P2971: PERFORMANCE OF THE MEDA ENVIRONMENTAL AND ...
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MEDA’s Expected measurements on Mars (comparison with its predecessor, REMS): MEDA’s Performance a?er integraAon tests: Science Goals Science Objectives Scientific Measurement Requirements Instrument Performance Observables Physical Parameters Characterize dynamics of the local environment Local Thermal environment Global dust and CO2 cycles Local wind transport and wind-driven erosion Local Surface temperature and fluxes with the low atmosphere Thermistors resistance (thermocouple) Air Temperature T range 150-300 K T accuracy ±1K T resolution ±0.1K Piezoelectric Capacitor (pressure sensor) Atmospheric Pressure p range 1-1200 Pa p accuracy ±10 Pa p resolution ± 0.5 Pa Heat fluxes to maintain constant ΔT between reference temperature and 4 dice ( hot plate anemometers ) Wind velocity and Wind direction u,v range 0-70 m/s w range 0-10 m/s u,v,w accuracy 1 m/s u.v,w resolution 0.5 m/s Directional accuracy ±15 deg Thermal radiation in bands 8-14 µm, 14.5-15.5 µm and 15.9 –19 µm ( ground looking thermal IR sensors ) Regolith surface temperature and emissivity. T range 173-293 K T accuracy ±5K T resolution ±1K Local hydrological cycle Local Water cycle Capacitance ( relative humidity sensor ) Relative humidity RH in temp. range 190-270 K RH accuracy 10% RH resolution 0.5% Local solar radiative cycle Astrobiology and dust cycle UV-VIS-NIR irradiance fluxes ( whole sky FOV photodiodes with filters ) UV flux O3, H2O, and dust columns Accuracy Spectral resol. 8% of full range (up to sol 200) Angular dependence of diffuse VIS solar light ( sideways cone radiation sensor ) Dust phase function, optical depth and size distribution Field of view Angular resolution 10 degrees 2 degrees Angular dependence of direct and forward scattered light near Sun (CCD ) Optical depth and size distribution Field of view Angular resolution 60 degrees 2 degrees Thermal radiation 8-14 µm, 14.5-15.5 µm and 15.9—19 µm (upward TIR sensors ) Air temperature at 0.6Pa and CO2 column T range 173-293 K T accuracy ± 5K T resolution ±1K P2971: PERFORMANCE OF THE MEDA ENVIRONMENTAL AND METEOROLOGICAL PACKAGE FOR MARS 2020 AFTER INTEGRATION. 2020 51 st LPSC, The Woodlands Copyright 2020. All rights reserved. Abstract ID: 2971 MEDA’s principal goal: MEDA will characterize the diurnal to seasonal cycles in (a) local environmental dust proper0es ( total column, size distribu0on, phase func0on which can be used to es9mate some shape proper9es) as well as its temporal response to the meteorology, and; (b) the local near-surface environmental pressure, air and surface temperatures , rela0ve humidity , wind , and UV-visible-IR solar radia0on. MEDA will measure autonomously and continuously at an adjustable sampling rate. MEDA’s Measurement Objectives: a.To determine the physical and optical properties of the local atmospheric aerosols. Particle abundance, size distribution, shape, phase function, and how these optical properties relate to the meteorological cycles (diurnal, seasonal, interannual) b.To determine the conditions leading to dust lifting and how the aerosol diurnal cycle responds to the local diurnal wind regime c.To determine how the current environmental pressure, temperature, relative humidity, solar radiation, net infrared radiation and winds at the landing site differ from those at the Viking, Pathfinder, Phoenix, Curiosity and InSight locations d.To probe the relationship between the surface environment and the large-scale dynamics observed from orbiting instruments e.To investigate the energy and water flux exchange between the surface and the lower atmosphere near the rover f.To measure the annual cycles of UV, visible, and near-IR radiation at the surface of Mars g.To obtain the environmental context for weathering and preservation potential of cached samples h.To investigate how pressure, temperature, humidity, winds, dust amount and size distribution influence the ISRU engineering efficiency i. To form linkages between the MEDA observations and models extrapolated to the Martian surface M. de la Torre Juárez 1 , J.A. Rodríguez-Manfredi 2,3 , V. Apéstigue 3 , I. Arruego 3 , D.J. Banfield 4 , J.S. Boland 1 , P.G. Conrad 5 , A. G. Fairén 1 , R. Ferrándiz 2,3 , E. Fischer 6 , M. Genzer 7 , J. Gómez-Elvira 3 , F. Gómez 2,3 , S.D. Guzewich 8 , A.-M. Harri 7 , M. Hieta 7 , R. Hueso 9 , J.J. Jiménez 3 , M.T. Lemmon 10 , A. Lepinette 2,3 , J. Martín-Soler 2,3 , G.M. Martínez 6,11 , A. Molina2 ,3 , L. Mora 2,3 , J.F. Moreno 12 , S. Navarro 2,3 , C. Newman 13 , C. Ortega 12 , V. Peinado 2,3 , J. Pla-García 2,3 , O. Prieto-Ballesteros 2,3 , S. Rafkin 17 , M. Ramos 14 , T. del Río 9 , J. Romeral 2,3 , K. Runyon1 5, A. Saiz-López 16 , A. Sánchez-Lavega 9 , J.T. Schofield 1 , E. Sebastián 2,3 , M.D. Smith 8 , R.J. Sullivan 4 , L. K. Tamppari 1 , D. Toledo 3 , J. Torres 2,3 , R. Urqui 2,3 , Á. Vicente-Retortillo 2,3,6 , D. Viúdez-Moreiras 2,3 and the MEDA 1,2,7 & M2020 1 teams 1 NASA Jet Propulsion Laboratory/California Institute of Technology, 2 Centro de Astrobiología, 3 Instituto Nacional de Técnica Aeroespacial, 4 Cornell University, 5 Carnegie Institution for Science, 6 University of Michigan, 7 Finnish Meteorological Institute, 8 NASA Goddard Space Flight Center, 9 University of the Basque Country, 10 Space Science Institute, 11 Lunar and Planetary Institute/USRA, 12 Airbus Defence and Space – CRISA, 13 Aeolis Research, 14 Universidad de Alcalá, 15 Johns Hopkins APL, 16 Institute Physical-Chemistry Rocasolano-CSIC, 17 Southwest Research Institute – Boulder.. 10 20 30 40 50 60 70 80 90 100 110 RH max (%) 180 270 360 450 540 630 720 Aerocentric Longitude L s (Until L s 767) 15 30 45 60 75 90 105 120 135 150 165 VMR max (ppmv) VMR(RH max ) (ppmv) 0 1 2 3 4 5 6 7 LTST (hr) Maximum humidity from 0 to 7 am and its time Fig. Curiosity REMS Relative Humidity nighttime measurements (black) for about 1.5 Mars years at Gale crater. The max. nighttime volume mixing ratio (VMR) is shown (green) and the VMR at max. relative humidity (red). Similar measurements will be made at the 2020 landing site by MEDA. 150 200 250 Min, mean and max REMS Min(ATS) (K) 180 360 540 720 Aerocentric Longitude L s Viking L1 40 sols Viking L2 1050 sols REMS 1104 sols Fig. Curiosity REMS atmospheric temperatures (mean, black curve) at Gale crater, compared to Viking Landers 1 (green) and 2 (blue). REMS min. and max. daily values are shown in red. MEDA has analogous temperature sensors (actually, 5 sensors) with significant improvements. Combined with 1 TIR sensor, MEDA has the ability to measure at 3 different heights. Their data can be used to inter-compare with temperatures measured by REMS on Curiosity and TWINS on InSight at the same time. It also adds data to the historical records form the Viking, Phoenix, and Pathfinder missions. 700 750 800 850 900 950 Sol average p (Pa) p 0 =847 Pa 100 200 300 400 500 600 700 800 900 1000 Sol (up to sol 1049) p 1 =−54 Pa p 2 =58 Pa −10 −5 0 5 10 p fit − p −4525 −4500 −4475 −4450 −4425 −4400 Rover altitude (m) L s until 735.3 Scale Height H=11069 m <T>=213.5 K z 0 =−4678 m 180 270 0 90 180 270 0 Fig. Curiosity REMS atmospheric pressures at Gale crater, showing seasonal pressure trends. The sol averaged pressures are shown in red. Curiosity changes altitude as it progresses toward Mt. Sharp. After accounting for the altitude and seasonal cycles, fluctuations reveal weather and global circulation (green). 160 180 200 220 240 260 280 300 0 100 200 300 400 500 600 700 800 151 208 272 333 25 70 116 167 227 Ground Temperature at Gale (K) Sol number L s Spring Summer Fall Winter Fig. Curiosity’s REMS surface temperatures as measured by the GTS. Min. and max. diurnal temperatures are shown throughout a Mars year. MEDA has an analogous sensor (TIRS), with significant improvements, which will help understand the environment from which samples are acquired. 200 300 400 500 600 700 800 900 0 5 10 15 20 25 30 35 LMST Speed (m/s) Mean speed and mean + std by sol Fig. Curiosity’s REMS wind measurements at Gale crater. Mean wind speed (red) and mean + standard deviation (blue) are shown. The MEDA instrument has two wind sensor units in different orientations (as in REMS), but with significant improvements in all aspects w.r.t. REMS and InSight (performance, electronics, redundancy, …). Fig. Phase functions will be calculated from the RDS sensors as was done for Spirit (MY 26, L s = 354º). Unlike its predecessor REMS, the MEDA instrument incorporates a dedicated CCD aimed at measuring the Solar aureole caused by light scattering from atmospheric aerosols. This CCD, specifically dedicated to sky observations, will also provide sequences of sky images that will be used for the study of clouds (morphologies and discriminating between ice or dust clouds), as well as to constrain the amount and size of the atmospheric aerosols (through the estimate of the phase functions). 120º Network of environmental stations : If REMS, on Curiosity, and TWINS, on InSight, remain functional until the landing of M2020, MEDA’s comparable set of atmospheric sensors will provide a network of atmospheric stations that characterizes the influence of changes in the global circulation on the surface environment at different locations on the surface of Mars.. Interna9onal Consor9um with 20 partners CAB INTA- CSIC Univ. Alcalá IMSE- CNM AVS Univ. Basque Country Inst. Physical Chemistry Rocasolano CSIC CRISA- AIRBUS INTA U of Michigan FMI LPI Aeolis SSI U Cornell Carnegie APL NASA- Goddard JPL/Caltech U di Padua • CCD • Deputy PI • Rad & Dust sensor • Environ testing • Pressure sensor • Humidity Sensor • ASIC design Univ. Politecnic Catalonia • Systems Eng. • MA&QA • FSW • ICU • ASIC Spec. • AIV • Model MAIT • Elec Wind sensor (WS) • Testing • WS mechanical design • Wind sensor design Spanish contribution Finnish contribution US contribution Italian contribution Technolog. contribution Science contribution • PI • Systems Eng. support • TIR Sensor • AT Sensor • WS design concept • Procurement • Environ tests • Ground SW • Calibration Testing • Ops Credit: CAB / C. Lara
Transcript of P2971: PERFORMANCE OF THE MEDA ENVIRONMENTAL AND ...
2971.PDFMEDA’s Expected measurements on Mars (comparison with its
predecessor, REMS):
MEDA’s Performance a?er integraAon tests:
Science Goals Science
ΔT between reference
plate anemometers)
Wind velocity
µm, 14.5-15.5 µm and 15.9 –19
µm (ground looking thermal IR
sensors)
RH accuracy 10%
RH resolution 0.5%
Local solar radiative
radiation sensor)
Sun (CCD)
(upward TIR sensors)
Air temperature at
0.6Pa and CO2
FOR MARS 2020 AFTER INTEGRATION.
2020 51st LPSC, The Woodlands
Copyright 2020. All rights reserved.
Abstract ID: 2971
in
size distribu0on, phase func0on which can be used to
es9mate some shape proper9es) as well as its
temporal response to the meteorology, and;
(b) the local near-surface environmental pressure, air
and surface temperatures, rela0ve humidity, wind,
and UV-visible-IR solar radia0on.
at an adjustable sampling rate.
MEDA’s Measurement Objectives: a.To determine the physical and optical properties of the local atmospheric aerosols. Particle abundance, size distribution,
shape, phase function, and how these optical properties relate to the meteorological cycles (diurnal, seasonal, interannual)
b.To determine the conditions leading to dust lifting and how the aerosol diurnal cycle responds to the local diurnal wind
regime
c.To determine how the current environmental pressure, temperature, relative humidity, solar radiation, net infrared
radiation and winds at the landing site differ from those at the Viking, Pathfinder, Phoenix, Curiosity and InSight locations
d.To probe the relationship between the surface environment and the large-scale dynamics observed from orbiting
instruments
e.To investigate the energy and water flux exchange between the surface and the lower atmosphere near the rover
f. To measure the annual cycles of UV, visible, and near-IR radiation at the surface of Mars
g.To obtain the environmental context for weathering and preservation potential of cached samples
h.To investigate how pressure, temperature, humidity, winds, dust amount and size distribution influence the ISRU
engineering efficiency
i. To form linkages between the MEDA observations and models extrapolated to the Martian surface
M. de la Torre Juárez1, J.A. Rodríguez-Manfredi2,3, V. Apéstigue3, I. Arruego3, D.J. Banfield4, J.S. Boland1, P.G. Conrad5, A. G. Fairén1, R. Ferrándiz2,3, E. Fischer6, M. Genzer7, J. Gómez-Elvira3, F. Gómez2,3, S.D. Guzewich8, A.-M. Harri7, M. Hieta7, R. Hueso9, J.J. Jiménez3, M.T. Lemmon10, A. Lepinette2,3, J. Martín-Soler2,3, G.M. Martínez6,11, A. Molina2,3, L. Mora2,3, J.F. Moreno12, S. Navarro2,3, C. Newman13, C. Ortega12, V. Peinado2,3, J. Pla-García2,3, O. Prieto-Ballesteros2,3, S. Rafkin17, M. Ramos14, T. del Río9, J. Romeral2,3,
K. Runyon15, A. Saiz-López16, A. Sánchez-Lavega9, J.T. Schofield1, E. Sebastián2,3, M.D. Smith8, R.J. Sullivan4, L. K. Tamppari1, D. Toledo3, J. Torres2,3, R. Urqui2,3, Á. Vicente-Retortillo2,3,6, D. Viúdez-Moreiras2,3 and the MEDA1,2,7 & M20201 teams 1NASA Jet Propulsion Laboratory/California Institute of Technology, 2Centro de Astrobiología, 3Instituto Nacional de Técnica Aeroespacial, 4Cornell University, 5Carnegie Institution for Science, 6University of Michigan, 7Finnish Meteorological Institute, 8NASA Goddard Space Flight Center, 9University of the Basque Country, 10Space Science Institute,
11Lunar and Planetary Institute/USRA, 12Airbus Defence and Space – CRISA, 13Aeolis Research, 14Universidad de Alcalá, 15Johns Hopkins APL, 16Institute Physical-Chemistry Rocasolano-CSIC, 17Southwest Research Institute – Boulder..
10
20
30
40
50
60
70
80
90
100
110
Aerocentric Longitude Ls (Until Ls 767)
15
30
45
60
75
90
105
120
135
150
165
L T
S T
( h r)
Maximum humidity from 0 to 7 am and its time
Fig. Curiosity
volume mixing ratio (VMR) is shown
(green) and the
(red). Similar measurements will
be made at the
150
200
250
Aerocentric Longitude Ls
Viking L1 40 sols Viking L2 1050 sols REMS 1104 sols
Fig. Curiosity REMS atmospheric temperatures (mean, black curve) at Gale crater, compared to Viking Landers 1 (green) and 2 (blue). REMS min. and max. daily values are shown in red. MEDA has analogous temperature
sensors (actually, 5 sensors) with significant improvements. Combined with 1 TIR sensor, MEDA has the ability to measure at 3 different heights. Their
data can be used to inter-compare with temperatures measured by REMS on Curiosity and TWINS on InSight at the same time. It also adds data to the historical records form the Viking, Phoenix, and Pathfinder missions.
700
750
800
850
900
950
g e p
100 200 300 400 500 600 700 800 900 1000
Sol (up to sol 1049)
p1=−54 Pa p2=58 Pa −10
−5
0
5
10
e (
m )
<T>=213.5 K
z0=−4678 m
crater, showing seasonal pressure
shown in red. Curiosity changes
altitude as it progresses toward Mt. Sharp. After
accounting for the altitude and
seasonal cycles, fluctuations reveal weather and global
circulation (green).
G ro
measured by the GTS. Min. and
max. diurnal temperatures are shown throughout a
Mars year. MEDA has an analogous
sensor (TIRS), with significant improvements,
which will help understand the
environment from which samples are acquired.
200 300 400 500 600 700 800 900 0
5
10
15
20
25
30
35
LMST
m /s
Mean speed and mean + std by sol
Fig. Curiosity’s REMS wind measurements at Gale crater. Mean wind speed
(red) and mean + standard deviation (blue) are shown.
The MEDA instrument has two wind sensor units in different orientations (as in
REMS), but with significant improvements in all aspects
w.r.t. REMS and InSight (performance, electronics, redundancy, …).
Fig. Phase functions will be calculated from the RDS sensors as
was done for Spirit (MY 26, Ls =
354º). Unlike its predecessor REMS, the
MEDA instrument incorporates a dedicated CCD aimed at measuring
the Solar aureole caused by light
scattering from atmospheric aerosols.
This CCD, specifically dedicated to sky observations, will also provide
sequences of sky images that will be
used for the study of clouds (morphologies and discriminating
between ice or dust clouds), as well as to constrain the amount and size
of the atmospheric aerosols (through
the estimate of the phase functions).
120º
Network of environmental stations: If REMS, on Curiosity, and TWINS, on InSight, remain functional until the landing of M2020, MEDA’s comparable set of atmospheric sensors will provide a network of atmospheric stations that characterizes the influence of
changes in the global circulation on the surface environment at different locations on the surface of Mars..
Interna9onal
Consor9um
MEDA’s Performance a?er integraAon tests:
Science Goals Science
ΔT between reference
plate anemometers)
Wind velocity
µm, 14.5-15.5 µm and 15.9 –19
µm (ground looking thermal IR
sensors)
RH accuracy 10%
RH resolution 0.5%
Local solar radiative
radiation sensor)
Sun (CCD)
(upward TIR sensors)
Air temperature at
0.6Pa and CO2
FOR MARS 2020 AFTER INTEGRATION.
2020 51st LPSC, The Woodlands
Copyright 2020. All rights reserved.
Abstract ID: 2971
in
size distribu0on, phase func0on which can be used to
es9mate some shape proper9es) as well as its
temporal response to the meteorology, and;
(b) the local near-surface environmental pressure, air
and surface temperatures, rela0ve humidity, wind,
and UV-visible-IR solar radia0on.
at an adjustable sampling rate.
MEDA’s Measurement Objectives: a.To determine the physical and optical properties of the local atmospheric aerosols. Particle abundance, size distribution,
shape, phase function, and how these optical properties relate to the meteorological cycles (diurnal, seasonal, interannual)
b.To determine the conditions leading to dust lifting and how the aerosol diurnal cycle responds to the local diurnal wind
regime
c.To determine how the current environmental pressure, temperature, relative humidity, solar radiation, net infrared
radiation and winds at the landing site differ from those at the Viking, Pathfinder, Phoenix, Curiosity and InSight locations
d.To probe the relationship between the surface environment and the large-scale dynamics observed from orbiting
instruments
e.To investigate the energy and water flux exchange between the surface and the lower atmosphere near the rover
f. To measure the annual cycles of UV, visible, and near-IR radiation at the surface of Mars
g.To obtain the environmental context for weathering and preservation potential of cached samples
h.To investigate how pressure, temperature, humidity, winds, dust amount and size distribution influence the ISRU
engineering efficiency
i. To form linkages between the MEDA observations and models extrapolated to the Martian surface
M. de la Torre Juárez1, J.A. Rodríguez-Manfredi2,3, V. Apéstigue3, I. Arruego3, D.J. Banfield4, J.S. Boland1, P.G. Conrad5, A. G. Fairén1, R. Ferrándiz2,3, E. Fischer6, M. Genzer7, J. Gómez-Elvira3, F. Gómez2,3, S.D. Guzewich8, A.-M. Harri7, M. Hieta7, R. Hueso9, J.J. Jiménez3, M.T. Lemmon10, A. Lepinette2,3, J. Martín-Soler2,3, G.M. Martínez6,11, A. Molina2,3, L. Mora2,3, J.F. Moreno12, S. Navarro2,3, C. Newman13, C. Ortega12, V. Peinado2,3, J. Pla-García2,3, O. Prieto-Ballesteros2,3, S. Rafkin17, M. Ramos14, T. del Río9, J. Romeral2,3,
K. Runyon15, A. Saiz-López16, A. Sánchez-Lavega9, J.T. Schofield1, E. Sebastián2,3, M.D. Smith8, R.J. Sullivan4, L. K. Tamppari1, D. Toledo3, J. Torres2,3, R. Urqui2,3, Á. Vicente-Retortillo2,3,6, D. Viúdez-Moreiras2,3 and the MEDA1,2,7 & M20201 teams 1NASA Jet Propulsion Laboratory/California Institute of Technology, 2Centro de Astrobiología, 3Instituto Nacional de Técnica Aeroespacial, 4Cornell University, 5Carnegie Institution for Science, 6University of Michigan, 7Finnish Meteorological Institute, 8NASA Goddard Space Flight Center, 9University of the Basque Country, 10Space Science Institute,
11Lunar and Planetary Institute/USRA, 12Airbus Defence and Space – CRISA, 13Aeolis Research, 14Universidad de Alcalá, 15Johns Hopkins APL, 16Institute Physical-Chemistry Rocasolano-CSIC, 17Southwest Research Institute – Boulder..
10
20
30
40
50
60
70
80
90
100
110
Aerocentric Longitude Ls (Until Ls 767)
15
30
45
60
75
90
105
120
135
150
165
L T
S T
( h r)
Maximum humidity from 0 to 7 am and its time
Fig. Curiosity
volume mixing ratio (VMR) is shown
(green) and the
(red). Similar measurements will
be made at the
150
200
250
Aerocentric Longitude Ls
Viking L1 40 sols Viking L2 1050 sols REMS 1104 sols
Fig. Curiosity REMS atmospheric temperatures (mean, black curve) at Gale crater, compared to Viking Landers 1 (green) and 2 (blue). REMS min. and max. daily values are shown in red. MEDA has analogous temperature
sensors (actually, 5 sensors) with significant improvements. Combined with 1 TIR sensor, MEDA has the ability to measure at 3 different heights. Their
data can be used to inter-compare with temperatures measured by REMS on Curiosity and TWINS on InSight at the same time. It also adds data to the historical records form the Viking, Phoenix, and Pathfinder missions.
700
750
800
850
900
950
g e p
100 200 300 400 500 600 700 800 900 1000
Sol (up to sol 1049)
p1=−54 Pa p2=58 Pa −10
−5
0
5
10
e (
m )
<T>=213.5 K
z0=−4678 m
crater, showing seasonal pressure
shown in red. Curiosity changes
altitude as it progresses toward Mt. Sharp. After
accounting for the altitude and
seasonal cycles, fluctuations reveal weather and global
circulation (green).
G ro
measured by the GTS. Min. and
max. diurnal temperatures are shown throughout a
Mars year. MEDA has an analogous
sensor (TIRS), with significant improvements,
which will help understand the
environment from which samples are acquired.
200 300 400 500 600 700 800 900 0
5
10
15
20
25
30
35
LMST
m /s
Mean speed and mean + std by sol
Fig. Curiosity’s REMS wind measurements at Gale crater. Mean wind speed
(red) and mean + standard deviation (blue) are shown.
The MEDA instrument has two wind sensor units in different orientations (as in
REMS), but with significant improvements in all aspects
w.r.t. REMS and InSight (performance, electronics, redundancy, …).
Fig. Phase functions will be calculated from the RDS sensors as
was done for Spirit (MY 26, Ls =
354º). Unlike its predecessor REMS, the
MEDA instrument incorporates a dedicated CCD aimed at measuring
the Solar aureole caused by light
scattering from atmospheric aerosols.
This CCD, specifically dedicated to sky observations, will also provide
sequences of sky images that will be
used for the study of clouds (morphologies and discriminating
between ice or dust clouds), as well as to constrain the amount and size
of the atmospheric aerosols (through
the estimate of the phase functions).
120º
Network of environmental stations: If REMS, on Curiosity, and TWINS, on InSight, remain functional until the landing of M2020, MEDA’s comparable set of atmospheric sensors will provide a network of atmospheric stations that characterizes the influence of
changes in the global circulation on the surface environment at different locations on the surface of Mars..
Interna9onal
Consor9um
