MEDAMars Environmental Dynamics

Analyzer

for NASA/JPL’s Mars 2020 mission

Jose A Rodriguez-ManfrediArrábida, July 1st

Centro de Astrobiologia 2015/07/01

MEDA Instrument in NASA’s rover Mars2020

Importance of characterizing the Martian environment

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From the NASA’s Mars Exploration Program:• Goal I Objective B “Characterize present habitability and search

for evidence of extant life”; • Goal II Objective A: “Characterize Mars’ atmosphere, present

climate, and climate processes under current orbital configuration”;

• Goal IV Objective A: “Obtain knowledge of Mars sufficient to design and implement a human mission with acceptable cost, risk, and performance”;

Importance of characterizing the Martian environment

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From the Findings and Strategic knowledge Gaps of MEPAG document P-SAG 2012:

• Finding #3: “The early robotic precursor program needed to support a human mission to the Martian surface would consist of at least: one orbiter, a surface sample return, a lander/rover in-situ set of measurements (which could be made from a sample-caching rover), and certain technology demonstrations.”

• Finding #5: “Several landed measurements need to be made simultaneously with orbital measurements”

• SKG Group A.2: “The atmospheric models for Mars have not been well validated due to a lack of sufficient observational data, and thus our confidence in them (for use in mission engineering) is significantly limited.”

• SKG Group B.1: “Lower Atmosphere: We do not have sufficient Martian atmospheric observations to confidently model winds, which significantly affect EDL design…”

• SKG Group B.6: “Atmospheric ISRU: We do not understand in sufficient detail the properties of atmospheric constituents near the surface to determine the adverse effects on ISRU atmospheric processing system life and performance within acceptable risk for human missions.”

Importance of characterizing the Martian environment

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“ 1.3 Life and habitability in the Solar System [...] Mars is an ideal goal [...] A major question is: how did continued evolution of the planet affect the habitable environment and what happened to the planet to make its surface uninhabitable today?. [...] The spacecraft will need to investigate [...] measurements of climatic conditions are also required, to trace their evolution and the conditions of habitats back in time. [...] Monitoring of the present environment is also needed to understand the present condition of the habitat and also in preparation of future manned missions.”

ESA Cosmic Vision. Space Science for Europe 2015-2025

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International strategy

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Met packages over the Martian surfaceViking (1975). Meteorology Sensor Assembly

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Met packages over the Martian surface

Pathfinder (1996).ASI/MET (Atmospheric Structure Instrument and Meteorology)

Met packages over the Martian surface

Beagle 2 (2003). Environmental Sensor Suite

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Met packages over the Martian surface

Sensor Temperatura del Aire Sensor Presión Sensor Viento

Phoenix (2008). MET Package

Source: JPL/NASAWheel base: 2.8 m

Height (deck / mast): 1.1 m / 2.2 m

Ground clearance: 0.66 m

Family portrait

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Source: JPL/NASA, CAB: D.Cabezas

Curiosity’s primary scientific goal is to explore and quantitatively assess a local

region on Mars’s surface as a potential habitat for life (present or past).

Determine the nature and inventory of organic carbon compounds, searching for the chemical building blocks of life, and identifying features that may record the actions of biologically relevant processes.

Characterize the geology of the site at all spatial scales, by investigating the chemical, isotopic and mineralogical composition of materials, and interpreting the geological processes.

Investigate planetary processes of relevance to past habitability by assessing the long timescale atmospheric evolution and determine present state, distribution and cycling of water and carbon dioxide.

Characterize the broad spectrum of surface radiation, including galactic cosmic radiation, solar proton events and secondary neutrons.

Habitability

Curiosity’s science objectives

REMS Instrument

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REMS is a suite of sensors:

• 2x 3-D Wind sensors

• 2x Air temperature sensors

• IR ground temperature sensor

• Pressure sensor

• Relative humidity sensor

• Downward UV radiation

detector (200 to 400 nm)

1-Hz sampling observations

Boom 1 (Wind sensor, Air Temp. sensor, Ground Temp. sensor)

Boom 2 (Wind sensor, Air Temp. sensor, Relative Humidity sensor)

UV Radiation sensor

Instrument ControlUnit

- Microscale dynamics and Boundary Layer.Characterization of the near-surface meteorological environment and MBL processes of free

or forced convection.

Video tomado por el rover Spirit (Source: NASA/JPL-Caltech)

- Mesoscale dynamics.Flows forced by interaction of solar heating and large-scale winds with topography.

Niebla en Valles Marineris. (Source: ESA/HRSC)

- Synoptic meteorology and influence of dust.Atmospheric circulation regimes, cyclones, thermal tides, ...

Imagen de Hubble Space Telescope (Source: Cornell Univ, Univ. Colorado, NASA)

- Quantification of local UV radiation environmentAssess its role in chemical and biological processes.

- Global cyclesWater and dust cycle.

Atmosphere-regolith exchange.

Imagen de MGS (Source NASA)

REMS’ science

Landing site

Jack MRocknest

Yellowknife BayJohn Klein

Behind Sun

CumberlandShaler Waypoint 1 WP 2 Dingo Gap

Drive to Mt. Sharp

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NH Autumn EquinoxSH Spring Equinox

168

Perihelion

198

NH Winter solsticeSH Summer Solstice

352

NH Spring EquinoxSH Autumn Equinox

Aphelion

500 545

NH Summer SolsticeSH Winter Equinox

Extrapolation curves

REMS’ science: results from Gale

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54

NH Autumn EquinoxSH Spring Equinox

168

Perihelion

198

NH Winter solsticeSH Summer Solstice

352

NH Spring EquinoxSH Autumn Equinox

Aphelion

500 545

NH Summer SolsticeSH Winter Equinox

Landing siteJack M

RocknestYellowknife Bay

John KleinBehind Sun

CumberlandShaler Waypoint 1 WP 2 Dingo Gap

Drive to Mt. Sharp

SUNRISE SUNSET

REMS’ science: results from Gale

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Backuphttp://cab.inta-csic.es/rems/marsweather.html

• Gómez-Elvira, Javier. Centro de Astrobiología (PI)

• Alcon, Miguel Angel. EADS/CRISA• Alves, José. Centro de Astrobiología• Angona, Javier. EADS/CRISA• Armiens, Carlos. Centro de Astrobiología• Bell, Julia. JPL• Carlin, Jessica. EADS/CRISA• Castañer, Luis. U. Politécnica de Cataluña• Castellanos, Alberto. EADS/CRISA• Contreras, Jorge. EADS/CRISA• Diaz, Antonio. EADS/CRISA• Diaz, Fernando. EADS/CRISA• Fernandez Agudo, Sergio. EADS/CRISA• Galan, Carmen. EADS/CRISA• Garcia Manchado, Alvaro. EADS/CRISA• Genzer, Maria. FMI• Gil de Blas, Juan Ignacio. EADS/CRISA• Gomez, Andres. EADS/CRISA• Gomez, Felipe. Centro de Astrobiología• Goñi, Ana María. EADS/CRISA• Goyanes, Javier. EADS/CRISA• Guerrero, Antonio. EADS/CRISA• Haberle, Robert. NASA Ames• Herrero, Maria. EADS/CRISA• Harri, Ari-Matti. FMI• Harris, Ian. JPL

• Kok, Jasper. Univ. Michigan • Heninger, Rebeca. JPL• Jimenez, Vicente. U. Politécnica de Cataluña• Kowalski, Lukas. U. Politécnica de Cataluña• Lepinette, Alain. Centro de Astrobiología• Martínez-Frías, Jesús. Centro de Astrobiología• Martín-Soler, Javier. Centro de Astrobiología• Martín-Torres, Javier. Centro de Astrobiología• McEwan, Ian. Hashima• Mehta, Manish. Univ. Michigan• Mico, Cristobal. EADS/CRISA• Mora, Luis. Centro de Astrobiología• Moreno, José. EADS/CRISA• Muñoz, Guillermo. Centro de Astrobiología• Navarro, Sara. Centro de Astrobiología• Pablo, Miguel A. Univ. Alcalá de Henares• Paniagua, Moises. EADS/CRISA• Pavri, Betina. JPL• Peinado, Verónica. Centro de Astrobiología• Peña, Antonio. EADS/CRISA• Perez Casas, Francisco. EADS/CRISA• Perez Gracia, Fernando. EADS/CRISA• Perez-Mercader, Juan. Centro de Astrobiología• Plaza, Jose Manuel. EADS/CRISA• Polkko, Jouni. Finnish Meteorological Inst.

• Pumar, Manuel. U. Politécnica de Cataluña• Ramos, Miguel. Univ. Alcalá de Henares• Redondo, M. Carmen. EADS/CRISA• Renno, Nilton. Univ. Michigan• Ricard, Jordi. U. Politénica de Cataluña• Richardson, Mark. Ashima• Romeral, Julio. Centro de Astrobiología• Rodriguez-Manfredi, J.A. Centro de Astrobiología• Rubio, Pedro. EADS/CRISA• Scodary, Anthony. JPL• Sebastian, Eduardo. Centro de Astrobiología• Serrano, Jaime. EADS/CRISA• Simmonds, Jeff. JPL• Serviss, Orin. JPL• Thompson , Art. JPL• Torrero, Francisco. EADS/CRISA• Torres, Josefina. Centro de Astrobiología• Urqui, Roser. Centro de Astrobiología• Vazquez, Luis. Universidad Complutense• Velasco, Tirso. EADS/CRISA• Vasavada, Ashwin. JPL• Zorzano, Paz M. Centro de Astrobiología

REMS team

Instrument

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TWINS comprises:

• 2x 3-D Wind sensors

• 2x Air temperature sensors

1 Hz sampling observations over the entire mission.

InSight: Interior Exploration using Seismic Investigations, Geodesy and Heat Transport

InSight will delve deep beneath the surface of Mars, detecting the fingerprints of the processes of terrestrial planet formation, as well as measuring the planet's "vital signs": Its "pulse" (seismology), "temperature" (heat flow probe), and "reflexes" (precision tracking).

TWINS’ goals

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• During the commissioning phase (first 40-60 sols), TWINS shall characterize the environment (thermal and wind patterns) to find the best conditions and time to deploy the instruments onboard the lander (robotic arm with a hung magnetic grip).

• After deployment, TWINS shall record the winds and will let SEIS discard false-positive seismologic events (over the mission).

• Enable correlation with data from Gale (REMS): validate environmental models at different scales, and enable an enhanced understanding of Martian atmospheric processes:

• Atmospheric diurnal tides• Seasonal variations• Meso-scale circulation• Katabatic / anabatic winds• Dust devils

Mars 2020

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Characterize the processes that formed and modified the geologic record within a field exploration area on

Mars selected for evidence of an astrobiologically relevant ancient environment and geologic diversity

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HabitabilityBiosignatures

Prepare for humansSampling

caching

Perform the following astrobiologically-relevant investigations on the geologic materials at the landing site:- Determine the habitability of an ancient environment- For ancient environments interpreted to have been habitable,

search for materials with high biosignature preservation potential.

- Search for potential evidence of past life using the observations regarding habitability and preservation as a guide.

Assemble a returnable cache of samples for possible future return to Earth.- Obtain samples that are scientifically selected, for

which the field context is documented, that contain the most promising samples identified in Objective B and that represent the geologic diversity of the field site.

- Ensure compliance with future needs in the areas of planetary protection and engineering so that the cache could be returned in the future if NASA chooses to do so.

Contribute to the preparation for human exploration of Mars by making significant progress towards filling at least one major Strategic Knowledge Gap. The highest priority SKG measurements that are synergistic with Mars 2020 science objectives and compatible with the mission concept are (in priority order):- Demonstration of In-Situ Resource Utilization (ISRU)

technologies to enable propellant and consumable oxygen production from the Martian atmosphere for future exploration missions.

- Characterization of atmospheric dust size and morphology to understands its effects on the operation of surface systems and human health.

- Surface weather measurements to validate global atmospheric models.

Mars2020’s science

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From the Announcement of Opportunity (AO):A. Characterize the processes that formed and modified the geologic record within a

field exploration area on Mars selected for evidence of an astrobiologically-relevant ancient environment and geologic diversity.

B. Perform the following astrobiologically-relevant investigations on the geologic materials…

1. Determine the habitability of an ancient environment. 2. For ancient environments interpreted to have been habitable, search for materials with high biosignature preservation potential. 3. Search for potential evidence of past life using the observations regarding habitability and preservation as a guide.

C. Assemble a returnable cache of samples for possible future return to Earth1. Obtain samples that are scientifically selected, for which the field context is documented… 2. …

D. Contribute to the preparation for human exploration of Mars by making significant progress towards filling at least one major Strategic Knowledge Gap. The highest priority SKG measurements that are …:

1. Demonstration of In-Situ Resource Utilization (ISRU) technologies to enable propellant and consumable oxygen production from the Martian atmosphere for future exploration missions.2. Characterization of atmospheric dust size and morphology to understands its effects on the operation of surface systems and human health.3. Surface weather measurements to validate global atmospheric models.

Importance of characterizing the environment for Mars2020

MEDA’s Principal goal

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“…MEDA will characterize the diurnal to seasonal cycles in

(a) local environmental dust properties (total column, size distribution, phase function which can be used to estimate some shape properties) as well as its temporal response to the meteorology, and;

(b) the local near-surface environmental pressure, air and surface temperatures, relative humidity, wind, and UV-visible-IR solar radiation. “

How?- with a light weight and low power modular suite of sensors- high heritage (REMS@MSL, TWINS@InSight,

PanCam/Hazcam@MSL) in technology and experienced sci & eng team

- around the clock- to measure autonomously and continuously- at an adjustable sampling rate

MEDA Investigations k

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Objective D.2: Characterization of atmospheric dust size, morphology, and temporal variability

• The diurnal dust opacity cycle, its relationship to local environmental conditions and its variability with season will be measured with a set of 8 sky-viewing photodiodes with 7 narrow spectral band, ranging from UV to near IR, and one panchromatic (white) filter pointed at the sky plus one dedicated CCD.

• The dust size distribution will be measured with the dedicated CCD element to measure the intensity decay of the solar aureole. The observed sky brightness comes from sunlight scattered by aerosols into the line-of-sight of each pixel, and thus depends primarily on a few basic quantities: aerosol optical depth, vertical distribution, and angular scattering properties.

• Information about dust shape will be inferred from the phase function measured with an additional set of 8 photodiodes pointing at a low angle of 15º above the horizon. The multiangular scattering of solar light depends on several atmospheric aerosol properties, including particle size, orientation and shape.

MEDA Investigations

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WS2

WS1

TIRS

ATS1

ATS3ATS2 at 120deg

HS

RDS

Objective D.3: Surface weather measurements to validate global atmospheric models• The environmental pressure and relative humidity will be

measured with the same pressure and relative humidity sensors as on MSL. Near-surface air temperature will be measured with thermocouples like those flown on Mars Pathfinder. Winds will be measured using identical constant delta-T hot plate anemometry as on MSL.

• The diurnal cycle of shortwave and near IR solar radiation at the surface will be measured with the same set of photodiodes used for dust opacity measurements. The CCD camera will also enable the occurrence and morphology of water ice and dust clouds to be monitored.

• Local thermal IR forcing from the atmosphere and surface will be measured with two sets of thermopiles oriented upward and to the surface, respectively, to complete the characterization of atmospheric forcing.

• Microscale and mesoscale dynamics will be characterized by measuring local winds, pressure, temperature, relative humidity, and surface temperature cycles, capturing the response to the measured solar forcing and the interplay between atmospheric components.

Synergy with other investigations and missions

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Synergy with investigations targeting other Mars 2020 objectives• MEDA wind measurements connect current conditions to the aeolian record as

preserved by the characteristics of depositional bedforms and erosional features. • MEDA measurements help constrain models of how the environmental context

affects weathering and preservation potential of a possible cache sample.• MEDA measurements help define the conditions required to transport or store a

cache sample with minimal alteration of its habitability potential.• MEDA’s continuous coverage helps determine how the environment influences the

ISRU’s operation and its efficiency cycles.

Enhancement of data returned by other Mars missions• MEDA measurements will augment the temporal and geographical record of

environmental observations on the surface of Mars.• MEDA measurements will aid in the extrapolation of satellite observations to the

surface.• MEDA’s dominant REMS-heritage will allow direct comparison with how the

environment differs from that measured by MSL in Gale Crater.

Great international consortium

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Accommodation challenges

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Besides Main requirements:• EDL Protection in stowed configuration• Minimizing thermal and rover geometry

influence• Maximizing unobstructed FOV of other

instruments and telecomm. Antennas.

Winds deflect the rover thermal plume and may throw it over the sensors. Finding an optimal accommodation is mandatory to minimize the rover thermal and geometrical influence on an environmental instrument.

Wind speed = 0 m/sWind speed = 2 m/s

CFD simulations help assess performance and impact of accommodation (confirmed by REMS experience).

Accommodation challenges

5ms

10ms

1ms

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Protection challenge

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REMS on MSL

Suite of sensors

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Evolution in environmental instruments

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Magnitudesp = pressure, Ta = air temperature, w = wind, u = speed, q = azimuth, u* = friction speed, z0 = roughness height, Tg = ground temperature, RH = relative humidity, H = UV-VIS-IR irradiance flux, TIR = downward thermal flux, d = dust properties