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1. Properties of a Martian local dust storm in Atlantis Chaos from OMEGA/MEX data

Author

Oliva, F., Geminale, A., D'Aversa, E., Altieri, F., Bellucci, G., Carrozzo, F. G., Sindoni, G., and Grassi, D.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

In this study we present the analysis of the dust properties of a local storm imaged in the Atlantis Chaos region on Mars by the OMEGA imaging spectrometer on March 2nd 2005. We use the radiative transfer model MITRA to study the dust properties at solar wavelengths between 0.5 {\mu}m and 2.5 {\mu}m and infer the connection between the local storm dynamics and the topography. We retrieve maps of effective grain radius (reff), optical depth at 9.3 {\mu}m ({\tau}9.3) and top altitude (ta) of the dust layer. Our results show that large particles (reff = 1.6 {\mu}m) are gathered in the centre of the storm (lat=33.5{\deg} S; lon=183.5 W{\deg}), where the optical depth is maximum ({\tau}9.3 > 7.0) and the top altitude exceeds 18 km. Outside the storm, we obtain {\tau}9.3 < 0.2, in agreement with the estimates derived from global climate models (GCM). We speculate that a low thermal inertia region at the western border of Atlantis Chaos is a possible source of the dust storm. Moreover, we find evidence that topography plays a role in confining the local storm in Atlantis Chaos. The vertical wind component from the GCM does not provide any hint for the triggering of dust lifting. On the other hand, the combination of the horizontal and vertical wind profiles suggests that the dust, once lifted, is pushed eastward and then downward and gets confined within the north-east ridge of Atlantis Chaos. (continues in article)

Published
2017
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2. CryoSat Long-Term Ocean Data Analysis and Validation: Final Words on GOP Baseline-C

Author

Marc Naeije, Alessandro Di Bella, Teresa Geminale, and Pieter Visser

Subjects
altimetry, CAL/VAL, bias, CryoSat-2, GOP Baseline-C, cross-over and tide gauge analyses, Science
Abstract

ESA’s Earth explorer mission CryoSat-2 has an ice-monitoring objective, but it has proven to also be a valuable source of observations for measuring impacts of climate change over oceans. In this paper, we report on our long-term ocean data analysis and validation and give our final words on CryoSat-2’s Geophysical Ocean Products (GOP) Baseline-C. The validation is based on a cross comparison with concurrent altimetry and with in situ tide gauges. The highlights of our findings include GOP Baseline-C showing issues with the ionosphere and pole tide correction. The latter gives rise to an east–west pattern in range bias. Between Synthetic Aperture Radar (SAR) and Low-Resolution Mode (LRM), a 1.4 cm jump in range bias is explained by a 0.5 cm jump in sea state bias, which relates to a significant wave height SAR-LRM jump of 10.5 cm. The remaining 0.9 cm is due to a range bias between ascending and descending passes, exhibiting a clear north–south pattern and ascribed to a timing bias of +0.367 ms, affecting both time-tag and elevation. The overall range bias of GOP Baseline-C is established at −2.9 cm, referenced to all calibrated concurrent altimeter missions. The bias drift does not exceed 0.2 mm/yr, leading to the conclusion that GOP Baseline-C is substantially stable and measures up to the altimeter reference missions. This is confirmed by tide gauge comparison with a selected set of 309 PSMSL tide gauges over 2010–2022: we determined a correlation of R = 0.82, a mean standard deviation of σ=5.7 cm (common reference and GIA corrected), and a drift of 0.17 mm/yr. In conclusion, the quality, continuity, and reference of GOP Baseline-C is exceptionally good and stable over time, and no proof of any deterioration or platform aging has been found. Any improvements for the next CryoSat-2 Baselines could come from sea state bias optimization, ionosphere and pole tide correction improvement, and applying a calibrated value for any timing biases.

Published
2023
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3. Evaluation, Description and Magnitude of Readmission Phenomenon in Azienda Ospedaliero Universitaria Pisana (AOUP) for Chronic-Degenerative Diseases in the Period 2018–2021

Author

Matteo Filippi, Erika Del Prete, Ferruccio Aquilini, Michele Totaro, Francesca Di Serafino, Sara Civitelli, Giulia Geminale, David Rocchi, Nunzio Zotti, and Angelo Baggiani

Subjects
readmissions, health economics, Diagnosis Related Group, chronic diseases, continuity of care, Medicine
Abstract

Background: Readmissions are hospitalizations following a previous hospitalization (called index hospitalization) of the same patient that occurred in the same facility or nursing home. They may be a consequence of the progression of the natural history of a disease, but they may also reveal a previous suboptimal stay, or ineffective management of the underlying clinical condition. Preventing avoidable readmissions has the potential to improve both a patient’s quality of life, by avoiding exposure to the risks of re-hospitalization, and the financial well-being of health care systems. Methods: We investigated the magnitude of 30 day repeat hospitalizations for the same Major Diagnostic Category (MDC) in the Azienda Ospedaliero Universitaria Pisana (AOUP) over the period from 2018 to 2021. Records were divided into only admissions, index admissions and repeated admission. The length of the stay of all groups was compared using analysis of variance and subsequent multi-comparison tests. Results: Results showed a reduction in readmissions over the period examined (from 5.36% in 2018 to 4.46% in 2021), likely due to reduced access to care during the COVID-19 pandemic. We also observed that readmissions predominantly affect the male sex, older age groups, and patients with medical Diagnosis Related Groups (DRGs). The length of stay of readmissions was longer than that of index hospitalization (difference of 1.57 days, 95% CI 1.36–1.78 days, p < 0.001). The length of stay of index hospitalization is longer than that of single hospitalization (difference of 0.62 days, 95% CI 0.52–0.72 days, p < 0.001). Conclusions: A patient who goes for readmission thus has an overall hospitalization duration of almost two and a half times the length of the stay of a patient with single hospitalization, considering both index hospitalization and readmission. This represents a heavy use of hospital resources, about 10,200 more inpatient days than single hospitalizations, corresponding to a 30-bed ward working with an occupancy rate of 95%. Knowledge of readmissions is an important piece of information in health planning and a useful tool for monitoring the quality of models of patient care.

Published
2023
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5. A test for the universality of extinction curve shape

Author

Geminale, Anna and Popowski, Piotr

Subjects
Astrophysics
Abstract

We present an analysis of 436 lines of sight with extinction data covering wavelength range from near-infrared (NIR) to ultraviolet (UV). We use J, H, K photometry from 2MASS database, the IR intrinsic colors from Wegner (1994), and UV extinction data from Wegner (2002). We exclude 19 lines of sight (4%) from the original sample because of suspected photometric problems. We derive total to selective extinction ratios (R_V) based on the Cardelli, Clayton, and Mathis (1989; CCM) law, which is typically used to fit the extinction data for both diffuse and dense interstellar medium. We conclude that CCM law is able to fit well most of the extinction curves in our sample (71%), and we present a catalog of R_V and visual extinction (A_V) values for those cases. We divide the remaining lines of sight with peculiar extinction into two groups according to two main behaviors: a) the NIR or/and UV wavelength regions cannot be reproduced by CCM formula (14% of the entire sample), b) the NIR and UV extinction data taken separately are best fit by CCM laws with significantly different values of R_V (10% of the entire sample). We present examples of such curves. We caution that some peculiarities of the extinction curves may not be intrinsic but simply caused by faulty data. The study of the intrinsically peculiar cases could help us to learn about the physical processes that affect dust in the interstellar medium, e.g., formation of mantles on the surface of grains, evaporation, growing or shattering., Comment: 22 pages, 6 figures, 4 tables, submitted to MNRAS

Published
2005

6. Can CCM law properly represent all extinction curves?

Author

Geminale, Anna and Popowski, Piotr

Subjects
Astrophysics
Abstract

We present the analysis of a large sample of lines of sight with extinction curves covering wavelength range from near-infrared (NIR) to ultraviolet (UV). We derive total to selective extinction ratios based on the Cardelli, Clayton and Mathis (1989, CCM) law, which is typically used to fit the extinction data both for diffuse and dense interstellar medium. We conclude that the CCM law is able to fit most of the extinction curves in our sample. We divide the remaining lines of sight with peculiar extinction into two groups according to two main behaviors: a) the optical/IR or/and UV wavelength region cannot be reproduced by the CCM formula; b) the optical/NIR and UV extinction data are best fit by the CCM law with different values of R_V. We present examples of such curves. The study of both types of peculiar cases can help us to learn about the physical processes that affect dust in the interstellar medium, e.g., formation of mantles on the surface of grains, evaporation, growing or shattering., Comment: 6 pages, 4 figures, in "Light, dust and chemical evolution", Journal of Physics: Conference Series

Published
2005
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7. Total to Selective Extinction Ratios and Visual Extinctions from Ultraviolet Data

Author

Geminale, Anna and Popowski, Piotr

Subjects
Astrophysics
Abstract

We present determinations of the total to selective extinction ratio R_V and visual extinction A_V values for Milky Way stars using ultraviolet color excesses. We extend the analysis of Gnacinski and Sikorski (1999) by using non-equal weights derived from observational errors. We present a detailed discussion of various statistical errors. In addition, we estimate the level of systematic errors by considering different normalization of the extinction curve adopted by Wegner (2002). Our catalog of 782 R_V and A_V values and their errors is available in the electronic form on the World Wide Web., Comment: 20 pages, 7 figures, submitted to Acta Astronomica

Published
2004

8. Optical photometry and spectral classification in the field of the open cluster NGC 6996 in the North America Nebula

Author

Villanova, Sandro, Baume, Gustavo, Carraro, Giovanni, and Geminale, Anna

Subjects
Astrophysics
Abstract

We present and discuss broad band CCD $UBV(I)_C$ photometry and low resolution spectroscopy for stars in the region of the open cluster NGC 6996, located in the North America Nebula. The new data allow us to tightly constrain the basic properties of this object. We revise the cluster size, which in the past has been significantly underestimated. The width of the Main Sequence is mainly interpreted in terms of differential reddening, and indeed the stars' color excess $E_{B-V}$ ranges from 0.43 to 0.65, implying the presence of a significant and evenly distributed dust component. We cross-correlate our optical photometry with near infrared from 2MASS, and by means of spectral classification we are able to build up extinction curves for an handful of bright members. We find that the reddening slope and the total to selective absorption ratio $R_V$ toward NGC 6996 are anomalous. Moreover the reddening corrected colors and magnitudes allow us to derive estimates for the cluster distance and age, which turn out to be $760 \pm 70 pc$ ($V_{0}-M_{V} = 9.4 \pm 0.2$) and $\sim 350$ Myr, respectively. Basing on our results, we suggest that NGC 6996 is located in front of the North America Nebula, and does not seem to have any apparent relationship with it., Comment: 19 pages, 12 eps figures, in press in A&A

Published
2004
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10. CryoSat Long-Term Ocean Data Analysis and Validation: Final Words on GOP Baseline-C

Author

Naeije, M.C. (author), Di Bella, Alessandro (author), Geminale, Teresa (author), Visser, P.N.A.M. (author), Naeije, M.C. (author), Di Bella, Alessandro (author), Geminale, Teresa (author), and Visser, P.N.A.M. (author)

Abstract

ESA’s Earth explorer mission CryoSat-2 has an ice-monitoring objective, but it has proven to also be a valuable source of observations for measuring impacts of climate change over oceans. In this paper, we report on our long-term ocean data analysis and validation and give our final words on CryoSat-2’s Geophysical Ocean Products (GOP) Baseline-C. The validation is based on a cross comparison with concurrent altimetry and with in situ tide gauges. The highlights of our findings include GOP Baseline-C showing issues with the ionosphere and pole tide correction. The latter gives rise to an east–west pattern in range bias. Between Synthetic Aperture Radar (SAR) and Low-Resolution Mode (LRM), a 1.4 cm jump in range bias is explained by a 0.5 cm jump in sea state bias, which relates to a significant wave height SAR-LRM jump of 10.5 cm. The remaining 0.9 cm is due to a range bias between ascending and descending passes, exhibiting a clear north–south pattern and ascribed to a timing bias of +0.367 ms, affecting both time-tag and elevation. The overall range bias of GOP Baseline-C is established at −2.9 cm, referenced to all calibrated concurrent altimeter missions. The bias drift does not exceed 0.2 mm/yr, leading to the conclusion that GOP Baseline-C is substantially stable and measures up to the altimeter reference missions. This is confirmed by tide gauge comparison with a selected set of 309 PSMSL tide gauges over 2010–2022: we determined a correlation of R = 0.82, a mean standard deviation of (Formula presented.) cm (common reference and GIA corrected), and a drift of 0.17 mm/yr. In conclusion, the quality, continuity, and reference of GOP Baseline-C is exceptionally good and stable over time, and no proof of any deterioration or platform aging has been found. Any improvements for the next CryoSat-2 Baselines could come from sea state bias optimization, ionosphere and pole tide correction improvement, and applying a calibrated value for any timing biases., Astrodynamics & Space Missions, Space Engineering

Published
2023
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12. CryoSat Long-Term Ocean Data Analysis and Validation: Final Words on GOP Baseline-C.

Author

Naeije, Marc, Di Bella, Alessandro, Geminale, Teresa, and Visser, Pieter

Subjects
SYNTHETIC aperture radar, DATA analysis
Abstract

ESA's Earth explorer mission CryoSat-2 has an ice-monitoring objective, but it has proven to also be a valuable source of observations for measuring impacts of climate change over oceans. In this paper, we report on our long-term ocean data analysis and validation and give our final words on CryoSat-2's Geophysical Ocean Products (GOP) Baseline-C. The validation is based on a cross comparison with concurrent altimetry and with in situ tide gauges. The highlights of our findings include GOP Baseline-C showing issues with the ionosphere and pole tide correction. The latter gives rise to an east–west pattern in range bias. Between Synthetic Aperture Radar (SAR) and Low-Resolution Mode (LRM), a 1.4 cm jump in range bias is explained by a 0.5 cm jump in sea state bias, which relates to a significant wave height SAR-LRM jump of 10.5 cm. The remaining 0.9 cm is due to a range bias between ascending and descending passes, exhibiting a clear north–south pattern and ascribed to a timing bias of +0.367 ms, affecting both time-tag and elevation. The overall range bias of GOP Baseline-C is established at −2.9 cm, referenced to all calibrated concurrent altimeter missions. The bias drift does not exceed 0.2 mm/yr, leading to the conclusion that GOP Baseline-C is substantially stable and measures up to the altimeter reference missions. This is confirmed by tide gauge comparison with a selected set of 309 PSMSL tide gauges over 2010–2022: we determined a correlation of R = 0.82, a mean standard deviation of σ = 5.7 cm (common reference and GIA corrected), and a drift of 0.17 mm/yr. In conclusion, the quality, continuity, and reference of GOP Baseline-C is exceptionally good and stable over time, and no proof of any deterioration or platform aging has been found. Any improvements for the next CryoSat-2 Baselines could come from sea state bias optimization, ionosphere and pole tide correction improvement, and applying a calibrated value for any timing biases. [ABSTRACT FROM AUTHOR]

Published
2023
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13. Evaluation, Description and Magnitude of Readmission Phenomenon in Azienda Ospedaliero Universitaria Pisana (AOUP) for Chronic-Degenerative Diseases in the Period 2018–2021

Author

Filippi, Matteo, primary, Del Prete, Erika, additional, Aquilini, Ferruccio, additional, Totaro, Michele, additional, Di Serafino, Francesca, additional, Civitelli, Sara, additional, Geminale, Giulia, additional, Rocchi, David, additional, Zotti, Nunzio, additional, and Baggiani, Angelo, additional

Published
2023
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14. Retrieval of the water ice column and physical properties of water-ice clouds in the martian atmosphere using the OMEGA imaging spectrometer

Author

François Forget, Fabrizio Oliva, A. Szantai, Francesca Altieri, Luca Montabone, Joachim Audouard, A. Geminale, Kevin Olsen, Jean-Baptiste Madeleine, M. J. Wolff, Giancarlo Bellucci, PLANETO - 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-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Space Science Institute [Boulder] (SSI), European Project: 633127,H2020,H2020-COMPET-2014,UPWARDS(2015), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris)

Subjects
010504 meteorology & atmospheric sciences, media_common.quotation_subject, Imaging spectrometer, 01 natural sciences, Omega, Standard deviation, Mars atmosphere, Clouds, 0103 physical sciences, Mars Express, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, media_common, Remote sensing, Effective radius, Aerosols, Climatology, Ice cloud, ICI, Astronomy and Astrophysics, Mars Exploration Program, Atmosphere of Mars, Retrievals, OMEGA, Water ice, 13. Climate action, Space and Planetary Science, Sky, [SDU]Sciences of the Universe [physics], Environmental science
Abstract

International audience Using spectral images recorded by the OMEGA instrument on Mars Express (Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité), we are able to derive physical properties of aerosols in water-ice clouds on Mars for a distribution of pixels over an observed cloud formation. These properties, mean effective radius, reff, and optical depth (at 0.67 μm), τi, were used to estimate the water ice-column (WIC), and we found an empirical relationship between the WIC and an ice cloud index (ICI). The overall mean of retrieved reff is ∼2.2 μm, with a standard deviation of 0.8 μm, and cloud formations with reff between 4.4 and 5.4 μm are observed. The optical depth varies between 0.2 and 2.0. The OMEGA spectra are primarily sensitive to water ice mass due to absorption, and we find that the ICI, very easy to compute, is a good proxy for the mass of the water-ice column (WIC) along the optical line of sight. Our retrieval of physical properties is limited in time (to before 2010) by the exhaustion of coolant for one of the OMEGA channels, and in space (to equatorial observations between 140∘W and 90∘E) by the availability of surface albedo measurements. However, we used the ICI to compute WIC values for the entire OMEGA data set, which has near-global coverage for Mars years 26–32, and we present a climatology of the WIC derived from the OMEGA data, which features enhancements on the order of 1.2–1.6 pr. μm over the aphelion cloud belt, and 1.5–2.5 pr. μm over the polar hoods. The data set analyzed is for observations between 140°W and 90°E, and between 35∘S and 35∘N. No restriction is placed on season, but the majority of cloudy observations were during the aphelion period from Ls 35∘ to 135∘. This work was motivated by the ability of the OMEGA instrument to observe the distribution of water-ice cloud physical properties, and by the availability of new a priori data sets, especially multi-spectral, aerosol-free surface albedo retrieved from a subset of the OMEGA data featuring a cloud-free sky. The main limitations of the retrieval algorithm are linked to the uncertainties on surface albedo, the dust opacity, and the quantity of water-ice suspended in the atmosphere, which can lead to spectral fits with lower accuracy or unrealistic results. We present distributions of each retrieved parameter, goodness of fit, ICI, and cloud mass, and our investigation of relationships between each parameter. Our approach was to maximize the amount of data analyzed, apply stringent data quality cuts and take a statistical approach to interpretation.

Published
2021

15. Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author

Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., ALTIERI, FRANCESCA, López-Valverde, Miguel, Villanueva, Geronimo, Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Bertaux, Jean-Loup, Betsis, Daria, Bolsée, David, Clancy, R. Todd, CLOUTIS, EDWARD, Depiesse, Cédric, Funke, Bernd, Garcia-Comas, Maia, Gérard, Jean-Claude, GIURANNA, MARCO, Gonzalez-Galindo, Francisco, Grigoriev, Alexey V., Ivanov, Yuriy S., Kaminski, Jacek, Karatekin, Ozgur, Lefèvre, Franck, Lewis, Stephen, López-Puertas, Manuel, Mahieux, Arnaud, Maslov, Igor, Mason, Jon, Mumma, Michael J., Neary, Lori, Neefs, Eddy, Patrakeev, Andrey, Patsaev, Dmitry, Ristic, Bojan, Robert, Séverine, Schmidt, Frédéric, Shakun, Alexey, Teanby, Nicholas A., Viscardy, Sébastien, Willame, Yannick, Whiteway, James, Wilquet, Valérie, Wolff, Michael J., BELLUCCI, Giancarlo, Patel, Manish R., López-Moreno, Jose-Juan, Forget, François, Wilson, Colin F., Svedhem, Håkan, Vago, Jorge L., Rodionov, Daniel, NOMAD Science Team, Alonso-Rodrigo, Gustavo, Bauduin, Sophie, Carrozzo, Giacomo, Crismani, Matteo, da Pieve, Fabiana, D'AVERSA, EMILIANO, Etiope, Giuseppe, Fussen, Didier, Geminale, Anna, Gkouvelis, Leo, Holmes, James, Hubert, Benoît, Ignatiev, Nicolay I., Kasaba, Yasumasa, Kass, David, Kleinböhl, Armin, LANCIANO, ORIETTA, Nakagawa, Hiromu, Novak, Robert E., Oliva, Fabrizio, Piccialli, Arianna, Renotte, Etienne, Ritter, Birgit, Schneider, Nick, SINDONI, Giuseppe, Thiemann, Ed, Vander Auwera, Jean, Wilquet, Valerie, WOLKENBERG, PAULINA MARIA, Yelle, Roger, ACS Science Team, Anufreychik, Konstantin, Arnold, Gabriele, Duxbury, Natalia, Fouchet, Thierry, GRASSI, Davide, Guerlet, Sandrine, Hartogh, Paul, Khatuntsev, Igor, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, Lellouch, Emmanuel, Määttänen, Anni, Marcq, Emmanuel, Martin-Torres, Javier, Medvedev, Alexander, Millour, Ehouarn, Moshkin, Boris, Quantin-Nataf, Cathy, Rodin, Alexander, Shematovich, Valery, Thomas, Nicolas, Trokhimovsky, Alexander, Vazquez, Luis, Vincendon, Matthieu, Young, Roland, Zasova, Ludmila, Zelenyi, Lev, Zorzano, Maria Paz, Parejo, J, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, NASA Goddard Space Flight Center (GSFC), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Agenzia Spaziale Italiana (ASI), Graduate School of Information Sciences [Sendai], Tohoku University [Sendai], Advanced Mechanical and Optical Systems SA (AMOS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], School of Earth Sciences [Bristol], University of Bristol [Bristol], Centre for Research in Earth and Space Science [Toronto] (CRESS), York University [Toronto], Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Department of Physics [Oxford], University of Oxford [Oxford], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), Lomonosov Moscow State University (MSU), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Institute for Astrophysics and Computational Sciences [Washington], Catholic University of America, Department of Computer Science, Electrical and Space Engineering [Luleå], Luleå University of Technology (LUT), 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), Moscow Institute of Physics and Technology [Moscow] (MIPT), Institute of Astronomy of the Russian Academy of Sciences (INASAN), University of Bern, Universidad Complutense de Madrid = Complutense University of 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), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Libre de Bruxelles [Bruxelles] (ULB), The Open University [Milton Keynes] (OU), Polska Akademia Nauk (PAN), Royal Observatory of Belgium [Brussels], IMPEC - 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS 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), Universidad Complutense de Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, 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), 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), 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), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Ministerio de Ciencia e Innovación (España), European Space Agency, Belgian Science Policy Office, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Centre National de la Recherche Scientifique (France), and Russian Government

Subjects
Martian, Ice cloud, Multidisciplinary, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Storm, Atmosphere of Mars, Atmospheric sciences, 01 natural sciences, Trace gas, chemistry.chemical_compound, chemistry, 13. Climate action, Dust storm, 0103 physical sciences, Environmental science, Semiheavy water, 010303 astronomy & astrophysics, Water vapor, 0105 earth and related environmental sciences, Sciences exactes et naturelles
Abstract

A publisher correction to this article was published on 17 April 2019, Global dust storms on Mars are rare1,2 but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere3, primarily owing to solar heating of the dust3. In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars4. Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes5,6, as well as a decrease in the water column at low latitudes7,8. Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H2O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H2O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals3. The observed changes in H2O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere. © 2019, The Author(s), under exclusive licence to Springer Nature Limited., This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493); by the Spanish MICINN through its Plan Nacional and by European funds under grants ESP2015-65064-C2-1-P and ESP2017-87143-R (MINECO/FEDER); by the UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, ST/S00145X/1, ST/R001367/1, ST/P001572/1 and ST/R001502/1; and the Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique - FNRS under grant number 30442502 (ET_HOME). The ACS experiment is led by IKI, Space Research Institute in Moscow, assisted by LATMOS in France. The project acknowledges funding by Roscosmos and CNES. The science operations of ACS are funded by Roscosmos and ESA. IKI affiliates acknowledge funding under grant number 14.W03.31.0017 and contract number 0120.0 602993 (0028-2014-0004) of the Russian government.

Published
2019

16. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD

Author

Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Smith, M.D., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, S., Gomez, A., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, R., Perez-grande, I., Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), and Canadian Space Agency

Subjects
010504 meteorology & atmospheric sciences, Storm, Atmosphere of Mars, Mars Exploration Program, Atmospheric sciences, 01 natural sciences, Trace gas, Atmosphere, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Dust storm, Earth and Planetary Sciences (miscellaneous), Environmental science, Hadley cell, Water vapor, 0105 earth and related environmental sciences
Abstract

It has been suggested that dust storms efficiently transport water vapor from the near-surface to the middle atmosphere on Mars. Knowledge of the water vapor vertical profile during dust storms is important to understand water escape. During Martian Year 34, two dust storms occurred on Mars: a global dust storm (June to mid-September 2018) and a regional storm (January 2019). Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). We show a significant increase of water vapor abundance in the middle atmosphere (40–100 km) during the global dust storm. The water enhancement rapidly occurs following the onset of the storm (Ls~190°) and has a peak at the most active period (Ls~200°). Water vapor reaches very high altitudes (up to 100 km) with a volume mixing ratio of ~50 ppm. The water vapor abundance in the middle atmosphere shows high values consistently at 60°S-60°N at the growth phase of the dust storm (Ls = 195°–220°), and peaks at latitudes greater than 60°S at the decay phase (Ls = 220°–260°). This is explained by the seasonal change of meridional circulation: from equinoctial Hadley circulation (two cells) to the solstitial one (a single pole-to-pole cell). We also find a conspicuous increase of water vapor density in the middle atmosphere at the period of the regional dust storm (Ls = 322–327°), in particular at latitudes greater than 60°S. ©2019. American Geophysical Union. All Rights Reserved., S. A. is >Charge de Recherches> of the F.R.S.-FNRS. ExoMars is a space mission of the European Space Agency and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASBBIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office, with the financial and contractual coordination by the European Space Agency Prodex Office (PEA 4000103401 and 4000121493), by the Spanish MICINN through its Plan Nacional and by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, and ST/S00145X/1 and Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique-FNRS under grant numbers 30442502 (ET_HOME) and T.0171.16 (CRAMIC) and Belgian Science Policy Office BrainBe SCOOP Project. U.S. investigators were supported by the National Aeronautics and Space Administration. Canadian investigators were supported by the Canadian Space Agency. The results retrieved from the NOMAD measurements used in this article are available on the BIRA-IASB data repository: http://repository.aeronomie.be/?doi= 10.18758/71021054 (Aoki et al., 2019).

Published
2019

17. Methane on Mars: New insights into the sensitivity of CH4 with the NOMAD/ExoMars spectrometer through its first in flight calibration

Author

Liuzzi, Giuliano, Villanueva, Geronimo L., Mumma, Michael J., Smith, Michael D., Daerden, Frank, Ristic, Bojan, Thomas, Ian R., Vandaele, Ann Carine, Patel, Manish R., Lopez-Moreno, José-Juan, Bellucci, Giancarlo, Allen, M., Alonso-Rodrigo, G., Altieri, Francesca, Aoki, Shohei, Bauduin, Sophie, Bolsée, David, Clancy, Todd, Cloutis, Edward, D'Aversa, Emiliano, Depiesse, Cédric, Erwin, Justin T., Fedorova, Anna A., Formisano, V., Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez-Galindo, Francisco, Hewson, Will, Holmes, James, Ignatiev, Nikolay I., Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Y., Lanciano, Orietta, Lefèvre, Franck, Lewis, Stephen S.P., López-Puertas, Manuel, López-Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mc Connell, Jack, Nakagawa, Hiromu, Neary, Lori, Neefs, Eddy, Novak, Robert E., Oliva, Fabrizio, Piccialli, A., Renotte, E., Robert, Séverine, Sindoni, G., Stiepen, A., Trokhimovskiy, Alexander, Vander Auwera, Jean, Viscardy, Sébastien, Whiteway, James J.A., Willame, Yannick, Wilquet, Valérie, Wolff, Michael J., Wolkenberg, Paulina, Aparicio del Moral, Beatriz, Barzin, Pascal, Beeckman, Bram, BenMoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, S., Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Hathi, Brijen, Jeronimo, Zafra, Leese, M., Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, José., Morales, Rafael, Orban, Anne, Pastor-Morales, M., Perez-grande, Isabel, Queirolo, Claudio, Gómez-Rodriguez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan-Felipe, Thibert, Tanguy, Liuzzi, Giuliano, Villanueva, Geronimo L., Mumma, Michael J., Smith, Michael D., Daerden, Frank, Ristic, Bojan, Thomas, Ian R., Vandaele, Ann Carine, Patel, Manish R., Lopez-Moreno, José-Juan, Bellucci, Giancarlo, Allen, M., Alonso-Rodrigo, G., Altieri, Francesca, Aoki, Shohei, Bauduin, Sophie, Bolsée, David, Clancy, Todd, Cloutis, Edward, D'Aversa, Emiliano, Depiesse, Cédric, Erwin, Justin T., Fedorova, Anna A., Formisano, V., Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez-Galindo, Francisco, Hewson, Will, Holmes, James, Ignatiev, Nikolay I., Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Y., Lanciano, Orietta, Lefèvre, Franck, Lewis, Stephen S.P., López-Puertas, Manuel, López-Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mc Connell, Jack, Nakagawa, Hiromu, Neary, Lori, Neefs, Eddy, Novak, Robert E., Oliva, Fabrizio, Piccialli, A., Renotte, E., Robert, Séverine, Sindoni, G., Stiepen, A., Trokhimovskiy, Alexander, Vander Auwera, Jean, Viscardy, Sébastien, Whiteway, James J.A., Willame, Yannick, Wilquet, Valérie, Wolff, Michael J., Wolkenberg, Paulina, Aparicio del Moral, Beatriz, Barzin, Pascal, Beeckman, Bram, BenMoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, S., Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Hathi, Brijen, Jeronimo, Zafra, Leese, M., Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, José., Morales, Rafael, Orban, Anne, Pastor-Morales, M., Perez-grande, Isabel, Queirolo, Claudio, Gómez-Rodriguez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan-Felipe, and Thibert, Tanguy

Abstract

info:eu-repo/semantics/published

Published
2019

18. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD

Author

Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), Canadian Space Agency, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Pérez Grande, Isabel, Ristic, Bojan, Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Smith, M.D., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Patel, Manish R., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, Samuel, Gomez, A., Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), Canadian Space Agency, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Pérez Grande, Isabel, Ristic, Bojan, Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Smith, M.D., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Patel, Manish R., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, Samuel, and Gomez, A.

Abstract

It has been suggested that dust storms efficiently transport water vapor from the near-surface to the middle atmosphere on Mars. Knowledge of the water vapor vertical profile during dust storms is important to understand water escape. During Martian Year 34, two dust storms occurred on Mars: a global dust storm (June to mid-September 2018) and a regional storm (January 2019). Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). We show a significant increase of water vapor abundance in the middle atmosphere (40–100 km) during the global dust storm. The water enhancement rapidly occurs following the onset of the storm (Ls~190°) and has a peak at the most active period (Ls~200°). Water vapor reaches very high altitudes (up to 100 km) with a volume mixing ratio of ~50 ppm. The water vapor abundance in the middle atmosphere shows high values consistently at 60°S-60°N at the growth phase of the dust storm (Ls = 195°–220°), and peaks at latitudes greater than 60°S at the decay phase (Ls = 220°–260°). This is explained by the seasonal change of meridional circulation: from equinoctial Hadley circulation (two cells) to the solstitial one (a single pole-to-pole cell). We also find a conspicuous increase of water vapor density in the middle atmosphere at the period of the regional dust storm (Ls = 322–327°), in particular at latitudes greater than 60°S. ©2019. American Geophysical Union. All Rights Reserved.

Published
2019

19. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

Vandaele, Ann Carine, López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Daerden, Frank, Ristic, Bojan, Robert, S., Thomas, Ian R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, S., Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Perez-Grande, I., Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, The NOMAD Team, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Tohoku University [Sendai], 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), Fonds National de la Recherche Scientifique [Bruxelles] (FNRS), York University [Toronto], NASA Goddard Space Flight Center (GSFC), Centre Spatial de Liège (CSL), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Catholic University of America, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, and Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles)

Subjects
010504 meteorology & atmospheric sciences, Solar occultation, education, Physique atomique et moléculaire, Exploration of Mars, 01 natural sciences, Occultation, law.invention, Orbiter, Mars atmosphere, law, 0103 physical sciences, Nadir, Chimie, natural sciences, 010303 astronomy & astrophysics, Spectroscopy, 0105 earth and related environmental sciences, Remote sensing, Ultraviolet, Martian, Astronomy and Astrophysics, Dust, Atmosphere of Mars, Mars Exploration Program, Nadir observations, ExoMars, Trace gas, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Spectroscopie [électromagnétisme, optique, acoustique], 13. Climate action, Space and Planetary Science, Visible, Environmental science, Infrared, Methane, Composition
Abstract

Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.© 2018, The Author(s)., The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by Spanish MICINN through its Plan Nacional and by European funds under grant ESP2015-65064-C2-1-P (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1 and ST/R001405/1 and Italian Space Agency through grant 2018-2-HH.0. The research was performed as part of the >Excellence of Science> project >Evolution and Tracers of Habitability on Mars and the Earth> (30442502). SA acknowledge support from the FNRS, Be.

Published
2018

20. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

Vandaele, A. C., López-Moreno, José Juan, Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, S., Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Perez-Grande, I., Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, The NOMAD Team, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, and Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles)

Subjects
Mars atmosphere, Solar occultation, Visible, Dust, Infrared, Methane, ExoMars, Nadir observations, Spectroscopy, Composition, Ultraviolet
Abstract

Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/) The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.© 2018, The Author(s). The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by Spanish MICINN through its Plan Nacional and by European funds under grant ESP2015-65064-C2-1-P (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1 and ST/R001405/1 and Italian Space Agency through grant 2018-2-HH.0. The research was performed as part of the >Excellence of Science> project >Evolution and Tracers of Habitability on Mars and the Earth> (30442502). SA acknowledge support from the FNRS, Be.

Published
2018

21. Search of CH4 on Mars using EXES aboard SOFIA

Author

Aoki, S., Richter, M. J., DeWitt, C., Boogert, A., Encrenaz, T., Sagawa, H., Nakagawa, H., Vandaele, A. C., GIURANNA, MARCO, Greathouse, T. K., Fouchet, T., Geminale, A., Sindoni, G., McKelvey, M., Case, M., and Kasaba, Y.

Published
2018

22. Search for hydrogen peroxide in the Martian atmosphere by the Planetary Fourier Spectrometer onboard Mars Express

Author

Yasumasa Kasaba, Vittorio Formisano, A. Geminale, Shohei Aoki, Giuseppe Sindoni, Marco Giuranna, and Hiromu Nakagawa

Subjects
Martian, Space and Planetary Science, Planetary Fourier Spectrometer, Mixing ratio, Analytical chemistry, Astronomy and Astrophysics, Mars Exploration Program, Atmosphere of Mars, Spectroscopy, Atmospheric sciences, Spectral line, Latitude
Abstract

We searched for hydrogen peroxide (H2O2) in the Martian atmosphere using data measured by the Planetary Fourier Spectrometer (PFS) onboard Mars Express during five martian years (MY27-31). It is well known that H2O2 plays a key role in the oxidizing capacity of the Martian atmosphere. However, only a few studies based on ground-based observations can be found in the literature. Here, we performed the first analysis of H2O2 using long-term measurements by a spacecraft-borne instrument. We used the ν4 band of H2O2 in the spectral range between 359 cm-1 and 382 cm-1 where strong features of H2O2 are present around 362 cm-1 and 379 cm-1. Since the features were expected to be very weak even at the strong band, sensitive data calibrations were performed and a large number of spectra were selected and averaged. We made three averaged spectra for different seasons over relatively low latitudes (50°S-50°N). We found features of H2O2 at 379 cm-1, whereas no clear features were detected at 362 cm-1 due to large amounts of uncertainty in the data. The derived mixing ratios of H2O2 were close to the detection limits: 16 ± 19 ppb at Ls = 0-120°, 35 ± 32 ppb at Ls = 120-240°, and 41 ± 28 ppb at Ls = 240-360°. The retrieved value showed the detection of H2O2 only for the third seasonal period, and the values in the other periods provided the upper limits. These long-term averaged abundances derived by the PFS generally agreed with the ones reported by ground-based observations. From our derived mixing ratio of H2O2, the lifetime of CH4 in the Martian atmosphere is estimated to be several decades in the shortest case. Our results and sporadic detections of CH4 suggest the presence of strong CH4 sinks not subject to atmospheric oxidation.

Published
2015

23. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Vandaele, Ann Carine, López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Daerden, Frank, Ristic, Bojan, Robert, S., Thomas, Ian R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, Samuel, Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Pérez Grande, Isabel, Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, The NOMAD Team, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Vandaele, Ann Carine, López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Daerden, Frank, Ristic, Bojan, Robert, S., Thomas, Ian R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, Samuel, Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Pérez Grande, Isabel, Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, and The NOMAD Team

Abstract

The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.© 2018, The Author(s).

Published
2018

24. Sensitive search of CH4 on Mars by SOFIA/EXES

Author

Aoki, S., Richter, M. J., DeWitt, C., Boogert, A., Encrenaz, T., Sagawa, H., Nakagawa, H., Vandaele, A. C., GIURANNA, MARCO, Greathouse, T. K., Fouchet, T., Geminale, A., Sindoni, G., McKelvey, M., Case, M., Kasaba, Y., Department of Physics and Astronomy [Univ California Davis] (Physics - UC Davis), University of California [Davis] (UC Davis), University of California (UC)-University of California (UC), Universities Space Research Association, Stratospheric Observatory for Infrared Astronomy, NASA Ames Research Center, MS 232-11, Moffett Field, CA 94035, USA, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Faculty of Science, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan, Department of Geophysics, Tohoku University, Institut royal d'Aéronomie Spatiale de Belgique (IASB), Istituto di Astrofisica e Planetologia Spaziali, INAF (IAPS), and Southwest Research Institute, Division 15

Subjects
Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; We present the results of our sensitive search of CH4 on Mars using the Echelon-Cross-Echelle Spectrograph (EXES) onboard the Stratospheric Observatory for Infrared Astronomy (SOFIA).

Published
2017

25. Properties of a Martian local dust storm in Atlantis Chaos from OMEGA/MEX data

Author

Giuseppe Sindoni, Fabrizio Oliva, Giancarlo Bellucci, Davide Grassi, A. Geminale, Filippo Giacomo Carrozzo, Francesca Altieri, Emiliano D'Aversa, and ITA

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Atmospheric sciences, 01 natural sciences, Physics::Geophysics, Atmosphere, Atmospheric radiative transfer codes, Dust storm, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, Optical depth, 0105 earth and related environmental sciences, Martian, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Storm, Atmosphere of Mars, Mars Exploration Program, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

In this study we present the analysis of the dust properties of a local storm imaged in the Atlantis Chaos region on Mars by the OMEGA imaging spectrometer on March 2nd, 2005. We use the radiative transfer model MITRA to study the dust properties at solar wavelengths between 0.5 μm and 2.5 μm and infer the connection between the local storm dynamics and the topography. We retrieve maps of effective grain radius (reff), optical depth at 9.3 μm (τ9.3) and top altitude (ta) of the dust layer. Our results show that large particles (reff = 1.6 μm) are gathered in the centre of the storm (lat = 33.5° S; lon = 183.5° W), where the optical depth is maximum (τ9.3 > 7.0) and the top altitude exceeds 18 km. Outside the storm, we obtain τ9.3We speculate that a low thermal inertia region at the western border of Atlantis Chaos is a possible source of the dust storm. Moreover, we find evidence that topography plays a role in confining the local storm in Atlantis Chaos. The vertical wind component from the GCM does not provide any hint for the triggering of dust lifting. On the other hand, the combination of the horizontal and vertical wind profiles suggests that the dust, once lifted, is pushed eastward and then downward and gets confined within the north-east ridge of Atlantis Chaos. From our results, the thickness of the dust layer collapsed on the surface ranges from about 1 μm at the storm boundaries up to more than 100 μm at its centre. We verify that a layer of dust thicker than 1 μm, deposited on the surface, can prevent the detection of mafic absorption features. However, such features are still present in OMEGA data of Atlantis Chaos registered after the storm. Hence, we deduce that, once the storm is over, the dust deposited on an area larger than the one where it has been observed.

Published
2017
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27. Science objectives and performances of NOMAD, a spectrometer suite for the ExoMars TGO mission

Author

Vandaele, A. C, Neefs, E., Drummond, R., Thomas, I. R., Daerden, F., Lopez Moreno, J. J., Rodriguez, J., Patel, M. R., Bellucci, G., Allen, M., Altieri, F., Bolsée, D., Clancy, T., Delanoye, S., Depiesse, C., Cloutis, E., Fedorova, A., Formisano, V., Funke, B., Fussen, D., Geminale, A., Gérard, J. C., Giuranna, M., Ignatiev, N., Kaminski, J., Karatekin, O., Lefèvre, F., López Puertas, M., López Valverde, M., Mahieux, A., Mcconnell, J., Mumma, M., Neary, L., Renotte, E., Ristic, B., Robert, S., Smith, M., Trokhimovsky, S., Vanderauwera, J., Villanueva, G., Whiteway, J., Wilquet, V., Wolff, M., Vandaele, Ann Carine, Lopez Moreno, Jose Juan, Bellucci, Giancarlo, Patel, Manish, Allen, Mark, Altieri, Francesca, Aoki, Shohei, Bolsée, David, Clancy, Todd, Cloutis, Edward, Daerden, Frank, Depiesse, Cédric, Fedorova, Anna, Formisano, Vittorio, Funke, Bernd, Fussen, Didier, Garcia Comas, Maya, Geminale, Anna, Gérard, Jean Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez Galindo, Francisco, Ignatiev, Nicolai, Kaminski, Jacek, Karatekin, Ozgur, Kasabe, Yasumasa, Lefèvre, Franck, Lewis, Stephen, López Puertas, Manuel, López Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mumma, Mike, Neary, Lori, Neefs, Eddy, Renotte, Etienne, Robert, Séverine, Sindoni, Giuseppe, Smith, Mike, Thomas, Ian R., Trokhimovsky, Sacha, Vander Auwera, Jean, Villanueva, Geronimo, Whiteway, Jim, Willame, Yannick, Wilquet, Valerie, Wolff, Mike, Alonso Rodrigo, Gustavo, Aparicio Del Moral, Beatriz, Barzin, Pascal, Ben Moussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, Sabrina, Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Delanoye, Sofie, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Zafra, Jose Jeronimo, Leese, Mark, Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, Jose, Morales, Rafael, Orban, Anne, Pastor Morales, Maria Del Carmen, Perez Grande, Isabel, Ristic, Bojan, Rodriguez Gomez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan Felipe, Thibert, Tanguy, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), The Open University [Milton Keynes] (OU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, York University [Toronto], Royal Observatory of Belgium [Brussels] (ROB), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Centre Spatial de Liège (CSL), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), and Catholic University of America

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Solar, Occultation, law.invention, Orbiter, Mars atmosphere, law, Nadir, Aerosol, Observations, Spectroscopy, Ultraviolet, Remote sensing, Spectrometer, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Suite, Astronomy and Astrophysics, Mars Exploration Program, Atmosphere of Mars, ExoMars, Trace gas, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, Visible, Composition, Infrared, Methane, Occultation Nadir, Environmental science
Abstract

International audience; The NOMAD spectrometer suite on the ExoMars Trace Gas Orbiter will map the composition and distribution of Mars' atmospheric trace species in unprecedented detail, fulfilling many of the scientific objectives of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument is a combination of three channels, covering a spectral range from the UV to the IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and how these objectives have influenced the design of the channels. We also discuss the expected performance of the instrument in terms of coverage and detection sensitivity.

Published
2015

28. Stringent upper limit of CH4 on Mars based on SOFIA/EXES observations

Author

Aoki, S., primary, Richter, M.J., additional, DeWitt, C., additional, Boogert, A., additional, Encrenaz, T., additional, Sagawa, H., additional, Nakagawa, H., additional, Vandaele, A. C., additional, Giuranna, M., additional, Greathouse, T. K., additional, Fouchet, T., additional, Geminale, A., additional, Sindoni, G., additional, McKelvey, M., additional, Case, M., additional, and Kasaba, Y., additional

Published
2018
Full Text
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29. Expected performances of the NOMAD/ExoMars instrument

Author

Robert, S, Vandaele, A. C., Thomas, I., Willame, Y., Daerden, F., Delanoye, S., Depiesse, C., Drummond, R., Neefs, E., Neary, L., Ristic, B., Mason, J., Lopez Moreno, J. J., Rodriguez Gomez, J., Patel, M. R., Bellucci, G., Patel, M., Allen, M., Altieri, F., Aoki, S., Bolsée, D., Clancy, T., Cloutis, E., Fedorova, A., Formisano, V., Funke, B., Fussen, D., Garcia Comas, M., Geminale, A., Gérard, J. C., Gillotay, D., Giuranna, M., Gonzalez Galindo, F., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Lefèvre, F., Lewis, S., López Puertas, M., López Valverde, M., Mahieux, A., Mcconnell, J., Mumma, M., Novak, R., Renotte, E., Robert, S., Sindoni, G., Smith, M., Thomas, I. R., Trokhimovskiy, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Wilquet, V., Wolff, M., Alonso Rodrigo, G., Aparicio Del Moral, B., Barzin, P., Ben Moussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G., Clairquin, R., Cubas, J., Giordanengo, B., Gissot, S., Gomez, A., Zafra, J. J., Leese, M., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, R., Orban, A., Pastor Morales, M., Perez Grande, I., Saggin, Bortolino, Samain, V., Sanz Andres, A., Sanz, R., Simar, J. F., Thibert, T., UK Space Agency, Belgian Science Policy Office, European Commission, and European Space Agency

Subjects
ExoMars ESA mission, 010504 meteorology & atmospheric sciences, Mars, NOMAD instrument, 01 natural sciences, Occultation, law.invention, Orbiter, law, 0103 physical sciences, Nadir, Radiative transfer, Abundances, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, atmosphere [Mars], Spectrometer, Mars, atmosphere, Astronomy and Astrophysics, Space and Planetary Science, Astronomy, Mars Exploration Program, Atmosphere of Mars, Trace gas, 13. Climate action, atmosphere, Mars: atmosphere, Environmental science
Abstract

NOMAD (Nadir and Occultation for MArs Discovery) is one of the four instruments on board the ExoMars Trace Gas Orbiter, scheduled for launch in March 2016. It consists of a suite of three high-resolution spectrometers - SO (Solar Occultation), LNO (Limb, Nadir and Occultation) and UVIS (Ultraviolet and Visible Spectrometer). Based upon the characteristics of the channels and the values of Signal-to-Noise Ratio obtained from radiometric models discussed in (Vandaele et al., 2015a, 2015b; Thomas et al., 2016), the expected performances of the instrument in terms of sensitivity to detection have been investigated. The analysis led to the determination of detection limits for 18 molecules, namely CO, HO, HDO, CH, CH, CH, HCO, CH, SO, HS, HCl, HCN, HO, NH, NO, NO, OCS, O. NOMAD should have the ability to measure methane concentrations, NOMAD has been made possible thanks to funding by the Belgian Science Policy Office (BELSPO) and financial and contractual coordination by the ESA Prodex Office (PlanetADAM no 4000107727). The research was performed as part of the >Inter-university Attraction Poles> programme financed by the Belgian Government (Planet TOPERS no P7-15) and a BRAIN Research Grant BR/143/A2/SCOOP. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under Grant Agreement no. 607177 CrossDrive. UK funding is acknowledged under the UK Space Agency Grant ST/I003061/1.

Published
2016

30. Optical and radiometric models of the NOMAD instrument part II: The infrared channels - SO and LNO

Author

Thomas, I. R., Vandaele, A. C., Robert, S., Neefs, E., Drummond, R., Daerden, F., Delanoye, S., Ristic, B., Berkenbosch, S., Clairquin, R., Maes, J., Bonnewijn, S., Depiesse, C., Mahieux, A., Trompet, L., Neary, L., Willame, Y., Wilquet, V., Nevejans, D., Aballea, L., Moelans, W., De Vos, L., Lesschaeve, S., Van Vooren, N., Lopez Moreno, J. J., Patel, M. R., Bellucci, G., Vandaele, Ann Carine, Moreno, Lopez, Juan, Jose, Bellucci, Giancarlo, Patel, Manish, Allen, Mark, Altieri, Francesca, Aoki, Shohei, Bolsée, David, Clancy, Todd, Cloutis, Edward, Daerden, Frank, Depiesse, Cédric, Fedorova, Anna, Formisano, Vittorio, Funke, Bernd, Fussen, Didier, Garcia Comas, Maya, Geminale, Anna, Gérard, Jean Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez Galindo, Francisco, Ignatiev, Nicolai, Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Yasumasa, Lefèvre, Franck, Lewis, Stephen, López Puertas, Manuel, López Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mcconnell, Jack, Mumma, Mike, Neary, Lori, Neefs, Eddy, Novak, Robert, Renotte, Etienne, Robert, Séverine, Sindoni, Giuseppe, Smith, Mike, Thomas, Ian R., Trokhimovsky, Sacha, Vander Auwera, Jean, Villanueva, Geronimo, Whiteway, Jim, Willame, Yannick, Wilquet, Valerie, Wolff, Mike, Alonso Rodrigo, Gustavo, Aparicio Del Moral, Beatriz, Barzin, Pascal, Benmoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, Sabrina, Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Delanoye, Sofie, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Zafra, Jose Jeronimo, Leese, Mark, Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, Jose, Morales, Rafael, Orban, Anne, Del Carmen Pastor Morales, Maria, Perez Grande, Isabel, Ristic, Bojan, Rodriguez Gomez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan Felipe, Thibert, Tanguy, Belgian Science Policy Office, European Space Agency, and UK Space Agency

Subjects
Physics, Martian, 010504 meteorology & atmospheric sciences, Spectrometer, Atmospheric composition, Spectrometers and spectroscopic instrumentation, 01 natural sciences, Occultation, Atomic and Molecular Physics, and Optics, Trace gas, law.invention, Remote sensing and sensors, Orbiter, Space instrumentation, Atmosphere of Earth, law, Atomic and Molecular Physics, Martian surface, 0103 physical sciences, Nadir, Radiative transfer, and Optics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing
Abstract

NOMAD is a suite of three spectrometers that will be launched in 2016 as part of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument contains three channels that cover the IR and UV spectral ranges and can perform solar occultation, nadir and limb observations, to detect and map a wide variety of Martian atmospheric gases and trace species. Part I of this work described the models of the UVIS channel; in this second part, we present the optical models representing the two IR channels, SO (Solar Occultation) and LNO (Limb, Nadir and Occultation), and use them to determine signal to noise ratios (SNRs) for many expected observational cases. In solar occultation mode, both the SO and LNO channel exhibit very high SNRs >5000. SNRs of around 100 were found for the LNO channel in nadir mode, depending on the atmospheric conditions, Martian surface properties, and observation geometry., NOMAD has been made possible thanks to funding by the Belgian Science Policy Office (BELSPO) and financial and contractual coordination by the ESA Prodex Office. The research was performed as part of the “Interuniversity Attraction Poles” programme financed by the Belgian government (Planet TOPERS). UK funding is acknowledged under the UK Space Agency grant ST/I003061/1.

Published
2016

31. Stringent upper limit of CH4 on Mars based on SOFIA/EXES observations

Author

Matthew J. Richter, M. Case, Hiromu Nakagawa, C. DeWitt, Adwin Boogert, Giuseppe Sindoni, Thomas K. Greathouse, Marco Giuranna, Yasumasa Kasaba, Hideo Sagawa, Thérèse Encrenaz, Ann Carine Vandaele, Shohei Aoki, M. McKelvey, A. Geminale, Thierry Fouchet, University of California [Davis] (UC Davis), University of California, 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), Center for Mathematical Sciences, The University of Aizu, National Agriculture and Food Research Organization, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Southwest Research Institute [San Antonio] (SwRI), Tohoku University [Sendai], 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), and National Agriculture and Food Research Organization (NARO)

Subjects
[PHYS]Physics [physics], Martian, Physics, 010504 meteorology & atmospheric sciences, Stratospheric Observatory for Infrared Astronomy, Northern Hemisphere, Astronomy and Astrophysics, Atmosphere of Mars, Mars Exploration Program, Effects of high altitude on humans, 01 natural sciences, Astrobiology, Atmosphere, 13. Climate action, Space and Planetary Science, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Spectrograph, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

Discovery of CH4 in the Martian atmosphere has led to much discussion since it could be a signature of biological and/or geological activities on Mars. However, the presence of CH4 and its temporal and spatial variations are still under discussion because of the large uncertainties embedded in the previous observations. We performed sensitive measurements of Martian CH4 by using the Echelon-Cross-Echelle Spectrograph (EXES) onboard the Stratospheric Observatory for Infrared Astronomy (SOFIA) on 16 March 2016, which corresponds to summer (Ls = 123.2∘) in the northern hemisphere on Mars. The high altitude of SOFIA (~13.7 km) enables us to significantly reduce the effects of terrestrial atmosphere. Thanks to this, SOFIA/EXES improves our chances of detecting Martian CH4 lines because it reduces the impact of telluric CH4 on Martian CH4, and allows us to use CH4 lines in the 7.5 μm band which has less contamination. However, our results show no unambiguous detection of Martian CH4. The Martian disk was spatially resolved into 3 × 3 areas, and the upper limits on the CH4 volume mixing ratio range from 1 to 9 ppb across the Martian atmosphere, which is significantly less than detections in several other studies. These results emphasize that release of CH4 on Mars is sporadic and/or localized if the process is present.

Published
2018

32. Optical and radiometric models of the NOMAD instrument part I: the UVIS channel

Author

Vandaele, Ann C., Willame, Yannick, Depiesse, Cédric, Thomas, Ian R., Robert, Séverine, Bolsée, David, Patel, Manish R., Mason, Jon P., Leese, Mark, Lesschaeve, Stefan, Antoine, Philippe, Daerden, Frank, Delanoye, Sofie, Drummond, Rachel, Neefs, Eddy, Ristic, Bojan, Lopez Moreno, José Juan, Bellucci, Giancarlo, Allen, M., Altieri, F., Aoki, S., Clancy, T., Cloutis, E., Fedorova, A., Formisano, V., Funke, B., Fussen, D., Garcia Comas, M., Geminale, A., Gérard, J. C., Gillotay, D., Giuranna, M., Gonzalez Galindo, F., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Lefèvre, F., Lewis, S., López Puertas, M., López Valverde, M., Mahieux, A., Mumma, M., Neary, L., Novak, R., Renotte, E., Sindoni, G., Smith, M., Trokhimovskiy, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Wilquet, V., Wolff, M., Alonso Rodrigo, G., Aparicio Del Moral, B., Barzin, P., Benmoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G., Clairquin, R., Cubas, J., Giordanengo, B., Gissot, S., Gomez, A., Zafra, J. J., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, R., Orban, A., Pastor Morales, M., Perez Grande, I., Rodriguez Gomez, J., Saggin, Bortolino, Samain, V., Sanz Andres, A., Sanz, R., Simar, J. F., Thibert, T., European Space Agency, UK Space Agency, and Belgian Science Policy Office

Subjects
Solar occultation, Radiometric model, Occultation, Signal, law.invention, Orbiter, Optics, law, Atomic and Molecular Physics, Nadir, Optical constants, Science objectives, Remote sensing, Physics, Martian, business.industry, Signal to noise, Atmosphere of Mars, IR spectral range, Atomic and Molecular Physics, and Optics, Trace gas, Wavelength, Optical models, Atmospheric absorption, and Optics, business, Martian atmospheres
Abstract

The NOMAD instrument has been designed to best fulfil the science objectives of the ExoMars Trace Gas Orbiter mission that will be launched in 2016. The instrument is a combination of three channels that cover the UV, visible and IR spectral ranges and can perform solar occultation, nadir and limb observations. In this series of two papers, we present the optical models representing the three channels of the instrument and use them to determine signal to noise levels for different observation modes and Martian conditions. In this first part, we focus on the UVIS channel, which will sound the Martian atmosphere using nadir and solar occultation viewing modes, covering the 200-650nm spectral range. High SNR levels (, NOMAD has been made possible thanks to funding by the Belgian Science Policy Office (BELSPO) and financial and contractual coordination by the ESA Prodex Office (contracts no 4000107727 and 4000103401). The research was performed as part of the >Interuniversity Attraction Poles> programme financed by the Belgian government (Planet TOPERS, contract PAI no P7/15). UK funding is acknowledged under the UK Space Agency grant ST/I003061/1.

Published
2015

33. Anomalous dust to gas ratios in the Galaxy

Author

Paola Mazzei, G. Barbaro, Emanuele Congiu, and Anna Geminale

Subjects
Interstellar medium, Physics, History, Hydrogen molecule, Extinction (astronomy), Astrophysics, Galaxy, Computer Science Applications, Education
Abstract

Lines of sight with E(B-V)/N(HI) considerably smaller than the average value for the solar neighbourhood have been selected from the catalogue of Diplas and Savage. In order to develop quantitative considerations, estimates of the molecular hydrogen column density were obtained using the relation of Savage et al. extended to E(B-V)>0.4 with the recent data of Rachford et al. Contrary to the prevaling opinion in the literature for lines of sight with similar behaviour, we found that only 22 per cent of our sample was characterized by both an average gas density larger than 1 cm−3 and a value of RV larger than that in the diffuse interstellar medium. By computing extinction models, we were able to fit the E(B-V)/N(HI) by changing the value of RV only for some lines of sight. For the remaining ones, a ρd/ρH ratio different from the average Galactic value must be invoked. The application of the Kramers-Kronig relation to the observed extinction curves confirmed this possibility. Moreover, attemps to fit such curves with models having grain volumes corresponding to the standard ρd/ρH ratio failed.

Published
2005

34. Expected performances of the NOMAD/ExoMars instrument

Author

UK Space Agency, Belgian Science Policy Office, European Commission, European Space Agency, Vandaele, Ann Carine, López-Moreno, José Juan, Bellucci, Giancarlo, Patel, M., Allen, M., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Daerden, Frank, Depiesse, C., Fedorova, A., Formisano, V., Funke, Bernd, Fussen, D., García Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, D., Giuranna, M., González-Galindo, F., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Lefèvre, F., Lewis, S., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Novak, R., Renotte, E., Robert, S., Sindoni, G., Smith, M., Thomas, Ian R., Trokhimovskiy, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wilquet, V., Wolff, Michael T., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G., Clairquin, R., Cubas, J., Delanoye, S., Giordanengo, B., Gissot, Samuel, Gomez, A., Zafra, J.-J., Leese, M., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Pérez Grande, Isabel, Ristic, Bojan, Rodríguez Gómez, Julio, Saggin, B., Samain, V., Sanz Andres, A., Sanz, R., Simar, J.-F., Thibert, T., Alonso-Rodrigo, G., UK Space Agency, Belgian Science Policy Office, European Commission, European Space Agency, Vandaele, Ann Carine, López-Moreno, José Juan, Bellucci, Giancarlo, Patel, M., Allen, M., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Daerden, Frank, Depiesse, C., Fedorova, A., Formisano, V., Funke, Bernd, Fussen, D., García Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, D., Giuranna, M., González-Galindo, F., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Lefèvre, F., Lewis, S., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Novak, R., Renotte, E., Robert, S., Sindoni, G., Smith, M., Thomas, Ian R., Trokhimovskiy, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wilquet, V., Wolff, Michael T., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G., Clairquin, R., Cubas, J., Delanoye, S., Giordanengo, B., Gissot, Samuel, Gomez, A., Zafra, J.-J., Leese, M., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Pérez Grande, Isabel, Ristic, Bojan, Rodríguez Gómez, Julio, Saggin, B., Samain, V., Sanz Andres, A., Sanz, R., Simar, J.-F., Thibert, T., and Alonso-Rodrigo, G.

Abstract

NOMAD (Nadir and Occultation for MArs Discovery) is one of the four instruments on board the ExoMars Trace Gas Orbiter, scheduled for launch in March 2016. It consists of a suite of three high-resolution spectrometers - SO (Solar Occultation), LNO (Limb, Nadir and Occultation) and UVIS (Ultraviolet and Visible Spectrometer). Based upon the characteristics of the channels and the values of Signal-to-Noise Ratio obtained from radiometric models discussed in (Vandaele et al., 2015a, 2015b; Thomas et al., 2016), the expected performances of the instrument in terms of sensitivity to detection have been investigated. The analysis led to the determination of detection limits for 18 molecules, namely CO, HO, HDO, CH, CH, CH, HCO, CH, SO, HS, HCl, HCN, HO, NH, NO, NO, OCS, O. NOMAD should have the ability to measure methane concentrations <25 parts per trillion (ppt) in solar occultation mode, and 11 parts per billion in nadir mode. Occultation detections as low as 10 ppt could be made if spectra are averaged (Drummond et al., 2011). Results have been obtained for all three channels in nadir and in solar occultation.© 2016 The Authors. Published by Elsevier Ltd.

Published
2016

35. Optical and radiometric models of the NOMAD instrument part II: The infrared channels - SO and LNO

Author

Belgian Science Policy Office, European Space Agency, UK Space Agency, Thomas, Ian R., Vandaele, Ann Carine, Robert, S., Neefs, E., Drummond, R., Daerden, Frank, Delanoye, S., Ristic, Bojan, Berkenbosch, S., Clairquin, R., Maes, J., Bonnewijn, S., Depiesse, C., Mahieux, A., Trompet, L., Neary, L., Willame, Y., Wilquet, V., Nevejans, D., Aballea, L., Moelans, W., De Vos, L., Lesschaeve, S., Van Vooren, N., López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Moreno, L., Juan, J., Patel, M., Allen, M., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Fedorova, A., Formisano, V., Funke, Bernd, Fussen, D., García Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, D., Giuranna, M., Belgian Science Policy Office, European Space Agency, UK Space Agency, Thomas, Ian R., Vandaele, Ann Carine, Robert, S., Neefs, E., Drummond, R., Daerden, Frank, Delanoye, S., Ristic, Bojan, Berkenbosch, S., Clairquin, R., Maes, J., Bonnewijn, S., Depiesse, C., Mahieux, A., Trompet, L., Neary, L., Willame, Y., Wilquet, V., Nevejans, D., Aballea, L., Moelans, W., De Vos, L., Lesschaeve, S., Van Vooren, N., López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Moreno, L., Juan, J., Patel, M., Allen, M., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Fedorova, A., Formisano, V., Funke, Bernd, Fussen, D., García Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, D., and Giuranna, M.

Abstract

NOMAD is a suite of three spectrometers that will be launched in 2016 as part of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument contains three channels that cover the IR and UV spectral ranges and can perform solar occultation, nadir and limb observations, to detect and map a wide variety of Martian atmospheric gases and trace species. Part I of this work described the models of the UVIS channel; in this second part, we present the optical models representing the two IR channels, SO (Solar Occultation) and LNO (Limb, Nadir and Occultation), and use them to determine signal to noise ratios (SNRs) for many expected observational cases. In solar occultation mode, both the SO and LNO channel exhibit very high SNRs >5000. SNRs of around 100 were found for the LNO channel in nadir mode, depending on the atmospheric conditions, Martian surface properties, and observation geometry.

Published
2016

36. Science objectives and performances of NOMAD, a spectrometer suite for the ExoMars TGO mission

Author

Vandaele, Ann Carine, Neefs, Eddy, Drummond, Rachel, Thomas, I.R., Daerden, F., Lopez-Moreno, J.-J., Rodriguez, J., Patel, M.R., Bellucci, G., Allen, M., Altieri, F., Bolsée, D., Clancy, T., Delanoye, S., Depiesse, Cédric, Cloutis, E., Fedorova, A., Formissano, V., Funke, Bernd, Fussen, Didier, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Ignatiev, N., Kaminski, J., Karatekin, Ozgur, Lefèvre, F., Lopez-Puertas, Manuel, Lopez-Valverde, M.A., Mahieux, Arnaud, McConnell, John, Mumma, M., Neary, L., Renotte, E., Ristic, B., Robert, Séverine, Smith, M, Trokhimovsky, S., Vander Auwera, Jean, Villanueva, G., Whiteway, J.A., Wilquet, Valérie, Wolff, Michel, Vandaele, Ann Carine, Neefs, Eddy, Drummond, Rachel, Thomas, I.R., Daerden, F., Lopez-Moreno, J.-J., Rodriguez, J., Patel, M.R., Bellucci, G., Allen, M., Altieri, F., Bolsée, D., Clancy, T., Delanoye, S., Depiesse, Cédric, Cloutis, E., Fedorova, A., Formissano, V., Funke, Bernd, Fussen, Didier, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Ignatiev, N., Kaminski, J., Karatekin, Ozgur, Lefèvre, F., Lopez-Puertas, Manuel, Lopez-Valverde, M.A., Mahieux, Arnaud, McConnell, John, Mumma, M., Neary, L., Renotte, E., Ristic, B., Robert, Séverine, Smith, M, Trokhimovsky, S., Vander Auwera, Jean, Villanueva, G., Whiteway, J.A., Wilquet, Valérie, and Wolff, Michel

Abstract

The NOMAD spectrometer suite on the ExoMars Trace Gas Orbiter will map the composition and distribution of Mars atmospheric trace species in unprecedented detail, fulfilling many of the scientific objectives of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument is a combination of three channels, covering a spectral range from the UV to the IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and how these objectives have influenced the design of the channels. We also discuss the expected performance of the instrument in terms of coverage and detection sensitivity., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2015

37. Can CCM law properly represent all extinction curves?

Author

Anna Geminale and P. Popowski

Subjects
Physics, History, Wavelength range, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, medicine.disease_cause, Computer Science Applications, Education, Large sample, Interstellar medium, Wavelength, Extinction (optical mineralogy), Law, medicine, Ultraviolet, Astrophysics::Galaxy Astrophysics
Abstract

We present the analysis of a large sample of lines of sight with extinction curves covering wavelength range from near-infrared (NIR) to ultraviolet (UV). We derive total to selective extinction ratios based on the Cardelli, Clayton and Mathis (1989, CCM) law, which is typically used to fit the extinction data both for diffuse and dense interstellar medium. We conclude that the CCM law is able to fit most of the extinction curves in our sample. We divide the remaining lines of sight with peculiar extinction into two groups according to two main behaviors: a) the optical/IR or/and UV wavelength region cannot be reproduced by the CCM formula; b) the optical/NIR and UV extinction data are best fit by the CCM law with different values of R_V. We present examples of such curves. The study of both types of peculiar cases can help us to learn about the physical processes that affect dust in the interstellar medium, e.g., formation of mantles on the surface of grains, evaporation, growing or shattering., 6 pages, 4 figures, in "Light, dust and chemical evolution", Journal of Physics: Conference Series

Published
2005

38. Optical photometry and spectral classification in the field of the open cluster NGC 6996 in the North America Nebula

Author

Gustavo Baume, Giovanni Carraro, Sandro Villanova, and Anna Geminale

Subjects
Physics, Nebula, Ciencias Astronómicas, Galaxy: open clusters and associations: individual NGC 6996, Astrophysics (astro-ph), Extinction (astronomy), Near-infrared spectroscopy, FOS: Physical sciences, Astronomy and Astrophysics, Galaxy: Open clusters and associations: general, Astrophysics, Open clusters and associations: general [Galaxy], Stellar classification, Photometry (astronomy), Stars, Space and Planetary Science, Cluster (physics), open clusters and associations: individual NGC 6996 [Galaxy], Open cluster
Abstract

We present and discuss broad band CCD $UBV(I)_C$ photometry and low resolution spectroscopy for stars in the region of the open cluster NGC 6996, located in the North America Nebula. The new data allow us to tightly constrain the basic properties of this object. We revise the cluster size, which in the past has been significantly underestimated. The width of the Main Sequence is mainly interpreted in terms of differential reddening, and indeed the stars' color excess $E_{B-V}$ ranges from 0.43 to 0.65, implying the presence of a significant and evenly distributed dust component. We cross-correlate our optical photometry with near infrared from 2MASS, and by means of spectral classification we are able to build up extinction curves for an handful of bright members. We find that the reddening slope and the total to selective absorption ratio $R_V$ toward NGC 6996 are anomalous. Moreover the reddening corrected colors and magnitudes allow us to derive estimates for the cluster distance and age, which turn out to be $760 \pm 70 pc$ ($V_{0}-M_{V} = 9.4 \pm 0.2$) and $\sim 350$ Myr, respectively. Basing on our results, we suggest that NGC 6996 is located in front of the North America Nebula, and does not seem to have any apparent relationship with it., Comment: 19 pages, 12 eps figures, in press in A&A

Published
2004

43. Removal of atmospheric features in near infrared spectra by means of principal component analysis and target transformation on Mars: I. Method

Author

Roberto Orosei, Emiliano D'Aversa, Filippo Giacomo Carrozzo, Francesca Altieri, A. Geminale, Giovanna Serventi, Maria Sgavetti, Davide Grassi, Alessandro Frigeri, Cristian Carli, Giancarlo Bellucci, and ITA

Subjects
Mineral hydration, education.field_of_study, Materials science, 010504 meteorology & atmospheric sciences, Population, Mineralogy, Astronomy and Astrophysics, Context (language use), Atmosphere of Mars, Mars Exploration Program, 01 natural sciences, Spectral line, Space and Planetary Science, Martian surface, 0103 physical sciences, Principal component analysis, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing
Abstract

Acknowledgments We thank the Italian Institute of Astrophysics INAF for the financial support within the project PRIN-INAF 2011. We are thankful to OMEGA team and ESA staff for scientific, operational and technical supports. The aim of this work is to extract the surface contribution in the martian visible/near-infrared spectra removing the atmospheric components by means of Principal Component Analysis (PCA) and target transformation (TT). The developed technique is suitable for separating spectral components in a data set large enough to enable an effective usage of statistical methods, in support to the more common approaches to remove the gaseous component. In this context, a key role is played by the estimation, from the spectral population, of the covariance matrix that describes the statistical correlation of the signal among different points in the spectrum. As a general rule, the covariance matrix becomes more and more meaningful increasing the size of initial population, justifying therefore the importance of sizable datasets. Data collected by imaging spectrometers, such as the OMEGA (Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité) instrument on board the ESA mission Mars Express (MEx), are particularly suitable for this purpose since it includes in the same session of observation a large number of spectra with different content of aerosols, gases and mineralogy. The methodology presented in this work has been first validated using a simulated dataset of spectra to evaluate its accuracy. Then, it has been applied to the analysis of OMEGA sessions over Nili Fossae and Mawrth Vallis regions, which have been already widely studied because of the presence of hydrated minerals. These minerals are key components of the surface to investigate the presence of liquid water flowing on the martian surface in the Noachian period. Moreover, since a correction for the atmospheric aerosols (dust) component is also applied to these observations, the present work is able to completely remove the atmospheric contribution from the analysed spectra. Once the surface reflectance, free from atmospheric contributions, has been obtained, the Modified Gaussian Model (MGM) has been applied to spectra showing the hydrated phase. Silicates and iron-bearing hydrated minerals have been identified by means of the electronic transitions of Fe2+ between 0.8 and 1.2 μm, while at longer wavelengths the hydrated mineralogy is identified by overtones of the OH group. Surface reflectance spectra, as derived through the method discussed in this paper, clearly show a lower level of the atmospheric residuals in the 1.9 hydration band, thus resulting in a better match with the MGM deconvolution parameters found for the laboratory spectra of martian hydrated mineral analogues and allowing a deeper investigation of this spectral range.

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44. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

Vandaele, A. C., Lopez-Moreno, J. -J., Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, R. T., Cloutis, E., Depiesse, C., Drummond, R. J., Fedorova, A., Formisano, V., Funke, B., González-Galindo, F., Geminale, A., Gérard, J. -C., Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, M., López-Valverde, M., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, M. J., the NOMAD team, Vandaele, A. C., Lopez-Moreno, J. -J., Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, R. T., Cloutis, E., Depiesse, C., Drummond, R. J., Fedorova, A., Formisano, V., Funke, B., González-Galindo, F., Geminale, A., Gérard, J. -C., Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, M., López-Valverde, M., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, M. J., and the NOMAD team

Abstract

The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.

45. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

Vandaele, A. C., Lopez-Moreno, J. -J., Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, R. T., Cloutis, E., Depiesse, C., Drummond, R. J., Fedorova, A., Formisano, V., Funke, B., González-Galindo, F., Geminale, A., Gérard, J. -C., Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, M., López-Valverde, M., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, M. J., the NOMAD team, Vandaele, A. C., Lopez-Moreno, J. -J., Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, R. T., Cloutis, E., Depiesse, C., Drummond, R. J., Fedorova, A., Formisano, V., Funke, B., González-Galindo, F., Geminale, A., Gérard, J. -C., Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, M., López-Valverde, M., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, M. J., and the NOMAD team

Abstract

The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.

46. Core and Panmetabolism in Escherichia coli

Author

David Vallenet, François Le Fèvre, Pierre-Yves Bourguignon, Maxime Durot, Victor Sabarly, Claudine Médigue, Vincent Schächter, Gilles Vieira, Odile Bouvet, Damien Mornico, Erick Denamur, Unité de recherche en génomique végétale (URGV), Institut National de la Recherche Agronomique (INRA)-Université d'Évry-Val-d'Essonne (UEVE)-Centre National de la Recherche Scientifique (CNRS), Génomique métabolique (UMR 8030), Genoscope - Centre national de séquençage [Evry] (GENOSCOPE), Université Paris-Saclay-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université d'Évry-Val-d'Essonne (UEVE)-Centre National de la Recherche Scientifique (CNRS), Génétique Quantitative et Evolution - Le Moulon (Génétique Végétale) (GQE-Le Moulon), Centre National de la Recherche Scientifique (CNRS)-AgroParisTech-Université Paris-Sud - Paris 11 (UP11)-Institut National de la Recherche Agronomique (INRA), Université Paris Diderot - Paris 7 (UPD7), French National Research Agency (ANR) [ANR-08-SYSC-011], European Commission [222886-2], Fondation pour le Recherche Medicale, Delegation Geminale pour l'Armement, and Institut National de la Recherche Agronomique (INRA)-Université Paris-Sud - Paris 11 (UP11)-AgroParisTech-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDV]Life Sciences [q-bio], medicine.disease_cause, Microbiology, Genome, 03 medical and health sciences, Phylogenetics, SHIGELLA, Escherichia coli, medicine, ANTIVIRULENCE LOCI, COMPLETE GENOME SEQUENCE, [SDV.BV]Life Sciences [q-bio]/Vegetal Biology, Shigella, RECONSTRUCTION, Molecular Biology, Gene, 030304 developmental biology, Genetics, 0303 health sciences, biology, IDENTIFICATION, 030306 microbiology, METABOLIC NETWORKS, Computational Biology, Genetic Variation, PATHWAY/GENOME DATABASES, biology.organism_classification, Commensalism, Enterobacteriaceae, EVOLUTION, COMMENSAL, Genome, Bacterial, Metabolic Networks and Pathways, Bacteria, PATHOGENICITY
Abstract

Escherichia coli exhibits a wide range of lifestyles encompassing commensalism and various pathogenic behaviors which its highly dynamic genome contributes to develop. How environmental and host factors shape the genetic structure of E. coli strains remains, however, largely unknown. Following a previous study of E. coli genomic diversity, we investigated its diversity at the metabolic level by building and analyzing the genome-scale metabolic networks of 29 E. coli strains (8 commensal and 21 pathogenic strains, including 6 Shigella strains). Using a tailor-made reconstruction strategy, we significantly improved the completeness and accuracy of the metabolic networks over default automatic reconstruction processes. Among the 1,545 reactions forming E. coli panmetabolism, 885 reactions were common to all strains. This high proportion of core reactions (57%) was found to be in sharp contrast to the low proportion (13%) of core genes in the E. coli pangenome, suggesting less diversity of metabolic functions compared to that of all gene functions. Core reactions were significantly overrepresented among biosynthetic reactions compared to the more variable degradation processes. Differences between metabolic networks were found to follow E. coli phylogeny rather than pathogenic phenotypes, except for Shigella networks, which were significantly more distant from the others. This suggests that most metabolic changes in non- Shigella strains were not driven by their pathogenic phenotypes. Using a supervised method, we were yet able to identify small sets of reactions related to pathogenicity or commensalism. The quality of our reconstructed networks also makes them reliable bases for building metabolic models.

Published
2011

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