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1. The Far Side of Mars: Two Distant Marsquakes Detected by InSight

Author: Anna C. Horleston, John F. Clinton, Savas Ceylan, Domenico Giardini, Constantinos Charalambous, Jessica C. E. Irving, Philippe Lognonné, Simon C. Stähler, Géraldine Zenhäusern, Nikolaj L. Dahmen, Cecilia Duran, Taichi Kawamura, Amir Khan, Doyeon Kim, Matthieu Plasman, Fabian Euchner, Caroline Beghein, Éric Beucler, Quancheng Huang, Martin Knapmeyer, Brigitte Knapmeyer-Endrun, Vedran Lekić, Jiaqi Li, Clément Perrin, Martin Schimmel, Nicholas C. Schmerr, Alexander E. Stott, Eléonore Stutzmann, Nicholas A. Teanby, Zongbo Xu, Mark Panning, and William B. Banerdt
Subjects: Geology, QE1-996.5
Abstract: For over three Earth years the Marsquake Service has been analyzing the data sent back from the Seismic Experiment for Interior Structure—the seismometer placed on the surface of Mars by NASA’s InSight lander. Although by October 2021, the Mars seismic catalog included 951 events, until recently all these events have been assessed as lying within a radius of 100° of InSight. Here we report two distant events that occurred within days of each other, located on the far side of Mars, giving us our first glimpse into Mars’ core shadow zone. The first event, recorded on 25 August 2021 (InSight sol 976), shows clear polarized arrivals that we interpret to be PP and SS phases at low frequencies and locates to Valles Marineris, 146° ± 7° from InSight. The second event, occurring on 18 September 2021 (sol 1000), has significantly more broadband energy with emergent PP and SS arrivals, and a weak phase arriving before PP that we interpret as Pdiff. Considering uncertain pick times and poorly constrained travel times for Pdiff, we estimate this event is at a distance between 107° and 147° from InSight. With magnitudes of MwMa 4.2 and 4.1, respectively, these are the largest seismic events recorded so far on Mars.
Published: 2022
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2. Investigating Diurnal and Seasonal Turbulence Variations of the Martian Atmosphere Using a Spectral Approach

Author: Naomi Murdoch, Alexander E. Stott, David Mimoun, Baptiste Pinot, Audrey Chatain, Aymeric Spiga, Orkun Temel, Jorge Pla Garcia, Keisuke Onodera, Ralph Lorenz, Martin Gillier, Claire Newman, Raphael F. Garcia, Lucas Lange, and Don Banfield
Subjects: Atmospheric dynamics, Mars, Astronomy, QB1-991
Abstract: We use a spectral approach to analyze the pressure and wind data from the InSight mission and investigate the diurnal and seasonal trends. Our analyses show that the daytime pressure and wind spectra have slopes of approximately −1.7 and −1.3 and, therefore, do not follow the Kolmogorov scaling (as was also previously reported for a reduced data set in Banfield et al.). We find that the nighttime pressure spectral slope is close to −1 (as reported in Temel et al.), and that the wind speed spectral slope is close to −0.5, flatter than the theoretical slope expected for the shear-dominated regime. We observe strong nocturnal (likely shear-generated) turbulent behavior starting around L _s = 150° (InSight sol 440) that shifts to progressively earlier local times before reaching the “5th season” (InSight sols 530–710) identified by Chatain et al.. The diurnal spectral slope analyses indicate an asymmetry in the diurnal behavior of the Martian boundary layer, with a slow growth and fast collapse mechanism. Finally, the low-frequency (5–30 mHz) pressure data exhibit large spectral slope oscillations. These occur particularly during the periods with a highly stable atmosphere and, therefore, may be linked to gravity wave activity.
Published: 2023
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3. A class of multidimensional NIPALS algorithms for quaternion and tensor partial least squares regression.

Author: Alexander E. Stott, Bruno Scalzo Dees, Ilia Kisil, and Danilo P. Mandic
Published: 2019
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4. An online NIPALS algorithm for Partial Least Squares.

Author: Alexander E. Stott, Sithan Kanna, Danilo P. Mandic, and William T. Pike
Published: 2017
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5. Simultaneous diagonalisation of the covariance and complementary covariance matrices in quaternion widely linear signal processing.

Author: Min Xiang, Shirin Enshaeifar, Alexander E. Stott, Clive Cheong Took, Yili Xia, Sithan Kanna, and Danilo P. Mandic
Published: 2018
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6. Widely linear complex partial least squares for latent subspace regression.

Author: Alexander E. Stott, Sithan Kanna, and Danilo P. Mandic
Published: 2018
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7. Detection, Analysis, and Removal of Glitches From InSight's Seismic Data From Mars

Author: John‐Robert Scholz, Rudolf Widmer‐Schnidrig, Paul Davis, Philippe Lognonné, Baptiste Pinot, Raphaël F. Garcia, Kenneth Hurst, Laurent Pou, Francis Nimmo, Salma Barkaoui, Sébastien de Raucourt, Brigitte Knapmeyer‐Endrun, Martin Knapmeyer, Guénolé Orhand‐Mainsant, Nicolas Compaire, Arthur Cuvier, Éric Beucler, Mickaël Bonnin, Rakshit Joshi, Grégory Sainton, Eléonore Stutzmann, Martin Schimmel, Anna Horleston, Maren Böse, Savas Ceylan, John Clinton, Martin van Driel, Taichi Kawamura, Amir Khan, Simon C. Stähler, Domenico Giardini, Constantinos Charalambous, Alexander E. Stott, William T. Pike, Ulrich R. Christensen, and W. Bruce Banerdt
Subjects: InSight, seismometer, Mars, data processing, glitches, removal, Astronomy, QB1-991, Geology, QE1-996.5
Abstract: Abstract The instrument package SEIS (Seismic Experiment for Internal Structure) with the three very broadband and three short‐period seismic sensors is installed on the surface on Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is deployed in a very harsh wind and temperature environment that leads to inevitable degradation of the quality of the recorded data. One ubiquitous artifact in the raw data is an abundance of transient one‐sided pulses often accompanied by high‐frequency spikes. These pulses, which we term “glitches”, can be modeled as the response of the instrument to a step in acceleration, while the spikes can be modeled as the response to a simultaneous step in displacement. We attribute the glitches primarily to SEIS‐internal stress relaxations caused by the large temperature variations to which the instrument is exposed during a Martian day. Only a small fraction of glitches correspond to a motion of the SEIS package as a whole caused by minuscule tilts of either the instrument or the ground. In this study, we focus on the analysis of the glitch+spike phenomenon and present how these signals can be automatically detected and removed from SEIS's raw data. As glitches affect many standard seismological analysis methods such as receiver functions, spectral decomposition and source inversions, we anticipate that studies of the Martian seismicity as well as studies of Mars' internal structure should benefit from deglitched seismic data.
Published: 2020
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8. Wind and Turbulence Observations With the Mars Microphone on Perseverance

Author: Alexander E. Stott, Naomi Murdoch, Martin Gillier, Don Banfield, Tanguy Bertrand, Baptiste Chide, Manuel De la Torre Juarez, Ricardo Hueso, Ralph Lorenz, German Martinez, Asier Munguira, Luis Mora Sotomayor, Sara Navarro, Claire Newman, Paolo Pilleri, Jorge Pla‐Garcia, Jose Antonio Rodriguez‐Manfredi, Agustin Sanchez‐Lavega, Michael Smith, Daniel Viudez Moreiras, Nathan Williams, Sylvestre Maurice, Roger C. Wiens, and David Mimoun
Subjects: Geophysics, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous)
Published: 2023
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9. MarsQuakeNet: A More Complete Marsquake Catalog Obtained by Deep Learning Techniques

Author: Nikolaj L. Dahmen, John F. Clinton, Men‐Andrin Meier, Simon C. Stähler, Savas Ceylan, Doyeon Kim, Alexander E. Stott, and Domenico Giardini
Subjects: Geophysics, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Marsquakes detection, Deep learning, Seismology, Denoising, Seasonality, NASA InSight
Abstract: NASA's Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) seismometer has been recording Martian seismicity since early 2019, and to date, over 1,300 marsquakes have been cataloged by the Marsquake Service (MQS). Due to typically low signal-to-noise ratios (SNR) of marsquakes, their detection and analysis remain challenging: while event amplitudes are relatively low, the background noise has large diurnal and seasonal variations and contains various signals originating from the interactions of the local atmosphere with the lander and seismometer system. Since noise can resemble marsquakes in a number of ways, the use of conventional detection methods for catalog curation is limited. Instead, MQS finds events through manual data inspection. Here, we present MarsQuakeNet (MQNet), a deep convolutional neural network for the detection of marsquakes and the removal of noise contamination. Based on three-component seismic data, MQNet predicts segmentation masks that identify and separate event and noise energy in time-frequency domain. As the number of cataloged MQS events is small, we combine synthetic event waveforms with recorded noise to generate a training data set. We apply MQNet to the entire continuous 20 samples-per-second waveform data set available to date (>1,000 Martian days), for automatic event detection and for retrieving denoised amplitudes. The algorithm reproduces all high quality, as well as majority of low quality events in the manual, carefully curated MQS catalog. Furthermore, MQNet detects ∼60% additional events that were previously unknown with mostly low SNR, that are verified in manual review. Our analysis on the event rate confirms seasonal trends and shows a substantial increase in the second Martian year. ISSN:0148-0227 ISSN:2169-9097 ISSN:2169-9100
Published: 2022
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10. Nocturnal turbulence at Jezero crater, as determined from MEDA measurements and modeling

Author: Jorge Pla-García, Asier Munguira, Claire Newman, Tanguy Bertrand, German Martinez, Ricardo Hueso, Agustín Sánchez-Lavega, Teresa del Rio-Gaztelurrutia, Alexander E Stott, Naomi Murdoch, Manuel de la Torre Juárez, Mark T Lemmon, Hannu Savijärvi, Mark Ian Richardson, Eduardo Sebastian Martínez, Alain Lepinette Malvitte, Luis Mora Sotomayor, José A Rodriguez-Manfredi, Daniel Viúdez-Moreiras, Mercedes Marin, Scot Rafkin, and Baptiste Chide
Published: 2022
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11. A Deep Catalogue of Marsquakes

Author: Nikolaj L. Dahmen, John F. Clinton, Men-Andrin Meier, Simon C. Stähler, Savas Ceylan, Doyeon Kim, Alexander E. Stott, and Domenico Giardini
Published: 2022
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12. The dynamic atmospheric and aeolian environment of Jezero crater, Mars

Author: Claire E. Newman, Ricardo Hueso, Mark T. Lemmon, Asier Munguira, Álvaro Vicente-Retortillo, Víctor Apestigue, Germán M. Martínez, Daniel Toledo, Rob Sullivan, Ken E. Herkenhoff, Manuel de la Torre Juárez, Mark I. Richardson, Alexander E. Stott, Naomi Murdoch, Agustín Sanchez-Lavega, Michael J. Wolff, Ignacio Arruego, Eduardo Sebastián, Sara Navarro, Javier Gómez-Elvira, Leslie Tamppari, Michael D. Smith, Alain Lepinette, Daniel Viúdez-Moreiras, Ari-Matti Harri, Maria Genzer, Maria Hieta, Ralph D. Lorenz, Pan Conrad, Felipe Gómez, Timothy H. McConnochie, David Mimoun, Christian Tate, Tanguy Bertrand, James F. Bell, Justin N. Maki, Jose Antonio Rodriguez-Manfredi, Roger C. Wiens, Baptiste Chide, Sylvestre Maurice, Maria-Paz Zorzano, Luis Mora, Mariah M. Baker, Don Banfield, Jorge Pla-Garcia, Olivier Beyssac, Adrian Brown, Ben Clark, Franck Montmessin, Erik Fischer, Priyaben Patel, Teresa del Río-Gaztelurrutia, Thierry Fouchet, Raymond Francis, Scott D. Guzewich, Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Instituto Nacional de Técnica Aeroespacial (INTA), Ministerio de Ciencia e Innovación (MICINN), Ministerio de Economía y Competitividad (MINECO), Agencia Estatal de Investigación (AEI), Gobierno Vasco, National Aeronautics and Space Administration (NASA), Aeolis Research, Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Space Science Institute [Boulder] (SSI), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Lunar and Planetary Institute [Houston] (LPI), University of Michigan [Ann Arbor], University of Michigan System, Cornell University [New York], Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Finnish Meteorological Institute (FMI), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Carnegie Institution for Science, University of Maryland [College Park], University of Maryland System, 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), Arizona State University [Tempe] (ASU), Los Alamos National Laboratory (LANL), Purdue University [West Lafayette], Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Smithsonian National Air and Space Museum, Smithsonian Institution, NASA Ames Research Center (ARC), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Plancius Research LLC, 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), University College of London [London] (UCL), and NASA Goddard Space Flight Center (GSFC)
Subjects: Multidisciplinary, Aeolian, Atmosphere, rems, Mars 2020, large eddy simulation, Mars, Dust, earth, [SDU]Sciences of the Universe [physics], Clouds, bagnold dunes, dust devils, thermal tides, surface, wind, gale crater, convection
Abstract: This article has a correction. Please see: Erratum for the Research Article: “The dynamic atmospheric and aeolian environment of Jezero crater, Mars” - 10 February 2023 Despite the importance of sand and dust to Mars geomorphology, weather, and exploration, the processes that move sand and that raise dust to maintain Mars’ ubiquitous dust haze and to produce dust storms have not been well quantified in situ, with missions lacking either the necessary sensors or a sufficiently active aeolian environment. Perseverance rover’s novel environmental sensors and Jezero crater’s dusty environment remedy this. In Perseverance’s first 216 sols, four convective vortices raised dust locally, while, on average, four passed the rover daily, over 25% of which were significantly dusty (“dust devils”). More rarely, dust lifting by nonvortex wind gusts was produced by daytime convection cells advected over the crater by strong regional daytime upslope winds, which also control aeolian surface features. One such event covered 10 times more area than the largest dust devil, suggesting that dust devils and wind gusts could raise equal amounts of dust under nonstorm conditions. We gratefully acknowledge the huge effort by the entire Mars 2020 team to meet our launch date despite the COVID-19 pandemic, to land and deploy instruments successfully in Jezero crater, and to conduct operations on the surface of Mars since February 2021. This paper arose from discussions within the Mars 2020 Atmospheres Working Group but would not have been possible without the tremendous contributions of everyone involved in Mars 2020 operations. We wish to especially pay tribute to the many team members based in Europe who regularly work through the night as MEDA or SuperCam Payload Uplink and Downlink Leads (PULs/PDLs) or in other roles and to all those who had shifts as Atmospheres Working Group representatives during this period. Last, we gratefully acknowledge the very helpful and constructive comments from both anonymous reviewers. Funding: R.H., A.S.-L., A.M., and T.d.R.-G. are supported by Spanish Ministry of Science and Innovation project PID2019-109467GB-I00 funded by MCIN/AEI/10.13039/501100011033/ and Grupos Gobierno Vasco IT1366-19. I.A., D.T., and V.A. are supported by the Spanish National Research, Development, and Innovation Program through the grants RTI2018-099825-B-C31, ESP2016-80320-C2-1-R, and ESP2014-54256-C4-3-R. L.M., S.N., and J.G.-E. are supported by the Spanish Ministry of Economy and Competitiveness, projects ESP2014-54256-C4-1-R and AYA2015-65041-P; the Spanish Ministry of Science, Innovation, and Universities, projects ESP2016-79612-C3-1-R, ESP2016-80320-C2-1-R, RTI2018-098728-B-C31, and RTI2018-099825-B-C31; and the Spanish Ministry of Science and Innovation’s Centre for the Development of Industrial Technology, projects RTI2018-098728-B-C31 and RTI2018-099825-B-C31. Á.V.-R. and M.-P.Z. are supported by Spanish State Research Agency (AEI) project no. MDM-2017-0737 Unidad de Excelencia “María de Maeztu”–Centro de Astrobiología (INTA-CSIC). M.-P.Z. is supported by the Spanish Ministry of Science and Innovation, PID2019-104205GB-C21. M.M.B. and M.-P.Z. are supported by NASA’s Mars 2020 Participating Scientist Program. All other authors were supported by funding from the Mars 2020 mission, part of the NASA Mars Exploration Program. Work by C.E.N. was additionally funded by the InSight Participating Scientist Program.A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA and funding by SMD, GCD, and STMD. Peerreview
Published: 2022
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13. The marsquake catalogue from InSight, sols 0-1011

Author: Savas Ceylan, John F. Clinton, Domenico Giardini, Simon C. Stähler, Anna Horleston, Taichi Kawamura, Maren Böse, Constantinos Charalambous, Nikolaj L. Dahmen, Martin van Driel, Cecilia Durán, Fabian Euchner, Amir Khan, Doyeon Kim, Matthieu Plasman, John-Robert Scholz, Géraldine Zenhäusern, Eric Beucler, Raphaël F. Garcia, Sharon Kedar, Martin Knapmeyer, Philippe Lognonné, Mark P. Panning, Clément Perrin, William T. Pike, Alexander E. Stott, and William B. Banerdt
Subjects: Mars InSight Seismische Aktivität, Geophysics, Physics and Astronomy (miscellaneous), Space and Planetary Science, Astronomy and Astrophysics
Abstract: The InSight mission (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) has been collecting high-quality seismic data from Mars since February 2019, shortly after its landing. The Marsquake Service (MQS) is the team responsible for the prompt review of all seismic data recorded by the InSight's seismometer (SEIS), marsquake event detection, and curating seismicity catalogues. Until sol 1011 (end of September 2021), MQS have identified 951 marsquakes that we interpret to occur at regional and teleseismic distances, and 1062 very short duration events that are most likely generated by local thermal stresses nearby the SEIS package. Here, we summarize the seismic data collected until sol 1011, version 9 of the InSight seismicity catalogue. We focus on the significant seismicity that occurred after sol 478, the end date of version 3, the last catalogue described in a dedicated paper. In this new period, almost a full Martian year of new data has been collected, allowing us to observe seasonal variations in seismicity that are largely driven by strong changes in atmospheric noise that couples into the seismic signal. Further, the largest, closest and most distant events have been identified, and the number of fully located events has increased from 3 to 7. In addition to the new seismicity, we document improvements in the catalogue that include the adoption of InSight-calibrated Martian models and magnitude scales, the inclusion of additional seismic body-wave phases, and first focal mechanism solutions for three of the regional marsquakes at distances ∼30°.
Published: 2022
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14. The site tilt and lander transfer function from the short period seismometer on InSight on Mars

Author: Alexander E. Stott, Nicholas A Teanby, William T. Pike, Philippe Lognonné, K. J. Hurst, Raphaël F. Garcia, Grace Lim, Naomi Murdoch, David Mimoun, Ashitey Trebi-Ollennu, William B. Banerdt, Anna Horleston, Sharon Kedar, Robert Myhill, J. B. McClean, M. Bierwirth, Constantinos Charalambous, Tristram Warren, and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Subjects: Seismometer, Geophysics, Tilt (optics), Geochemistry and Petrology, Period (geology), Mars Exploration Program, Geodesy, Transfer function, Geology, Mars Seismology, Planétologie
Abstract: The National Aeronautics and Space Administration InSight mission has deployed the seismic experiment, SEIS, on the surface of Mars, and has recorded a variety of signals including marsquakes and dust devils. This work presents results on the tilt and local noise sources, which provide context to aid interpretation of the observed signals and allow an examination of the near-surface properties. Our analysis uses data recorded by the short-period sensors on the deck, throughout deployment and in the final configuration. We use thermal decorrelation to provide an estimate of the sol-to-sol tilt. This tilt is examined across deployment and over a Martian year. After each modification to the site, the tilt is seen to stabilize over 3–20 sols depending on the action, and the total change in tilt is
Published: 2021
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15. A class of multidimensional NIPALS algorithms for quaternion and tensor partial least squares regression

Author: Ilia Kisil, Bruno Scalzo Dees, Alexander E. Stott, and Danilo P. Mandic
Subjects: Signal processing, Contextual image classification, MathematicsofComputing_NUMERICALANALYSIS, 020206 networking & telecommunications, 02 engineering and technology, Latent variable, Mutual information, Range (mathematics), Control and Systems Engineering, Signal Processing, Partial least squares regression, 0202 electrical engineering, electronic engineering, information engineering, 020201 artificial intelligence & image processing, Computer Vision and Pattern Recognition, Tensor, Electrical and Electronic Engineering, Quaternion, Algorithm, Software, Mathematics
Abstract: Quaternion and tensor-based signal processing benefits from exploiting higher dimensional structure in data to outperform the corresponding approaches using multivariate real algebras. Along with the extended range of processing options, these methods produce opportunities for a physically-meaningful interpretation. In this paper, we propose a class of novel partial least squares (PLS) algorithms for tensor- and quaternion-valued data, the widely linear quaternion PLS (WL-QPLS), the higher order nonlinear iterative PLS (HONIPALS) and the generalised higher order PLS (GHOPLS). This enables a regularised regression solution along with a latent variable decomposition of the original data based on the mutual information in the input and output block. The performance of the proposed algorithms is verified through analysis, together with a detailed comparison between quaternions and tensors and their application for image classification.
Published: 2019
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16. Vortex‐Dominated Aeolian Activity at InSight's Landing Site, Part 1: Multi‐Instrument Observations, Analysis, and Implications

Author: Alexander E. Stott, L. M. Sotomayor, Constantinos Charalambous, John A. Grant, Sebastien Rodriguez, Nicholas H. Warner, Veronique Ansan, Don Banfield, William T. Pike, Naomi Murdoch, Aymeric Spiga, Maria E. Banks, Daniel Viúdez-Moreiras, William B. Banerdt, P. H. Lognonné, Ernst Hauber, Jorge Pla-Garcia, Matthew P. Golombek, Clément Perrin, Ralph D. Lorenz, Justin N. Maki, T. Warren, Anna Mittelholz, Claire E. Newman, Antoine Lucas, Matthew E. Baker, Catherine L. Johnson, J. B. Garvin, Ingrid Daubar, Mark T. Lemmon, Sara Navarro, Catherine M. Weitz, J. B. McClean, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Department of Electrical and Electronic Engineering [London] (DEEE), Imperial College London, MIT Haystack Observatory, Massachusetts Institute of Technology (MIT), Johns Hopkins University (JHU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Science Institute [Boulder] (SSI), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut de Physique du Globe de Paris (IPG Paris), 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), Institut Pierre-Simon-Laplace (IPSL (FR_636)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), NASA Goddard Space Flight Center (GSFC), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Planetary Science Institute [Tucson] (PSI), Smithsonian Institution, State University of New York at Geneseo (SUNY Geneseo), State University of New York (SUNY), Brown University, German Aerospace Center (DLR), University of British Columbia (UBC), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Oxford, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Cornell University [New York], Aeolis Research, ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), Rodriguez, Sébastien, and MArs Geophysical InSight - - MAGIS2019 - ANR-19-CE31-0008 - AAPG2019 - VALID
Subjects: Convection, Seismometer, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, 01 natural sciences, Wind speed, Physics::Geophysics, aeolian changes at the InSight landing site on Mars, convective vortices as a primary driver of particle motion, dust lifting and saltation, multi-instrument measurements constrain the timing and atmospheric conditions of aeolian changes, passing vortices lifting dust are correlated with magnetic signatures, surface creep, surface tracks, particle transport, Geochemistry and Petrology, Planet, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), wind, 14. Life underwater, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, InSight, 0105 earth and related environmental sciences, Mars landing, Mars Exploration Program, Geophysics, Vortex, Planetengeologie, [PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 13. Climate action, Space and Planetary Science, Aeolian processes, Astrophysics::Earth and Planetary Astrophysics, Geology, camera
Abstract: International audience; We report the aeolian changes observed in situ by NASA's InSight lander during the first 400 sols of operations: Granule creep, saltation, dust removal, and the formation of dark surface tracks. Aeolian changes are infrequent and sporadic. However, on sols, when they do occur, they consistently appear between noon to 3 p.m., and are associated with the passage of convective vortices during periods of high vortex activity. Aeolian changes are more frequent at elevated locations, such as the top surfaces of rocks and lander footpads. InSight observed these changes using, for the first time, simultaneous insitu and orbital imaging and high-frequency meteorological, seismological, and magnetic measurements. Seismometer measurements of ground acceleration constrain the timing and trajectory of convective vortex encounters, linking surface changes to source vortices. Magnetometer measurements show perturbations in magnetic field strength during the passage of convective vortices consistent with chargedparticle motion. Detachment of sand-scale particles occurs when high background winds and vortexinduced turbulence provide a peak surface friction wind speed above the classic saltation fluid threshold. However, detachment of dust-and granule-scale particles also occurred when the surface friction wind speed remained below this threshold. This may be explained by local enhancement of the surface roughness and other effects described here and further studied in Part 2 (Baker et al., 2021). The lack of saltation and bright dust-coated surfaces at the InSight landing site implies surface stability and the onset of particle motion may be suppressed by dust "cushioning." This differentiates the InSight landing site from other areas on Mars that exhibit more aeolian activity. Plain Language Summary Aeolian activity, the movement of dust and sand by the wind, is common on Earth and has been observed on other planets, including Mars. A new Mars lander, InSight, has for the first time monitored aeolian changes by combining imaging with weather, seismic and CHARALAMBOUS ET AL.
Published: 2021
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17. Atmospherically driven ground motion at InSight: a machine learning perspective

Author: William T. Pike, Don Banfield, Naomi Murdoch, Sara Navarro, David Mimoun, Philippe Lognonné, Anna Horleston, Aymeric Spiga, Baptiste Pinot, Constantinos Charalambous, Raphaël F. Garcia, Luis Mora-Sotomayor, and Alexander E. Stott
Subjects: Ground motion, Computer science, Human–computer interaction, Perspective (graphical)
Abstract: The NASA InSight lander is a geophysical and meteorological observatory operating on Mars for over a Martian year/two Earth years. Continuous records of seismic, pressure, wind and temperature data over this period have led to significant breakthroughs in determining the planet's structure and climate. With such a wealth of data now received, machine learning offers a nascent tool to extract further information. The seismic data is extremely correlated to the atmospheric conditions. Discerning the coupling between the atmosphere and ground motion is of significant interest and this work aims to predict the ground motion generated by wind and pressure forcing using machine learning techniques. From this prediction we can untangle the various contributions to ground motion, determine atmospheric/ground properties, analyse/discriminate marsquakes and potentially decorrelate waveforms to remove the atmospheric contribution. While a physical model for this atmospheric forcing is desirable, machine learning approaches the problem from an alternative view point where mathematical and algorithmic tools add the necessary complexity for fitting the data. In this way, we may be able to capture detailed variation and inform further modelling efforts.We will detail the initial application of machine learning for predicting the ground motion from the atmospheric data inputs of wind speed, wind direction, pressure and temperature. First though, we will describe the issues that need to be tackled to obtain a good prediction using the InSight data. To illustrate some of some of these problems, consider that glitches are known to occur in the seismic data. They offer a way to detect overfitting as they should not in general be predicted from atmospheric forcing. However, a subset of the glitches are correlated to temperature on top of the fact they are only visible during quiet enough periods, as are marsquakes. Therefore, they are not a normally distributed source of noise or uncorrelated from the input atmospheric data, breaking typical assumptions used for regression. A similar issue is presented by the changing weather conditions throughout a Martian sol, where the time series distribution varies. As a result, prior information on the instrumentation and data qualities is essential for applying the machine learning methods and interpretation of the results.We demonstrate the specifics of the InSight data with respect to 1) how a curve fitting problem can be constructed, 2) the necessary degrees of freedom of the problem, 3) consideration of non-stationary/heteroscedastic errors and 4) the optimisation and machine learning method applied. Current results will be presented from the implementation of random forests and gaussian processes. These results demonstrate a good performance so far for capturing the global variation and we will offer perspectives on how these results can be used and improved.
Published: 2021
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18. A complete Martian year of atmospheric observations with InSight instruments

Author: Anna Horleston, Claire E. Newman, Naomi Murdoch, M. M. Baker, Alexander E. Stott, Daniel Viúdez-Moreiras, Savas Ceylan, Raphaël F. Garcia, Anna Mittelholz, Ralph D. Lorenz, Constantinos Charalambous, Jorge Pla-Garcia, L. Martire, Aymeric Spiga, Don Banfield, Eléonore Stutzmann, Clément Perrin, François Forget, Mark T. Lemmon, and Nils Mueller
Subjects: Environmental science, Timekeeping on Mars, Astrobiology
Abstract: On the first hundreds of sols in which the InSight lander operated on the surface of Mars, its instrumentation has proven to be particularly suitable to unveil and understand atmospheric variability at all temporal scales, from the synoptic scale (baroclinic waves) to the sub-hour scale (gravity waves, bores) down to the turbulent scale (vortices, gusts, infrasounds). Recently, the InSight lander achieved a complete Martian year of observations of the atmosphere of Mars -- allowing for the seasonal variability of the Martian atmosphere and its phenomena at all scales to be monitored almost continuously, including during several large dust storms episodes. In this presentation, based on this Martian year of InSight observations, we will review the annual CO2 sublimation / condensation cycle, the variability of large-scale meteorology, the statistics of a year of wind observations -- and insightful comparisons with global climate models, the strong seasonal variability of gravity wave and turbulent activity, including a burst of activity of convective vortices in Mars' southern summer. We will also discuss how the atmosphere influences seismic and magnetic signals captured by InSight -- and the search for Martian infrasound.
Published: 2021
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19. A Comodulation Analysis of Atmospheric Energy Injection into the Ground Motion at InSight, Mars

Author: M. van Driel, John Clinton, Constantinos Charalambous, L. M. Sotomayor, Domenico Giardini, Naomi Murdoch, Simon Stähler, Anna Horleston, T. Warren, William B. Banerdt, William T. Pike, John-Robert Scholz, Aymeric Spiga, Guenolé Orhand-Mainsant, Savas Ceylan, Don Banfield, Amir Khan, Maren Böse, Alexander E. Stott, Raphaël F. Garcia, J. B. McClean, Taichi Kawamura, P. H. Lognonné, Sara Navarro, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Murdoch, N. [0000-0002-9701-4075], Lognonne, P. [0000-0002-1014-920X], Charalambous, C. [0000-0002-9139-3895], Stott, A. E. [0000-0001-6121-705X], Spiga, A. [0000-0002-6776-6268], Stähler, S. [0000-0002-0783-2489], Scholz, J. R. [0000-0003-1404-2335], Ceylan, S. [0000-0002-6552-6850], Khan, A. [0000-0003-4462-3173], Van Driel, M. [0000-0002-8938-4615], Horleston, A. [0000-0002-6748-6522], Giardini, D. [0000-0002-5573-7638], and Banerdt, W. B. [0000-0003-3125-1542]
Subjects: Ground motion, 010504 meteorology & atmospheric sciences, ground motion, marsquakes, Method of moments (statistics), 01 natural sciences, Mars Atmosphere, Atmosphere, atmosphere‐induced noise, comodulation, method of moments, noise discrimination, Autre, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), 0105 earth and related environmental sciences, Martian, Mars Exploration Program, Geophysics, Space and Planetary Science, Environmental science, Atmospheric electricity, Mars seismology, Noise (radio)
Abstract: Seismic observations involve signals that can be easily masked by noise injection. For the NASA Mars lander InSight, the atmosphere is a significant noise contributor, impeding the identification of seismic events for two thirds of a Martian day. While the noise is below that seen at even the quietest sites on Earth, the amplitude of seismic signals on Mars is also considerably lower, requiring an understanding and quantification of environmental injection at unprecedented levels. Mars' ground and atmosphere are a continuously‐coupled seismic system, and although atmospheric functions are of distinct origins, the superposition of these noise contributions is poorly understood, making separation a challenging task. We present a novel method for partitioning the observed signal into seismic and environmental contributions. Atmospheric pressure and wind fluctuations are shown to exhibit temporal cross‐frequency coupling across multiple bands, injecting noise that is neither random nor coherent. We investigate this through comodulation, quantifying the synchrony of the seismic motion, wind and pressure signals. By working in the time‐frequency domain, we discriminate between the different origins of underlying processes and determine the site's environmental sensitivity. Our method aims to create a virtual vault at InSight's landing site on Mars, shielding the seismometers with effective post‐processing in lieu of a physical vault. This allows us to describe the environmental and seismic signals over a sequence of sols, to quantify the wind and pressure injection and estimate the seismic content of possible marsquakes with a signal‐to‐noise ratio that can be quantified in terms of environmental independence. Finally, we exploit the relationship between the comodulated signals to identify their sources., Journal of Geophysical Research: Planets, 126 (4), ISSN:0148-0227, ISSN:2169-9097
Published: 2021
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20. Resonances of the InSight Seismometer on Mars

Author: K. Hurst, Taichi Kawamura, Savas Ceylan, William B. Banerdt, M. Bierwirth, Sharon Kedar, T. Nebut, Cedric Schmelzbach, Oliver Robert, Maren Böse, William T. Pike, Domenico Giardini, Simon Stähler, Constantino Charalambous, Alexander E. Stott, John-Robert Scholz, Anna Horleston, Jennifer Stevanović, Amir Khan, Tristram Warren, Joan Ervin, Brigitte Knapmeyer-Endrun, S. B. Calcutt, Guenolé Orhand-Mainsant, Lucile Fayon, Martin van Driel, Philippe Lognonné, John Clinton, T. Gabsi, S. Tillier, and Sebastien de Raucourt
Subjects: Seismometer, Geophysics, Geochemistry and Petrology, Mars Exploration Program, Geology, Astrobiology
Abstract: The Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) seismometer was deployed to the surface of Mars in December 2018–February 2019. The specific deployment conditions, which are very different from those of a standard broadband instrument on the Earth, result in resonances caused by different parts of the sensor assembly (SA) that are recorded by the seismometer. Here, we present and characterize the resonances known to be present in the SA and their causes to aid interpretation of the seismic signals observed on Mars. Briefly, there are resonances in the SA at about 2.9, 5.3, 9.5, 12, 14, 23–28, and 51 Hz. We discuss various methods and tests that were used to characterize these resonances, and provide evidence for some of them in data collected on Mars. In addition to their relevance for the high frequency analysis of seismic data from InSight, specifically for phase measurements near the resonant frequencies, the tests and observations described here are also of potential use in the further development of planetary seismometers, for example, for Mars, the Moon, or Europa.
Published: 2021
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21. Companion guide to the Marsquake catalog from InSight, sols 0–478: Data content and non-seismic events

Author: Clément Perrin, Nikolaj Dahmen, Suzanne E. Smrekar, Raphaël F. Garcia, Martin Schimmel, Simon Stähler, Maren Böse, William B. Banerdt, Anna Horleston, Alexander E. Stott, Sharon Kedar, Eléonore Stutzmann, Ralph D. Lorenz, Jan ten Pierick, K. Hurst, Don Banfield, John Clinton, Taichi Kawamura, Constantinos Charalambous, Fabian Euchner, Aymeric Spiga, Eric Beucler, Amir Khan, William T. Pike, Vincent Conejero, Philippe Lognonné, Savas Ceylan, Martin van Driel, Domenico Giardini, Mark P. Panning, Constanza Pardo, Guenolé Orhand-Mainsant, John-Robert Scholz, Swiss National Science Foundation, Agence Nationale de la Recherche (France), Swiss National Supercomputing Centre, UK Space Agency, Centre National D'Etudes Spatiales (France), ETH Zurich, State Secretariat for Education, Research and Innovation (Switzerland), Schimmel, Martin, Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), and Schimmel, Martin [0000-0003-2601-4462]
Subjects: [SPI.OTHER]Engineering Sciences [physics]/Other, Seismometer, 010504 meteorology & atmospheric sciences, Physics and Astronomy (miscellaneous), Mars, Data inventory, 010502 geochemistry & geophysics, 01 natural sciences, Autre, Broadband, Data content, InSight mission, Non-seismic signals, Marsquakes, 0105 earth and related environmental sciences, Scientific instrument, Martian, Payload, Astronomy and Astrophysics, Mars Exploration Program, Geophysics, 13. Climate action, Space and Planetary Science, Noise (video), Mars seismology, Geology, Seismology
Abstract: The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed on the surface of Mars on November 26, 2018. One of the scientific instruments in the payload that is essential to the mission is the SEIS package (Seismic Experiment for Interior Structure) which includes a very broadband and a short period seismometer. More than one year since the landing, SEIS continues to be fully operational and has been collecting an exceptional data set which contains not only the signals of seismic origins, but also noise and artifacts induced by the martian environment, the hardware on the ground that includes the seismic sensors, and the programmed operational activities of the lander. Many of these non-seismic signals will be unfamiliar to the scientific community. In addition, many of these signals have signatures that may resemble seismic events either or both in time and frequency domains. Here, we report our observations of common non-seismic signals as seen during the first 478 sols of the SEIS data, i.e. from landing until the end of March 2020. This manuscript is intended to provide a guide to scientists who use the data recorded on SEIS, detailing the general attributes of the most commonly observed non-seismic features. It will help to clarify the characteristics of the seismic dataset for future research, and to avoid misinterpretations when searching for marsquakes., We acknowledge NASA, CNES, their partner agencies and institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC, MPS-MPG) and the flight operations team at JPL, SISMOC, MSDS, IRIS-DMC and PDS for providing SEED SEIS data. We also acknowledge the funding by (1) Swiss National Science Foundation and French Agence Nationale de la Recherche (SNF-ANR project “Seismology on Mars”, ANR-14-CE36-0012-02 and MAGIS, ANR-19-CE31-0008-08), (2) Swiss State Secretariat for Education, Research and Innovation (SEFRI project “MarsQuake Service-Preparatory Phase”), (3) ETH Research grant ETH-06 17-02 and, for French co-authors, (4) the French Space agency CNES. Additional support came from the Swiss National Supercomputing Centre (CSCS) under project ID s922. AH is funded by UKSA through grant #ST/R002096/1. Visualizations were created using Matplotlib (Hunter, 2007). The data was processed with NumPy (Oliphant, 2006), Scipy (Jones et al., 2001), ObsPy (Krischer et al., 2015) and custom software developed by gempa GmbH. This paper is InSight Contribution Number 150.
Published: 2021
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22. Detection, Analysis, and Removal of Glitches From InSight's Seismic Data From Mars

Author: L. Pou, Martin Knapmeyer, S. Barkaoui, Taichi Kawamura, Eric Beucler, Amir Khan, Baptiste Pinot, Bruce Banerdt, Rakshit Joshi, Brigitte Knapmeyer-Endrun, John Clinton, Raphaël F. Garcia, Mickael Bonnin, Arthur Cuvier, Grégory Sainton, Constantinos Charalambous, Savas Ceylan, Sebastien de Raucourt, Eléonore Stutzmann, Simon Stähler, John-Robert Scholz, Paul M. Davis, Anna Horleston, Guenolé Orhand-Mainsant, Nicolas Compaire, Francis Nimmo, Ulrich R. Christensen, Martin van Driel, Domenico Giardini, William T. Pike, Martin Schimmel, Maren Böse, Alexander E. Stott, K. Hurst, Rudolf Widmer-Schnidrig, Philippe Lognonné, Agence Nationale de la Recherche (France), Swiss Space Office, Schimmel, Martin [0000-0003-2601-4462], Schimmel, Martin, Widmer‐Schnidrig, Rudolf, 2 Black Forest Observatory, Institute of Geodesy Stuttgart University Stuttgart Germany, Davis, Paul, 3 Department of Earth, Planetary, and Space Sciences University of California Los Angeles Los Angeles CA USA, Lognonné, Philippe, 4 Université de Paris, Institut de physique du globe de Paris, CNRS Paris France, Pinot, Baptiste, 5 Institut Supérieur de l'Aéronautique et de l'Espace SUPAERO Toulouse France, Garcia, Raphaël F., Hurst, Kenneth, 6 Jet Propulsion Laboratory California Institute of Technology Pasadena USA, Pou, Laurent, 7 Department of Earth and Planetary Sciences University of California Santa Cruz Santa Cruz CA USA, Nimmo, Francis, Barkaoui, Salma, de Raucourt, Sébastien, Knapmeyer‐Endrun, Brigitte, 8 Bensberg Observatory University of Cologne Bergisch Gladbach Germany, Knapmeyer, Martin, 9 DLR Institute of Planetary Research Berlin Germany, Orhand‐Mainsant, Guénolé, Compaire, Nicolas, Cuvier, Arthur, 10 Laboratoire de Planétologie et Géodynamique, Université de Nantes, Université d'Angers Nantes France, Beucler, Éric, Bonnin, Mickaël, Joshi, Rakshit, 1 Max Planck Institute for Solar System Research Göttingen Germany, Sainton, Grégory, Stutzmann, Eléonore, 11 Institute of Earth Sciences Jaume Almera ‐ CSIC Barcelona Spain, Horleston, Anna, 12 School of Earth Sciences University of Bristol Bristol UK, Böse, Maren, 13 Swiss Seismological Service (SED) ETH Zurich Zurich, Switzerland, Ceylan, Savas, 14 Institute of Geophysics ETH Zürich Zurich Switzerland, Clinton, John, van Driel, Martin, Kawamura, Taichi, Khan, Amir, Stähler, Simon C., Giardini, Domenico, Charalambous, Constantinos, 16 Department of Electrical and Electronic Engineering Imperial College London London UK, Stott, Alexander E., Pike, William T., Christensen, Ulrich R., Banerdt, W. Bruce, and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, lcsh:Astronomy, glitches, seismometer, Mars, Environmental Science (miscellaneous), 010502 geochemistry & geophysics, 01 natural sciences, Glitches, lcsh:QB1-991, Autre, Broadband, 0105 earth and related environmental sciences, InSight, Data processing, removal, lcsh:QE1-996.5, Mars Exploration Program, lcsh:Geology, General Earth and Planetary Sciences, InSight Mars Seismogramme Datenbearbeitung, Mars seismology, Removal, Geology, Seismology, data processing
Abstract: The instrument package SEIS (Seismic Experiment for Internal Structure) with the three very broadband and three short‐period seismic sensors is installed on the surface on Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is deployed in a very harsh wind and temperature environment that leads to inevitable degradation of the quality of the recorded data. One ubiquitous artifact in the raw data is an abundance of transient one‐sided pulses often accompanied by high‐frequency spikes. These pulses, which we term “glitches”, can be modeled as the response of the instrument to a step in acceleration, while the spikes can be modeled as the response to a simultaneous step in displacement. We attribute the glitches primarily to SEIS‐internal stress relaxations caused by the large temperature variations to which the instrument is exposed during a Martian day. Only a small fraction of glitches correspond to a motion of the SEIS package as a whole caused by minuscule tilts of either the instrument or the ground. In this study, we focus on the analysis of the glitch+spike phenomenon and present how these signals can be automatically detected and removed from SEIS's raw data. As glitches affect many standard seismological analysis methods such as receiver functions, spectral decomposition and source inversions, we anticipate that studies of the Martian seismicity as well as studies of Mars' internal structure should benefit from deglitched seismic data., Plain Language Summary: The instrument package SEIS (Seismic Experiment for Internal Structure) with two fully equipped seismometers is installed on the surface of Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is more exposed to wind and daily temperature changes that leads to inevitable degradation of the quality of the recorded data. One consequence is the occurrence of a specific type of transient noise that we term “glitch”. Glitches show up in the recorded data as one‐sided pulses and have strong implications for the typical seismic data analysis. Glitches can be understood as step‐like changes in the acceleration sensed by the seismometers. We attribute them primarily to SEIS‐internal stress relaxations caused by the large temperature variations to which the instrument is exposed during a Martian day. Only a small fraction of glitches correspond to a motion of the whole SEIS instrument. In this study, we focus on the detection and removal of glitches and anticipate that studies of the Martian seismicity as well as studies of Mars's internal structure should benefit from deglitched seismic data., Key Points: Glitches due to steps in acceleration significantly complicate seismic records on Mars. Glitches are mostly due to relaxations of thermal stresses and instrument tilt. We provide a toolbox to automatically detect and remove glitches., Centre National d'Etudes Spatiales (CNES), InSight PSP Program, Agence Nationale de la Recherche http://dx.doi.org/10.13039/501100001665, ANR‐19‐CE31‐0008‐08
Published: 2020

23. The Marsquake Catalogue from InSight, Sols 0-478

Author: John Clinton, Savas Ceylan, Martin van Driel, Domenico Giardini, Simon C. Stähler, Maren Böse, Constantinos Charalambous, Nikolaj L. Dahmen, Anna Horleston, Taichi Kawamura, Amir Khan, Guenole Orhand-Mainsant, John-Robert Scholz, Fabian Euchner, William B. Banerdt, Philippe Lognonne, Don Banfield, Eric Beucler, Sharon Kedar, Mark Panning, Clement Perrin, William T. Pike, Suzanne E. Smrekar, Aymeric Spiga, and Alexander E. Stott
Abstract: The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission began collecting high quality seismic data on Mars from February 2019. This manuscript documents the seismicity observed by SEIS, InSight’s seismometer, since this time until the end of March, 2020. Within the InSight project, the Marsquake Service (MQS) is responsible for prompt review of all seismic data collected by InSight, detection of events that are likely to be of seismic origin, and curation and release of seismic catalogues. In the first year of data collection, MQS have identified 465 seismic events that we interpret to be from regional and teleseismic marsquakes. Seismic events are grouped into 2 different event families: the low frequency family are dominated by energy at long period below 1 second, and the high frequency family primarily include energy at and above 2.4~Hz. Event magnitudes, from Mars-specific scales, range from 1.3 to 3.7. A third class of events with very short duration but high frequency bursts have been observed 712 times. These are likely associated with a local source driven by thermal stresses. This paper describes the data collected so far in the mission and the procedures under which MQS operates; summarises the content of the current MQS seismic catalogue; and presents the key features of the events we have observed so far, using the largest events as examples.
Published: 2020
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24. Global quieting of high-frequency seismic noise due to COVID-19 pandemic lockdown measures

Author: Han Xiao, Ben A. van der Pluijm, Simon Richard Proud, Adolfo Inza, Stephen Hicks, T. Megies, Alexander E. Stott, William G. Minarik, Efthimios Sokos, Mika McKinnon, Kasper van Wijk, Anna Horleston, Victor H. Márquez-Ramírez, Läslo Evers, Bogdan Grecu, Esteban J. Chaves, Joachim Wassermann, Claudio Satriano, Christos Evangelidis, Paula Koelemeijer, David Craig, Frédérick Massin, Sebastián Carrasco, György Hetényi, Mario Arroyo-Solórzano, Eric Larose, Jay J. Pulli, Társilo Girona, Lise Retailleau, Javier Ojeda, Olivier F. C. den Ouden, Alan L. Kafka, Gonzalo A. Fernandez, Marc Grunberg, Tommi Vuorinen, Robert E. Anthony, Steven J. Gibbons, Stefanie Donner, Martin Möllhoff, Nathaniel J. Lindsey, Jordi Diaz, C. R. Labedz, Meghan S. Miller, Taka'aki Taira, Dave Cornwell, Mathijs Koymans, Corentin Caudron, Klaus Stammler, Andrea Cannata, Flavio Cannavò, Reinoud Sleeman, Mark Vanstone, Shiba Subedi, Raphael S. M. De Plaen, Shankho Niyogi, Koen Van Noten, Shahar Shani-Kadmiel, Jelle Assink, Tristram Warren, Jessica C. E. Irving, Ian M. Nesbitt, Dimitrios Giannopoulos, Martha K. Savage, Mohammadreza Jamalreyhani, Louis Moresi, Maria-Theresia Apoloner, Gregor Hillers, Jérôme Vergne, Benoit Fauville, Fatih Turhan, Annukka E. Rintamäki, Pınar Büyükakpınar, Adrien Oth, Mathilde B. Sørensen, Mar Tapia, Thomas Lecocq, Royal Society (UK), German Research Centre for Geosciences, Boğaziçi Üniversity, Netherlands Organization for Scientific Research, Air Force Office of Scientific Research (US), National Science Foundation (US), Consejo Nacional de Ciencia y Tecnología (México), Universidad Nacional Autónoma de México, Agencia Nacional de Investigación y Desarrollo (Chile), Natural Environment Research Council (UK), University of California, Commonwealth Scientific and Industrial Research Organisation (Australia), Belgian Science Policy Office, Fonds National de la Recherche Luxembourg, Lecocq, Thomas, Hicks, Stephen, Noten, Koen Van, Wijk, Kasper van, Plaen, Raphael de, Massin, Frédérick, Hillers, Gregor, Apoloner, Maria-Theresia, Arroyo-Solórzano, Mario, Assink, Jelle, Büyükakpınar, Pinar, Cannata, Andrea, Cannavó, Flavio, Carrasco, Sebastián, Caudron, Corentin, Chaves, Esteban, Cornwell, David G., Craig, David, Diaz, J., Donner, Stefanie, Evangelidis, Christos, Evers, Läslo, Fernández, Gonzalo A., Giannopoulos, Dimitrios, Gibbons, Steven J., Girona, Társilo, Grecu, Bogdan, Grunberg, Marc, Hetényi, Gyorgy, Horleston, Anna, Inza, Adolfo, Irving, Jessica C. E., Jamalreyhani, Mohammadreza, Kafka, Alan, Labedz, Celeste, Lindsey, Nathaniel, McKinno, Mika, Megies, Tobias, Miller, Meghan, Minarik, William, Moresi, Louis, Márquez-Ramirez, V. H., Möllhoff, Martin, Nesbitt, Ian M., Niyogi, Shankho, Ojeda, Javier, Oth, Adrien, Proud, Simon, Retailleau, Lise, Satriano, Claudio, Savage, Martha, Shani-Kadmiel, Shahar, Sleeman,Reinoud, Sokos, Efthimios, Stott, Alexander, Subedi, Shiba, Sørensen, Mathilde, Taira, Taka'aki, Turhan, Fatih, Pluijm, Ben van der, Vergne, Jérôme, Vuorinen, Tommi A. T., Warren, Tristram, Wassermann, Joachim, Xiao, Han, Lecocq, Thomas [0000-0002-4988-6477], Hicks, Stephen [0000-0002-7476-3284], Noten, Koen Van [0000-0001-8933-4426], Wijk, Kasper van [0000-0003-4994-8030], Plaen, Raphael de [0000-0003-3477-2001], Massin, Frédérick [0000-0002-7532-5139], Hillers, Gregor [0000-0003-2341-1892], Apoloner, Maria-Theresia [0000-0002-4006-1284], Arroyo-Solórzano, Mario [0000-0002-1653-2680], Assink, Jelle [0000-0002-4990-6845], Büyükakpınar, Pinar [0000-0001-8461-674X], Cannata, Andrea [0000-0002-0028-5822], Cannavó, Flavio [0000-0001-7550-8579], Carrasco, Sebastián [0000-0002-6207-8757], Caudron, Corentin [0000-0002-3748-0007], Chaves, Esteban [0000-0002-5724-1513], Cornwell, David G. [0000-0002-9843-7811], Craig, David [0000-0001-9414-1725], Diaz, J. [0000-0003-1801-0541], Donner, Stefanie [0000-0001-7351-8079], Evangelidis, Christos [0000-0001-8733-8984], Evers, Läslo [0000-0003-2825-6211], Fernández, Gonzalo A. [0000-0001-8284-9566], Giannopoulos, Dimitrios [0000-0002-8314-0759], Gibbons, Steven J. [0000-0002-7822-0244], Girona, Társilo [0000-0001-6422-0422], Grecu, Bogdan [0000-0002-7662-996X], Grunberg, Marc [0000-0002-1307-7790], Hetényi, Gyorgy [0000-0001-9036-4761], Horleston, Anna [0000-0002-6748-6522], Inza, Adolfo [0000-0001-5381-9042], Irving, Jessica C. E. [0000-0002-0866-8246], Jamalreyhani, Mohammadreza [0000-0003-4181-7175], Kafka, Alan [0000-0001-6643-1602], Labedz, Celeste [0000-0001-7339-2170], Lindsey, Nathaniel [0000-0001-9522-6683], McKinno, Mika [0000-0002-9274-0377], Megies, Tobias [0000-0002-5033-9921], Miller, Meghan [0000-0001-5494-2296], Minarik, William [0000-0001-5509-5543], Moresi, Louis [0000-0003-3685-174X], Márquez-Ramirez, V. H. [0000-0003-1494-2229], Möllhoff, Martin [0000-0003-1848-1554], Nesbitt, Ian M. [0000-0001-5828-6070], Niyogi, Shankho [0000-0002-8362-4569], Ojeda, Javier [0000-0002-7188-8356], Oth, Adrien [0000-0003-4859-6504], Proud, Simon [0000-0003-3880-6774], Retailleau, Lise [0000-0002-0711-4540], Satriano, Claudio [0000-0002-3039-2530], Savage, Martha [0000-0002-2080-0676], Shani-Kadmiel, Shahar [0000-0003-2215-6164], Sleeman,Reinoud [0000-0002-1928-5056], Sokos, Efthimios [0000-0002-7742-7251], Stott, Alexander [0000-0001-6121-705X], Subedi, Shiba [0000-0002-7009-7333], Sørensen, Mathilde [0000-0002-8589-7480], Taira, Taka'aki [0000-0002-6170-797X], Turhan, Fatih [0000-0003-4612-7421], Pluijm, Ben van der [0000-0001-7737-2791], Vergne, Jérôme [0000-0003-1731-9360], Vuorinen, Tommi A. T. [0000-0002-8186-012X], Warren, Tristram [0000-0003-3877-0046], Wassermann, Joachim [0000-0002-4088-1792], and Xiao, Han [0000-0001-8727-8053]
Subjects: Seismometer, 2019-20 coronavirus outbreak, 010504 meteorology & atmospheric sciences, Coronavirus disease 2019 (COVID-19), General Science & Technology, Pneumonia, Viral, Seismic noise, 010502 geochemistry & geophysics, 01 natural sciences, Seismic wave, Activities of Daily Living, Humans, Pandemics, 0105 earth and related environmental sciences, Multidisciplinary, COVID-19, Covid19, Noise, Quiet period, Quarantine, Séismologie, Coronavirus Infections, Geology, Seismology
Abstract: Human activity causes vibrations that propagate into the ground as high-frequency seismic waves. Measures to mitigate the COVID-19 pandemic caused widespread changes in human activity, leading to a months-long reduction in seismic noise of up to 50%. The 2020 seismic noise quiet period is the longest and most prominent global anthropogenic seismic noise reduction on record. While the reduction is strongest at surface seismometers in populated areas, this seismic quiescence extends for many kilometers radially and hundreds of meters in depth. This provides an opportunity to detect subtle signals from subsurface seismic sources that would have been concealed in noisier times and to benchmark sources of anthropogenic noise. A strong correlation between seismic noise and independent measurements of human mobility suggests that seismology provides an absolute, real-time estimate of population dynamics., P.K. was funded by a Royal Society University Research Fellowship (URF\R1\180377). P.B. and M.J. acknowledge support from the International Training Course “Seismology and Seismic Hazard Assessment” funded by the GeoForschungsZentrum Potsdam (GFZ) and the German Federal Foreign Office through the German Humanitarian Assistance program (grant S08-60 321.50 ALL 03/19). P.B also acknowledges financial support from the Boğaziçi University Research Fund (BAP 15683). O.F.C.d.O acknowledges funding from a Young Investigator Grant from the Human Frontier Science Program (HFSP - project number RGY0072/2017). C.P.E. and E.S. acknowledge funding from the HELPOS Project “Hellenic Plate Observing System” (MIS 5002697). L.E. and S.S.-K. acknowledge funding from a VIDI project from the Dutch Research Council (NWO project number 864.14.005). G.A.F. acknowledges contributions from the Observatorio San Calixto, which is supported by the Air Force Technical Application Center (AFTAC). C.R.L. acknowledge funding from the NSF Graduate Research Fellowship Program (grant No. DGE‐1745301). V.-H.M. and R.D.P. acknowledge support from grant CONACYT-299766. R.D.P. acknowledges support from the UNAM-DGAPA postdoctoral scholarship. J.O. acknowledges support from the Agencia Nacional de Investigación y Desarrollo (Scholarship ANID-PFCHA / Doctorado Nacional / 2020-21200903). S.P. acknowledges financial support from the Natural Environment Research Council (NE/R013144/1). A.E.R. acknowledges support from the K.H. Renlund foundation. M.K.S. acknowledges the New Zealand Earthquake Commission (EQC Project No 20796). H.X. acknowledges support from a Multidisciplinary Research on the Coronavirus and its Impacts (MRCI) grant from UC Santa Barbara. The Australian Seismometers in Schools data used in this research are supported by AuScope, enabled by the Australian Commonwealth NCRIS program. A.O. acknowledges support from the project RESIST, funded by the Belgian Federal Science Policy (contract SR/00/305) and the Luxembourg National Research Fund
Published: 2020
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25. Detection, analysis and removal of glitches from InSight's 1 seismic data from Mars

Author: John-Robert Scholz, Rudolf Widmer-Schnidrig, Paul Davis, Philippe Lognonné, Baptiste Pinot, Raphaël F Garcia, Francis Nimmo, Kenneth Hurst, Salma Barkaoui, Sébastien De Raucourt, Laurent Pou, Guénolé Mainsant, Nicolas Compaire, Arthur Cuvier, Eric Beucler, Mickaël Bonnin, Rakshit Joshi, Eléonore Stutzmann, Martin Schimmel, Anna Horleston, Maren Böse, Savas Ceylan, John Clinton, Martin Van Driel, Taichi Kawamura, Amir Khan, Simon C Stähler, Domenico Giardini, Constantinos Charalambous, Alexander E Stott, William T Pike, Ulrich R Christensen, and W Bruce Banerdt
Published: 2020
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26. A Comodulation Analysis of Atmospheric Energy Injection into the Ground Motion at InSight, Mars

Author: Constantinos Charalambous, Alexander E Stott, Tom Pike, John McClean, Tristram Warren, Aymeric Spiga, Donald Banfield, Raphaël F. Garcia, John Clinton, Simon C. Stähler, Sara Navarro López, Philippe Henri Lognonné, Taichi Kawamura, Martin van Driel, Maren Böse, Savas Ceylan, Amir Khan, Anna Catherine Horleston, Guénolé Orhand-Mainsant, Luis Mora Sotomayor, Naomi Murdoch, Domenico Giardini, and William Bruce Banerdt
Published: 2020
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27. Aeolian Changes at the InSight Landing Site on Mars: Multi-instrument Observations

Author: John A. Grant, Sebastien Rodriguez, Naomi Murdoch, Catherine M. Weitz, Mark T. Lemmon, Nicholas H. Warner, William B. Banerdt, T. Pike, Aymeric Spiga, Jorge Pla-Garcia, J. B. McClean, Philippe Lognonné, M. M. Baker, Alexander E. Stott, Ralph D. Lorenz, Catherine Johnson, Don Banfield, Tristram Warren, Veronique Ansan, Constantinos Charalambous, Ingrid Daubar, Antoine Lucas, Matthew P. Golombek, Clément Perrin, Daniel Viúdez-Moreiras, Sara Navarro Lopez, Luis Mora Sotomayor, Ernst Hauber, Justin N. Maki, Anna Mittelholz, Maria E. Banks, and Claire E. Newman
Subjects: Aeolian processes, Mars Exploration Program, Geology, Astrobiology
Abstract: Orbital and surface observations demonstrate that aeolian activity is occurring on Mars. Here we report the aeolian changes observed in situ by NASA's InSight lander during the first 400 sols of op...
Published: 2020
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28. Aeolian Changes at the Insight Landing Site on Mars: Multi-instrument Observations

Author: Constantinos Charalambous, Justin N. Maki, Naomi Murdoch, M. M. Baker, Alexander E. Stott, Mark T. Lemmon, Anna Mittelholz, Maria E. Banks, Aymeric Spiga, Catherine M. Weitz, T. Pike, Matthew P. Golombek, J. B. McClean, Catherine Johnson, Veronique Ansan, John A. Grant, Sebastien Rodriguez, Nicholas H. Warner, Ingrid Daubar, and Ralph D. Lorenz
Subjects: Aeolian processes, Mars Exploration Program, Geology, Astrobiology
Abstract: The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed in western Elysium Planitia on November 26, 2018. Because of its stationary position and a multi-instrument package, InSight offers the unique opportunity of detecting changes induced by aeolian activity and constraining the atmospheric conditions responsible for particle motion.In this work, we present the most significant changes from aeolian activity as detected by the InSight lander during its first 400 Martian days of operations. We will show that particle entrainment by wind activity around InSight is a subtle process and report simultaneous measurements observed across multiple instruments. The changes observed are episodic and are seen correlated with excursions in both seismic and magnetic signals, which will be discussed further. Our observations show that all aeolian movements are consistent with the passage of deep convective vortices between noon to 3 pm local time. These vortices may be the primary initiators for aeolian transportation at InSight, inducing episodic particulate motion of grains up to 3 mm in diameter.
Published: 2020
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29. On-deck seismology: Lessons from InSight for future planetary seismology

Author: Alexander E. Stott, Simon Stähler, Philippe Lognonné, Constantinos Charalambous, Sharon Kedar, Angela G. Marusiak, William T. Pike, Ralph D. Lorenz, Mark P. Panning, J. B. McClean, Don Banfield, William B. Banerdt, Naomi Murdoch, Ceri Nunn, Tristram Warren, and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Mars, Induced seismicity, Exploration of Mars, 01 natural sciences, Wind speed, Physics - Geophysics, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysique, Seismology, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Mars Exploration Program, Geophysics (physics.geo-ph), Geophysics, Planetary science, 13. Climate action, Space and Planetary Science, QUIET, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract: Before deploying to the surface of Mars, the short-period (SP) seismometer of the InSight mission operated on deck for a total of 48 hours. This dataset can be used to understand how deck-mounted seismometers can be used in future landed missions to Mars, Europa, and other planetary bodies. While operating on deck, the SP seismometer showed signals comparable to the Viking-2 seismometer near 3 Hz where the sensitivity of the Viking instrument peaked. Wind sensitivity showed similar patterns to the Viking instrument, although amplitudes on InSight were ~80% larger for a given wind velocity. However, during the low wind evening hours the instrument noise levels at frequencies between 0.1 and 1 Hz were comparable to quiet stations on Earth, although deployment to the surface below the Wind and Thermal Shield lowered installation noise by roughly 40 dB in acceleration power. With the observed noise levels and estimated seismicity rates for Mars, detection probability for quakes for a deck-mounted instrument are low enough that up to years of on-deck recordings may be necessary to observe an event. Because the noise is dominated by wind acting on the lander, though, deck-mounted seismometers may be more practical for deployment on airless bodies, and it is important to evaluate the seismicity of the target body and the specific design of the lander. Detection probabilities for operation on Europa reach over 99% for some proposed seismicity models for a similar duration of operation if noise levels are comparable to low-wind time periods on Mars., 20 pages, 7 figures, accepted to Journal of Geophysical Research: Planets
Published: 2020

30. The seismicity of Mars

Author: Simon Stähler, Anna Horleston, Sharon Kedar, John-Robert Scholz, L. Luno, J. B. McClean, Henri Samuel, Fabian Euchner, S. Barkaoui, Tristram Warren, Mélanie Drilleau, Martin Schimmel, Maren Böse, M. Nonon, M. van Driel, Nicholas A Teanby, Alexander E. Stott, Savas Ceylan, Ludovic Margerin, A. Jacob, Brigitte Knapmeyer-Endrun, William B. Banerdt, Guenole Mainsant, Tamara Gudkova, Antoine Lucas, T. Gabsi, Renee Weber, Taichi Kawamura, Vincent Conejero, Eléonore Stutzmann, Daniele Antonangeli, C. Agard, Constantinos Charalambous, C. Ferrier, P. Combes, K. Hurst, Philippe Lognonné, Don Banfield, Aymeric Spiga, William T. Pike, Constanza Pardo, J. A Rodriguez Manfredi, Martin Knapmeyer, Attilio Rivoldini, Francis Nimmo, U. R. Christensen, Sue Smrekar, Ingrid Daubar, R. Llorca-Cejudo, Mark P. Panning, Scott D. King, Eric Beucler, Foivos Karakostas, Amir Khan, E. Barrett, Mark A. Wieczorek, Raphaël F. Garcia, Clément Perrin, Naomi Murdoch, David Mimoun, C. Yana, John Clinton, Domenico Giardini, Swiss National Supercomputing Centre, Swiss National Science Foundation, Agence Nationale de la Recherche (France), State Secretariat for Education, Research and Innovation (Switzerland), UK Space Agency, California Institute of Technology, German Centre for Air and Space Travel, Schimmel, Martin, Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPGP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut de Physique du Globe de Paris, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Mechanical Engineering [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, INSTITUT OF GEOPHYSICS ETHZ, Swiss Seismological Service, Department of Earth and Environmental Sciences [München], Ludwig-Maximilians-Universität München (LMU), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Cornell University [New York], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Academy-EURAC, Institute for Applied Remote Sensing, Kyoto University [Kyoto], Departments of Anesthesiology and Physiology and Biophysics, University of Alabama at Birmingham [ Birmingham] (UAB), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), unité de recherche de l'institut du thorax UMR1087 UMR6291 (ITX), Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), De la Préhistoire à l'Actuel : Culture, Environnement et Anthropologie (PACEA), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Schmidt United Institute of Physics of the Earth [Moscow] (IPE), Russian Academy of Sciences [Moscow] (RAS), NASA, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Ingénierie des Matériaux (LIM), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), UNS-CNRS-Observatoire de la Côte d'Azur, Department of Earth and Planetary Sciences [Santa Cruz], University of California [Santa Cruz] (UCSC), University of California-University of California, School of Earth Sciences [Bristol], University of Bristol [Bristol], Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), California Institute of Technology (CALTECH)-NASA, Department of Geological Sciences, University of Florida [Gainesville], Oncogenesis Stress Signaling (OSS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-CRLCC Eugène Marquis (CRLCC), Cornell University, Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), Schimmel, Martin [0000-0003-2601-4462], Department of Earth and Environmental Sciences [Munich], Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Laboratoire de Géophysique Interne et Tectonophysique (LGIT), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Laboratoire Central des Ponts et Chaussées (LCPC)-Institut des Sciences de la Terre (ISTerre), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPG Paris), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Unité de recherche de l'institut du thorax (ITX-lab), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Induced seismicity, InSight Mars Marsbeben Seismizität, 010502 geochemistry & geophysics, seismology, 01 natural sciences, Mantle (geology), Elysium, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Autre, Planet, inner planets, ComputingMilieux_MISCELLANEOUS, Seismology, InSight, 0105 earth and related environmental sciences, Seismicity, Crust, Geology, Mars Exploration Program, [SDU]Sciences of the Universe [physics], 13. Climate action, General Earth and Planetary Sciences
Abstract: The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed in Elysium Planitia on Mars on 26 November 2018 and fully deployed its seismometer by the end of February 2019. The mission aims to detect, characterize and locate seismic activity on Mars, and to further constrain the internal structure, composition and dynamics of the planet. Here, we present seismometer data recorded until 30 September 2019, which reveal that Mars is seismically active. We identify 174 marsquakes, comprising two distinct populations: 150 small-magnitude, high-frequency events with waves propagating at crustal depths and 24 low-frequency, subcrustal events of magnitude Mw 3–4 with waves propagating at various depths in the mantle. These marsquakes have spectral characteristics similar to the seismicity observed on the Earth and Moon. We determine that two of the largest detected marsquakes were located near the Cerberus Fossae fracture system. From the recorded seismicity, we constrain attenuation in the crust and mantle, and find indications of a potential low-S-wave-velocity layer in the upper mantle. © 2020, The Author(s), under exclusive licence to Springer Nature Limited., We acknowledge NASA, CNES and its partner agencies and institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC and MPS-MPG) and the flight operations team at JPL, SISMOC, MSDS, IRIS-DMC and PDS for providing SEIS data. The Swiss co-authors were jointly funded by (1) the Swiss National Science Foundation and French Agence Nationale de la Recherche (SNF-ANR project 157133 ‘Seismology on Mars’), (2) the Swiss National Science Foundation (SNF project 172508 ‘Mapping the internal structure of Mars’), (3) the Swiss State Secretariat for Education, Research and Innovation (SEFRI project ‘MarsQuake Service-Preparatory Phase’) and (4) ETH Research grant no. ETH-06 17-02. Additional support came from the Swiss National Supercomputing Centre (CSCS) under project ID s922. The Swiss contribution in the implementation of the SEIS electronics was made possible by funding from the federal Swiss Space Office (SSO) and contractual and technical support from the ESA-PRODEX office. The French Team acknowledge the French Space Agency CNES, which has supported and funded all SEIS-related contracts and CNES employees, as well as CNRS and the French team universities for personal and infrastructure support. Additional support was provided by ANR (ANR-14-CE36-0012-02 and ANR-19-CE31-0008-08) and, for the IPGP team, by the UnivEarthS Labex programme (ANR-10-LABX-0023), IDEX Sorbonne Paris Cité (ANR-11-IDEX-0005-0). SEIS-SP development and delivery were funded by the UK Space Agency. A portion of the work was carried out at the InSight Project at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The MPS SEIS team acknowledges funding for development of the SEIS leveling system by the DLR German Space Agency. We thank gempa GmbH for software development related to the MQS tools. This paper is InSight contribution number 102.
Published: 2020
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31. The atmosphere of Mars as observed by InSight

Author: Justin N. Maki, A. Jacob, Stephen R. Lewis, Nicholas A Teanby, Mercedes Marin-Jimenez, Anna Mittelholz, Constantinos Charalambous, Sara Navarro, M. M. Baker, Mark T. Lemmon, Tristram Warren, Javier Gómez-Elvira, Alexander E. Stott, Matthew P. Golombek, Antoine Lucas, Jorge Pla-Garcia, J. Torres, Eric Beucler, Balthasar Kenda, Aymeric Spiga, Rudolf Widmer-Schnidrig, Philippe Lognonné, Veronique Ansan, V. Peinado, Özgür Karatekin, William T. Pike, Nils Mueller, Savas Ceylan, K. Hurst, Daniel Viúdez-Moreiras, Christopher T. Russell, Antonio Molina, Sebastien Rodriguez, Clément Perrin, Naomi Murdoch, David Mimoun, Claire E. Newman, Ralph D. Lorenz, L. Martire, Luis Mora-Sotomayor, Simon Stähler, Tilman Spohn, Lucie Rolland, Stephen Sackett, Ingrid Daubar, Raphaël F. Garcia, W. Bruce Banerdt, Catherine L. Johnson, Domenico Giardini, Brian Carcich, Don Banfield, Suzanne E. Smrekar, John Clinton, François Forget, Ehouarn Millour, Taichi Kawamura, J. A. Rodríguez-Manfredi, Bart Van Hove, A. Lepinette, Anni Määttänen, J. B. McClean, Cornell Center for Astrophysics and Planetary Science (CCAPS), Cornell University, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Aeolis Research, Space Science Institute [Boulder] (SSI), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Royal Observatory of Belgium [Brussels], School of Earth Sciences [Bristol], University of Bristol [Bristol], Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Department of Electrical and Electronic Engineering [London] (DEEE), Imperial College London, Department of Earth, Ocean and Atmospheric Sciences [Vancouver] (EOAS), University of British Columbia (UBC), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Sorbonne Université (SU), School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] (OU), Swiss Seismological Service [ETH Zurich] (SED), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Department of Physics [Oxford], University of Oxford [Oxford], Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Université Côte d'Azur (UCA), Universität Stuttgart [Stuttgart], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Morton K. Blaustein Department of Earth and Planetary Sciences [Baltimore], Johns Hopkins University (JHU), Center for Earth and Planetary Studies [Washington] (CEPS), Smithsonian National Air and Space Museum, Smithsonian Institution-Smithsonian Institution, Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California-University of California, Département Electronique, Optronique et Signal (DEOS), Cornell University [New York], 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), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Royal Observatory of Belgium [Brussels] (ROB), NASA-California Institute of Technology (CALTECH), Department of Earth, Ocean and Atmospheric Sciences [Vancouver] (UBC EOAS), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)-Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), University of Oxford, University of California (UC)-University of California (UC), ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Määttänen, A. [0000-0002-7326-8492], Martire, L. [0000-0002-9402-6150], Rodríguez Manfredi, J. A. [0000-0003-0461-9815], Lognonné, P. [0000-0002-1014-920X], Rodríguez, S. [0000-0003-1219-0641], Spiga, A. [0000-0002-6776-6268], Perrin, C. [0000-0002-7200-5682], Molina, A. [0000-0002-5038-2022], García, R. [0000-0003-1460-6663], Murdoch, N. [0000-0002-9701-4075], Lorenz, R. [0000-0001-8528-4644], Mittelholz, A. [0000-0002-5603-7334], Kawamura, T. [0000-0001-5246-5561], Widmer Schnidrig, R. [0000-0001-9698-2739], McClean, J. [0000-0002-7863-0120], Mueller, N. [0000-0001-9229-8921], Lewis, S. [0000-0001-7237-6494], Teanby, N. [0000-0003-3108-5775], Warren, T. [0000-0003-3877-0046], Milliour, E. [0000-0003-4808-9203], Lemmon, M. [0000-0002-4504-5136], Clinton, J. [0000-0001-8626-2703], Ceylan, S. [0000-0002-6552-6850], Banfield, D. [0000-0003-2664-0164], Agence Nationale de la Recherche (ANR), and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)
Subjects: Martian, 010504 meteorology & atmospheric sciences, Atmosphere, Mars, Mars Exploration Program, Atmosphere of Mars, 010502 geochemistry & geophysics, Mars Atmosphere, 01 natural sciences, Wind speed, Astrobiology, Autre, 13. Climate action, Dust storm, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, Environmental science, Aeolian processes, [SDU.OTHER]Sciences of the Universe [physics]/Other, Meteorologie, InSight mission, Dust devil, 0105 earth and related environmental sciences, InSight
Abstract: Banfield, D. et al., The atmosphere of Mars is thin, although rich in dust aerosols, and covers a dry surface. As such, Mars provides an opportunity to expand our knowledge of atmospheres beyond that attainable from the atmosphere of the Earth. The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander is measuring Mars’s atmosphere with unprecedented continuity, accuracy and sampling frequency. Here we show that InSight unveils new atmospheric phenomena at Mars, especially in the higher-frequency range, and extends our understanding of Mars’s meteorology at all scales. InSight is uniquely sensitive to large-scale and regional weather and obtained detailed in situ coverage of a regional dust storm on Mars. Images have enabled high-altitude wind speeds to be measured and revealed airglow—faint emissions produced by photochemical reactions—in the middle atmosphere. InSight observations show a paradox of aeolian science on Mars: despite having the largest recorded Martian vortex activity and dust-devil tracks close to the lander, no visible dust devils have been seen. Meteorological measurements have produced a catalogue of atmospheric gravity waves, which included bores (soliton-like waves). From these measurements, we have discovered Martian infrasound and unexpected similarities between atmospheric turbulence on Earth and Mars. We suggest that the observations of Mars’s atmosphere by InSight will be key for prediction capabilities and future exploration., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737); Centro de Desarrollo Tecnológico e Industrial (CDTI), Ministerio de Economía y Competitividad and the Instituto Nacional de Técnica Aeroespacial (INTA).
Published: 2020
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32. Full-Band Signal Extraction From Sensors in Extreme Environments: The NASA InSight Microseismometer

Author: Alexander E. Stott, Constantinos Charalambous, William T. Pike, Tristram Warren, and Science & Technology Facilities Council
Subjects: Technology, Computer science, instrument response correction, 0205 Optical Physics, 02 engineering and technology, 01 natural sciences, Physics, Applied, NOISE, Analytical Chemistry, Engineering, 0103 physical sciences, Electrical and Electronic Engineering, MEMS seismometer, temperature dependence, Instruments & Instrumentation, 010303 astronomy & astrophysics, Instrumentation, Decorrelation, Remote sensing, Sensor fusion, Signal processing, Science & Technology, Physics, Attenuation, Bandwidth (signal processing), Engineering, Electrical & Electronic, Kalman filter, Mars Exploration Program, 021001 nanoscience & nanotechnology, 0906 Electrical and Electronic Engineering, Physical Sciences, space applications, SEISMOMETER, 0210 nano-technology, 0913 Mechanical Engineering
Abstract: Physically meaningful signal extraction from sensors deployed in extreme environments requires a combination of attenuation of confounding inputs and the removal of their residual using decorrelation techniques. In space applications where the resources for physical attenuation are limited, there is a necessity to apply the most effective post-processing analysis available. This paper describes the extraction of the seismic signal from an MEMS microseismometer to be deployed on the surface of Mars. The signal processing, which covers the full bandwidth $1 \times 10^{-5}$ Hz to 40 Hz, uses a novel application of sensor fusion through an indirect Kalman Filter in combination with a thermal model of the microseismometer to remove the aseismic contribution of temperature over the frequency range. Owing to the full-band decorrelation, the analysis (based on pre-landing testing in analogous scenarios) produces both a characterization of the microseismomter and a signal processing approach for information retrieval on Mars, along with other planetary and terrestrial planetary deployments.
Published: 2018
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33. Simultaneous diagonalisation of the covariance and complementary covariance matrices in quaternion widely linear signal processing

Author: Clive Cheong Took, Shirin Enshaeifar, Alexander E. Stott, Danilo P. Mandic, Min Xiang, Sithan Kanna, and Yili Xia
Subjects: FOS: Computer and information sciences, Computer science, Computer Science - Information Theory, Structure (category theory), 02 engineering and technology, Domain (mathematical analysis), Factorization, FOS: Mathematics, 0202 electrical engineering, electronic engineering, information engineering, Electrical and Electronic Engineering, Quaternion, Signal processing, Basis (linear algebra), Information Theory (cs.IT), Computer Science - Numerical Analysis, 020206 networking & telecommunications, Numerical Analysis (math.NA), Covariance, Control and Systems Engineering, Product (mathematics), Signal Processing, 020201 artificial intelligence & image processing, Mathematics::Differential Geometry, Computer Vision and Pattern Recognition, Algorithm, Software
Abstract: Recent developments in quaternion-valued widely linear processing have established that the exploitation of complete second-order statistics requires consideration of both the standard covariance and the three complementary covariance matrices. Although such matrices have a tremendous amount of structure and their decomposition is a powerful tool in a variety of applications, the non-commutative nature of the quaternion product has been prohibitive to the development of quaternion uncorrelating transforms. To this end, we introduce novel techniques for a simultaneous decomposition of the covariance and complementary covariance matrices in the quaternion domain, whereby the quaternion version of the Takagi factorisation is explored to diagonalise symmetric quaternion-valued matrices. This gives new insights into the quaternion uncorrelating transform (QUT) and forms a basis for the proposed quaternion approximate uncorrelating transform (QAUT) which simultaneously diagonalises all four covariance matrices associated with improper quaternion signals. The effectiveness of the proposed uncorrelating transforms is validated by simulations on both synthetic and real-world quaternion-valued signals., Comment: 41 pages, single column, 10 figures
Published: 2018
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34. Passive Method for Reducing Temperature Sensitivity of a Microelectromechanical Seismic Accelerometer for Marsquake Monitoring Below 1 Nano- g

Author: Alexander E. Stott, William T. Pike, Constantinos Charalambous, and Huafeng Liu
Subjects: Materials science, Gravimeter, Acoustics, General Physics and Astronomy, 02 engineering and technology, 021001 nanoscience & nanotechnology, Accelerometer, 01 natural sciences, Displacement (vector), Thermal expansion, Acceleration, Thermoelastic damping, 0103 physical sciences, Sensitivity (control systems), 010306 general physics, 0210 nano-technology, Reduction (mathematics)
Abstract: The passive technology described in this paper is important for reducing the thermoelastic response of silicon-based high-precision accelerometers and gravimeters. This study uses the angular strain induced by mismatched coefficients of thermal expansion to passively compensate for the sag displacement in Si-based spring-mass systems in environments with fluctuating temperature. The hundredfold reduction in temperature sensitivity allows a top acceleration sensitivity of less than 10${}^{\ensuremath{-}9}$ $g$. Such a temperature-compensated seismic accelerometer has already been used as a science payload of the InSight Mars lander, which touched down in November 2018, for marsquake monitoring.
Published: 2019
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35. SEIS: Insight’s Seismic Experiment for Internal Structure of Mars

Author: L. Perrin, C. Bonjour, N. Toulemont, Jean-Luc Berenguer, G. Perez, James Wookey, A. G. Mukherjee, Hallie Gengl, Edward A. Miller, Delphine Faye, Antoine Mocquet, J. Sicre, B. Vella, D. Dilhan, C. Larigauderie, John C. Bousman, M. Nonon, Y. Bennour, Véronique Dehant, Jeffrey W. Umland, T. Nebut, D. Hernandez, M. Eberhardt, Vincent Conejero, Rudolf Widmer-Schnidrig, Philippe Lognonné, G. de los Santos, S. A. D’Agostino, Savas Ceylan, Justin N. Maki, G. Aveni, P. Revuz, S. de Raucourt, C. Aicardi, Clément Perrin, A. K. Delahunty, Constanza Pardo, Domenico Giardini, L. Pou, Robert J. Calvet, D. Savoie, O. Robert, V. Gharakanian, S. Ben Charef, Constantinos Charalambous, Kerry Klein, S. M. Madzunkov, J. M. Desmarres, Sue Smrekar, S. B. Calcutt, F. Grinblat, Nicholas A Teanby, I. M. Standley, Naomi Murdoch, Brigitte Knapmeyer-Endrun, M. Deleuze, C. Doucet, William T. Pike, Tom L. Hoffman, F. Mialhe, Cecily M. Sunday, J. Paredes-Garcia, Matthew P. Golombek, P. Bhandari, Huafeng Liu, B. Pouilloux, E. Blanco, Gabriel Pont, Simon Stähler, M. E. Johnson, Nicolas Verdier, L. Luno, Ned W. Ferraro, R. Perez, Mélanie Drilleau, F. Ijpelaan, B. Lecomte, M. van Driel, A. Sauron, I. Estève, Mark P. Panning, David Mimoun, P. A. Dandonneau, B. Kenda, T. Gabsi, W. Raff, P. Boutte, T. Warren, Joan Ervin, Fabian Euchner, S. Tillier, K. J. Hurst, Stephen Larson, Davor Mance, Mark A. Wieczorek, J. A. Rodriguez-Manfredi, Justin Lin, Jaime Singer, M. Monecke, Robert W. Denise, E.-P. Miettinen, Maren Böse, E. Locatelli, I. Savin de Larclause, J. Gagnepain-Beyneix, L. Khachikyan, Philippe Laudet, T. Carlier, Alexander E. Stott, Neil Bowles, Brian Bone, C. Imbert, Sharon Kedar, A. Rosak, Fred Calef, O. Pot, O. M. Avalos, P. Labrot, Jeroen Tromp, Lucile Fayon, C. Moreau, J. Baroukh, William B. Banerdt, M. Bierwirth, Ranah Irshad, M. André, Christopher T. Russell, S. L. Marshall, M. Parise, J.-R. Meyer, P. Pasquier, N. Faye-Refalo, Ingrid Daubar, M. A. Balzer, R. Gonzalez, M. Hetzel, K. Brethomé, Y. Pahn, Raphaël F. Garcia, J. tenPierick, U. R. Christensen, Farah Alibay, Renee Weber, Robert G. Deen, Eléonore Stutzmann, J. Temple, Don Banfield, A. Bouisset, D. B. Klein, A. Borrien, Ashitey Trebi-Ollennu, R. Llorca-Cejudo, L. J. Facto, J. M. Mouret, Alexis Paillet, Peter Zweifel, P. Bruneau, Catherine L. Johnson, C. Brysbaert, J. E. Feldman, A. Kramer, Luigi Ferraioli, Jane Hurley, Taichi Kawamura, Nicholas Onufer, W. Kühne, Eric Beucler, Amir Khan, M. Sodki, L. Kerjean, A. Sylvestre-Baron, C. Desfoux, C. Yana, John Clinton, J. R. Willis, Juan Villalvazo, Pierre Delage, Mihail P. Petkov, M. C. Wallace, T. Camus, Ioannis G. Mikellides, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Mechanical Engineering [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Centre National d'Études Spatiales [Toulouse] (CNES), Geological Institute (ETHZ), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Oxford, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Marshall Space Flight Center (MSFC), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Mecanique des Fluides et d'Acoustique (LMFA), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), Advanced Technology and Research, 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), Clarendon Laboratory [Oxford], Huazhong University of Science and Technology [Wuhan] (HUST), Kinemetrics, Cornell University [New York], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of California [Los Angeles] (UCLA), University of California (UC), Institut of GeophysicsETHZ, Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Swiss Seismological Service, Royal Observatory of Belgium [Brussels] (ROB), Géotechnique (cermes), Laboratoire Navier (navier umr 8205), Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of British Columbia (UBC), Planetary Science Institute [Tucson] (PSI), Laboratoire national de métrologie et d'essais - Systèmes de Référence Temps-Espace (LNE - SYRTE), Systèmes de Référence Temps Espace (SYRTE), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), University of Bristol [Bristol], Department of Geosciences [Princeton], Princeton University, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universität Stuttgart [Stuttgart], School of Earth Sciences [Bristol], Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), University of Oxford [Oxford], Max Planck Institute for Solar System Research (MPS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California, INSTITUT OF GEOPHYSICS ETHZ, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Karlsruhe Institute of Technology and Stuttgart University, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), California Institute of Technology (CALTECH)-NASA, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Département Electronique, Optronique et Signal (DEOS), Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Cornell University, Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Royal Observatory of Belgium [Brussels], PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), School of Earth Sciences University of Bristol, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Seismometer, DISSIPATIVE FACTOR, 010504 meteorology & atmospheric sciences, FREE OSCILLATIONS, BULK COMPOSITION, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Astronomy & Astrophysics, 01 natural sciences, Transfer function, Article, NETWORK SCIENCE, Autre, 0103 physical sciences, 0201 Astronomical and Space Sciences, INTERIOR STRUCTURE, ddc:530, Ground segment, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, InSight, Data processing, Science & Technology, Physics, Bandwidth (signal processing), Mars seismology, Astronomy and Astrophysics, Moment magnitude scale, SINGLE-STATION, THERMAL EVOLUTION, Mars Exploration Program, Geodesy, Space and Planetary Science, Physical Sciences, WAVE PROPAGATION, ELYSIUM PLANITIA, [SDU.OTHER]Sciences of the Universe [physics]/Other, Robotic arm, SEIS, Geology, METEORITE IMPACTS
Abstract: By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars’ surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking’s Mars seismic monitoring by a factor of ∼2500 at 1 Hz and ∼200000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars’ surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of Mw∼3 at 40∘ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution., Space Science Reviews, 215 (1), ISSN:1572-9672, ISSN:0038-6308
Published: 2019
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36. The Marsquake catalogue from InSight, sols 0–478

Author: Don Banfield, Alexander E. Stott, Maren Böse, Philippe Lognonné, Guenolé Orhand-Mainsant, William T. Pike, Fabian Euchner, Eric Beucler, Mark P. Panning, Amir Khan, Raphaël F. Garcia, Constantinos Charalambous, Savas Ceylan, John Clinton, Aymeric Spiga, Simon Stähler, Anna Horleston, Sharon Kedar, Taichi Kawamura, Suzanne E. Smrekar, Nikolaj Dahmen, William B. Banerdt, John-Robert Scholz, Clément Perrin, Domenico Giardini, Martin van Driel, Swiss Seismological Service [ETH Zurich] (SED), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)-Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Imperial College London, School of Earth Sciences [Bristol], University of Bristol [Bristol], Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, California Institute of Technology (CALTECH), Cornell Center for Astrophysics and Planetary Science (CCAPS), Cornell University [New York], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), 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), and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, Physics and Astronomy (miscellaneous), [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Marsquakes, Mars seismicity catalogue, InSight mission, Induced seismicity, 010502 geochemistry & geophysics, 01 natural sciences, Mars Seismology, Autre, Long period, Short duration, 0105 earth and related environmental sciences, Data collection, Event (computing), Astronomy and Astrophysics, Mars Exploration Program, Key features, Geophysics, 13. Climate action, Space and Planetary Science, Geology, Seismology
Abstract: The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission began collecting high quality seismic data on Mars in February 2019. This manuscript documents the seismicity observed by SEIS, InSightâ€™s seismometer, from this time until the end of March 2020. Within the InSight project, the Marsquake Service (MQS) is responsible for prompt review of all seismic data collected by InSight, detection of events that are likely to be of seismic origin, and curation and release of seismic catalogues. In the first year of data collection, MQS have identified 465 seismic events that we interpret to be from regional and teleseismic marsquakes. Seismic events are grouped into 2 different event families: the low frequency family is dominated by energy at long period below 1 s, and the high frequency family primarily include energy at and above 2.4 Hz. Event magnitudes, from Mars-specific scales, range from 1.3 to 3.7. A third class of events with very short duration but high frequency bursts have been observed 712 times. These are likely associated with a local source driven by thermal stresses. This paper describes the data collected so far in the mission and the procedures under which MQS operates; summarises the content of the current MQS seismic catalogue; and presents the key features of the events we have observed so far, using the largest events as examples. ISSN:0031-9201 ISSN:1872-7395
Published: 2021
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37. An online NIPALS algorithm for Partial Least Squares

Author: William T. Pike, Alexander E. Stott, Danilo P. Mandic, and Sithan Kanna
Subjects: Multivariate analysis, Computer science, MathematicsofComputing_NUMERICALANALYSIS, 020206 networking & telecommunications, 02 engineering and technology, Covariance, Non-linear iterative partial least squares, Matrix decomposition, Matrix (mathematics), Partial least squares regression, Linear regression, 0202 electrical engineering, electronic engineering, information engineering, Statistics::Methodology, 020201 artificial intelligence & image processing, Algorithm design, Algorithm, Eigenvalues and eigenvectors
Abstract: Partial Least Squares (PLS) has been gaining popularity as a multivariate data analysis tool due to its ability to cater for noisy, collinear and incomplete data-sets. However, most PLS solutions are designed as block-based algorithms, rendering them unsuitable for environments with streaming data and non-stationary statistics. To this end, we propose an online version of the nonlinear iterative PLS (NIPALS) algorithm, based on a recursive computation of covariance matrices and gradient-based techniques to compute eigenvectors of the relevant matrices. Simulations over synthetic data show that the regression coefficients from the proposed online PLS algorithm converge to those of its block-based counterparts.
Published: 2017
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