picam sur mars express: ( putain ,)10 ans !
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PICAM sur Mars Express: ( putain ,)10 ans !. F. Montmessin et l’équipe SPICAM au LATMOS France : LATMOS, LMD, IAS Russia : IKI Belgium : IASB, Univ. Liège U.S .: SwRI , Univ. of Arizona. L’équipe SPICAM. - PowerPoint PPT PresentationTRANSCRIPT
PICAM sur Mars Express: (putain,)10 ans !
F. Montmessin et l’équipe SPICAM au LATMOS France: LATMOS, LMD, IASRussia: IKIBelgium: IASB, Univ. LiègeU.S.: SwRI, Univ. of Arizona
L’équipe SPICAM• France (LATMOS, LMD, IAS):
F. Montmessin (PI), J.-L. Bertaux (ex-PI), A. Reberac, G. Lacombe, N. Chapron, F. Lefèvre, J.-Y. Chaufray, F. Leblanc, F. Forget, S. Lebonnois, E. Quémerais, L. Maltagliati, A. Määttänen, C. Listowski, B. Gondet
• Russie (IKI) : O. Korablev (CoPI), A. Fedorova, A. Trokhimovsky, A.V. Rodin
• Belgique (IASB, Univ. de Liège) : A.-C. Vandaele, N. Mateshvili, Y. Willamme, J.-C. Gérard, A. Stiepen, D. Fussen, C. Simon
• U.S. (LPL): B. Sandel, A. Stern
• Collaborations: P. Withers, S. Bougher, T. McDunn, N. Schneider, etc.
SPICAM on Mars 96: 40 kg
SPICAM « light » on Mars Express:4.8 kg
UV Grating Imaging
Spectrometer (4 kg)
IR AOTF Spectromete
r (0.8 kg) SPICAM IR solar (23 kg)
SPICAM UV/Vis étoile (17 kg)
Schéma Optique
Nadirdirection
M
Ø30
Light trap
Telescope
FOV diaphragm
AOTF
IR detectors
Sundirection
Nadirdirection
40x40
Parabolicmirror Slit
Grating
Intensifier
CCD
M
FibreUV
IR
Bertaux et al. (JGR,2006)
Instrument développé au LATMOS (ex-Service d’aéronomie).
Le même instrument vole sur la mission ESA Venus Express.
Bande spectrale / Résolution:UV: 118-320 nm R=150 IR: 1.0-1.7 µm
R=1300
Modes d’observation : • Occultation (étoile /
soleil)• Nadir• Limbe
UV Spectrometer -3
kg-
IR Spectrometer -
800 g-
Light IN OUT
RF IN
TeO2 crystal
Transducer
Mars Express spacecraft
orbit
MARS
NADIR : l’instrument vise dans la direction du centre de la planète = mesure du spectre de la lumière solaire réfléchie par la surface et l’atmosphère Colonne d’abondance des
constituants CO2, O3, H2O responsables des absorptions observées
Mars Express spacecraft
orbit
MARS
LIMBE : L’instrument vise le “bord”de la planète = mesure du spectre des émissions et diffusion du spectre solaire par l’atmosphère Profil vertical en altitude des émissions aéronomiques et des poussières
Spectrum of the star :
outside the atmosphere
through the atmosphere
star
Mars Express spacecraft
orbit
MARS
Line of sight
OCCULTATION : L’instrument vise une étoile à travers l’atmosphère de la planète = mesure du spectre de l’étoile à travers et hors atmosphère profils verticaux des constituants responsables des absorptions observées (CO2, O3, O2, CO, H2O, aérosols)
NO δ C2 – X2
NO γ A2 + – X2
H Lyα
Spectre UV (côté nuit)
Bertaux et al. (Science, 2005)
O21Dg
The oxygen O21Dg emission line
at 1.27 mm is produced by UV dissociation of O3
H2O ice
CO2 ice
Korablev et al. (JGR, 2006)
Etat des lieux• Instrument health:
• UV channel defects noticed since orbit #2639 = additional “cleaning” stage in the pipeline
• Further degradation since Safe Mode #25 of Mars Express in summer 2011
• IR channel has operated flawlessly and continues to do so• Data Production:
• MEx has completed its 10,000th orbit in 2011• SPICAM has achieved >10,000 observations and collected
13,500,000 UV spectra and 2,000,000 IR spectra to date • 63 Giga-Octets of data transmitted to Earth
• Science Production:• 60 publications • JGR special edition (SPICAM results) in 2006• >180 communications in workshops/conferences
Thèmes scientifiques couverts
1. Emissions spontanées de l’atmosphère:• NO detection and characterization (UV )• Auroras and Dayglows (CO2
+, CO, etc.) (UV) • Hydrogen and Oxygen corona (UV)• O2 dayglow/nightglow (IR) (also relevant to 2.)
2. Composition et climat:• Ozone, carbon dioxide (temperature) and water vapor mapping
and vertical profiling (UV & IR) • Aerosols and clouds characterization (UV & IR)
3. Surface(s) :• Phobos and Deimos observations (UV)
Quelques accomplissements SPICAMesques…..
1. Martian Airglows:• First detection of Nitric Oxide emissions, revealing atmospheric global
circulation pattern;• First detection of auroras above crustal magnetic field anomalies;• Characterization of dayglow and nightglow emissions;• Characterization of the O and H Martian corona.
2. Atmospheric Composition & Climate• Detection of mesospheric (>100 km) cloud layers, of likely CO2
ice origin;• First annual mapping of O3, simultaneously with H2O;• 4D (x,y,z,t) distribution of O3 and H2O through combination of
occultation and nadir modes;• Compilation of the largest density/temperature dataset in the
mesospheric/thermospheric 70 to 140 km altitude range;• Detection of water vapor in a high supersaturation state.
Spectrum of the star :
outside the atmosphere
through the atmosphere ratio
star
Atmospheric Transmission
Mars Express spacecraft
orbit
SPICAM Ultra-Violet
observations, orbit #17
13 jan. 2004
MARS
Line of sight
Occultation sequence
1 spectrum / second Dz~1-3 km
Prominent signatures of CO2, O3 and
aerosols
CO2 profile gives T(z)
Aerosols affect wholespectral range and
exhibits a pronounced spectral slope
Forget et al. (JGR, 2009)
• Large differences between SPICAM observations and LMD GCM predictions for the mesopause altitude and temperature
• O underestimated by model = CO2 cooling underestimated
Nuages mésosphériques martiens
Montmessin et al. (Icarus, 2006)
Simultaneous temperature
profile inversion indicates that layers appear partly inside
supersaturated pockets of CO2
Nuages mésosphériques martiens : de la glace de CO2 ?
Määttänen et al., Icarus, 2013
Evolution spatio-temporelle de l’activité nuages/aérosols :
• Occultations stellaires/solaires confondues
• Suivi de la hauteur max (plafond) des aérosols correspondant à une opacité colonne le long de la ligne de visée de 1
Ztop
Mars Express spacecraft
orbit
MARS
NADIR : l’instrument vise dans la direction du centre de la planète = mesure du spectre de la lumière solaire réfléchie par la surface de la planète après qu’elle est traversée l’atmosphère
comparaison spectre mesuré/spectre solaire : Colonne d’abondance des constituants CO2, O3, H2O responsables des absorptions observées
1.4
1.2
1.0
0.8
0.6
0.4
0.2
0.0
Rel
ativ
e al
bedo
320300280260240220200 wavelength (nm)
SPICAM relative albedo model with Earth O3/200 model with Earth O3
Observation nadir : principe
θ1
Scattering by surface with albedo A
MEX/ SPICAM
tv vertical optical thickness of absorption, varies strongly with wavelength
Absorptionby gas CO2
Water vapour band
SPICAM – near Infrared observations, orbit 8, 9 jan. 2004
SPICAM – Ultra-Violet observations, orbit 8, 9 jan. 2004
UV
IR
Perrier et al. (J. Geophys. Res., 2006)
Lefèvre et al. (2013)
MY29
MY27
MY28
Multi-annual monitoring of H2O water vapor
MY30
MY27
MY28
H2O, pr.mm
Ls
Annual water vapor cycle: an average view
All years combined
1 km3
of ice
H2O pr.mm
MY29
MY27
Interannual variability of H2O vapor
MY30
MY28
H2O, pr.mm
sun
Atmospheric Transmission
Mars Express spacecraft
orbitSPICAM Infrared
observations
Line of sight
SPICAM data LMD GCM predictions
north
south
northern spring-summerMaltagliati et al. (Science,
2011)
Maltagliati et al. (Science, 2011)
Credit: ESA/AOES Medialab
north
south
southern spring
SPICAM data LMD GCM predictions
Maltagliati et al. (Icarus, 2013)
Meeting SPICAM/SPICAVPoros Island (Greece): 28 june to 2 july 2010
50 – 100 ppm of water vapor at 60 km, for ~5 Ls
60 km
Climate Model results:Water vapor contours (colors) superimposed on circulation pattern
Montmessin et al., 2004
0.1 50 200ppm
Northern summer Southern summer
Aphelion cloud belt formation
at z ~15 km
On an annual average, the climatic asymmetry favors accumulation/storage of water in the north.
60 km
Montmessin et al., 2004
0.1 50 200ppm
Aphelion cloud belt formation
at z ~15 km
Southern summerNorthern summer
60 km
Montmessin et al., 2004
0.1 50 200ppm
Southern summerNorthern summer
SPICAMGCM
MY29
MY27
MY30
MY28
H2O, pr.mmInterannual variability of H2O vapor
MY29
MY27
MY30
MY28
H2O, pr.mmInterannual variability of H2O vapor