atmospheric water experiment for a small orbiter at mars (awesom) paul hayne 1, matt siegler 1,2,...
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Atmospheric Water Experiment for a Small Orbiter at Mars (AWESOM)
Paul Hayne1, Matt Siegler1,2, Imran Mehdi1, Erich Schlecht1, Goutam Chattopadhyay1, and David Paige3
1Jet Propulsion Laboratory – Caltech, 2Planetary Science Institute, 3UCLA
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Overview
• Possible liquid-water features recently observed on Mars indicate potentially habitable environments
• Submillimeter (microwave) spectroscopy is a powerful technique for observing water vapor and constraining its concentration and isotopic composition
• Recent developments at JPL have led to miniaturized instruments compatible with cubesats
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3
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McEwen et al., 2013Ojha et al., 2014
“Recurring slope lineae” (RSL)
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Hypotheses: 1. Spring and summer temperatures get warm enough to melt subsurface (salty) ice2. Deliquescence draws H2O vapor out of the atmosphere gradually, until droplets form
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Could Evaporation at RSL Generate H2O Plumes?
Mumma et al., 2003
(Not water)
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Seasonal (background) Water Vapor
Smith, 2002
Continuous coverage at all local times needed in order to detect (or rule out) water plumes
Time
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Why Microwaves?
MIRO (Rosetta)
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Why Microwaves?
Can measure water vapor at ~10-6 pr-μm!
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Heterodyne Instruments(JPL has a long and distinguished history)
Earth Science: Atmospheric science, temperature and pressure profiling, cloud physics and dynamics, ozone depletion, wind velocity etc
Astrophysics: Study galaxies far away, star formation, star decay, D/H ratio measurement, water detection, C+ detection, HD detection, etc HIFI on Herschel
MLS on Aura
MIRO on Rosetta(sending data right now!!)
STO
Planetary Science: Planetary atmospheres and the search for water and life signatures, sounding, etc
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Heterodyne Technology Development (1 of 2)JPL continues to lead with MDL fabricated diode MMICS and silicon
micro-machining that are robust and enabling
Integrated Receiver Front-ends provide compact foot-print and lower mass
W-band input waveguide
RF input waveguide
LO waveguide
SH
M
Trip
ler
Complete Receiver in
silicon package
2-11 GHz IF output
85-100 GHz30-80 mW
520-600 GHzIntegral feedhorn
20 mm
Low-parasitic membrane MMICs
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Heterodyne Technology Development (2 of 2) Infusion of advanced CMOS technologyEnhance functionality with lower mass and power
28 GHz – 35 GHz Frequency Synthesizer for Local Oscillator (LO)
Total Power Consumption: Less than 100 mW
• A Full 2.0 GS/s spectrum analyzer chip in advanced 65nm CMOS is developed in collaboration with UCLA.
• Integrated 7b digitizers, offset and interleaving calibration functions, clock management system and vector accumulation.
• 512 channel quadrature output with integrated USB 2.0 controller.
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• Reduce volume, mass, and power consumption! • Investigate simplified testing and calibration schemes
Approx. 20 cm
SHM Tripler PA
X3
Sextupler
X6
VCOAntenna
> 50xReducedVolume size
Challenges for Cubesat Accommodation
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Possible Discoveries
• Water vapor available for deliquescence?
• Water vapor plume after RSL activity?
• Diurnal water vapor variations• Water vapor isotopic
abundances (origins?)• Vertical winds, surface
temperatures, pressures
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Summary
• Possibility of liquid H2O activity on present-day Mars is real, but controversial
• Water vapor measurements could resolve debate
• Microwave spectroscopy is an ideal technique for measuring H2O vapor abundance and composition
• Highly-compact JPL microwave spectrometers are being developed for cubesats