MEDA
Mars Environmental Dynamics Analyzer
for NASA/JPL’s Mars 2020 mission
MEDA Instrument in
NASA’s rover Mars2020
Jose A Rodriguez-Manfredi
Arrábida, July 1st
Centro de Astrobiologia
2015/07/01
Importance of characterizing the
Martian environment
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”;
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Importance of characterizing the
Martian environment
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 samplecaching 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.”
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Importance of characterizing the
Martian environment
ESA Cosmic Vision. Space Science for Europe 2015-2025
“ 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.”
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International strategy
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Met packages over the Martian surface
Viking (1975).
Meteorology Sensor
Assembly
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Met packages over the Martian surface
Pathfinder (1996).
ASI/MET (Atmospheric
Structure Instrument and
Meteorology)
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Met packages over the Martian surface
Beagle 2 (2003). Environmental Sensor Suite
Met packages over the Martian surface
Phoenix (2008). MET
Package
Sensor Temperatura del Aire
Sensor Presión
Sensor Viento
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Family portrait
Wheel base: 2.8 m
Height (deck / mast): 1.1 m / 2.2 m
Ground clearance: 0.66 m
Source: JPL/NASA
Source: JPL/NASA, CAB: D.Cabezas
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Curiosity’s science objectives
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.
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 geology of the site
at all spatial scales, by investigating
the chemical, isotopic and
mineralogical composition of
materials, and interpreting the
geological processes.
Habitability
Characterize the broad
spectrum of surface radiation,
including galactic cosmic radiation,
solar proton events and secondary
neutrons.
REMS Instrument
Boom 1 (Wind sensor, Air Temp.
sensor, Ground Temp. sensor)
REMS is a suite of sensors:
Boom 2 (Wind sensor, Air
Temp. sensor, Relative
Humidity sensor)
• 2x 3-D Wind sensors
• 2x Air temperature sensors
• IR ground temperature sensor
• Pressure sensor
UV Radiation sensor
• Relative humidity sensor
• Downward UV radiation
detector (200 to 400 nm)
Instrument
Control
Unit
1-Hz sampling observations
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REMS’ science
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Microscale dynamics and Boundary Layer.
Characterization of the near-surface meteorological environment and MBL processes of free or
forced convection.
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Mesoscale dynamics.
Flows forced by interaction of solar heating and large-scale winds with topography.
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Synoptic meteorology and influence of dust.
Atmospheric circulation regimes, cyclones, thermal tides, ...
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Quantification of local UV radiation environment
Assess its role in chemical and biological processes.
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Global cycles
Water and dust cycle.
Video tomado por el rover Spirit (Source: NASA/JPL-Caltech)
Atmosphere-regolith exchange.
Imagen de Hubble Space Telescope (Source: Cornell
Univ, Univ. Colorado, NASA)
Niebla en Valles Marineris. (Source: ESA/HRSC)
Imagen de MGS (Source NASA)
REMS’ science: results from Gale
NH Winter solstice
SH Summer Solstice
NH Autumn Equinox
SH Spring Equinox
168
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NH Spring Equinox
SH Autumn Equinox
NH Summer Solstice
SH Winter Equinox
198
500
545
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Extrapolation curves
Perihelion
Aphelion
Yellowknife Bay
Jack M
Rocknest
Landing site
John Klein
NH Autumn Equinox
SH Spring Equinox
Behind
Sun
Cumberland
Shaler
NH Winter solstice
SH Summer Solstice
168
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Drive to Mt. Sharp
Waypoint 1
WP 2
Dingo Gap
NH Spring Equinox
SH Autumn Equinox
NH Summer Solstice
SH Winter Equinox
198
500
545
352
Jack M
Landing site
Rocknest
Yellowknife Bay
John Klein
Perihelion
Behind Cumberland
Shaler
Sun
Drive to Mt. Sharp
WP 2
Waypoint 1
Dingo Gap
Aphelion
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REMS’ science: results from Gale
SUNRISE
SUNSET
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REMS team
• Gómez-Elvira, Javier. Centro de Astrobiología •
(PI)
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• Alcon, Miguel Angel. EADS/CRISA
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• Alves, José. Centro de Astrobiología
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• Angona, Javier. EADS/CRISA
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• Armiens, Carlos. Centro de Astrobiología
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• Bell, Julia. JPL
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• Carlin, Jessica. EADS/CRISA
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• Castañer, Luis. U. Politécnica de Cataluña
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• Castellanos, Alberto. EADS/CRISA
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• Contreras, Jorge. EADS/CRISA
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• Diaz, Antonio. EADS/CRISA
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• Diaz, Fernando. EADS/CRISA
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• Fernandez Agudo, Sergio. EADS/CRISA
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• Galan, Carmen. EADS/CRISA
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• Garcia Manchado, Alvaro. EADS/CRISA
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• Genzer, Maria. FMI
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• Gil de Blas, Juan Ignacio. EADS/CRISA
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• Gomez, Andres. EADS/CRISA
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• Gomez, Felipe. Centro de Astrobiología
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• Goñi, Ana María. EADS/CRISA
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• Goyanes, Javier. EADS/CRISA
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• Guerrero, Antonio. EADS/CRISA
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• Haberle, Robert. NASA Ames
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• Herrero, Maria. EADS/CRISA
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• 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.
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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
Instrument
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).
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PROGRAMA E
R
TWINS’ goals
MEMORIA CIENTÍFICO-TÉCNICA DE PROYEC
B)
• 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
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Mars 2020
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Mars2020’s science
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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Habitability
Sampling
caching
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.
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.
Biosignatures
Prepare for
humans
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.
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Importance of characterizing the
environment for Mars2020
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 Earth
1. 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 …:
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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.
MEDA’s Principal goal
“…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. “
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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
Objective D.2: Characterization of atmospheric dust size,
morphology, and temporal variability
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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.
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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.
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MEDA Investigations
WS2
WS1
TIRS
HS
ATS3
ATS2 at 120deg
ATS1
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.
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Synergy with other investigations and
missions
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.
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Great international consortium
• Rad & Dust
sensor
• Environ.
tests
• CCD
• Deputy-PI
JPL
INTA
Univ.
Padua
CRISA
John
Hopkins
APL
CAB
INTA-CSIC
NASA
Goddard
Texas A&M
Univ.
Spanish contrib.
US contrib.
Finnish contrib.
Ashima
Michigan
Univ.
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PI / PM
System Eng. Support
TIR sensor
AT sensor
WS design concept
Sensor procur.
GSW
Environ. tests
Calibra on tests
Ops
FMI
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System Eng.
MA & QA
FSW
ICU
ASIC dev.
AIV
Model MAIT
Boom dev.
Tests
Ins tute of
PhysicalChemistry
Rocasolano
Univ. Basque
Country
Univ.
Alcala
• Pressure sensor
• Humidity sensor
Italian contrib.
Scientific contrib.
Technological contrib.
Sci/Tech contrib.
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Accommodation challenges
Wind speed = 0 m/s
Besides Main requirements:
• EDL Protection in stowed configuration
• Minimizing thermal and rover geometry
influence
• Maximizing unobstructed FOV of other
instruments and telecomm. Antennas.
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Wind speed = 2 m/s
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.
CFD simulations help assess performance and
impact of accommodation (confirmed by REMS
experience).
Accommodation challenges
1ms
5ms
10ms
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Protection challenge
REMS on MSL
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Suite of sensors
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Evolution in environmental instruments
Magnitudes
p = 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
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