J-P. Bibring N. Thomas F. Westall M. Berthé V. Leroi on behalf of the entire MicrOmega team
description
Transcript of J-P. Bibring N. Thomas F. Westall M. Berthé V. Leroi on behalf of the entire MicrOmega team
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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
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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
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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
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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
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MicrOmega / V
Raman
MicrOmega / V
Raman
drilled core sample
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Current Baseline
Front view Top view
MicrOmega / V
Raman
MicrOmega / V
Raman
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MicrOmega / VIS
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MicrOmega / VIS
1. 2k x 2k CCD, 4 µm spatial sampling
2. 12 color LEDs
3. White LEDs + polarizers
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Front view Top viewMicrOmega / IR
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MicrOmega / IRMicrOmega / IR
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samplesample
white
sourceAOTF
IR
monochrom
atic
MicrOmega / IR
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samplesample
LED
visible
sources
LED
visible
sources
white
sourceAOTF
IR
monochrom
atic mon
ochr
omat
ic
MicrOmega / IR
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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
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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
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samplesample
white
sourceAOTF
IR
monochrom
atic
MicrOmega / IR
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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
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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
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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
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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)
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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.
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MicrOmega IR breadboard
illum
inat
ion
sample
cold finger
electronics
detector
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Radiator Detector
AOTF
Imaging Optics
Sample
Baffle
MicrOmega IR breadboard
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MicrOmega IR: smectite sample
smectite samplesize = 6 x 7.5 mm²
MicrOmega spectrumbining 3X3 (69 x 69 µm2)
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MicrOmega spectrumbining 3X3 (69 x 69 µm2)
lab (LPG) spectrum4 cm² size sample
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Nontronite + Kieserite mixture Sample
MicrOmega Spectrumbinning 3X3
USGS Reference
NONTRONITE KIESERITE
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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