J-P. Bibring

N. Thomas

F. Westall

M. Berthé

V. Leroi

on behalf of

the entire

MicrOmega team

Phyllo workshop, Paris, October22, 2008

MicrOmega / ExoMars

MicrOmega / ExoMars

MicrOmega is a set of two microscopes (VIS and IR) designed to analyze the samples prior to and after having been processed, to

● characterize in a purely non destructive manner their structure, morphology and composition (mineralogical, molecular) at a microscopic scale, and

● enable the selection of phases of interest for their further analyses.

Phyllo workshop, Paris, October22, 2008

MicrOmega / ExoMars

Amongst the goals:

● to identify, at a grain scale, small carbonates within phyllosilicates, fully characterized, to derive the pCO2 as a record of the environment at the time water was liquid at the Mars surface;

● to identify potential C-rich phases coupled to these phases, to be further analyzed by other investigations.

Phyllo workshop, Paris, October22, 2008

MicrOmega / ExoMars

MicrOmega / VIS will observe the preprocessed (drilled) core samples, with the molecular complement provided by Raman;

MicrOmega / IR will image and characterize the processed (crushed) samples, in conjunction with XRD and MOMA.

Phyllo workshop, Paris, October22, 2008

MicrOmega / V

Raman

MicrOmega / V

Raman

drilled core sample

Current Baseline

Front view Top view

MicrOmega / V

Raman

MicrOmega / V

Raman

MicrOmega / VIS

MicrOmega / VIS

1. 2k x 2k CCD, 4 µm spatial sampling

2. 12 color LEDs

3. White LEDs + polarizers

Front view Top viewMicrOmega / IR

MicrOmega / IRMicrOmega / IR

samplesample

white

sourceAOTF

IR

monochrom

atic

MicrOmega / IR

samplesample

LED

visible

sources

LED

visible

sources

white

sourceAOTF

IR

monochrom

atic mon

ochr

omat

ic

MicrOmega / IR

samplesample

Detector assembly with TEC

Imaging

optics

Imaging

optics

LED

visible

sources

LED

visible

sources

white

sourceAOTF

IR

monochrom

atic mon

ochr

omat

ic

MicrOmega / IR

samplesample

Detector assembly with TEC

Imaging

optics

Imaging

optics

LED

visible

sources

LED

visible

sources

white

sourceAOTF

IR

monochrom

atic mon

ochr

omat

ic

MicrOmega / IR

MicrOmega / IR

samplesample

white

sourceAOTF

IR

monochrom

atic

MicrOmega / IR

samplesample

white

sourceAOTF

IR

monochrom

atic

For a given RF frequency, the sample is illuminated

with a monochromatic light. By scanning the frequency,

one builds a 3 D (x,y,λ) hyperspectral image cube

MicrOmega IR, AOTF

MicrOmega IR, AOTF

For a given RF frequency, the sample is illuminated

with a monochromatic light. By scanning the frequency,

one builds a 3 D (x,y,λ) hyperspectral image cube

0.0E+00

5.0E+12

1.0E+13

1.5E+13

2.0E+13

2.5E+13

0.85 1.05 1.25 1.45 1.65Lambda (µm)

Flu

x (p

h/c

m²/

nm

)

52 MHz

60 MHz

70 MHz

80 MHz

90 MHz

100 MHz

RF ON : only one optical wavelength is transmitted

All other optical wavelength are trapped in the crystal

AOTF Output spectra at various RF settings

MicrOmega IR, AOTF

samplesample

Detector assembly with TEC

Imaging

optics

Imaging

optics

LED

visible

sources

LED

visible

sources

white

sourceAOTF

IR

monochrom

atic mon

ochr

omat

ic

The focal play is an integrated hermetic package

including a 256x256 IR (HgCdTe) matrix mounted onto a dedicated TEC to provide its operational temperature (~190 K)

MicrOmega Breadboard IR detector

Focal plane:

256 x 320 pixels: 30 µm x 30 µm

Responsivity: 0.8 µm à 2.6 µm

Pixel capacity > 1.3 106 e-

4 Readout lines

Up to 30 MHz out freq.

MicrOmega IR breadboard

illum

inat

ion

sample

cold finger

electronics

detector

Radiator Detector

AOTF

Imaging Optics

Sample

Baffle

MicrOmega IR breadboard

MicrOmega IR: smectite sample

smectite samplesize = 6 x 7.5 mm²

MicrOmega spectrumbining 3X3 (69 x 69 µm2)

MicrOmega spectrumbining 3X3 (69 x 69 µm2)

lab (LPG) spectrum4 cm² size sample

Nontronite + Kieserite mixture Sample

MicrOmega Spectrumbinning 3X3

USGS Reference

NONTRONITE KIESERITE

MicrOmega / ExoMars

MicrOmega is ready to pass (in two weeks) its PDR successfully, and could have been delivered for a 2013 launch.

The unfortunate shift decided last week by ESA to be endorsed by the C/MIN late November might lead to a consolidated mission, towards a robust partnership in the upcoming joined missions.

Phyllo workshop, Paris, October22, 2008