We have designed and developed a breadboard of a small atmospheric lidar to measure the vertical profiles of dust, water vapor and winds in the lower Mars atmosphere from its surface. Our approach remotely profiles aerosols, atmospheric water vapor and winds by using a laser that emits near 1911 nm and using a direct detection receiver. The lidar measures vertically resolved profiles of water vapor by using a tunable single-frequency Tm-fiber laser pulsed at a 10 kHz pulse rate. The laser is tuned onto and off the strong isolated water vapor absorption lines and water vapor profiles will be determined via the differential absorption lidar (DIAL) technique. The same laser is used for measuring the aerosol and wind profiles by tuning the laser off-line and by resolving the Doppler shift in the aerosol backscatter profiles. The lidar receiver uses a 12-cm lens-type telescope and a 16-pixel HgCdTe avalanche photodiode (APD) as the detector.

Clouds play a crucial role in the past and current climate of Mars. Cloud particles impact the planet's energy balance and atmospheric dynamics, as well as influence the vertical distribution of dust particles through dust scavenging. This process of dust scavenging by clouds has significant consequences for the planet's water cycle. For example, regions in the atmosphere with insufficient quantities of dust particles, or condensation nuclei, can inhibit the formation of H2O clouds, leading to the presence of water vapor in excess of saturation [1]. Recent observations made by the MEDA Radiation and Dust Sensor (RDS) [2,3] have shown a marked decline in mesospheric cloud activity (above 35-40 km) when Mars is near its aphelion (within the Aphelion Cloud Belt-ACB season), notably occurring during solar longitudes (Ls) between Ls 70° and 80° [4] (see Figure 1).In order to investigate the possible factors leading to this decrease in water ice abundance, we used a one-dimensional cloud microphysical model [5,6], which includes the processes of nucleation, condensation, coagulation, evaporation, precipitation, and coalescence, and where the vertical mixing is parameterized using an eddy diffusion profile (Keddy). Combining cloud microphysics modeling with ground-based (Mars 2020 and InSight) and orbital observations (TGO and MRO) of clouds, water vapor, and temperature, we will discuss in this presentation the main factors controlling the water abundance in the Martian mesosphere during the ACB season.References: [1] Maltagliati, Luca, et al. "Evidence of water vapor in excess of saturation in the atmosphere of Mars." science 333.6051 (2011): 1868-1871. [2] Apestigue, V., et al. “Radiation and Dust Sensor for Mars Environmental Dynamic Analyzer Onboard M2020 Rover”. Sensor 22.8 (2022): 2907. [3] Rodriguez-Manfredi, Jose Antonio, et al. “The Mars Enviromental Dynamics Analyzer, MEDA. Asuite of enviromental sensors for the Mars 2020 mission.” Space science reviews 217.3 (2021): 1-86. [4] Toledo, D., et al. “Measurement of aerosol optical depth and sub-visual cloud detection using the optical depth sensor (ODS)”. Atmospheric Measurement Techniques 9.2 (2016): 455-467. [5] Montmessin, F., Rannou, P., Cabane, M.: New insights into martian dust distribution and water-ice cloud microphysics. Journal of Geophysical Research: Planets 107(E6), 41 (2002). [6] Rannou, P., Montmessin, F., Hourdin, F., Lebonnois, S.: The latitudinal distribution of clouds on titan. science 311(5758), 201205 (2006).

The Ultraviolet and Visible Spectrometer (UVIS) channel [1] of the Nadir and Occultation for Mars Discovery (NOMAD) instrument [2] aboard the ExoMars Trace Gas Orbiter has been making observations of the vertical, latitudinal and seasonal distributions of ozone. Here, we present ~1.5 Mars Years (MY) of vertical profiles of ozone, from LS = 163° in MY34 to LS = 320° in MY35. This period includes the occurrence of the MY34 Global Dust Storm. The relative abundance of both ozone and water (from coincident NOMAD measurements) increases with decreasing altitude below ~40 km at perihelion and at aphelion, localised decreases in ozone abundance exist between 25-35 km coincident with the location of modelled peak water abundances. High latitude (> ± 55°), high altitude (40-55 km) equinoctial ozone enhancements are observed in both hemispheres (LS ~350‑40°). Morning terminator observations show elevated ozone abundances with respect to evening observations, most likely attributed to diurnal photochemical partitioning along the line of sight between ozone and O. The ozone retrievals presented here provide the most complete global description of Mars ozone vertical distributions to date as a function of season and latitude

On top of listening to laser shots, rover sounds and the Ingenuity rotorcraft, SuperCam’s Mars microphone has recorded over 7 hours of ambient background noise on Mars. These background recordings contain signal due to the Martian wind. Through a comparison to the meteorological data recorded by the MEDA (Mars Environmental Dynamics Analyzer), we can determine the relationships between the microphone data, the wind and the atmospheric stability. Based on these relationships, we have determined a way to estimate the wind speed using the microphone through Gaussian process regression, a machine learning technique. Owing to the sampling rate of 25 000 samples per second, the microphone data can be used to examine Mars’ atmospheric dynamics at high frequencies, as yet unexplored on Mars. We will demonstrate how the wind speed estimates from the microphone provide an assessment of turbulence at fine scales, shedding light on the dissipative regime on Mars. One particularly interesting signal recorded by the microphone was a dust devil, which had fast varying winds within the walls of its vortex and signal from dust particles hitting the rover. Combining the microphone data with information from the MEDA sensors and navigation camera (Navcam) images enabled a full parameterization of this event.

We utilize SuperCam's Mars microphone to provide information on wind speed and turbulence at high frequencies on Mars. To do so, we first demonstrate the sensitivity of the microphone signal level to wind speed, yielding a power law dependence. We then show the relationship between the microphone signal level and pressure, air and ground temperatures. A calibration function is constructed using Gaussian process regression (a machine learning technique) taking the microphone signal and air temperature as inputs to produce an estimate of the wind speed. This provides a high rate wind speed estimate on Mars, with a sample every 0.01 s. As a result, we determine the fast fluctuations of the wind at Jezero crater which highlights the nature of wind gusts over the Martian day. To analyze the turbulent behavior of this wind speed estimate, we calculate its normalized standard deviation, known as gustiness. To characterize the behavior of this high frequency turbulent intensity at Jezero crater, correlations are shown between the evaluated gustiness statistic and pressure drop rates/sizes, temperature and energy fluxes. This has implications for future atmospheric models on Mars, taking into account turbulence at the finest scales.

Neary, L.; Daerden, F.; Aoki, S.; Whiteway, J.; Clancy, R.T.; Smith, M.; Viscardy, S.; Erwin, J.T.; Thomas, I.R.; Villanueva, G.; Liuzzi, G.; Crismani, M.; Wolff, M.; Lewis, S.R.; Holmes, J.A.; Patel, M.R.; Giuranna, M.; Depiesse, C.; Piccialli, A.; Robert, S.; Trompet, L.; Willame, Y.; Ristic, B. and Vandaele, A.C. (2019). Explanation the increase in high altitude water on Mars observed by NOMAD during the 2018 global dust storm. Geophysical Research Letters Early access.

IntroductionPrivacy preserving record linkage (PPRL) using encoded or hashed data has potential to enable large-scale record linkage of previously inaccessible data. With limited real-world evaluation and implementation of PPRL at scale it is challenging for linkage practitioners to judiciously balance data protection with the accuracy and usability of linked datasets. Objectives and ApproachWe evaluated the performance of PPRL techniques using Bloom filters for linkage of data across primary and secondary care settings. This technique limits the need to disclose personal information for linkage activities. Primary care data included 272,202 records from 16 general practices in NSW. This was linked to 42.8 million records from a 7 year series of emergency presentations, hospitalisations and death registrations. For the purpose of evaluation, personal information was encoded within the data linkage centre. The quality of PPRL linkage was assessed against the true match status based on a gold standard probabilistic linkage using full personal identifiers. ResultsCompared to the gold standard probabilistic linkage using full personal identifiers, the PPRL techniques produced quality metrics of precision, recall and F measure in excess of 0.90. When configured to leverage pre-existing links between emergency department, hospital and mortality data, quality metrics around 0.98-0.99 were achieved. Lower rates of linkage quality were associated with missing demographic information and some residual variation in linkage quality across practices was observed. Conclusion/ImplicationsPPRL using Bloom filters is a promising technique for achieving high quality linkage across primary and secondary care in Australia. Further evaluation will assess scalability and quality in Australia but international collaborations are encouraged to more rapidly develop the evidence base and tactical approaches to support real world implementations.

IntroductionMortality inequalities by income and education levels have historically been estimated using an area-based approach in Canada. Although useful in measuring socioeconomic inequalities overtime, this method underestimates the level of inequality and only allows the examination of a single dimension at a time. Objectives and ApproachTo create a series of census linked datasets that allowed for the examination of health inequalities across different socioeconomic dimensions. Specifically, five census cycles (beginning with the 1991 Census) were probabilistically and deterministically linked to different health outcomes (mortality, cancer, hospitalization) to create the Canadian Census Health and Environment Cohort (CanCHEC). Each dataset was created using a similar methodological approach which allowed for the measurement of these health inequalities over time. Mortality inequalities by both income and education level (including multidimensional) for all causes and cause-specific groups were examined. ResultsFive census linked datasets were constructed that followed mortality for a period of up to 20 years. The 1991 CanCHEC includes 2.6 million adults, the 1996 and 2001 CanCHECs include 3.5 million adults respectively, and the 2006 and 2011 CanCHECs include 5.9 and 6.5 million people respectively. Findings revealed a stair-stepped gradient in all-cause and cause-specific mortality by educational attainment and income quintile across each time period. The lowest mortality rates were among the university educated and richest income quintile and highest mortality rates among those with less than high school graduation and the poorest income quintile. The gradient differed by cause of death groupings. Over the 25-year time period, the mortality gradient trend varied by socioeconomic dimension and cause of death. Conclusion/ImplicationsThese data show clear mortality inequalities by socioeconomic position across the different time periods. These linked datasets can help advance knowledge in understanding health inequalities in Canada as well as provide a tool for on-going surveillance of health inequalities by different socioeconomic dimensions.

BASED CURIOSITY AND ORBITAL MARS EXPRESS OBSERVATIONS. G. M. Martinez, M. Giuranna, T. McConnochie, L. K. Tamppari, M. D. Smith, A. Vicente-Retortillo, N. O. Renno, J. L. Kloos, J. E. Moores and S. D. Guzewich, University of Michigan, Ann Arbor, Michigan, USA, Institute for Space Astrophysics and Planetology (IAPS), National Institute of Astrophysics (INAF), Roma, Italy, University of Maryland, College Park, MD, USA, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, NASA Goddard Space Flight Center, Greenbelt, MD, USA, Centre for Research in Earth and Space Sciences, York University, Toronto, Ontario, Canada.

Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO) has started the science measurements on 21 April, 2018. We present the preliminary results on the retrievals of water vapor in the Martian atmosphere from the first data measured by TGO/NOMAD. 1. The NOMAD instrument NOMAD is a spectrometer operating in the spectral ranges between 0.2 and 4.3 μm onboard ExoMars TGO [1]. NOMAD has 3 spectral channels: a solar occultation channel (SO – Solar Occultation; 2.3-4.3 μm), a second infrared channel capable of nadir, solar occultation, and limb sounding (LNO – Limb Nadir and solar Occultation; 2.3-3.8 μm), and an ultraviolet/visible channel (UVIS – UV visible, 200650 nm). The infrared channels (SO and LNO) have high spectral resolution (λ/dλ~ 20,000) provided by echelle grating in combination with an AcoustoOptic Tunable Filter (AOTF) which selects diffraction orders [2]. The concept of the infrared channels are derived from the Solar Occultation in the IR (SOIR) instrument [3] onboard Venus Express. The sampling rate for the solar occultation measurement is 1 km, which provides unprecedented vertical resolution spanning altitudes from the surface to 200 km. Nadir sounding by the LNO channel will acquire spectra with an instantaneous footprint of 0.5 x 17 km, which allows us to obtain maps of trace gases and aerosols in the Martian atmosphere. One of the most remarkable capabilities of NOMAD is its high spectral resolution in the near infrared range. It allows us (1) to investigate vertical profiles of the atmospheric constituents (such as carbon dioxide, carbon monoxide, water vapor, and their isotopic ratio) and (2) to perform sensitive search of organic species (such as CH4, C2H4, C2H6, H2CO) and other trace gases (such as HCl, HCN, HO2, H2S, N2O, OCS) by solar occultation measurements with the SO channel, and (3) to obtain maps of the atmospheric constituents (such as carbon dioxide, carbon monoxide, water vapor, and their isotopic ratio) across the planet by nadir viewing with the LNO channel. 2. Retrieval of Water Vapor Measurements of water and its heavier isotopologue (HDO) are a key diagnostic to the escape processes acting on water on Mars. These first vertical profiles provide an unprecedented view on how water is transported into the upper atmosphere, where it is further dissociated and lost into space. Deuterium fractionation also reveals information about the cycle of water on the planet and informs us of its stability on shortand long-term scales. We plan to analyze the data measured at diffraction order 167, 168, 169, 170, 171 for the H2O retrieval, and at diffraction order 119, 120, 121, 124 for HDO (see Table 1 for the corresponding wavenumbers). The NOMAD spectra at these diffraction orders will be compared with the one calculated by radiative transfer models in order to retrieve their abundances. In the presentation, the preliminary results of the retrievals will be discussed. EPSC Abstracts Vol. 12, EPSC2018-773, 2018 European Planetary Science Congress 2018 c © Author(s) 2018 EPSC European Planetary Science Congress Table1: Wavenumber range of the diffraction orders for the water vapor analysis by the NOMAD SO and

The radiation environment at the Martian surface is, apart from occasional solar energetic particle events, dominated by galactic cosmic radiation, secondary particles produced in their interaction with the Martian atmosphere and albedo particles from the Martian regolith. The highly energetic primary cosmic radiation consists mainly of fully ionized nuclei creating a complex radiation field at the Martian surface. This complex field, its formation and its potential health risk posed to astronauts on future manned missions to Mars can only be fully understood using a combination of measurements and model calculations. In this work the outcome of a workshop held in June 2016 in Boulder, CO, USA is presented: experimental results from the Radiation Assessment Detector of the Mars Science Laboratory are compared to model results from GEANT4, HETC-HEDS, HZETRN, MCNP6, and PHITS. Charged and neutral particle spectra and dose rates measured between 15 November 2015 and 15 January 2016 and model results calculated for this time period are investigated.