10 th International Planetary Probe Workshop San Jose, CA - June 2013 1 Tim Brockwell, Hunter Waite...

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The MAss Spectrometer for Planetary EXploration (MASPEX)

10th International Planetary Probe Workshop

San Jose, CA - June 2013

Tim Brockwell, Hunter Waite and Mark Libardoni

Department of Space Science and EngineeringSouthwest Research Institute, San Antonio, TX

Libardoni, et.al (2013)2

Roadmap

• Introduction to MASPEX

• Operational and Performance Characteristics

• Mating MASPEX with GC×GC

• Proposed Flight Missions

• Questions and Discussions


MASPEX is a next generation spectrometer with significantly improved performance over existing instruments

Areas of enhanced performance include:◦ Extended mass range (>1000 amu) for heavy organic molecules◦ Enhanced mass resolution (>30,000 M/dM) for critical isotopes◦ Enhanced dynamic range (109 in a 1s period) for high S/N◦ Improved sensitivity (better than 1ppt with cryo) for rare noble gases◦ High throughput (>5000 samples/s) for rapid descent probes

MASPEX Overview

Libardoni, et.al (2013)

MASPEX Built on MB-TOF BackboneAnalyzer development has mainly concentrated on: - Improved mechanical tolerance of the ion optics.- Titanium and ceramic construction of mirror elements and strong back.- Mass relieving of the major portions of the ion optics.- Vibration testing of the analyzer with mass models of the ion source

and detector.

Generation-1

Generation-3

Generation-2 with orthogonal ion source


Numerical simulations of ion trajectories showing focusing of multi-bounce ion packets.

Third generation MBTOF has successfully undergone vacuum and vibration tests.

R(N) = NTo/2(Dt+NdT)40cm & < 8kg

Development of Multi-Bounce Time of Flight (MBTOF)


CATHODE HEATING [ 0-10 V @0.65 A ]

CATHODE BIAS [-150 -> +15 V ]

ACCELERATION - 1 [NEG. 200 - 1000 V ]

ACCELERATION - 2 [NEG. 1500 - 3000 V ]

SOURCE SHIELD [NEG. 1500 - 2000 V ]

SOURCE FOCUS [NEG. 1500 - 5000 V ] SOURCE EXIT[NEG. 500 - 2000 V ]

MIRROR-1 DIVIDER [NEG. 0 - 500 V ]

MIRROR-1 [ PULSED ]

+500 V

0PUSHER [ PULSED ]

0

+500 V

+350 V

0EXTR. [ PULSED ]

BUNCHERS (1,2) [NEG. 500 - 5000 V ]

MCP DET. [NEG. 0 - 4500 V ]

DRIFT ENERGY [NEG. 1500 - 3000 V ]

0

+500 V

MIRROR-2 [ PULSED ]

MIRROR (1,2) DIVIDER [NEG. 1500 - 2500 V ]

MIRROR-2 DIVIDER[NEG. 0 - 500 V]

MBTOF ION OPTICS

Ion SourceDrift tube

Ion Bunchersused to modify the focal lengths of the mirrors for stable ion motion

Reflectron-1

Reflectron-2

Detector


Bulk Resistive Ceramic Mirrors

Conventional Lab Reflectron

Resistivemirrors

Test fit. Ceramics when fired turn black


Dual Pickoff Detector Development Fast < 2 ns FwHM response time Low timing jitter Can be baked to 300 degree C High dynamic range >10^5 Fast recovery time ( no current “sag”) after large

multiple ion events. Rugged Tested in a radiation environment

Original Concept

Two-stage dual pickoff detector

Magnet

B


sign

al (c

ount

s)

HD H3

CH3D

Survey Resolution

High Resolution

3He

13CH4

Low Resolution

13CH2D

m/∆m = 513m/∆m = 1800

m/∆m = 10,200m/∆m = 5968

MBTOF Performance

Simulations demonstrate resolution using line shapes obtained in the lab. Performance allows MBTOF to separate isotopologues of CH4 and H2 in order to determine hydrogen and helium abundances.


MBTOF Performance (Survey Mode)

Survey Mode Tiles(6000 resolution)

Window

number

Low mass

High mass

1 2.0 2.8

2 2.8 4.0

3 4.0 5.7

4 5.7 8.0

5 8.0 11.4

6 11.4 16.1

7 16.1 22.8

8 22.8 32.3

9 32.3 45.8

10 45.8 64.8

11 64.8 91.7

12 91.7 129.9

13 129.9 183.9

14 183.9 260.4

15 260.4 368.7

16 368.7 522.1

17 522.1 739.3

Lab data


MBTOF Performance (High-Resolution Mode)

M/DM = 3000

Separation of CO from N2 M/DM = 13,500


Resolution◦ D/H ratio in water is important for formation conditions of

the Galilean satellites (H217O and HD

16O : 12,283)

Sensitivity◦ Noble gases and trace organic species provide information

about the formation and habitability. Using a cryo-trap in addition to a storage source enables ppb level organic materials to be measured

Spatial Resolution◦ The requirement to observe spatial features as small as

400km of orbital track need high scan rates to collect the data. MASPEX can operate at 5kHz across full mass range

Performance Overview


The versatility of the instrument allows application adaptability for multiple missions:

◦ Europa Jupiter System Mission (EJSM)

◦ Jupiter Icy Moons Explorer Missions (JUICE)

Stand Alone Missions for MASPEX


MACE – Mars Lander ProposalGC×GC

Pyrolysis

TOFMS


Comprehensive Two-Dimensional Gas Chromatography (GC×GC)

0 50000 100000 150000 200000 250000 0 50000 100000 150000 200000 250000

•1st Dimension Column-Long (non-polar)•2nd Dimension Column - Short (polar)•Connected via a Modulator

Benefits•Large available peak capacity• Increased detectibility•Structured chromatograms

1D Text 2D Plot 3D View


Commercial Modulator Performance

C8 C10 C12 C14 C16 C18 C20

0.7415

0.9415

1.1415

1.34151st Time (s)

2nd Time (s)

3

57


The Modulator is the heart of a GC×GC◦ Requires LN2 or other media

◦ Requires large amount of Carrier Gas (valve based)

Goal is to build a modulator that requires no cryogenic media, requires no external compressed gas and can effectively modulate from nC1 – nC100

GC×GC Hardware Development


Resistive Heating Modulator

Modulator Housing

Insulating Sleeve

O-ring

Modulator Support

Retaining Cap

Thermal Modulator

Cooling Lines

Libardoni, et al. - 2004


2-Stage Resistive Heating• Two-Stage modulator evaluation• Qualitative and quantitative studies• Two-Stage will eliminate sweep

through



2-Stage Resistive Heating

Time (min)

Tim

e (s

)C6 – C20 Alkane mixture

0 5 10 15 20 25 30 35

W1/2 – 32 ms



2-Stage Resistive Heating

Isometric View of Thermal Modulator

Two-Stage Modulator Design

Cross Section of Modulator

SMARTMod Modulator AssemblyPower Supply and Electronics

Thermodynamic Modeling

z

l

ne

nL

z

Ka

ILTT

tC

Kln

n

oddno

P

cos

214

21

8

2

21

_

2

2

22


GC×GC-MBTOF


GC-MS Performance


GC×GC-TOF of Murchison


GC×GC-TOF of Oreugil


Tim

e (

sec)

pyrrole

methyl pyrrole

dimethyl pyrrole

trimethyl pyrrole

tetramethyl pyrrole

GC×GC-TOF of Tholin sample

Time (sec)


Multi-bed Trap GC×GC-MS

Experimental time (seconds)

-450 0

-400

-300

-200

-100

500

100

200

300

400

1000

600

700

800

900

1100

1200

1300

Gas Dynamics

Trap Heating

GC Oven Dynamics

Tem

pera

ture

(°C

)

100

220

190

160

130

70

40

250“Injection”

Sample loading GC Run

1 second heating pulse


Laser Thermal Desorption

2198

1399

0600

2798

1999

01200

50000

100000

150000

200000

250000

300000

350000

400000

450000

1st Time (s)2nd Time (s)

TIC

2198

1399

0600

2798

1999

01200

50000

75000

100000

125000

150000

175000

200000

225000

1st Time (s)2nd Time (s)

TIC

(a)

(d)

(b)

(e)

(c)

(f)


MASPEX Summary

Together these advanced capabilities will provide future missions with enhanced science return not previously available

Some examples:◦ PRIME: Exceptional resolution and sensitivity will allow unique

determinations of noble gas isotopic ratios and ratios of stable isotopes in major volatiles, which are key to understanding solar system formation.

◦ Saturn Probe: High sample throughput provides precise measurements of noble gases and key volatiles during rapid descent. Again, these are critical for understanding solar system evolution.

◦ Mars 2020 Rover: Mating of MASPEX with GC×GC will deliver unparallel results for the determination of organics

◦ Return to Titan and Enceladus : Identity of large organic molecules and chiral characteristics used to identify biological activity and enable the search for life.


Southwest Research Internal Research Funding (Grant #R8223)

NSF, NASA, JPL – Director’s Funding

University of Michigan◦ Department of Atmospheric Oceanic and Space Science◦ Department of Chemistry

• Tim Brockwell• Hunter Waite• Mark Libardoni• Greg Miller• Keith Pickens

• Dave Young• Ryan Blase

Acknowledgements

10 th International Planetary Probe Workshop San Jose, CA - June 2013 1 Tim Brockwell, Hunter Waite...

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