######## NRA-02-OSS-01-MIDP Mars Instrument Development Project (MIDP)

######## 

**Last updated: April 25, 2002**

######## **COVER PAGE FROM WEB**

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**Tunable Laser Spectrometer for Atmospheric and Sub-surface Gas
Measurements on Mars Scout and Smart Lander Missions**

**Principal Investigator:** **Dr. Christopher R. Webster**

Jet Propulsion Laboratory

> California Institute of Technology

**Co Investigator:** **Dr. Kamjou Mansour**

> Jet Propulsion Laboratory
>
> California Institute of Technology

[SUMMARY FOR ELECTRONIC INPUT (\<2000 characters)]{.underline}

We propose to extend our PIDDP instrument prototyping of near-IR laser
spectrometers for H2O, CO2 and their isotopomers by building and testing
a Protoflight Spectrometer specifically suited for Mars Scout and Smart
Lander applications. The Protoflight Spectrometer would include a
redesign of our electronics board to include only flight-qualified
parts, and development of a laser source at 1.87 m from a group of 20
flight-qualified devices that we will produce. The Protoflight
Spectrometer will undergo therm-vac, vibration, high-G testing to ensure
its broad applicability to current and future Mars Scout and Smart
Lander Missions.

The development of near-IR tunable diode laser spectrometers for
measurement of H2O and CO2 and their isotopomers will enable several
investigations identified in the MEPAG 2001 report (see later). This
includes determining the quantity of adsorbed H2O and CO2 in Martian
soil, quantifying subsurface, surface, and atmospheric water, the
abundance of volatile-bearing minerals, and identifying climate records.

The laser spectrometer development is urgently needed for Mars Scout
missions for 3 different applications: (i) for high-impact surface
sampling probes; (ii) for balloon, lander or rover surface stations; and
(iii) for sub-surface exploration such as cryobots or deep drilling
probes. Because tunable laser spectrometers are so readily light
weighted (200 g), with high sensitivity, fast response, low power, and
minimum interference, they are accepted as the standard for water and
carbon dioxide measurements on Mars. So large is the interest in the JPL
laser hygrometers, for example, that this instrument is included in 6 of
the current Mars Scout proposals. This number is believed to be
representative of interest in these instruments for future Mars Scout
and Smart Lander missions.

**TABLE OF CONTENTS**

**Cover page/ proposal summary from web**

**Summary of personnel commitments and costs**

######## SCIENTIFIC/TECHNICAL/MANAGEMENT SECTION:

[1. Objectives 1](#objectives)

[1.1. Mars Laser Spectrometer 1](#mars-laser-spectrometer)

[1.2. Expected significance of the proposed research
1](#expected-significance-of-the-proposed-research)

[1.3. Perceived impact 1](#perceived-impact)

[1.4. Relevance of proposed work to NASA OSS programs
2](#relevance-of-proposed-work-to-nasa-oss-programs)

[2. Scientific Background 6](#scientific-background)

[2.1. Water on Mars 6](#water-on-mars)

[2.2. Mars Climate Network 6](#mars-climate-network)

[2.3. Volatile Reservoir Exchange 7](#volatile-reservoir-exchange)

[2.4. Mapping the Mars Temperature Record
7](#mapping-the-mars-temperature-record)

[2.5. Isotope Ratios 7](#isotope-ratios)

[3. Technical Approach and Methodology
9](#technical-approach-and-methodology)

[3.1. Near-IR Tunable laser sources 9](#near-ir-tunable-laser-sources)

[3.2. Tunable laser absorption spectroscopy
9](#tunable-laser-absorption-spectroscopy)

[3.3. Isotope ratio measurements from laser absorption spectroscopy
10](#isotope-ratio-measurements-from-laser-absorption-spectroscopy)

[4. Earlier PIDDP Prototyping 10](#earlier-piddp-prototyping)

[4.1. Heritage 10](#heritage)

[4.2. The Mars Polar Lander MVACS TDL spectrometers
10](#the-mars-polar-lander-mvacs-tdl-spectrometers)

[4.3. The MOD TDL spectrometer 11](#the-mod-tdl-spectrometer)

[4.4. The Pascal Pre-Scout Prototype Laser Hygrometer
11](#the-pascal-pre-scout-prototype-laser-hygrometer)

[4.5. The PIDDP QC Laser Spectrometer
11](#the-piddp-qc-laser-spectrometer)

[5. Management Approach 12](#management-approach)

[5.1. Management 12](#management)

[5.2. Organizational structure, personnel
12](#organizational-structure-personnel)

[5.3. Work plan 13](#work-plan)

[5.4. Facilities 15](#facilities)

[5.5. Schedule 15](#schedule)

[6. Cost Plan Summary 16](#cost-plan-summary)

######## 

######## **ANCILLARY MATERIAL:**

######## **Curriculum vitae of PI and Co-I's**

######## 

######## **Current and Pending Support**

######## 

######## **Statement of commitments from Co-I's**

######## 

######## **Research Budget Summary and Details** 

######## 

######## **SUMMARY OF PERSONNEL COMMITMENTS AND COSTS**

######### (RESEARCH COMPONENT: INVESTIGATORS ONLY)

**FIRST YEAR (FY03)**

Name Work-years Unburdened Salary Cost

Dr. Christopher R. Webster (PI)

Dr. Kamjou Mansour

**SECOND YEAR (FY04**)

Name Work-years Unburdened Salary Cost

Dr. Christopher R. Webster (PI)

Dr. Kamjou Mansour

**THIRD YEAR (FY05**)

Name Work-years Unburdened Salary Cost

Dr. Christopher R. Webster (PI)

Dr. Kamjou Mansour - -

# Objectives

## Mars Laser Spectrometer 

We propose to extend our PIDDP instrument prototyping of near-IR laser
spectrometers for H2O, CO2 and their isotopomers by building and testing
a Protoflight Spectrometer specifically suited for Mars Scout and Smart
Lander applications.

The Protoflight Spectrometer would incorporate a redesign of our
electronics board to include only flight-qualified parts, and a laser
source at 1.87 m from a group of 20 flight-qualified devices that we
will produce. The Protoflight Spectrometer will undergo therm-vac,
vibration, high-G testing to ensure its broad applicability to current
and future Mars Scout and Smart Lander Missions.

## Expected significance of the proposed research

The development of near-IR tunable diode laser spectrometers for
measurement of H2O and CO2 and their isotopomers will enable several
investigations identified in the MEPAG 2001 report (see later). These
includes determining the quantity of adsorbed H2O and CO2 in Martian
soil, quantifying subsurface, surface, and atmospheric water, the
abundance of volatile-bearing minerals, and identifying climate records.

The detection of bound water (as water of hydration or
chemically/physically adsorbed) or carbonates in Martian soil or rock is
extremely important for understanding the Martian climate during
formation and chemical processes such as weathering. Measurements of H2O
and CO2 vapor pressures evolved from heating samples will allow the
identification of mineral phases (e.g. ferric carbonate (siderite),
magnesium carbonate, and calcium carbonate decompose at 350, 450, and
890 ^o^C, respectively.

Like on Earth, Mars climate history is to some extent recorded in the
delta-18 isotopic ratio in H2^18^O that can be measured in ice core
samples, e.g. from a cryobot technique.

## Perceived impact

The state of knowledge in the field of planetary measurements of
atmospheric, and evolved gases and their isotope ratios rests with the
significant technological advances and miniaturization efforts in two
key techniques: mass spectrometry (MS), and laser absorption (LA)
spectrometry.

Because tunable laser spectrometers are so readily light weighted (220
g), with high sensitivity, fast response, low power, and minimum
interference, they are accepted as the standard for water and carbon
dioxide measurements on Mars. So large is the interest in the Webster
group laser hygrometers, for example, that **this instrument is included
in 6 of the current Mars Scout proposals, a number believed to be
representative of interest in this instrument for future Mars Scout and
Smart Lander missions.**

+---------------------+---------------------+-------------------------+
| **Current (2002)    |                     |                         |
| Mars Scout Mission  |                     |                         |
| Proposals for which |                     |                         |
| Webster is          |                     |                         |
| Instrument Provider |                     |                         |
| Co-I**              |                     |                         |
+---------------------+---------------------+-------------------------+
| **Mars Scout        | **Mission PI**      | **Laser Spectrometer    |
| Mission**           |                     | Need**                  |
+---------------------+---------------------+-------------------------+
| 1\. Pascal Climate  | Robert Haberle      | 1.87 m for atmospheric  |
| Network             |                     | H~2~O and CO~2~         |
|                     | NASA Ames           |                         |
+---------------------+---------------------+-------------------------+
| 2\. Artemis         | David Paige         | 1.87 m for H~2~O and    |
| Multi-Scout         |                     | CO~2~, and 2.03 m for   |
|                     | UCLA                | isotopes of CO~2~, for  |
|                     |                     | both atmospheric and    |
|                     |                     | evolved gases           |
+---------------------+---------------------+-------------------------+
| 3\. SSTAMP Mars     | Paul Mahaffy        | Mid-IR QC laser         |
| Balloon             |                     | spectrometer for        |
|                     | NASA GSFC           | atmospheric biogenic    |
|                     |                     | gases                   |
+---------------------+---------------------+-------------------------+
| 4\. Mars Cryobot    | Steven Saunders JPL | 1.87 m for H~2~O and    |
|                     |                     | H~2~^18^O content of    |
|                     |                     | ice                     |
+---------------------+---------------------+-------------------------+
| 5\. Mars Penetrator | Albert Yen          | 1.87 m for H~2~O and    |
|                     |                     | CO~2~, and 2.03 m for   |
|                     | Caltech-JPL         | isotopes of CO~2~ in    |
|                     |                     | evolved gases           |
+---------------------+---------------------+-------------------------+
| 6\. Mars Lander     | Pascal Lee          | 1.87 m for H~2~O and    |
| HOMER               |                     | CO~2~, and 2.03 m for   |
|                     | NASA Ames           | isotopes of CO~2~, for  |
|                     |                     | both atmospheric and    |
|                     |                     | evolved gases           |
+---------------------+---------------------+-------------------------+

However, much work needs to be done, specifically in the instrument
development work that bridges from PIDDP activities to flight, and it is
in this area that we propose to focus our activities. It is anticipated
that this work will lead to producing flight-qualified designs tailored
to Mars Scout and Smart Lander missions that will significantly decrease
the cost to mission PI's interested in these spectrometers, while
increasing the reliability and operation at the Martian extreme
environmental conditions.

These laser spectrometers have a critical role to play in Human
Exploration and Development of Space (HEDS) *in situ* resource
utilization (see next section).

## Relevance of proposed work to NASA OSS programs

This proposal builds on the significant accomplishments to date under
the Planetary Instrument Definition and Development Program (PIDDP) in
developing prototype tunable laser absorption spectrometers for
planetary measurements.

The JPL Atmospheric Laser Spectroscopy Group has over the last 17 years
developed laser spectrometers for Earth (aircraft and balloon), Titan
(Cassini probe, not selected), and Mars (Mars98, two instruments on
failed payload; Mars 2007 Mars Organic Detector TDLS). Our expertise in
developing *in situ* laser spectrometers for Earth, Titan, and Mars
provides a unique foundation for carrying out this high-TRL level
instrument development program while maintaining focus on the key
scientific goals.

For Earth, in over 300 aircraft and balloon flights, the group has
demonstrated the high sensitivity of tunable laser absorption
spectroscopy for *in situ* measurement of atmospheric gases in both the
near-IR (1-3 m) and the mid-IR (3-8 m) wavelength regions. For water
measurements, using 1.37 m TDLs, we have built and flown several new
laser hygrometers for measuring water vapor in the Earth\'s atmosphere
for the aircraft ER-2, DC-8, and WB-57.

For Mars, the two miniature *in situ* gas spectrometers built for the
Mars 98 Surveyor's MVACS lander payload, and the Mars 2007 Mars Organic
Detector (MOD) are based on room-temperature TDLs at near-IR wavelengths
(1-2 m) for measurement of atmospheric H~2~O at 1.37 m and isotopic
CO~2~ at 2.04 m.

In our proposed Protoflight Spectrometer, we wish to specifically target
the 1.87 m wavelength region as more suitable for Mars application than
the 1.37 m region previously used**. The laser spectrometer would
provide wide-ranging and immediate application to measuring
concentrations of both H2O and CO2 and its isotopomers in atmospheric,
evolved gas, and ice samples.**

Selected parts of the MEPAG report (March 2002) are copied below to
underscore the need for *in situ* high-precision, accurate measurements
of

H2O, CO2, and their isotopomers on Mars.

## SELECTED TEXT FROM THE MARCH 2001 MEPAG REPORT UNDERSCORING THE NEED TO DEVELOP TUNABLE LASER SPECTROMETERS FOR H~2~O, CO~2~, THEIR ISOTOPOMERS, AND OTHER GASES

## GOAL I: DETERMINE IF LIFE EVER AROSE ON MARS

\[Although laser spectrometers can play an important role for achieving
this goal, needs for this goal are addressed by a different NASA
program\].

## GOAL II: DETERMINE CLIMATE ON MARS

**Objective A: Characterize Mars' present climate and climate processes
(investigations in priority order)**

***[Investigation 1:]{.underline} Determine the processes controlling
the present distributions of water,***

***carbon dioxide and dust.*** Understanding the factors that control
the annual variations of volatiles and dust is necessary to determine to
what extent today's processes have controlled climate change in the
past. Requires global mapping and then landed observations on daily and
seasonal time scales.

***Measurements***

b\. Estimate water vapor flux, requiring in situ daily, diurnally
resolved measurements of

near-surface water vapor concentration over (latitudinally dependent)
seasonal time scales (e.g., 60 sols in polar regions; 1 Mars year at
non-polar latitudes). Measurements needed at low, mid and high latitudes
and in a variety of terrain (not necessarily concurrently): low and high
thermal inertia regions, off and on the residual north polar cap.
Measurements from a site with subliming seasonal frost also desired.

c\. In situ measurements of adsorbed and solid water and carbon dioxide
in the soil concurrent with the measurements described in a and b above
to depths of a few cm at multiple times per day. Ice abundance
measurements should cover the range from 0.01 to 1.0 g cm^3^ with 10%
accuracy. Adsorbed H~2~O measurements should cover the range from 10^-4^
g/g to 10^-2^ g/g with 10% accuracy. Measurements of adsorbed CO~2~
should cover the range from 10^-5^g/g to l0^-3^g/g with 20% accuracy.
Measurements adsorbed H~2~0 and CO2 and water ice should also be
conducted to depths of \~1 meter, but do not require diurnal or even
seasonal temporal resolution. *Technology development needed: some.*

***[Investigation 2]{.underline}: Determine the present-day stable
isotopic and noble gas composition of the present-day bulk
atmosphere.*** These provide quantitative constraints on the evolution
of atmospheric composition and on the source and sinks of the major gas
inventories.

***Measurements***

a\. In situ, high-precision measurements of atmospheric isotopic
composition at one site. +/- 5 per mil for 18-O/16-O, 17-O/16-O,
13-C/12-C; +/- 250 per mil for D/H, anywhere on the planet.

***[Investigation 3]{.underline}: Determine long-term trends in the
present climate.*** This determination will test to what degree the
Martian climate is changing today.

***Measurements***

a\. Extension of the orbital and lander measurements of (A1) to multiple
Mars years.

***[Investigation 5:]{.underline} Search for micro-climates.***
Detection of exceptionally or recently wet or warm locales and areas of
significant change in surface accumulations of volatiles or dust would
identify sites for in situ exploration. Requires global search for sites
based on topography or changes in volatile distributions and surface
properties (e.g., temperature or albedo).

***Measurements***

b\. Detect local concentrations of water vapor, particularly within the
lowest l-3 km the atmosphere at spatial resolution \<100 m. Regions
repeatedly surveyed during spring and summer seasons.

***[Investigation 6:]{.underline} Determine the production and reaction
rates of key photochemical species (O~3~, H~2~O~2~, CO OH etc.) and
their interaction with surface materials.***

***Measurements***

a\. Measure species in the atmosphere with sensitivities of l0^9^ cm^-3^
as a function of insolation.

b\. Measure and identify surface complexes or chemabsorbed species on a
representative sample (sample return or in situ?) of surface materials
(primary and secondary materials).

**Objective B: Characterize Mars' present climate and climate processes
(investigations in priority order)**

***[Investigation 2:]{.underline} Characterize history of stratigraphic
records of climate change at the polar layered deposits, the residual
ice caps.*** The polar regions suggest repeated geologically recent
climate change. A key to understanding their histories is relative
dating of polar layering and volatile reservoirs. Requires orbital, in
situ observations and returned samples.

***Measurements***

c\. In situ, local exploration of layered deposits in north and south
polar regions t characterize the physical structure of layers, volatile
content, chemical and isotopic (especially H, N, and O) variations.
Measurements should be conducted at multiple stratigraphic locations at
each site. *Technology development needed: much.*

# GOAL III: DETERMINE THE EVOLUTION OF THE SURFACE AND INTERIOR OF MARS 

**Objective A: Determine the nature and sequence of the various geologic
processes (volcanism, impact, sedimentation, alteration etc.) that have
created and modified the Martian crust and surface (investigations in
priority order):**

***[Investigation 1:]{.underline} Determine the present state,
distribution, and cycling of water on Mars.*** Water is arguably the
most important geologic material that influences most geologic processes
including the formation of sedimentary, igneous and metamorphic rocks,
the weathering of geologic materials, and deformation of the
lithosphere. Requires global observations using geophysical sounding and
neutron spectroscopy, coupled with measurements from landers, rovers,
and the subsurface.

***Measurements***

d\. *In-situ* drilling to liquid water or ice to depths up to a
kilometer for at least one site and to depths of several hundred m for
several sites with down-hole instruments to determine elemental
abundances, mineralogy of volatile and other phases, including ices.

***[Investigation 4:]{.underline} Evaluate igneous processes and their
evolution through time, including the present.*** This study includes
volcanic outgassing and volatile evolution. Volcanic processes are the
primary mechanism for release of water and atmospheric gases that
support potential past and present life and human exploration. Sites of
present day volcanism, if any, may be prime sites for the search for
life. Requires global imaging, geologic mapping, techniques for
distinguishing igneous and sedimentary rocks, evaluation of current
activity from seismic monitoring, and returned samples.

***Measurements***

b\. *In situ* measurements from the surface for at least several
volcanic sites to determine chemistry, mineralogy, and petrology.
Characterization should be sufficient to identify the rock types and
will require a payload with significantly more capability than Athena.

***[Investigation 5]{.underline}: Characterize surface-atmosphere
interactions on Mars, including polar, eolian, chemical, weathering, and
mass-wasting processes.*** Interest here is in processes that have
operated for the last million years as recorded in the upper 1 m to 1 km
of geological materials. Understanding present geologic, hydrologic, and
atmospheric processes is the key to understanding past environments and
possible locations for near-surface water. Knowing the chemistry and
mineralogy of both near surface rocks and alteration products is
essential for calibrating remote sensing data. This study also has
strong implications for resources and hazards for future human
exploration. Requires orbital remote sensing of surface and subsurface,
and in situ measurements of sediments and atmospheric boundary layer
processes.

***Measurements***

d\. Network of at least 16 stations to monitor weather (temperature,
pressure, wind velocity and strength) with concurrent visual
observations from the surface and from orbit. Mission lifetime of three
Mars years to determine seasonal and internal variations.

## GOAL IV: PREPARE FOR HUMAN EXPLORATION

**Objective A: Acquire Martian environmental data sets (priority order
of investigations under review)**

***[Investigation2]{.underline}: Characterize the chemical and
biological properties of the soil and dust.*** Toxicity and reactivity
needed to develop hazard mitigation strategies to ensure safety of human
explorers on the Martian surface. Requires in-situ experiments.

***Measurements***

c\. Determine the chemical reactivities with a sensitivity of ppm (of
particular interest are changes in the reactivities upon heating, with
exposure to humidity, and with emphasis on the identification and
volatility of the gases evolved) and, up to a maximum depth of 150 cm.
Understand the solubility in water of martian soil (total weight loss
after water is equilibrated with the soil), the before and after
composition of the soil, and the composition of the aqueous phase in
equilibrium with martian soil.

d\. Determine the depth of the superoxidation zone at several locations.

***[Investigation 3:]{.underline} Understand the distribution of
accessible water in soils, regolith, and***

***Martian groundwater systems.*** Water is a principal resource to
humans. Requires geophysical investigations and subsurface drilling and
in situ sample analysis.

***Measurements***

b\. Measure the vertical distribution (and ultimately comprehensive
3-demensional subsurface maps) of permafrost, water ice and liquid water
with a vertical resolution of \~ 10 m at selected sites.

c\. Determine the adsorbed and bound water content of soil samples from
several provenances (air-borne dust, surface fines, sand dunes) with
precision of +/- 10% down to levels of 0.1%. Determine the release
temperature of water over the range 0^o^C-600 ^o^C.

***[Investigation 5:]{.underline} Access and extract water from the
atmosphere, soils, regolith, and Martian groundwater systems.*** Water
is a principal resource. Requires in-situ operations to determine
hydrologic characteristics of aquifers and aquicludes. Requires
subsurface drilling.

**Objective B: Conduct in situ engineering science demonstrations
(priority order of investigations under review)**

***[Investigation 4:]{.underline} Demonstrate in situ propellant
(methane, oxygen) production (ISPP) and in situ consumables production
(ISCP) (fuel cell reagents, oxygen, water, buffer gases).*** Components
which directly interact with the Martian environment should be evaluated
in a relevant environment to determine their performance. Requires
process verification with in situ experiments.

***Measurements***

a\. Demonstrate the intake and adsorption of carbon dioxide from the
Martian atmosphere;

***[Investigation 5:]{.underline} Access and extract water from the
atmosphere, soils, regolith, and Martian groundwater systems.*** Water
is a principal resource. Requires in situ operations to determine
hydrologic characteristics of aquifers and aquicludes. Requires
subsurface drilling.

***Measurements***

c,d,e,f. Demonstrate extraction of water from subsurface aquifers,
permafrost layers, atmosphere, and regolith.

# Scientific Background

## Water on Mars

The Laser Hygrometer described here directly measures the Martian water
cycle. Weather controls the movement of dust around Mars, the exchange
of water between the surface and atmosphere, and the seasonal cycling of
CO~2~ (the dominant atmospheric constituent) into and out of the polar
regions.

Previous measurements of atmospheric water vapor have been made either
from orbit or from Earth-based telescopes***. No direct in situ
measurements of water have yet been made.*** In situ measurements will
provide information on the nature of surface-atmosphere exchange
processes. Water vapor varies in space and time within the Martian
atmosphere suggesting there are surface sources and sinks. However, the
distribution of the sources and sinks is uncertain. This is a key
element of the Martian water cycle that is best addressed by long-term,
daily measurements.

Water vapor in the Martian atmosphere has been observed from orbiting
spacecraft and Earth-based telescopes. The latest measurements from the
MGS TES experiment show that Mars has an active hydrological cycle in
which water is exchanged between the surface and atmosphere on seasonal
and possibly diurnal time scales. The only known surface reservoir for
water is the residual north polar ice cap that is the source of water
for the north polar summertime maximum (Farmer et al., 1976; 1977; Smith
et al. 2001). No such reservoir has been detected at the south pole even
though a high latitude summertime maximum has been observed in the
southern hemisphere. In this case, the source is likely to be water ice
incorporated into the seasonal CO~2~ cap, or water desorbed from the
regolith as the cap retreats and the surface warms. Both hemispheres are
likely to have seasonal ice deposits and/or regolith water (Jakosky and
Farmer, 1982); however, aside from the north residual cap, the
distribution of exchangeable surface reservoirs for water is unknown.

Water is also the key to understanding the possibility for life on Mars.
Where water is and in what form are crucial data points in the search
for life. Liquid water is widely believed to be required for life. Most
of the water on Mars today is in the solid or gaseous form; however, it
now appears that liquid water has been on the surface in the relatively
recent past in the form of seepage gullies (Malin and Edgett, 2000).
Models indicate that there are certain places and times on present day
Mars that thin films of solar-heated liquid water could exist
temporarily given the right circumstances (Haberle et al., 2001). While
liquid water seems an unlikely possibility for Mars (e.g., Ingersoll,
1969), these recent observations and theoretical developments argue
against ruling it out completely.

## Mars Climate Network

By way of example of one application of laser hygrometers to Mars Scout
missions, the Pascal Mission (PI Haberle) is directed at producing a
detailed, global picture of Martian climate and weather.

Pascal will make daily measurements of near-surface atmospheric water
vapor at 24 globally distributed sites for 10 Mars years. These will be
the first in-situ measurements of water vapor on such a scale to
determine diurnal variations in water vapor, which can be used to infer
exchange between the surface and atmosphere. Numerical models of diurnal
exchange predict small diurnal variations in the vapor pressure of H~2~O
at a specific site, but large variations according to the latitude and
thermophysical characteristics of the surface (Zent et al., 1993).
Pascal will allow those models to be validated, and hence sharpen our
understanding of the diurnal regolith-atmosphere H~2~O exchange, which
ultimately controls seasonal exchange.

![](media/image1.jpeg){width="2.8604166666666666in"
height="2.1215277777777777in"}

## Volatile Reservoir Exchange

In addition to determining atmospheric, surface, and subsurface water,
the proposed Artemis Scout Mission (PI Paige) will identify volatile
reservoir exchange through additional measurements of carbon dioxide and
it isotopomers (see later).

## Mapping the Mars Temperature Record

Like on Earth, Mars climate history is to some extent recorded in the
delta-18 isotopic ratio in H2^18^O that can be measured in ice core
samples. Such a measurement is proposed for the Mars Scout Cryobot, in
which ice core samples would be analyzed to determine their delta-18
isotopic ratio in H2^18^O.

![](media/image2.jpeg){width="3.113888888888889in"
height="2.127083333333333in"}

##  Isotope Ratios

There are numerous sources of isotopic fractionation in atmospheric
gases. Isotopic fractionations in general fall into three categories:
kinetic, equilibrium, and non-mass-dependent fractionation. In kinetic
fractionation, discrimination between isotopomers is due to their
differing rates of chemical reaction, or differing rates of diffusion to
reaction sites. Kinetic fractionations are evident in reactions that
never reach equilibrium partitioning, including those associated with
biology, in diffusion-limited processes, and in issues involving
molecular escape from the atmosphere. Equilibrium fractionation, on the
other hand, refers to the equilibrium partitioning of isotopomers into
different chemical constituents or phases to achieve the lowest free
energy state. On the Earth, the most well-known example is the strong
fractionation involved in condensing water, due to the different vapor
pressures of ordinary and isotopically substituted water.

The stable isotopic compositions of low-mass (light) elements such as
oxygen, hydrogen, carbon, nitrogen, and sulfur are normally reported as
\"delta\" values in parts per thousand (denoted as ‰) enrichments or
depletions relative to a standard of known composition \[see
<http://wwwrcamnl.wr.usgs.gov/isoig/>\]. Delta or -values given in \"per
mil\" are calculated by:

(‰) = (R~sample~/R~standard~ - 1)1000

where \"R\" is the ratio of the heavy to light isotope in the sample or
standard. For the elements sulfur, carbon, nitrogen, and oxygen, the
average terrestrial abundance ratio of the heavy to the light isotope
ranges from 1:22 (sulfur) to 1:500 (oxygen); the ratio D:H is 1:6410. A
positive value means that the sample contains more of the heavy isotope
than the standard; a negative value means that the sample contains less
of the heavy isotope than the standard. A ^15^N value of +30‰ means that
there are 30 parts-per-thousand or 3% more ^15^N/^14^N in the sample
relative to the standard.

Isotopic fractionation has long been recognized as a powerful tool for
identifying chemical signatures of life. Because it is easier and faster
to process lighter isotopes, biological catalysts (enzymes) exhibit a
propensity for processing lighter isotopomers. Thus, the organic matter
of the biomass of living organisms is generally found to be enriched
with the lighter isotopes.

***CARBON ISOTOPES:***

Important reservoirs of carbon on Earth include biomass, atmospheric
CO~2~ and CH~4~, soils, and dissolved carbonate in the oceans. By far
the largest reservoirs of carbon are rocks like carbonate and oil shale,
but they do not rapidly exchange with the atmosphere or biosphere.
Dissolved carbonate in the upper ocean has a carbon isotopic composition
close to 0 per mil relative to the PeeDee Belemnite (PDB) carbonate
formation and appears to be in isotopic equilibrium with atmospheric
CO~2~ (^13^C = -7 per mil). Industrial CO~2~ is more depleted of ^13^C
(^13^C = -24 to -28 per mil), so fossil fuel usage is slowly reducing
the ^13^C of atmospheric CO~2~. Biomass in C3 plants contains
isotopically light carbon (^13^C = -25 per mil) relative to CO~2~ due to
the greater affinity of the carbon-fixing enzyme for ^12^CO~2~ and its
faster diffusion into plant leaves. In contrast, C4 plants are less
strongly fractionated (^13^C = -13 to --15 per mil), and marine organic
carbon has a wide range of isotopic compositions (^13^C = -10 to -30 per
mil). Carbon isotopes are not significantly fractionated between solid
and gas-phase CO~2~, so sublimation and condensation processes on Mars
are not expected to modify the isotopic composition of CO~2~ there
(except possibly due to kinetic isotope effects). Therefore, there is a
better chance of finding a biological signal in ^13^C of CO~2~ in the
Martian atmosphere.

Atmospheric CH~4~ is strongly fractionated by its biological sources and
sinks (^13^C \~ -46.5 per mil). Some bacteria produce CH~4~ with a
fractionation as large as --110 per mil (Ohmoto, 1986). Hence, CO~2~ and
CH~4~ samples are generally suspected to be biogenic if they have a
large negative ^13^C relative to abiotic carbon reservoirs. Similarly,
anomalously low ^13^C of carbonaceous inclusions in sedimentary rocks
strongly suggests that life existed on Earth more than 3.8 billion years
ago (Mojzsis et al., 1996). Clearly, carbon isotopes can provide an
important signature of geochemical and biological processes.

***OXYGEN ISOTOPES:***

On Earth, the largest reservoirs of oxygen exchangeable with the
atmosphere are the crust and the hydrosphere. Biological fractionation
is clearly seen in atmospheric O~2~: ^18^O = +23.5 per mil relative to
Standard Mean Ocean Water (SMOW). Respiring organisms preferentially use
light O~2~, with an average fractionation of --20 per mil, leaving the
atmospheric O~2~ at +20 per mil. The additional +3.5 per mil enrichment
comes from oxygen isotopic fractionation in leaf water. Unlike O~2~,
atmospheric H~2~O has a large range of oxygen isotopic compositions due
to Rayleigh distillation between gas-phase and condensed H~2~O. The
oxygen isotopic composition of precipitation ranges from close to 0 per
mil in the tropics to --22 per mil in Antarctica. Atmospheric CO~2~
exchanges oxygen with liquid H~2~O with a fractionation that is strongly
temperature-dependent. CO~2~ experiences oxygen fractionation between
condensed and gaseous phases. Like water, CO~2~ will thus have ^18^O
variations from condensation, sublimation, and transport effects on
Mars.

# Technical Approach and Methodology

## Near-IR Tunable laser sources

Room-temperature (TE cooler) tunable diode laser (TDL) sources of high
spectral purity (single mode) and high output powers (5-50 mW) are now
available in the near-IR region where molecules like H~2~O and CO~2~
have sufficiently strong IR absorption cross-sections. At wavelengths in
the 1-2 m-range, JPL's MicroDevices Lab (MDL) have produced single-mode
Distributed FeedBack (DFB) devices which have been tested and integrated
into the Mars MVACS lander payload of the Mars 98 Surveyor mission: one
for measurement of atmospheric H~2~O at 1.37 m and isotopic CO~2~ at
2.04 m (TDL Met); and a second as an analyzer for evolved H~2~O and
CO~2~ from heated soil (TEGA).

![](media/image3.bmp)

However, for H2O measurements, the 1.87 m wavelength lasers are much
preferred, since they access stronger water lines, can also access
isotopic H2^18^O lines, AND CO2 lines for pressure measurements.

## Tunable laser absorption spectroscopy

Tunable laser absorption spectroscopy is widely recognized as a direct,
non-invasive, simple measurement technique that is known for its high
sensitivity (sub-parts-per-billion) and specificity \[see review by
*Webster et al., 1988*\]. Minimum-detectable-absorptions as small as 2
parts in 10^6^ are possible, with 2 parts in 10^5^ readily achieved in
flight. For reasonable pathlengths, this translates to parts-per-billion
sensitivities for numerous species in the mid-infrared, and tens of ppb
in the near-IR region.

Shown below are our calculations for minimum detectable amounts of H~2~O
and CO~2~ on Mars.

MARS: NEAR-IR *REGIONS FOR H~2~O and CO~2~*

Pressure = 7 mbar (surface), T = 220 K,

path = 20 m, A~min~ = 2x10^-5^, 95%CO~2~

+------------+------------+----------+---------------+---------------+
| Molecule   | Wave-      | Wave-    | Expected      | Minim         |
|            |            |          | mixing ratio  | um-detectable |
|            | number     | Length   |               | mixing ratio  |
|            |            |          |               |               |
|            | (cm^-1^)   | (μm)     |               |               |
+------------+------------+----------+---------------+---------------+
| H~2~O      |            | 1.37     | 1-500 ppm     |               |
+------------+------------+----------+---------------+---------------+
| H~2~O      |            | 1.87     | 1-500 ppm     |               |
+------------+------------+----------+---------------+---------------+
| CO~2~      |            | 2.05     | 95.3%         | ppbv          |
|            |            |          |               |               |
| ^13^CO~2~  |            |          | 1%            |               |
|            |            |          |               |               |
| ^16^O      |            |          | 0.4%          |               |
| ^12^C^18^O |            |          |               |               |
|            |            |          | 0.08%         |               |
| ^16^O      |            |          |               |               |
| ^12^C^17^O |            |          |               |               |
+------------+------------+----------+---------------+---------------+

![](media/image4.jpeg){width="3.1944444444444446in"
height="1.9715277777777778in"}

![](media/image5.jpeg){width="3.75in"
height="2.4541666666666666in"}Shown below is a simulation illustrating
the powerful advantage of the 1.87 m wavelength region over the 1.37 m
region, in that a nearby CO~2~ line can be used for both calibration or
as a second pressure measurement (accuracy 2%). Furthermore, this region
can also access a pair of suitable H~2~^16^O/ H~2~^18^O lines for
isotopic analysis of solid, liquid, or gas phase water samples.

## Isotope ratio measurements from laser absorption spectroscopy

Tunable laser spectroscopy offers a powerful means of measuring isotope
ratios by selecting spectral regions where weaker features of the main
isotope have similar absorptance to adjacent isotopic lines. The use of
absorption lines of ^13^CO~2~ and ^12^CO~2~ near 4.3 m was first
proposed by Wall (1981) who found several isotopic line pairs with equal
absorptance despite the 90:1 isotopic ratio.

For CO~2~, isotope ratio determinations may be made using either near-IR
(2.05 m) or QC laser (4.3 m) laser sources.

Although in principal isotope ratios may be measured down to 1 per mil
using tunable laser spectroscopy, the ultimate measurement precision
depends not only on spectral SNR, but also the temperature (and to a
less extent, pressure) dependence of the chosen lines.

# ![](media/image6.wmf){width="2.461023622047244in" height="1.5661417322834645in"}![](media/image7.wmf){width="2.675196850393701in" height="1.7409448818897637in"}![](media/image8.wmf){width="3.344488188976378in" height="1.6346456692913385in"}Earlier PIDDP Prototyping

## Heritage

The JPL Webster group has over the last 17 years developed laser
spectrometers for Earth (aircraft and balloon), Titan (Cassini probe,
not selected), and Mars (Mars98, two instruments on failed payload; Mars
2007 Mars Organic Detector TDLS). In over 350 aircraft and balloon
flights, the group has demonstrated the high sensitivity of tunable
laser absorption spectroscopy for *in situ* measurement of atmospheric
gases in both the near-IR (1-3 m) and the mid-IR (3-8 m) wavelength
regions.

## The Mars Polar Lander MVACS TDL spectrometers

![](media/image9.jpeg){width="2.25in" height="2.201388888888889in"}The
two miniature *in situ* gas spectrometers built for the Mars 98
Surveyor's MVACS lander payload, and the Mars 2007 Mars Organic Detector
(MOD) are based on room-temperature TDLs at near-IR wavelengths (1-2 m)
for measurement of atmospheric H~2~O at 1.37 m and isotopic CO~2~ at
2.04 m.

## The MOD TDL spectrometer

In an application similar to the MVACS MET and TEGA spectrometers, we
developed a laboratory breadboard for the Mars Organic Detector that is
the basis for our Mars Scout Artemis and Lander spectrometers. However,
the 1.37 m TDL for water needs to be replaced with one at 1.87 m, and
the breadboard laboratory spectrometer needs to be taken to a higher TRL
level for flight consideration.

![](media/image10.jpeg){width="2.9819444444444443in"
height="2.2715277777777776in"}

## The Pascal Pre-Scout Prototype Laser Hygrometer

More recently, we have made a laboratory breadboard spectrometer version
of the miniature (220 g) spectrometer that we will propose for the Mars
Scout Pascal Mission. A single (unqualified) TDL at 1.87 m was used to
record the spectral region shown by way of proving sensitivities.
Otherwise, much work is needed to bring this prototype to the high TRL
levels.

![](media/image11.jpeg){width="3.2041666666666666in"
height="2.2104166666666667in"}

![](media/image15.jpeg){width="2.8868055555555556in"
height="2.1694444444444443in"}

## The PIDDP QC Laser Spectrometer

Under a separate task we are also breadboarding a state-of-the-art
Quantum Cascade tunable laser spectrometer for accessing a variety of
gases and their isotopomers in the mid-IR region. The high-TRL level
development work proposed here (e.g. of electronics) will also benefit
the mid-IR spectrometer capabilities.

# Management Approach

## Management

The Principal Investigator, **Dr. Christopher R. Webster,** will manage
the proposed research and have overall responsibility for all aspects of
the work. As PI he will ensure that the research is completed within
cost and schedule. The PI will coordinate and facilitate active
communication between the team members on technical, scientific, and
programmatic issues. Innovative, effective management processes and
institutionally supported tools will be available to assist the research
task. Critical issues and reviews will be accomplished in face-to-face
meetings. The PI, whose background includes management of numerous
previous JPL Earth and planetary science research, missions, and line
management, is the primary leader for this instrument development
research, with specific programmatic, personnel, technical, and
institutional responsibilities.

## Organizational structure, personnel

**JPL's Atmospheric Laser Spectroscopy Group** seeks to understand the
photochemistry, dynamics, and evolution of Earth and planetary
atmospheres through interpretation of *in situ* measurements of gas,
particulate, and mineral composition using state-of-the-art laser
spectrometers built by the group. Over the last 17 years we have
conceived, designed, and built a variety of tunable diode laser
spectrometers that have flown on balloon, aircraft (ER-2, DC-8, WB57),
and spacecraft (Cassini Mission, Mars Polar Lander) platforms. An active
laboratory instrument miniaturization program has produced
high-sensitivity spectrometers weighing less than 250 grams. ***A
summary of the activities of our group and personnel can be found at**
[http://laserweb.jpl.nasa.gov](http://laserweb.jpl.nasa.gov/)*

**Dr. Christopher R. Webster (Principal Investigator**) is a Senior
Research Scientist at Caltech's Jet Propulsion Laboratory (JPL) where he
has worked since 1981. He is the Group Supervisor of the Atmospheric
Laser Spectroscopy Group that he formed in 1985 to study the
photochemistry and dynamics of Earth and planetary atmospheres through a
program of developing and flying balloon, aircraft, and spacecraft
state-of-the-art laser spectrometers for gas and mineral detection
analysis. In 1984 Dr. Webster pioneered the miniaturization of laser
spectrometers for planetary application with the successful development
of the multi-gas and particle Probe Infrared Laser Spectrometer (PIRLS)
instrument for Saturn's moon Titan, and the 1991 Mars IR Laser
Spectrometer (MIRLS). He has proposed miniature laser spectrometers for
biogenic gas and isotope measurements on several missions, including
Mars96 Soviet Mission, the 1992 Jason Mars Discovery Mission, and more
recently the Mars Organic Detector TDLS for the HEDS 2007 Mars Mission.
He is also the PI for two new instrument development activities for a
Quantum-cascade laser spectrometer for Mars, Titan, and Venus. He is
Team Leader of the JPL Grand Challenge Initiative for identifying
chemical signatures of life. Dr. Webster received a NASA Exceptional
Scientific Achievement Medal (1992), 8 NASA Group Achievement Awards,
and has authored \>120 refereed scientific journal publications in
spectroscopy, chemical physics, atmospheric science, and laser
instrumentation.

**Dr. Kamjou Mansour (Co-Investigator)** is a senior Member of
Engineering Staff in the JPL Infrared Focal Planes and Photonics
Technology Group. He received his Ph.D. in quantum electronics from
Center for Research and Education in Optics(CREOL) and University of
North Texas in 1990 for work on optical characterization of
semiconductors, dielectrics and liquid suspensions. At JPL he has been
developing nanostructured materials and novel devices to demonstrate
sources at new wavelengths and with ultra-narrow spectral linewidths for
a wide range of sensor applications. He has been also involved in the
design, fabrication and characterization of novel photonic
optoelectronic circuits and high speed mode-locked semiconductor laser.
Of particular importance is his experience in the development of high
power, ultra narrow line width single frequency tunable diode lasers and
photonic components in the 1.7-2.1 m range for spectroscopy, LIDAR ,and
optical communication applications.

## Work plan

Our PIDDP and pre-Scout instrument development activities produced a
working prototype laser hygrometer weighing only 220 grams that was used
to demonstrate appropriate sensitivities for water at 1.87 m. As an
engineering unit (EU) the hygrometer form fit, size, mass is acceptable,
but no flight parts were used, nor were this spectrometer g-force
tested, vibration tested, nor therm-vac tested. Moreover, our laser
sources at 1.87 m were not flight qualified, and our EU prototype
electronics board based on a Motorolla HC-12 did not incorporate
flight-qualified (recommended) parts.

We propose here to conduct specific high-TRL-level activities centered
on producing a Protoflight Unit (PU) that will incorporate
flight-qualified lasers and electronics board. This Protoflight Unit
will be tested to high-g levels, therm-vac tested, and vibration tested
to flight qualification levels exceeding those of a flight unit. Our
proposed work plan is therefore divided into 5 categories:

1.  **Space qualification of 1.87 m TDLs**

2.  **Redesign, rebuild of electronics board** based on
    flight-qualifiable hardware.

3.  **Modifications to instrument software** based on electronics parts
    selected.

4.  **Build of Protoflight Unit** for testing.

5.  **Testing of Protoflight Unit**: Sensitivity analysis, Therm-vac
    testing, vibration and g-force testing.

6.  **Data Analysis and Reporting**.

Our work plan, schedule and costing follows these same categories
detailed below:

**1. Space Qualification of 1.87 m**

**TDLs**

For Mars applications, we first note that JPL DFB single-mode TDLs
operating at both 1.37 m and 2.03 m (for H2O and CO2 respectively) have
been previously qualified for use on the MVACS Mars Polar Lander.
However, for H2O measurements, the 1.87 m wavelength lasers are much
preferred, since they access stronger water lines, can also access
isotopic H2^18^O lines, AND CO2 lines for pressure measurements. The
qualification program proposed here for the 1.87 m devices should be
achievable since the device material is the same, and the wavelength
lies between that of 1.37 m and 2.03 m. **Furthermore, JPL (Co-I
Mansour) has already produced a few lasers at 1.87 m** that do scan over
the required region with good single mode power, and have been used (by
PI Webster) to demonstrate sensitivities for Mars applications.

**We propose to produce enough single-mode DFB TDLs at 1.87 m wavelength
to conduct a rigorous flight qualification program that will leave us
with 20 flight-qualified lasers for incorporation into selected Mars
Scout and Smart Lander missions, thereby significantly reducing the cost
to individual mission proposals.**

Reliability and packaging are often pushed aside in device development
despite the fact that they are crucial for mission success. The nature
of failures, and the ways in which the useful service life of a device
can be improved are very important. One of the objectives is to perform
a coordinated series of tests on Distributed Feedback (DFB) single mode
1.87 m wavelength lasers designed to determine the suitability of
integration of these lasers diodes into the MARS space flight
instruments program. JPL has extensive experience and expertise in
qualifying lasers for space flights, with fully supported laboratory
facilities capable of carrying out most tests listed. The table below
lists some of the tests to be conducted, and the approximate number of
lasers needed. We estimate that we will need to produce about 120
devices to leave 20 flight-qualified devices.

  ------------------------------------------- --------------- ------------
  Qualification Tests #lasers Destructive (X)                 

  Die Visual                                  All Devices     

  Internal visual inspection                                  

  Vacuum Bake                                                 

  Electrical/optical Tests                                    

  Temperature Cycling                                         

  Surge current                                               

  Thermal Impedance                                           

  Constant Acceleration                                       

  PIND                                                        

  High temp Reverse Bias                                      

  Burn in                                                     

  DC Electrical /Optical Test                                 

  Hermiticity (Gross Leak                                     

  Radiography                                                 

  External Visual Inspection                                  

  Temperture Charateristics                   3-5             x

  Sensitivity:optical feedback                3-5             

  Relative Intensity Noise                    3-5             

  Output Beam requirements                    3-5             

  Operating Voltage                           3-5             

  Reverse Bias BreakD Volt.                   3-5             x

  Storage Temperature                         3-5             x

  Operating Temp Range                        5-10            

  Survival Temperature Range                  3-5             x

  Thermal Shock                               3-5             

  Accelerated Life test                       10-15           x

  Destructive Physical Analysis               3-5             x

  Physical dimensions                         6               x

  Solderability                               3-5             x

  Resitance to solvent                        2-4             x

  Bond Strength                               3-5             x

  SEM                                         3-5             x

  Die Shear                                   3-5             x

  Intermittent Operation Life                 3-5             x

  Terminal Strength                           3-5             x

  Shock (Variable frequency)                  3-5             

  Steady State Life Test                      40-60           x

  Internal H2O Content                        3-5             x

  Neutron/ proton Irradiation                 3-5             

  Ionizing Radiation                          3-5             
  ------------------------------------------- --------------- ------------

**2. Redesign, rebuild of electronics board**

Under PIDDP funding, we have tried various laser drive techniques for cw
near-IR lasers. We have developed a laser control and signal processing
circuit based on the Motorola HC12 microcontroller. This has been
successfully applied to several protype instruments such as the Pascal
Mars Scout prototype. Developed under PIDDP and Code U funding, it
represents a great improvement over circuits used for Mars98 MVACS
spectrometers.

For the Mars Scout Missions, initial costing has identified an area of
concern regarding the flight qualification of parts currently in our
electronics board, especially the HC-12 microncontroller itself, and
also the SRAM chip. An estimate to build a flight qualified board is
about \$500,000 (!) Rather than rely on the expensive parts screening
approach, we propose to redesign our board using a parts list
pre-approved as flight hardware, thus increasing reliability and greatly
reducing the cost of this vital electronics board that has wide
applicability to several Mars Scout and Lander missions.

**3. Modifications to instrument software**

Software may have to be rewritten to accommodate new hardware parts
changes, since obtaining fully autonomous "on-the-fly" data processing
will require the development of robust pattern matching algorithms that
can identify spectral lines of interest and produce reliable,
high-precision isotope ratio measurements.

**4. Build of Protoflight Unit**

We will build a Protoflight Unit based on the Mars Scout Pascal design
shown below that would include upgrades to the optomechanical design
(more rigorous design to survive high-g force and Mars environment) in
preparation for the testing to be done in years 2 and 3.

![](media/image16.jpeg){width="3.1145833333333335in"
height="2.671527777777778in"}

The Protoflight Unit would incorporate one of the newly-qualified 1.87 m
lasers, and the newly built electronics board and instrument software.
We have much experience in building, testing, and flying laser
spectrometers for Earth and planetary applications. We have learned that
the instrument performance can only be fully characterized in a
full-prototype end-to-end testing, in a therm-vac environment, and we
propose to complete our task in this manner.

**5. Testing of Protoflight Unit**

The completed Protoflight Unit will be thoroughly tested for measurement
sensitivity analysis, Therm-vac testing, vibration and g-force testing
using existing service-facilities at JPL.

**6. Data Analysis and Reporting**.

We will analyze the engineering data and provide a detailed end-of-work
report that would be made available for consultation by any group
interested in proposing laser hygrometers for future Mars Missions.

##  Facilities

The instrument development will use several existing support facilities
and equipment at JPL owned by Webster's Atmospheric Laser Spectroscopy
Group, including: 3 instrument and spectroscopy laboratories; turbo
pumps, spectrometers, wave-meters, and vacuum equipment; computing
facilities (Linux workstations, numerous PC\'s); computer-aided-design
(CAD) for electronics and mechanical engineering. For laser production
and qualification testing, extensive clean-room facilities at JPL's
MicroDevices Laboratory will be used. For thermal-vacuum testing, flight
therm-vac chambers at JPL will be available for use of this project.

##  Schedule

The schedule is given in the schematic below, included with the cost
plan information.

END OF TECHNICAL SECTION

# Cost Plan Summary

![](media/image17.png){width="6.603472222222222in"
height="2.959722222222222in"}

Details of the proposed costs are included in the formal mandatory
material included in the appendix, and are presented here in summary for
ease of presentation. Laser fabrication will be done at JPL by Mansour
(Co-I) at 20% and a lab technician (50%), with \$40 K wafer and material
costs. The flight qualification testing will be done outside under
subcontract, supervised by Mansour, and with JPL reliability planning
involvement under flight instrument engineering.

BUDGET SUMMARY:

+---------------------------+-------------+-------------+-------------+
| Detail                    | **Year 1**  | **Year 2**  | **Year 3**  |
+---------------------------+-------------+-------------+-------------+
| **A. Labor with           |             |             |             |
| benefits**                |             |             |             |
|                           |             |             |             |
| PI Webster                |             |             |             |
|                           |             |             |             |
| CoI Mansour               |             |             |             |
|                           |             |             |             |
| Flight instrument         |             |             |             |
| Engineering               |             |             |             |
|                           |             |             |             |
| Technician                |             |             |             |
|                           |             |             |             |
| Software engineer         |             |             |             |
+---------------------------+-------------+-------------+-------------+
| **B. Travel**             |             |             |             |
+---------------------------+-------------+-------------+-------------+
| **C. Services**           |             |             |             |
|                           |             |             |             |
| Environmental test        |             |             |             |
| chamber                   |             |             |             |
|                           |             |             |             |
| Fabrication, machine &    |             |             |             |
| glass shops               |             |             |             |
+---------------------------+-------------+-------------+-------------+
| **D2. Contracts,          |             |             |             |
| subcontracts**            |             |             |             |
|                           |             |             |             |
| Flight qualification      |             |             |             |
| testing for lasers        |             |             |             |
+---------------------------+-------------+-------------+-------------+
| **D3. Procurements**      |             |             |             |
|                           |             |             |             |
| Electronics parts, test   |             |             |             |
| equipment                 |             |             |             |
|                           |             |             |             |
| Laser wafer, hardware     |             |             |             |
|                           |             |             |             |
| Optics, detector, vacuum  |             |             |             |
| parts, software           |             |             |             |
+---------------------------+-------------+-------------+-------------+
| **L. Fully-burdened total |             |             |             |
| costs**                   |             |             |             |
+---------------------------+-------------+-------------+-------------+

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68, 1393-1397, 1997.

**Owen, T**., "Titan", in The New Solar System, by Beatty and Chaikin
(Eds), 189-194, Cambridge University Press, (1990).

**Rahn, T**. and M. Wahlen. (1997). Science, 278, 1776.

**Rahn, T.,** Zhang, H., Wahlen, M. and Blake, G.A. (1998), Geophys.
Res. Lett., 25, 4489.

**Rothman, L.S**., C.P. Rinsland, A. Goldman, S.T. Massie, D.P. Edwards,
J.-M. Flaud, A. Perrin, C. Camy-Peyret, V. Dana, J.-Y. Mandin, J.
Schroeder, A. McCann, R.R. Gamache, R.B. Wattson, K. Yoshino, K.V.
Chance, K.W. Jucks, L.R. Brown, V. Nemtchinov, and P. Varanasi, The
HITRAN molecular spectroscopic database and HAWKS (HITRAN Atmospheric
Workstation): 1996 edition, *J. Quant. Spectrosc. Radiat. Transfer, 60*,
665-710, 1998.

**Samuelson, R.E**., W.C. Maguire, R.A. Hanel, V.G. Kunde, D.E.
Jennings, Y.L. Yung, and A.C. Aikin, 1983, CO~2~ on Titan. *J.*
*Geophys. Res*., 88, 8709-8715.

**Scott, D.C**., R.H. Herman, C.R. Webster, R.D. May, G. Flesch, and
W.S. Woodward, Aircraft Laser Infrared Absorption Spectrometer II
(ALIAS-II) for in-situ atmospheric measurements of N~2~O and CH~4~,
*Appl. Opt.*, (in press, 1999).

**Solderblom LA**, Chapter 17 "The Composition and Mineralogy of Martian
Surface from Spectroscopic Observations", in Mars, H.H. Kieffer et al.,
eds., University of Arizona, Tucson, 1992.

**Tacke M**, "New Developments and Applications of Tunable IR Lead Salt
Lasers", Infrared Phys. Technol., Vol. 36, No.1, pp 447-463,1995.

**Toth, R.A.,** Extensive measurements of H~2~^16^O line frequencies and
strengths: 5750 to 7965 cm-1, *Appl. Opt., 33*, 4851-4867, 1994.

**Webster, C.R**. and R.D. May, Simultaneous *in situ* measurements and
diurnal variations of NO, NO~2~, O~3~, *j*NO~2~, CH~4~, H~2~O, and CO~2~
in the 40 to 26 km region using an open path tunable diode laser
spectrometer, *J. Geophys. Res., 92*, 11931-11950, 1987.

**Webster, C.R**., R.T. Menzies, and E.D. Hinkley, Infrared laser
absorption: theory and applications, in *Laser Remote Chemical
Analysis*, Chapter 3, edited by R.M. Measures, John Wiley, New York,
1988.

**Webster, C.R.,** S.P. Sander, R, Beer, R.D. May, R.G. Knollenberg,
D.M. Hunten, and J. Ballard, Tunable diode laser IR spectrometer for in
situ measurements of the gas phase composition and particle size
distribution of Titan\'s atmosphere, *Appl. Opt.* *29*, 907-917, 1990.

**Webster, C.R**., R.D. May, R. Toumi, and J.A. Pyle, Active nitrogen
partitioning and the nighttime formation of N~2~O~5~ in the
stratosphere: simultaneous *in situ* measurements of NO, NO~2~, HNO~3~,
O~3~, and N~2~O using the BLISS diode laser spectrometer, *J. Geophys.
Res., 95*, 13851-13866, 1990.

**Webster, C.R**., R.D. May, C.A. Trimble, R.A. Chave, and J. Kendall,
Aircraft (ER-2) laser infrared absorption spectrometer (ALIAS) for
*in-situ* stratospheric measurements of HCl, N~2~O, CH~4~, NO~2~, and
HNO~3~, *Appl. Optics, 33*, 454-472, 1994.

**Webster CR**, G.J. Flesch, D.C. Scott, J. Swanson, R.D. May, W. S.
Woodward, C. Gmachl, F. Capasso, D.L. Sivco, J.N. Baillargeon, A.L.
Hutchinson, A.Y. Cho, "Quantum Cascade Laser Measurements of
Stratospheric Methane and Nitrous Oxide", Applied Optics, January 20
issue, 2001.

**Webster CR**, Sander SP, Beer R, May RD, Knollenberg RG,Hunten DM,
Ballard J,"Tunable Diode Laser IR Spectrometer for In Situ Measurements
of the Gas Phase Composition and Particle Size Distribution of Titan's
Atmosphere", Applied Optics 29, 907-917, 1990.

**Wennberg, P.O.,** R.C. Cohen, N.L. Hazen, L.B. Lapson, N.T. Allen,
T.F. Hamisco, J.F. Oliver, N.W. Lamham, J.N. Demusz, and J.G. Anderson
(1994), Rev. Sci. Instrum., 65, 1858-1876.

**Woodward, W.S**., and R.D. May, Flash-ROM-based multichannel
arbitrary-waveform generator, *Electronic Design*, April 19, 1999, pp.
86-88.

**Yung YL,** Allen M, and Pinto JP, "Photochemistry of the Atmosphere of
Titan: Comparison Between Model and Observations", The Astrophysical
Journal of Supplement Series, 55:465-506, 1984.

**Yung, Y.L., and W.B. DeMore**, "Photochemistry of the stratosphere of
Venus: Implications for atmospheric evolution", Icarus, 51, 199-247
(1982).

**Yung, Y.L.,** & W.B. DeMore, 1999, Photochemistry of Planetary
Atmospheres, Oxford University Press.

**Yung, Y.L.** and C.E. Miller. (1997), Science, 278, 1778.

**ANCILLARY INFORMATION**

ONE-PAGE RESUME

**DR. CHRISTOPHER R. WEBSTER**

Senior Research Scientist, Jet Propulsion Laboratory, Pasadena,
California 91109-8099

Tel: (818) 354-7478 Email: Chris.R.Webster@jpl.nasa.gov

**[EDUCATION:]{.underline}**

Ph.D. Molecular Spectroscopy, University of Bristol (UK), 1977, Prof. RN
Dixon, F.R.S.

B.Sc. (*Hons*) Chemical Physics, University of Reading (UK), 1974, Prof.
IM Mills.

**[PROFESSIONAL EXPERIENCE:]{.underline}**

2000-Present **Lead Scientist**, Atmospheric Chemistry Research Element,
JPL-Caltech

1990-Present **Senior Research Scientist**, JPL-Caltech

1992-93 **Visiting Full Professor**, Geological and Planetary Sciences,
Caltech

1988-90 **Section Manager**, Atmospheric and Oceanographic Sciences,
JPL-Caltech

1986-Present **Group Supervisor**, Atmospheric Laser Spectroscopy Group,
JPL-Caltech

1984-86 **Deputy Leader**, Laser Monitoring Group, JPL-Caltech

1981-84 **Senior Scientist** at Jet Propulsion Lab (JPL), California

1979-81 **Postdoc** with Prof. Richard N. Zare, Chemistry Department,
Stanford University, CA

1977-79 **Postdoc** with Dr. F Rostas, Royal Society Fellowship,
Paris-Observatory, France

1974-77 **Graduate Fellow**/ Teaching Assistant/ Math Tutor, University
of Bristol

**[TEACHING EXPERIENCE:]{.underline}**

1992-93 Spectroscopy and atmospheric chemistry: Caltech, CA

1980 Freshman Chemistry, Stanford University, CA

1974-77 TA in theoretical chemistry and mathematics, Bristol University,
England

**Graduate Student Advisor** to: Lyatt Jaegle (Ph.D.), Robert Herman
(Ph.D.), Elisabeth J. Moyer (Ph.D.)

**[PROFESSIONAL ACTIVITIES:]{.underline}**

-   **Principal Investigator** (2002-Present) (Code S) ASTID Laser
    Spectrometer for Biogenic Gases& Isotopes

-   **Co-Investigator** (2002-03) (Code S) Mars Scout Mission Laser
    Spectrometers (6)

-   **Co-Investigator** (2001-04) Code Y IIP CO~2~ Laser Absorption
    Spectrometer

-   **Principal Investigator** (2001) JPL (DRDF) Miniature CO~2~
    Airborne Laser Isotope Spectrometer (ALIS)

-   **Co-Investigator** (1999-2000) (Code U/HEDS) Mars Organic Detector
    (MOD)

-   **Team Leader** (1999-2001) (DRDF) Grand Challenge Biogenic Gases &
    Isotope Ratios for Detection of Life

-   **Principal Investigator** (1998-Present) JPL/NASA (Code S)
    Quantum-Cascade Laser Spectrometer for *in situ* measurement of
    atmospheric and evolved gases on Mars, Titan, Venus, & Europa.

-   **Principal Investigator** (1991-Present) NASA (Code Y) Aircraft
    Laser Infrared Absorption Spectrometer (ALIAS-II) for aircraft and
    balloon measurements of trace gases.

-   **Member**, NASA Aircraft Payloads Panel (Code Y) (1991-Present).

-   **Principal Investigator** (1988-Present) NASA (Code Y) Aircraft
    ER-2 Laser Infrared Absorption Spectrometer (ALIAS) for polar ozone
    depletion studies.

-   **Principal Investigator** (1997-99) JPL/NASA (Code S) CLARIS
    Absorption& Raman Mars Spectrometer.

-   **Principal Investigator** (1981-92) NASA (Code Y) Balloon-borne
    Laser In-Situ Sensor (BLISS) experiment for testing models of
    stratospheric photochemistry

-   **Principal Investigator** (1984-90) NASA/ESA/DRDF Titan Probe
    Infrared Laser Spectrometer

-   **Member**, NASA Balloon Working Group (1985-1988), Instrument
    Incubator Program (IIP) panel (1999)

-   **Principal Investigator** (1981-84), **Co-Investigator**
    (1984-Present) NASA Code Y Laser Laboratory spectroscopy Program.

-   **Technical Monitor**, several NASA-JPL SBIR technology
    developments.

-   **Reviewer** for NASA, NSF, NOAA, EPA, JGR, GRL, CPL, Phys Rev.

**[PUBLICATIONS, AWARDS, PATENTS:]{.underline}**

-   Refereed scientific journal publications (126)

-   NASA Certificates of Recognition; Tech Briefs (12); Patents (2)

-   NASA Exceptional Scientific Achievement Medal (1992)

-   NASA Group Achievement Award (1993-2001): AASE-II, SPADE, ASHOE,
    POLARIS, SOLVE

-   NASA Group Achievement Award (2000) Quantum Cascade Laser
    measurements

-   NASA Group Achievement Award (1997) Balloon/UAV Laser Spectrometer

-   NASA Group Achievement Award (1992) Aircraft Laser Infrared
    Absorption Spectrometer

-   NASA Group Achievement Award (1989) Balloon-borne Laser In-Situ
    Sensor

-   Royal Society of London Fellowship (1978-79).

***SELECTED JOURNAL PUBLICATIONS OF* CHRISTOPHER R. WEBSTER**

l\. \"Single Vibronic Level Fluorescence of CrO~2~Cl~2~ Excited by a
Tunable cw Dye Laser,\" R.N. Dixon and C.R. Webster, *J. Mol. Spec.
[62]{.underline}*, 27l-282 (l976).

2\. \"Lasers for Listening to Molecules,\" C.R. Webster, *New Scientist,
[73]{.underline}*, 383-385 (l977).

3\. \"Optoacoustic Spectroscopy with a Tunable cw Dye Laser: Forbidden
Transitions in Some Unstable Sulphur Compounds,\" R.N. Dixon, C.R.
Webster, and D.A. Haner, *Chem. Phys.* [22]{.underline}, l99-206 (l977).

6\. \"The Determination of the Electric Dipole Moment of H~2~CS in its
A,^1^A~2~ Excited State Using Dye Laser Electric Field Spectroscopy,\"
R.N. Dixon and C.R. Webster, *J. Mol. Spectros. [70]{.underline},*
3l4-322 (l978).

7\. \"The Dye Laser‑Induced Fluorescence and Emission Spectrum of the
KXe Molecule,\" C.R. Webster and F. Rostas, *Chem. Phys. Lett.
[59]{.underline}*, 57-61 (l978).

9\. \"Generation of UV Radiation from Intracavity Doubling of a
Single‑Mode Ring Dye Laser,\" C.R. Webster, L. Woste and R.N. Zare,
*Springer Series in Optical Sciences [26]{.underline},* l63-172 (l98l).

11\. \"Time‑Resolved Spectroscopy of RbXe Excimers Populated by
Superradiant Transitions,\" C.R. Webster and F. Rostas, *J. Phys. B
[14]{.underline},* 4497-4512 (1981).

12\. \"Narrow‑Band UV Radiation (250‑260 nm) by Intracavity Doubling a
Single‑Mode Ring Dye Laser,\" C.R. Webster, L. Woste and R.N. Zare,
*Opt. Comm. [35]{.underline},* 435-440 (1980).

13\. \"Photochemical Isotope Separation of Hg‑l96 by Reaction with
Hydrogen Halides,\" C.R. Webster and R.N. Zare, *J. Phys. Chem.
[35]{.underline},* l302-1305 (l98l).

14\. \"Laser Optogalvanic Effect in a Pure Iodine Discharge,\" C.T.
Rettner, C.R. Webster and R.N. Zare, *J. Phys. Chem. [85]{.underline},*
ll05-1107 (l98l).

16\. \"Determination of the Electric Dipole Moment of the HSO Radical in
its X^2^A^\"^(000) and A^2^A^\'^(003) Electronic States,\" C.R. Webster,
P.J. Brucat and R.N. Zare, *J. Mol. Spectros. [92]{.underline},* 184-202
(l982).

17\. \"Optogalvanic Wavelength Calibration for Laser Monitoring of
Reactive Atmospheric Species,\" C.R. Webster, *Appl. Opt.
[21]{.underline},* 2298-2300 (1982).

18\. \"Laser Optogalvanic Photodetachment Spectroscopy: A New Technique
for Studying Photodetachment Thresholds with Application to I^-^\", C.R.
Webster, I.S. McDermid and C.T. Rettner, *J. Chem Phys.
[78]{.underline},* 646-651 (1983).

19\. \"Infrared Laser Optogalvanic Spectroscopy of Molecules\", C.R.
Webster and R.T. Menzies, *J. Chem. Phys. [78]{.underline},* 2121-2128
(1983).

20\. \"Laboratory Simulation of Tunable Diode Laser Remote Measurement
of Atmospheric Gases Using Topographic Targets\", C.R. Webster and W.B.
Grant, *Apple. Opt. [22]{.underline},* 1952-1954 (1983).

21\. \"Laser Optogalvanic Spectroscopy of Molecules,\" C.R. Webster and
C.T. Rettner, *Laser Focus [19]{.underline}*, 41-48 (1983).

23\. \"Balloon‑borne Diode Laser Absorption Spectrometer for
Measurements of Stratospheric Trace Species,\" R.T. Menzies, C.R.
Webster and E.D. Hinkley, *Appl. Opt. [22]{.underline},* 2655-2664
(1983).

25\. \"Optogalvanic Photodetachment Spectroscopy,\" I.S. McDermid and
C.R. Webster, [J. de Physique 44,]{.underline} C7‑461-466 (1983).

26\. \"Infrared Optogalvanic Spectroscopy of NH~3~ and NO~2~,\" C.R.
Webster and

R.T. Menzies, *J. de Physique [44]{.underline},* C7‑429-437 (1983).

28\. \"Microprocessor‑Controlled Laser Tracker for Atmospheric
Sensing,\" R.A. Johnson, C.R. Webster, and R.T. Menzies,\" *Rev. Sci.
Instr. [56]{.underline},* 547-556 (1985).

30\. \"Tunable Diode Laser Stark Modulation Spectroscopy for Rotational
Assignment of the HNO~3~ 7.5 m Band,\" C.R. Webster, R.D. May, and M.R.
Gunson, *Chem. Phys. Lett. [121]{.underline},* 429-436 (1985).

31\. \"Infrared Laser Absorption: Theory and Applications\", C.R.
Webster, R.T. Menzies, E.D. Hinkley, *[Laser Remote Chemical
Analysis]{.underline},* Ch. 3, Ed. R. M. Measures, (1988).

34\. \"Stratospheric Composition Measurements of Earth and Titan Using
High‑ Resolution Tunable Diode Laser Spectroscopy\", C.R. Webster, *J.
Quant. Spectros. Radiat. Trans. [40]{.underline},* 239-248, (1988).

41\. \"Tunable Diode Laser Infrared Spectrometer for In-situ
Measurements of the Gas Phase Composition and Particle Size Distribution
of Titan\'s Atmosphere\", C.R. Webster, S.P. Sander, R. Beer, R.D. May,
R.G. Knollenberg, D.M. Hunten, and J. Ballard, *Appl. Opt.
[29]{.underline},* 907-917, (1990).

42\. \"Active Nitrogen Partitioning and the Nighttime Formation of
N~2~O~5~ in the Stratosphere: Simultaneous In-situ Measurements of NO,
NO~2~, HNO~3~, O~3~, N~2~O, and jNO~2~ Using the BLISS Diode Laser
Spectrometer\", C. R. Webster, R. D. May, R. Toumi, and J. Pyle, *J.
Geophys. Res. [95]{.underline},* 13,851-13,866, (1990).

48\. \"In-Situ Stratospheric Measurements of CH~4~, ^13^CH~4~, N~2~O,
and OC^18^O Using the BLISS Tunable Diode Laser Spectrometer\", C.R.
Webster and R.D. May, *Geophys. Res. Letters [19]{.underline},* 45-48,
(1992).

49\. \"Aircraft (ER-2) Laser Infrared Absorption Spectrometer (ALIAS)
for In-situ Stratospheric Measurements of HCl, N~2~O, CH~4~, NO~2~, and
HNO~3~\", C.R. Webster, R.D. May, C.A. Trimble, R.G. Chave and J.
Kendall, *Applied Optics, [33]{.underline}*, 454-472, 1994.

51\. \"Chlorine Chemistry on Polar Stratospheric Cloud Particles in the
Arctic Winter\", C.R. Webster, R.D. May, D.W. Toohey, L.M. Avallone,
J.G. Anderson, P. Newman, L. Lait, M.R. Schoeberl, J.W. Elkins and K.R.
Chan, *Science [261]{.underline},* 1130-1134 (1993).

58\. \"Balloon Profiles of Stratospheric NO~2~ and HNO~3~ for Testing
the Heterogeneous Hydrolysis of N~2~O~5~ on Sulfate Aerosols\", C.R.
Webster, R.D. May, M. Allen, L. Jaeglé, *Geophys. Res. Letters
[21]{.underline},* 53-56, 1994.

81\. "Evolution of HCl Concentrations in the Lower Stratosphere from
1991 to 1996 Following the Eruption of Mt. Pinatubo", C.R. Webster, R.D.
May, H.A. Michelsen, D.C. Scott, J.C. Wilson, H.H. Jonsson, C.A. Brock,
J.E. Dye, D. Baumgardner, R.M. Stimpfle, J.P. Koplow, J.J. Margitan,
M.H. Proffitt, L. Jaeglé, R.L. Herman, H. Hu, G.J. Flesch, M
Loewenstein, accepted, *Geophys. Res. Lett*., 1998.

85. \"*In situ* measurements of CO in the upper troposphere and lower
    stratosphere from the ER-2 aircraft", R.L. Herman, C.R. Webster,
    R.D. May, D.C. Scott, H. Hu, P.O Wennberg, E.J. Hintsa, T.P. Bui,
    and Y.L. Yung, in preparation for *J. Geophys. Res.,* 1998.

107\. "Quantum cascade laser measurements of stratospheric methane
(CH~4~) and nitrous oxide (N~2~O)", C.R. Webster, G.J. Flesch, D.C.
Scott, J. Swanson, R.D. May, W.S. Woodward, C. Gmachl, F. Capasso, D.L.
Sivco, J.N. Baillargeon, A.L. Hutchinson, A.Y. Cho, submitted to *Appl.
Opt.*, December 1999.

# RESUME Dr. Kamjou Mansour

**EDUCATION** Ph.D. in Quantum Electronics *(1990)*, Center for Res.&
Educ. in Optics(CREOL), Orlando, FL

M.Sc. in Physics *(1986)*, Center for Applied Quantum Electronics (CAQE)
UNT, Denton,TX

M.S. in Electrical Engineering (1984) Southern Methodist University,
Dallas, TX.

B.S. in Electrical Engineering and Physics *(1983)*, Southern Methodist
University , Dallas, TX.

**EXPERIENCE**

***2001- Present**,* Senior Member of engineering Staff in Infrared
Focal Planes and Photonic Technologies, microDevices Laboratory, Jet
Propulsion Laboratory, Pasadena, CA.

Developing nanostructured materials and novel devices to demonstrate
sources at new wavelengths and with ultra-narrow spectral linewidths for
a wide range of sensor and remote sensing applications. Developing
advanced electron beam lithography techniques to improve the grating
design of near-IR (1-2µm) distributed feedback (DFB) lasers for more
precise tuning to molecular absorption lines and to reduce spectral
linewidths to below 100kHz for LIDAR and interferometric space science
applications*.* Developing microcavity structures based on high-Q ring
and two dimensional (2D) photonic bandgap structures,with the goal of
producing improved chemical and biological sensors for life support and
planetary science. Developing advanced photonics and integrated
opto-electronics components for different NASA and DOD applications.

***1999- 2001**,* Member of Technical Staff, Photonic Technology Group,
Jet Propulsion Laboratory, Pasadena, CA.

Designed and developed high power, single frequency InGaAs strained
layer tunable semiconductor laser in the 1.8-2.1 µm range. Worked
extensively on design and fabrication of high speed transmitters
(mode-locked lasers) for high speed bit parallel dense division
multiplexing links. Fabricated and characterized low loss InP passive
waveguides for optoelectronic applications. Worked on design and
integration of high performance EO-polymers as passive and active
elements onto III-V semiconductor devices for optoelectronic
applications. In charge of testing and characterization of
optoelectronic components for JPL's photonic group

***1997 -- 1999**,* Associate Scientist, California Institute of
Technology, Pasadena, CA

Performed research and development on polymeric thin films of newly
developed two-photon absorbing molecules and conjugated planar
macrocyclic molecules for photonic applications.

***1995 -- 1997**,* Visiting Assistant Research Faculty, CREOL (center
for Research and Education in Optics and Lasers), Orlando, FL

Conducted research on the optical characteristics of liquid crystaline
fibers arrays doped with organic molecules for photonic switching
applications. Participated in the development of a beam propagation
program. Used to simulate the photonic switching and limiting processes
in reverse saturable absorbing molecules for optical limiting devices

**1991-1995**, Member of Technical Staff (Post-doctoral Position),
California Institute of Technology, Jet Propulsion Laboratory, Pasadena,
CA

Designed, fabricated and demonstrated the first multi-plate solid state
optical switching/limiting devices for senors and eye protection based
on strongly saturated excited state absortption in conjugated planar
macrocyclic molecules. Participated in the development of of thin-film
ferroelectric memory chips. Participated in the development of two
dimensional micro-lense array for flat docking target assembly for space
applications.

Demonstrated that HIFS is an excellent tool for assessing the elemental
composition of meterorites and planets.

**1990-1991**, Post-doctoral Research Scientist, CREOL, Orlando, FL

Performed research on nonlinear optical and ultra-fast electronic
properties of semiconductor materials.

## PUBLICATIONS Publications include over 38 journal and refereed and proceedings. 

**CURRENT AND PENDING RESEARCH SUPPORT**

**Dr. Christopher R. Webster**

**Jet Propulsion Laboratory (JPL)**

**A. CURRENT SUPPORT :**

1\. Source of Support: NASA's Upper Atmospheric Research Program (UARP)

2\. Project Title Aircraft measurements of the ALIAS instrument: PI
Webster

3\. Award Amount

4\. Period of Award ongoing

5\. Person-months 6.0 (50%)

1\. Source of Support: NASA's Radiation Sciences Program (RSP)

2\. Project Title Aircraft measurements for CRYSTAL-FACE: PI Webster

3\. Award Amount

4\. Period of Award ongoing

5\. Person-months 1.2 (10%)

1\. Source of Support: NASA's Planetary Instrument Definition and
Development Program (PIDDP)

2\. Project Title Tunable QC Laser Spectrometer : PI Webster

3\. Award Amount

4\. Period of Award FY01-FY02

5\. Person-months 2.4 (20%)

1\. Source of support: NASA Astrobiology Science and Technology
Instrument Development (ASTID) Program: PI Webster

2\. Project Title: Identifying Chemical Signatures of Life from *in
situ* Laser Spectroscopy of Biogenic Gases and Isotope Ratios on Mars,
Titan, and Europa

PI Webster

3\. Award Amount

4\. Period of Award FY02-FY03

5\. Person-months 1.2 (10%)

**B. PENDING PROPOSALS:**

This one.

**CURRENT AND PENDING RESEARCH SUPPORT**

**Dr. Kamjou Mansour**

**Jet Propulsion Laboratory (JPL)**

**A. CURRENT SUPPORT :**

1\. Source of Support: NASA Code R

2\. Project Title Advanced Semiconductor Lasers and Photonic Integrated
Circuits:

> PI Mansour

3\. Award Amount

4\. Period of Award 9/01/1999-9/01/2002, Last year

5\. Person-months 4 (35%)

1\. Source of Support: NASA Code Y

2\. Project Title Advanced optical heterodyne receiver development for
Coherent Doppler Wind Lidar:PI Tratt

3\. Award Amount

4\. Period of Award

5\. Person-months 4 (35%)

1\. Source of Support: NASA-JPL Director's Research and Development Fund

Title Single mode semiconductor lasers for LIDAR and other NASA
Applications:

> PI Mansour

3\. Award Amount

4\. Period of Award 3/02/02-9/02/03

5\. Person-months 1.2 (10%)

> Source of support: Army Research Laboratory Collaborative Technology
> Alliance Program (ARL-ASCTA)

2\. Project Title: 2-5 m Mid-Infrared Laser Development: PI Mansour

3\. Award Amount

4\. Period of Award 6/01/2001-6/01/2007

5\. Person-months 2 (15%)

**B. PENDING PROPOSALS:**

none

CO-INVESTIGATOR/COLLABORATOR COMMITMENT

Tunable Laser Spectrometers for Atmospheric and Sub-surface Gas
Measurements on Mars Scout and Smart Lander Missions

# Principal Investigator: Dr. Christopher R. Webster

Jet Propulsion Laboratory

California Institute of Technology

**Co-Investigator:** \_\_\_\_\_\_\_\_\_\_\_\_\_\_\_\_\_\_\_\_\_

> Dr. Kamjou Mansour
>
> Jet Propulsion Laboratory

California Institute of Technology

######## We acknowledge that we are identified by name as Co-Investigators to the investigation entitled "Tunable Laser Spectrometers for Atmospheric and Sub-surface Gas Measurements on Mars Scout and Smart Lander Missions". This proposal is submitted by Dr. C.R. Webster as Principal Investigator to the NRA-02-OSS-01-MIDP Mars Instrument Development Project (MIDP), and we intend to carry out all responsibilities identified for us in the proposal. We understand that the extent and justification of our participation as stated in this proposal will be evaluated during peer review in determining the merits of this proposal.