters that match the observed temperature response within its uncertainty both during the eclipse as well as the full diurnal cycle. The measurements indicate a thermal inertia (TI) of 103−16+22Jm−2K−1s−1/2 in the uppermost layer of 0.2–4 mm, significantly smaller than the TI of 200Jm−2K−1s−1/2 derived from the diurnal temperature curve. This could be explained by larger particles, higher density, or some or slightly higher amount of cementation in the lower layers. Plain Language Summary: The Mars moon Phobos passed in front of the Sun from the perspective of the InSight lander on several occasions. The Mars surface temperatures measured by the lander became slightly colder during these transits due to the lower amount of sunlight the surface received at this time. The transits only last 20–35 s and therefore only the very top layer, about 0.3–0.8 mm, of the ground has time to cool significantly. The top layer cools and heats up faster than we expected based on the temperature changes of the day‐night cycle, which affects about 4 cm of the ground. Based on this observation we conclude that the material in the top mm of the ground is different from that below. A possible explanation would be an increase of density with depth, a larger fraction of smaller particles such as dust at the top, or a layer where particles are slightly cemented together beginning at 0.2–4 mm below the surface. Key Points: The Martian surface temperature response to Phobos transits at the InSight landing site is interpretedThe thermal inertia of the uppermost layer of soil is 103−16+22Jm−2K−1s−1/2The thermal conductivity or density of the top 0.2–4 mm is significantly less than that of the top 4 cm [ABSTRACT FROM AUTHOR]

Published
2021
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175. Spatial Variation of Methane and Other Trace Gases Detected on Mars: Interpretation with a General Circulation Model

Author

Forget, F, Haberle, B, and Montmessin, F

Subjects
Lunar And Planetary Science And Exploration
Abstract

Several teams have recently reported the detection of methane in the Martian atmosphere [1-3]. Although the detection is at the limit of the instrument capacities, one of the most surprising findings by some of these teams is the apparent strong spatial variations observed in spite of the fact that a gas like methane was expected to have a relatively long lifetime in the Martian atmosphere and thus be well mixed. To better quantitatively understand how such spatial variations can form on Mars, we have performed multiple realistic 3D general circulation model simulations in which gases with different sources, lifetime or sinks are released and transported in the Martian atmosphere.

Published
2005

176. High LMD GCM Resolution Modeling of the Seasonal Evolution of the Martian Northern Permanent Cap: Comparison with Mars Express OMEGA Observations

Author

Levrard, B, Forget, F, Montmessin, F, Schmitt, B, Doute, S, Langevin, Y, Poulet, F, Bibring, J. P, and Gondet, B

Subjects
Lunar And Planetary Science And Exploration
Abstract

Analyses of imaging data from Mariner, Viking and MGS have shown that surface properties (albedo, temperature) of the northern cap present significant differences within the summer season and between Mars years. These observations include differential brightening and/or darkening between polar areas from the end of the spring to midsummer. These differences are attributed to changes in grain size or dust content of surface ice. To better understand the summer behavior of the permanent northern polar cap, we perfomed a high resolution modeling (approximately 1 deg x 1 deg.) of northern cap in the Martian Climate/water cycle as simulated by the Laboratoire de Meteorologie Dynamique (LMD) global climate model. We compare the predicted properties of the surface ice (ice thickness, temperature) with the Mars Express Omega summer observations of the northern cap. albedo and thermal inertia svariations model. In particular, albedo variations could be constrained by OMEGA data. Meteorological predictions of the LMD GCM wil be presented at the conference to interpret the unprecedently resolved OMEGA observations. The specific evolution of regions of interest (cap center, Chasma Boreal...) and the possibility of late summer global cap brightening will be discussed.

Published
2005

177. Mars Water Ice and Carbon Dioxide Seasonal Polar Caps: GCM Modeling and Comparison with Mars Express Omega Observations

Author

Forget, F, Levrard, B, Montmessin, F, Schmitt, B, Doute, S, Langevin, Y, and Bibring, J. P

Subjects
Lunar And Planetary Science And Exploration
Abstract

To better understand the behavior of the Mars CO2 ice seasonal polar caps, and in particular interpret the the Mars Express Omega observations of the recession of the northern seasonal cap, we present some simulations of the Martian Climate/CO2 cycle/ water cycle as modeled by the Laboratoire de Meteorologie Dynamique (LMD) global climate model.

Published
2005

178. A GCM Recent History of Northern Martian Polar Layered Deposits: Contribution from Past Equatorial Ice Reservoirs

Author

Levrard, B, Laskar, J, Montmessin, F, and Forget, F

Subjects
Lunar And Planetary Science And Exploration
Abstract

Polar layered deposits are exposed in the walls of the troughs cutting the north polar cap of Mars. They consist of alternating ice and dust layers or layers of an ice-dust mixture with varying proportions and are found throughout the cap. Layers thickness ranges from meters to several tens of meters with an approximately 30 meter dominant wavelength. Although their formation processes is not known, they are presumed to reflect changes in ice and dust stability over orbital and axial variations. Intensive 3-D LMD GCM simulations of the martian water cycle have been thus performed to determine the annual rates of exchange of surface ice between the northern cap and tropical areas for a wide range of obliquity and orbital parameters values.These rates have been employed to reconstruct an history of the northern cap and test simple models of dust-ice layers formation over the last 10 Ma orbital variations. We use the 3-D water cycle model simulated by the 3-D LMD GCM with an intermediate grid resolution (7.5 longitude x 5.625 latitude) and 25 vertical levels. The dust opacity is constant and set to 0,15. No exchange of ice with regolith is allowed. The evolution of the northern cap over obliquity and orbital changes (eccentricity, Longitude of perihelion) has been recently described with this model. High summer insolation favors transfer of ice from the northern pole to the Tharsis and Olympus Montes, while at low obliquity, unstable equatorial ice is redeposited in high-latitude and polar areas of both hemisphere. The disappearance of the equatorial ice reservoir leads to a poleward recession of icy high latitude reservoirs, providing an additional source for the cap accumulation during each obliquity or orbital cycle. Furthering the efforts, a quantitative evolution of ice reservoirs is here investigated for various astronomical conditions.

Published
2005

180. GCM Simulations of Tropical Ice Accumulations: Implications for Cold-based Glaciers

Author

Haberle, R. M, Montmessin, F, Forget, F, Levrard, B, Head, J. W., III, and Laskar, J

Subjects
Lunar And Planetary Science And Exploration
Abstract

Each of the three Tharsis Montes shield volcanoes on Mars has fan-shaped deposits on their flanks. A detailed analysis of the multiple facies of the Arsia Mons deposits, coupled with field observations of polar glaciers in Antarctica, shows that they are consistent with deposition from cold-based mountain glaciers. Key features of these glaciers are: (1) they formed only on the western flank of each volcano, (2) enough ice accumulated to cause them to flow but without basal melting, (3) there were multiple advances and retreats, (4) the last major glaciation was more than several million years ago, (5) the areal extent of the deposits they left behind decreases northward, (6) together the deposits range in elevation from a low of 1.5 to a high of 8.5 km, and (7) there are no signs that significant accumulation is occurring today.

Published
2004

181. Formation of Gullies on Mars: What Do We Learn from Earth?

Author

Mangold, N, Costard, F, Forget, F, and Baratoux, D

Subjects
Lunar And Planetary Science And Exploration
Abstract

The observation of gullies on Mars indicates the presence of liquid water in recent times [1]. They have been proposed to result of subsurface seepage of water [1], geothermal activity [2] or brines [3], near-surface ice melting at recent periods of high obliquity [4], snowmelt in more recent periods [5] or liquid CO2 breakout [6]. In this study, we describe how terrestrial studies help to understand better the formation of Martian gullies. We show that all characteristics of Martian gullies are consistent with some external process triggered by seasonal melting at high obliquity.

Published
2003

182. Obliquity Driven Climate Change in Mars' Recent Past

Author

Haberle, R. M, Montmessin, F, Forget, F, Spiga, A, and Colaprete, A

Subjects
Lunar And Planetary Science And Exploration
Abstract

Mars has a natural mechanism for experiencing significant climate change and redistributing surface ice. Obliquity changes alone are quite capable of moving ice into low latitudes and may provide an explanation for the many geological landforms that strongly indicate recent climate change.

Published
2003

183. A GCM Recent History of the Northern Martian Polar Layered Deposits

Author

Levrard, B, Laskar, J, Forget, F, and Montmessin, F

Subjects
Lunar And Planetary Science And Exploration
Abstract

The polar layered deposits are thought to contain alternate layers of water and dust in different proportions resulting from the astronomical forcing of the martian climate. In particular, longterm variations in the orbital and axial elements of Mars are presumed to generate variations of the latitudes of surface water ice stability and of the amount of water exchanged in the polar areas. At high obliquity, simplified climate models and independent general circulation simulations suggest a transfer of water ice from the north polar region to tropical areas, whereas at lower and present obliquities, water ice is expected to be stable only at the poles. If so, over obliquity cycles, water ice may be redistributed between the surface water reservoirs leading to their incremental building or disintegration depending on the rates of water transfer. If only a relative limited amount of the available water is exchanged on orbital timescales, this may provide an efficient mechanism for the formation of the observed polar deposits. Within this context, GCM simulations of the martian water cycle have been performed for various obliquities ranging from 15 degrees to 45 degrees and for a large set of initial water ice locations to determine the rate of water exchange between the surface water reservoirs as a function of the obliquity. Propagating these rates over the last 10 Ma orbital history gives a possible recent evolution of these reservoirs.

Published
2003

184. 3D Simulations of the Early Mars Climate with a General Circulation Model

Author

Forget, F, Haberle, R. M, Montmessin, F, Cha, S, Marcq, E, Schaeffer, J, and Wanherdrick, Y

Subjects
Lunar And Planetary Science And Exploration
Abstract

The environmental conditions that existed on Mars during the Noachian period are subject to debate in the community. In any case, there are compelling evidence that these conditions were different than what they became later in the amazonian and possibly the Hesperian periods. Indeed, most of the old cratered terrains are disected by valley networks (thought to have been carved by flowing liquid water), whereas younger surface are almost devoid of such valleys. In addition, there are evidence that the erosion rate was much higher during the early noachian than later. Flowing water is surprising on early Mars because the solar luminosity was significantly lower than today. Even with the thick atmosphere (up to several bars).To improve our understanding of the early Mars Climate, we have developed a 3D general circulation model similar to the one used on current Earth or Mars to study the details of the climate today. Our first objective is to answer the following questions : how is the Martian climate modified if 1) the surface pressure is increased up to several bars (our baseline: 2 bars) and 2) if the sun luminosity is decreased by 25 account the heat possibly released by impacts during short periods, although it may have played a role .For this purpose, we have coupled the Martian General Circulation model developed at LMD with a sophisticated correlated k distribution model developped at NASA Ames Research Center. It is a narrow band model which computes the radiative transfer at both solar and thermal wavelengths (from 0.3 to 250 microns).

Published
2003

185. Describing the Components of the Water Transport in the Martian Atmosphere

Author

Montmessin, F, Haberle, R. M, forget, F, Rannou, P, and Cabane, M

Subjects
Lunar And Planetary Science And Exploration
Abstract

In this paper, we examine the meteorological components driving water transport in the Martian atmosphere. A particular emphasis is given to the role of residual mean circulation and water ice clouds in determining the geographical partitioning of water vapor and frost.

Published
2003

187. Monitoring of the atmosphere of Mars with ACS TIRVIM nadir observations on ExoMars TGO

Author

Ignatiev, N., Grigoriev, A., Shakun, A., Moshkin, B., Patsaev, D., Trokhimovskiy, A., Korablev, O., Grassi, D., Vlasov, P., Zazova, L., Guerlet, S., Forget, F., Montmessin, F, Arnold, Gabriele, Sazonov, O., Zharkov, A., Maslov, I., Kungurov, A., Santos-Skripo, A., Shashkin, V., Martynovich, F., Stupin, I., Merzlyakov, A., Nikolskiy, Y., Gorinov, D., and De Sanctis, M.C.

Subjects
atmosphere, Leitungsbereich PF, TGO, Mars, ACS, climate, ExoMars, TIRVIM
Abstract

The ExoMars Trace Gas Orbiter (TGO), a mission by ESA and Roscosmos started its operational scientific phase in March 2018. The Atmospheric Chemistry Suite (ACS) is a set of three spectrometers (NIR, MIR, and TIRVIM) designed to observe the Martian atmosphere in solar occultation, nadir and limb geometry [1]. The thermal infrared channel — TIRVIM is a Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm, with the best spectral resolution 0.13 cm−1. In nadir operation mode, the primary goal of TIRVIM is the long-term monitoring of atmospheric temperature and aerosol (dust and ice clouds) state from the surface to approximately 60 km. We present the results of the first half year operation in orbit around Mars.

Published
2018

188. The Atmospheric Chemistry Suite (ACS) of three spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., Martin Torres, J., Medvedev, A. S., Millour, E., Olsen, K. S., Patel, M. R., Quantin-Nataf, C., Rodin, A. V., Shematovich, V. I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., Zorzano, M. P., Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), National Research Institute for Physical-technical and Radiotechnical Measurements (VNIIFTRI), Scientific Production Enterprise Astron Electronics, Faculty of Physics [MSU, Moscow], Lomonosov Moscow State University (MSU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Tohoku University [Sendai], Moscow Institute of Physics and Technology [Moscow] (MIPT), Catholic University of America, Vernadsky Institute of Geochemistry and Analytical Chemistry (GEOKHI), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Computer Science [Kiruna], Luleå University of Technology (LUT), Instituto Andaluz de Ciencias de la Tierra (IACT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universidad de Granada (UGR), The Open University [Milton Keynes] (OU), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Universität Bern [Bern], Facultad de Informática [Madrid], Universidad Complutense de Madrid [Madrid] (UCM), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada (UGR), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada = University of Granada (UGR), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Universität Bern [Bern] (UNIBE), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Oxford, and Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
Cross-dispersion, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Atmosphere, 520 Astronomy, Mars, Echelle, Fourier-spectrometer, 620 Engineering, High-resolution spectrometer, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph]
Abstract

International audience; The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm−1. TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described.

Published
2018

189. The CH4 cycles on Pluto over seasonal and astronomical timescales

Author

Bertrand, T., primary, Forget, F., additional, Umurhan, O.M., additional, Moore, J.M., additional, Young, L.A., additional, Protopapa, S., additional, Grundy, W.M., additional, Schmitt, B., additional, Dhingra, R.D., additional, Binzel, R.P., additional, Earle, A.M., additional, Cruikshank, D.P., additional, Stern, S.A., additional, Weaver, H.A., additional, Ennico, K., additional, and Olkin, C.B., additional

Published
2019
Full Text
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190. Ground-based infrared mapping of H2O2 on Mars near opposition

Author

Encrenaz, T., primary, Greathouse, T. K., additional, Aoki, S., additional, Daerden, F., additional, Giuranna, M., additional, Forget, F., additional, Lefèvre, F., additional, Montmessin, F., additional, Fouchet, T., additional, Bézard, B., additional, Atreya, S. K., additional, DeWitt, C., additional, Richter, M. J., additional, Neary, L., additional, and Viscardy, S., additional

Published
2019
Full Text
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191. Detection and Characterization of Martian Volatile-Rich Reservoirs: The Netlander Approach

Author

Banerdt, B, Costard, F, Berthelier, J. J, Musmann, G, Menvielle, M, Lognonne, P, Giardini, D, Harri, A.-M, and Forget, F

Subjects
Lunar And Planetary Science And Exploration
Abstract

Geological and theoretical modeling do indicate that, most probably, a significant part of the volatiles present in the past is presently stocked within the Martian subsurface as ground ice, and as clay minerals (water constitution). The detection of liquid water is of prime interest and should have deep implications in the understanding of the Martian hydrological cycle and also in exobiology. In the frame of the 2005 joint CNES-NASA mission to Mars, a set of 4 NETLANDERs developed by an European consortium is expected to be launched between 2005 and 2007. The geophysical package of each lander will include a geo-radar (GPR experiment), a magnetometer (MAGNET experiment), a seismometer (SEIS experiment) and a meteorological package (ATMIS experiment). The NETLANDER mission offers a unique opportunity to explore simultaneously the subsurface as well as deeper layers of the planetary interior on 4 different landing sites. The complementary contributions of all these geophysical soundings onboard the NETLANDER stations are presented.

Published
2000

192. The DYNAMO Orbiter Project: High Resolution Mapping of Gravity/Magnetic Fields and In Situ Investigation of Mars Atmospheric Escape

Author

Smrekar, S, Chassefiere, E, Forget, F, Reme, H, Mazelle, C, Blelly, P. -L, Acuna, M, Connerney, J, Purucker, M, and Lin, R

Subjects
Lunar And Planetary Science And Exploration
Abstract

Dynamo is a small Mars orbiter planned to be launched in 2005 or 2007, in the frame of the NASA/CNES Mars exploration program. It is aimed at improving gravity and magnetic field resolution, in order to better understand the magnetic, geologic and thermal history of Mars, and at characterizing current atmospheric escape, which is still poorly constrained. These objectives are achieved by using a low periapsis orbit, similar to the one used by the Mars Global Surveyor spacecraft during its aerobraking phases. The proposed periapsis altitude for Dynamo of 120-130 km, coupled with the global distribution of periapses to be obtained during one Martian year of operation, through about 5000 low passes, will produce a magnetic/gravity field data set with approximately five times the spatial resolution of MGS. Low periapsis provides a unique opportunity to investigate the chemical and dynamical properties of the deep ionosphere, thermosphere, and the interaction between the atmosphere and the solar wind, therefore atmospheric escape, which may have played a crucial role in removing atmosphere, and water, from the planet. There is much room for debate on the importance of current atmosphere escape processes in the evolution of the Martian atmosphere, as early "exotic" processes including hydrodynamic escape and impact erosion are traditionally invoked to explain the apparent sparse inventory of present-day volatiles. Yet, the combination of low surface gravity and the absence of a substantial internally generated magnetic field have undeniable effects on what we observe today. In addition to the current losses in the forms of Jeans and photochemical escape of neutrals, there are solar wind interaction-related erosion mechanisms because the upper atmosphere is directly exposed to the solar wind. The solar wind related loss rates, while now comparable to those of a modest comet, nonetheless occur continuously, with the intriguing possibility of important cumulative and/or enhanced effects over the several billion years of the solar system's life. If the detailed history of the Martian internal field could be traced back, and the current escape processes could be understood well enough to model the expected stronger losses under early Sun conditions, one could go a long way toward constraining this part of the mysterious history of Mars' atmosphere.

Published
2000

193. The Pascal Discovery Mission: A Mars Climate Network Mission

Author

Haberle, R. M, Catling, D. C, Chassefiere, E, Forget, F, Hourdin, F, Leovy, C. B, Magalhaes, J, Mihalov, J, Pommereau, J. P, and Murphy, J. R

Subjects
Lunar And Planetary Science And Exploration
Abstract

The climate of Mars is a major focus of Mars exploration. With the loss of MCO, however, it remains uncertain how it will be achieved. We argue that a truly dedicated climate mission to Mars should have both orbital and landed components, and that these should operate simultaneously for at least 1 Mars year if not longer. Pascal is a Discovery mission that emphasizes the landed component. Its principal goal is to establish a network of 24 small weather stations on the surface of Mars that will operate for 2 Mars years, with an extended mission option for an additional 8 Mars years bringing the total mission lifetime up to 10 Mars years. The stations will collect hourly measurements of pressure, temperature, and optical depth. After delivering the probes to Mars, Pascal's carrier spacecraft will go into an elliptical orbit which will serve as a relay for the landers, and a platform for synoptic imaging. These simultaneous measurements from the surface and from orbit will allow us to characterize the planet's general circulation and its interaction with the dust, water, and CO2 cycles. During entry, descent, and landing, each of Pascal's 24 probes will also measure the temperature structure of the atmosphere and acquire images of the surface. These data will allow us to determine the global structure of the atmosphere between 15 and 130 km, and characterize the local terrain to help interpret the landed data. The descent images are part of Pascal's outreach program, as the probe camera system will be developed by faculty-supervised student project. The intent is to generate enthusiasm for the Pascal mission by directly involving students. Pascal will be launched on a Delta II-7925 in August of 2005. A type I trajectory will deliver Pascal to Mars in January of 2006. On approach, the three-axis stabilized carrier spacecraft will spring deploy the Pascal probes in 4 separate salvo's of 6 each. Global coverage is achieved with small time-of-arrival adjustments in between each salvo. Pascal's probes utilize an aeroshell, parachute, and crushable material for entry, descent and landing. On the surface, their long life and global coverage is enabled by a Micro Thermal Power Source with demonstrated heritage. After all probes are released, the carrier spacecraft will execute a small burn for insertion into an elliptical orbit. The long lifetime of the Pascal network was chosen in part to maximize the chances that orbital sounding, like that planned with MCO, would occur at some point during the mission. If Pascal is selected for launch in '05, this could occur if MCO-like science is reflown in the '05 opportunity or, if it is reflown in '03, the mission is extended to overlap with Pascal. The combination of temperature sounding from orbit, and surface pressure mapping from the surface will allow a direct determination of the full 3-D wind field for the first time.

Published
2000

194. Lower atmosphere and pressure evolution on Pluto from ground-based stellar occultations, 1988–2016

Author

Meza, E., primary, Sicardy, B., additional, Assafin, M., additional, Ortiz, J. L., additional, Bertrand, T., additional, Lellouch, E., additional, Desmars, J., additional, Forget, F., additional, Bérard, D., additional, Doressoundiram, A., additional, Lecacheux, J., additional, Oliveira, J. Marques, additional, Roques, F., additional, Widemann, T., additional, Colas, F., additional, Vachier, F., additional, Renner, S., additional, Leiva, R., additional, Braga-Ribas, F., additional, Benedetti-Rossi, G., additional, Camargo, J. I. B., additional, Dias-Oliveira, A., additional, Morgado, B., additional, Gomes-Júnior, A. R., additional, Vieira-Martins, R., additional, Behrend, R., additional, Tirado, A. Castro, additional, Duffard, R., additional, Morales, N., additional, Santos-Sanz, P., additional, Jelínek, M., additional, Cunniffe, R., additional, Querel, R., additional, Harnisch, M., additional, Jansen, R., additional, Pennell, A., additional, Todd, S., additional, Ivanov, V. D., additional, Opitom, C., additional, Gillon, M., additional, Jehin, E., additional, Manfroid, J., additional, Pollock, J., additional, Reichart, D. E., additional, Haislip, J. B., additional, Ivarsen, K. M., additional, LaCluyze, A. P., additional, Maury, A., additional, Gil-Hutton, R., additional, Dhillon, V., additional, Littlefair, S., additional, Marsh, T., additional, Veillet, C., additional, Bath, K.-L., additional, Beisker, W., additional, Bode, H.-J., additional, Kretlow, M., additional, Herald, D., additional, Gault, D., additional, Kerr, S., additional, Pavlov, H., additional, Faragó, O., additional, Klös, O., additional, Frappa, E., additional, Lavayssière, M., additional, Cole, A. A., additional, Giles, A. B., additional, Greenhill, J. G., additional, Hill, K. M., additional, Buie, M. W., additional, Olkin, C. B., additional, Young, E. F., additional, Young, L. A., additional, Wasserman, L. H., additional, Devogèle, M., additional, French, R. G., additional, Bianco, F. B., additional, Marchis, F., additional, Brosch, N., additional, Kaspi, S., additional, Polishook, D., additional, Manulis, I., additional, Ait Moulay Larbi, M., additional, Benkhaldoun, Z., additional, Daassou, A., additional, El Azhari, Y., additional, Moulane, Y., additional, Broughton, J., additional, Milner, J., additional, Dobosz, T., additional, Bolt, G., additional, Lade, B., additional, Gilmore, A., additional, Kilmartin, P., additional, Allen, W. H., additional, Graham, P. B., additional, Loader, B., additional, McKay, G., additional, Talbot, J., additional, Parker, S., additional, Abe, L., additional, Bendjoya, Ph., additional, Rivet, J.-P., additional, Vernet, D., additional, Di Fabrizio, L., additional, Lorenzi, V., additional, Magazzú, A., additional, Molinari, E., additional, Gazeas, K., additional, Tzouganatos, L., additional, Carbognani, A., additional, Bonnoli, G., additional, Marchini, A., additional, Leto, G., additional, Sanchez, R. Zanmar, additional, Mancini, L., additional, Kattentidt, B., additional, Dohrmann, M., additional, Guhl, K., additional, Rothe, W., additional, Walzel, K., additional, Wortmann, G., additional, Eberle, A., additional, Hampf, D., additional, Ohlert, J., additional, Krannich, G., additional, Murawsky, G., additional, Gährken, B., additional, Gloistein, D., additional, Alonso, S., additional, Román, A., additional, Communal, J.-E., additional, Jabet, F., additional, deVisscher, S., additional, Sérot, J., additional, Janik, T., additional, Moravec, Z., additional, Machado, P., additional, Selva, A., additional, Perelló, C., additional, Rovira, J., additional, Conti, M., additional, Papini, R., additional, Salvaggio, F., additional, Noschese, A., additional, Tsamis, V., additional, Tigani, K., additional, Barroy, P., additional, Irzyk, M., additional, Neel, D., additional, Godard, J. P., additional, Lanoiselée, D., additional, Sogorb, P., additional, Vérilhac, D., additional, Bretton, M., additional, Signoret, F., additional, Ciabattari, F., additional, Naves, R., additional, Boutet, M., additional, De Queiroz, J., additional, Lindner, P., additional, Lindner, K., additional, Enskonatus, P., additional, Dangl, G., additional, Tordai, T., additional, Eichler, H., additional, Hattenbach, J., additional, Peterson, C., additional, Molnar, L. A., additional, and Howell, R. R., additional

Published
2019
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196. Abstract PD1-09: Phase 2 safety and efficacy results of TAK-228 in combination with exemestane or fulvestrant in postmenopausal women with ER-positive/HER2-negative metastatic breast cancer previously treated with everolimus

Author

Diamond, JR, primary, Potter, D, additional, Salkeni, M, additional, Silverman, P, additional, Haddad, T, additional, Forget, F, additional, Awada, A, additional, Canon, J-L, additional, Danso, M, additional, Lortholary, A, additional, Bourgeois, H, additional, Tan-Chiu, E, additional, Patel, C, additional, Neuwirth, R, additional, Leonard, EJ, additional, and Lim, B, additional

Published
2019
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197. Mars’ Background Free Oscillations

Author

Nishikawa, Y., primary, Lognonné, P., additional, Kawamura, T., additional, Spiga, A., additional, Stutzmann, E., additional, Schimmel, M., additional, Bertrand, T., additional, Forget, F., additional, and Kurita, K., additional

Published
2019
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198. The Pascal Discovery Mission: A Mars Climate Network Mission

Author

Haberle, Robert M, Catling, D. C, Chassefiere, E, Forget, F, Hourdin, F, Leovy, C. B, Magalhaes, J, Mihalov, J, Pommereau, J. P, Murphy, J. R, and DeVincenzi, Donald L

Subjects
Lunar And Planetary Science And Exploration
Abstract

The climate of Mars is a major focus of Mars exploration. With the loss of MCO, however, it remains uncertain how it will be achieved. We argue that a truly dedicated climate mission to Mars should have both orbital and landed components, and that these should operate simultaneously for at least I Mars year if not longer. Pascal is Discovery mission that emphasizes the landed component. Its principal goal is to establish a network of 24 small weather stations on the surface of Mars that will operate for 2 Mars years, with an extended mission option for an additional 8 Mars years bringing the total mission lifetime up to 10 Mars years. The stations will collect hourly measurements of pressure, temperature, and optical depth. After delivering the probes to Mars, Pascal's carrier spacecraft will go into an elliptical orbit which will serve as a relay for the landers, and a platform for synoptic imaging. These simultaneous measurements from the surface and from orbit will allow us to characterize the planet's general circulation and its interaction with the dust, water, and CO2 cycles. During entry, descent, and landing, each of Pascal's 24 probes will also measure the temperature structure of the atmosphere and acquire images of the surface. These data will allow us to determine the global structure of the atmosphere between 15 and 130 km, and characterize the local terrain to help interpret the landed data. The descent images are part of Pascal's outreach program, as the probe camera system will be developed by faculty-supervised student project. The intent is to generate enthusiasm for the Pascal mission by directly involving students. Pascal will be launched on a Delta 11-7925 in August of 2005. A type I trajectory will deliver Pascal to Mars in January of 2006. On approach, the three-axis stabilized carrier spacecraft will spring deploy the Pascal probes in 4 separate salvo's of 6 each. Global coverage is achieved with small time-of-arrival adjustments in between each salvo. Pascal's probes utilize an aeroshell, parachute, and crushable material for entry, descent and landing. On the surface, their long life and global coverage is enabled by a Micro Thermal Power Source with demonstrated heritage. After all probes are released, the carrier spacecraft will execute a small bum for insertion into an elliptical orbit. The long lifetime of the Pascal network was chosen in part to maximize the chances that orbital sounding, like that planned with MCO, would occur at some point during the mission. If Pascal is selected for launch in -05, this could occur if MCO-like science is reflown in the '05 opportunity or, if it is reflown in '03, the mission is extended to overlap with Pascal. The combination of temperature sounding from orbit, and surface pressure mapping from the surface will allow a direct determination of the full 3-D wind field for the first time.

Published
2000

199. Microwave Investigation of the Mars Atmosphere and Surface

Author

Gulkis, S, Forget, F, Janssen, M, Riley, A. L, Hartogh, P, Clancy, T, Allen, M, and Frerking, M

Subjects
Lunar And Planetary Science And Exploration
Abstract

The Microwave Investigation of the Mars Atmosphere and Surface Experiment (MIMAS) is designed to address two major scientific goals: 1) To understand the three dimensional general circulation of the Martian atmosphere, and 2) To understand the hydrologic cycle of water on Mars, including the time-variable sources, sinks, and atmospheric transport of water vapor. The proposed instrument is a submillimeter wave, heterodyne receiver, with both continuum and very high spectral resolution capability. A small reflector antenna will be used to feed the receiver. Instrument heritage comes from the MIRO receiver, currently under design for the ESA Rosetta Mission, and from SWAS, a NASA astrophysics mission. The instrument will be able to measure atmospheric spectral lines from both water and carbon monoxide and use these lines as tracers of atmospheric winds. Measurement objectives of MIMAS are to measure surface temperature, atmospheric temperature from the surface up to an altitude of 60 km or more, the distribution of CO and H2O in the atmosphere, and certain wind fields (zonal and meridional). The global distribution of CO, as well as temperature distributions, will be used as input data for GCMs (general circulation models). Water vapor profiles will be used to understand the sources and sinks of water on Mars and to understand how it is transported globally by the general circulation. Zonal and meridional wind fields will provide further tests of the GCMs. An important aspect of this experiment is that the temperature and humidity measurements are insensitive to dust and ice condensates thereby making the measurement capability independent of the presence of dust clouds and ice particles. Temperature measurements derived from the data can be used in conjunction with infrared measurements to determine dust profiles.

Published
2000

200. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, Franck, Trokhimovskiy, A., Fedorova, A.A., Shakun, A.V., Grigoriev, A.V., Moshkin, B.E., Ignatiev, N.I., Forget, F., Lefevre, F., Anufreychik, A., Dzuban, I., Ivanov, Y.S., Kalinnikov, Y.K., Kozlova, T. O., Kungurov, A., Markov, V., Martynovich, F., Mazlov, I., Merzlyakov, D., Moiseev, P.P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripo, A., Sazonov, O., Semena, N., Shashkin, V., Sidorov, A., Stepanov, A.V., Stupin, I., Timonin, D., Titov, A.Y., Viktorov, A., Zharkov, A., Alteri, F., Arnold, G., Belyaev, D.A., Bertaux, J.-L., Betsis, D.S., Duxbury, N., Encrenaz, T., Fouchet, T., Gerard, J.-C., Grassi, D., Guerlet, S., Hargtogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V.A., Kuzmin, R.O., Lellouch, E., Lopez-Valverde, M.A., Luginin, M., Määttänen, A., Marcq, M., Martin Torres, J., Medvedev, A.S., Millour, E., Olsen, K.S., Patel, M.R., Quantin-Nataf, C., Rodin, A.V., Shematovich, V.I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C.F., Zazova, L.V., Zelenyi, L.M., Zorzano, M.P., Russian Science Foundation, Ministerio de Economía y Competitividad (España), Svedhem, H., and Russel, C.T.

Subjects
Leitungsbereich PF, Mars · Atmosphere · High-resolution spectrometer · Fourier-spectrometer ·Echelle · Cross-dispersion
Abstract

The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm. TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described., ExoMars is a space mission by ESA and Roscosmos. The development and fabrication of ACS was funded by Roscosmos with contributions from LATMOS (France) funded by CNES. Science operations are funded by Roscosmos and ESA. AAF, NII, DAB, JLB, DSB, ML acknowledge the grant #14.W03.31.0017 of Ministry for Education and Science of Russian Federation for science support of the ACS experiment. AT, AVS, and BEM acknowledge support from Russian Science Foundation (grant RSF 16-12-10453), whichenabledassessmentofmeasurementcharacteristicsoftheinstrument andtheassociated modeling. LMZ acknowledges RSF funding (grant RSF 16-42-01103). Other authors affiliated with IKI acknowledge FANO, contracts 0120.06 02993 (0028-2014-0004) and 0120.03 03422 (0028-2014-0007). MRP acknowledges funding under the UK Space Agency grant ST/I003061/1 and ST/P001262/1. LV acknowledges the support of Ministerio de Economía y Competitividad of Spain under project ESP2016-79135-R. We are grateful to Richard Zurek and an anonymous reviewer for useful comments and suggestions, which helped improving this paper. We thank Sylvain Cnudde, Evgeny Germanyuk, and Ekaterina Korableva for help in rendering graphics. We also express our sincere gratitude to the space agencies, countries, companies, and project teams who made the ExoMars 2016 mission possible.

Published
2017

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