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Doppler Spectro Imager

Doppler Spectro Imager. PI: F.X. Schmider (Observatoire Côte d’Azur, F) PM: Fréderic Rouesnel (Institut d’Astrophysique Spatiale, F) DSI-ECHOES team. Cosmic Vision 2015-2025. Assessment Phase 0/A. Definition Phase A/B1. Implementation Phase B2/C/D.

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Doppler Spectro Imager

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  1. Doppler Spectro Imager PI: F.X. Schmider (Observatoire Côte d’Azur, F) PM: Fréderic Rouesnel (Institut d’Astrophysique Spatiale, F) DSI-ECHOES team

  2. Cosmic Vision 2015-2025 AssessmentPhase 0/A Definition Phase A/B1 Implementation Phase B2/C/D DOI: Declaration of InterestAO: Announcement of OpportunityLOE: Letter of EndorsementMLA: Multi-Lateral Agreement TRL ≥5 Euclid Plato M1 launch Spica M-class missions M2 launch Marco-Polo Cross-Scale Solar Orbiter Instruments AOLOE DOI MLA TRL ≥5 EJSM/Laplace TSSM/Tandem L1 launch Lisa L-class missions IXO Instruments DOI AOLOE MLA 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 2020 2008 2009

  3. Doppler Spectro Imager • Science goal : Formation and evolution of the Solar System • 2 objectives: Internal structure (M1) • Atmosphere study (L1 to L4)

  4. Main goal Solar system formation scenarii: accretion, gravitational instability ? Key question Does Jupiter have a core ? If any, what size/mass ? What happens at the transition metalic/molecular hydrogen ? The tool Seismology : most performant way to investigate planetary and stellar internal structures (e.g. SOHO for the Sun, CoRoT for the stars)‏ Measurement of mode frequencies up to degrees l=100 Complementarity with JUNO gravitational moments Jovian seismology from Guillot et al. 2004

  5. Study of the upper troposphere Main goals Origin of the global circulation of Jupiter, Structure of the troposphere: interaction between the envelope and the upper atmosphere Structure of the band system: its relation to differential rotation Key measurements - Travelling waves detection and characterisation (cross-correlation): dynamics and composition - Velocity field: thermodynamics quantities and the “potential vorticity” This latter quantity can be deduced from observations of the wind field, together with temperature profiles of the atmosphere. • The tool • Doppler measurements • 3D velocity maps‏ • wave propagation 5

  6. DSI – ECHOESProbing internal structure Theoretical works: Vorontsov 76, Bercovici & Schubert 87, Gudkova & Zarkhov 99, Lognonné 2007 obs - theoretical Inversion method obs - theoretical 6

  7. DSI – ECHOESDetection of acoustic modes • Best detection level: 1 bar • Velocity measurement • 2D images and velocity maps at 1 frame/mn • Mode frequencies = [0.5 - 3.5] mHz • Mode amplitudes = [10 - 50] cm/s (Bercovici and Schubert, 1987)

  8. Instrument StudyTeam organisation JPL (USA) Neil Murphy LESIA (France) B. Mosser 8

  9. Instrument StudyStudy Team

  10. Instrument StudyTeam members Sylvie Robbe OCA France

  11. DSI – ECHOES SYMPA results First instrument dedicated to Jovian seismology Fourier transform tachometer: velocity measurement with spatial resolution Ground based network: 2 (3) instrument on 1.5 m telescopes Presence of a periodicity of 156 µHz in the density power spectrum ℓ= 0 and ℓ =1 First clear evidence for Jovian acoustic mode (Gaulme et al 2010, to be submitted)

  12. DSI – ECHOESInstrument principle Fourier tachometer Fixed OPD Mach Zehnder interferometer Four output images in phase quadrature OPD modulation for calibration Solar reference for absolute velocity 12

  13. DSI – ECHOES Velocity measurement Measurement of combined vertical and horizontal velocities: sum of Doppler shifts in direction of the Sun + in direction of the S/C Seismology: search for velocity variations Global noise level < 1 cm²/s²/µHz up to l=100 Atmosphere: following of structure with jovian rotation separates vertical and horizontal components Precision: 20 m/s/px/hr (400x400 pxs @ 150 km )

  14. DSI – ECHOES Mission scenario Atmosphere Seismology 14

  15. DSI – ECHOESBlock diagram 15

  16. DSI-ECHOESOptical study Equivalent pupil diameter: 3.2 cm Equivalent focal lengh: Full field: 2.72 degrees Pixel size: 18 µm Mach-Zehnder

  17. Fine pointing mirror Filter Pupil Door Triplet Large pointing mirror Baffles Doublet Interferometerunit DSI - ECHOESMechanical design 17

  18. DSI - ECHOESMechanical design Mach-Zehnder support: Titanium plate Modulation PZT support Fine guiding mirror with PZT

  19. DSI - ECHOESThermal and mechanical studies

  20. DSI - ECHOESFocal Plane Assembly Hydra Startracker Sodern

  21. DSI - ECHOESCalibration concept The in-flight calibration should follow 3 steps: - Distortion calibration: A star is pointed by the S/C and acquired in the DSI field and its position measured on the four sub images. Differential positions on the sub-images provide the algorithm of distortion correction. - Flat field calibration: Uniform illumination of the field is performed, with an internal source. - Fringe calibration: with solar light uniform illumination, the MZ OPD is modulated at 0, p/2, p, 3p/2, allowing the determination of the OPD dependence in the field, i.e. the fringe contrast and phase (OPD) at any point in each sub-image.

  22. DSI – ECHOESInterface and resources 22

  23. DSI – ECHOESDescope options

  24. DSI – ECHOESFollow- up • Before the AO [..] will complete the study of each sub-system and will examine the technical descope options in order to reduce the S/C resources requirement. It will be focussed on the full data acquisition and treatment simulation, in order to eliminate possible redundancies in the calibration system and reduce the data rate. • […] also pay attention to the consolidation of the consortium for the AO answer. • Two TDAs are also being carried: • complete MZ breadboarding  R&T on going, • radiation mitigation. • “Other subsystems require a special attention to reach the TRL 5 before 2012. Although these subsystems are not technological development, these activities are listed in the planning.” • Calibration sub-system • Detector Unit (PRNU stability)  R&T submitted for 2011

  25. DSI – ECHOESGlobal budget • Global Budget for DSI-Echoes (overall PFM program) :

  26. DSI – ECHOESWBS

  27. DSI ECHOESMan Power OCA

  28. DSI – ECHOESTechnology Development Activity • Study Phase (TDAs) - ROM cost estimated to 587 k€ (2011 / 2012)

  29. R&T MZ • Objectif général • Atteindre TRL 5 pour le bloc Mach Zehnder: • s’assurer de la faisabilité du composant • contrôler ses performances dans un environnement thermique représentatif du S/C. • Plan général d’actions • Spécification du MZ • Etude du MZ (configuration géométrique et choix des verres) et du banc de test ; • Approvisionnement du prototype de MZ et autres composants pour le banc de tests ; • Intégration, réalisation des tests et rapport de qualification. • Financement CNES • 80 k€ 2010 • 90 k€ 2011-2012 (demandé)

  30. Thése Laurence Soulat Sujet de thèse « Mise en œuvre d’un interféromètre imageur de Mach-Zehnder pour la sismologie de Jupiter »

  31. R&T Schéma du banc de tests Masque de champ Masque pupille Sortie 2 Appareillage de mesure : -analyseur de front d’onde -optique + caméra -polariseur + détecteur… Sortie 1 • Contrôle de la ddm • Mesure de qualité de front d’onde dans les 2 sorties • Contrôle de l’échantillonnage, du contraste et de la régularité des franges Vide • Mesure de stabilité thermique de la ddm • Mesure de transmission dans les 2 voies, mesure de polarisation. Four • Contrôle de la fonction de calibration, ajustement de ddm en fonction de T°, stabilité de la platine

  32. R&T Partage des responsabilités

  33. Planning R&T MZ

  34. R&T MZ Manpower OCA

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