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(Novembre 10, Nice). Science Case Follow-up GAIA (1 milliard d’étoiles, positions et vitesses) : priority identified by: ESO/ESA working group on «The.

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Presentation on theme: "(Novembre 10, Nice). Science Case Follow-up GAIA (1 milliard d’étoiles, positions et vitesses) : priority identified by: ESO/ESA working group on «The."— Presentation transcript:

1 (Novembre 10, Nice)

2 Science Case Follow-up GAIA (1 milliard d’étoiles, positions et vitesses) : priority identified by: ESO/ESA working group on «The Galaxy» (Turon et al. 2008) Astronet Roadmap identifié lors de la prospective INSU 2009 Two cases identified: - low-resoluion spectroscopy (R~5000) for stars V>17 (3rd dim of velocities) - high-resolution spectroscopy (R~20000) for stars V>10 (detailed chemical abundances) Rien en Europe avant GYES; maintenant 2 projets low-R complémentaire: HERMES/AAO pour l’hemisphère sud

3 (Novembre 10, Nice) GYES science case Chemical labelling of galactic populations (équipe Gaia) discs disc-bulge interactions halo Galactic dynamics Other sciences with the survey paramètres fondamentaux des étoiles, physique stellaire ISM variable stars (N. Nardetto) Globular clusters (A. Recio-Blanco)

4 (Novembre 10, Nice) GYES Science Team (Phase A) P. François (PS), E. Caffau (co-PS), F. Arenou, C. Babusiaux, C. Balkowski, O. Bienaymé, P. Bonifacio, D. Briot, R. Carlberg, B. Famaey, Y. Frémat, A. Gomez, M. Haywood, V. Hill, R. Kudritzki, R. Lallement, P. de Laverny, B. Lemasle, C. Martayan, R. Monier, D. Mourard, N. Nardetto, A. Recio-Blanco, N. Robichon, A. Robin, M. Rodrigues, F. Royer, C. Soubiran, C. Turon, K. Venn, Y. Viala

5 (Novembre 10, Nice) GYES project & timelines Phase A (GEPI +Oxford ) January - Sept 2010 Phase A study financed by CSA-A : Jan - Sep 2010 July Mid-Term review (at SPIE San Diego) October 2010 Concept Design Review Delta-Phase A November March 2011 Phase B March April 2013 PAE July 2015 PAH & Comissioning July-Dec 2015 FAH December 2015 Survey

6 (Novembre 10, Nice) GYES System Team (Phase A) P. Bonifacio (PI) P. François (PS), E. Caffau (co-PS), F. Royer (IS), J.-L. Dournaux (PM),S. Mignot (SE), M. Cohen, D. Horville (optics), J.-M. Huet (Mechanics), I. Guinouard (fibres), G. Fasola (detectors & electronics), P. Laporte (thermal control), G. Dalton, I. Lewis (positioner)

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10 Structure Gantry extent 962x911mm Z-axis 1332mm behind last corrector lens Fibres exit through tumbler axis Field plates have small rotation (retractors rotate with the plate), independent of each other, to account for differential refraction and intrinsic field rotation Focal plane imager deployed between corrector and observing field plate Trade-off between footprint and height

11 (Novembre 10, Nice) Software simulations Full simulation of geometry, button manufacturing tolerances. Random target distribution 20 fibres reserved for sky allocation

12 (Novembre 10, Nice) Fibres etc. Ensure the link between the positioner and the spectrograph 500 mono-object fibres 80 µm core 40 m long Compatible with exchange procedure Perform simultaneous wavelength calibration 20 fibres 80 µm core short (within spectrograph) Close guiding control loop 5 to 10 7-fibre IFUs 33 µm core short (within PFUE)

13 (Novembre 10, Nice) Bundle Collaboration with Polymicro (fibre) and SEDI (French company specialised in fibre cables) Stiff structure to limit radius of curvature FRD breaking fibres Armoured cable withstand instrument exchange Need for individual protection buffer not determined yet

14 (Novembre 10, Nice) Transmission (I) Depending on the length and wavelength: impact on the location of the spectrograph.

15 (Novembre 10, Nice) Transmission (II) Worst case for non-telecentricity (one button type) & alignment Goal for alignment and FRD

16 (Novembre 10, Nice) Spectrograph Bench and feet (with pneumatic dampers) Cover (on bench or on ground) Mechanical mounts & optics: – collimator (3): – dichroic (1) – VPH gratings (2 x2) – cameras (2 pre-integrated) Slit exchange mechanism Detectors (2 x2) Dewars (2)

17 (Novembre 10, Nice) Baseline and back-up design Backup design: single VPH disperser → Consolidate the backup design to eventually consider it as the new baseline design Baseline: double VPH disperser

18 (Novembre 10, Nice) Disperser (I) Type : VPH grating (large size and gr. density) Backup design specification: Baseline specification:

19 (Novembre 10, Nice) Disperser (II) Baseline transmission efficiency: – Peak: 84% – Edges: 5% - 15%

20 (Novembre 10, Nice) Disperser (III) Backup design transmission efficiency: – Peak: close to 100% – Edges: 40% - 47%

21 (Novembre 10, Nice) Resolution

22 (Novembre 10, Nice) Transmission (II)

23 (Novembre 10, Nice) Transmission (III) Estimates of SNR per pixel in V=16 centre of slit only the photon noise

24 (Novembre 10, Nice) GYES Survey Survey Strategy : 262 nights over 5 years ~ 3 ×10 5 stars in the disc, halo, bulge & clusters Survey Management Plan: (~30FTE over 5 yrs) Input catalog & observation preparation Spectra analysis pipeline development Spectra analysis Output catalog production & distribution

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26 GYES project & timelines Phase A (GEPI +Oxford ) January - Sept 2010 Delta-Phase A November March 2011 Consortium build-up: + GEPI + OCA: ICS, AIT, Optics (corrector ? tbd), Survey Data Analysis, Science Team (PS) + LAB: ICE, Science Team + Oxford: positionner (hard and software) Consolidate Management plan (+ AIT plan, +++) Science tradeoffs (impact of new baseline design) Phase B March April 2013 PAE July 2015 PAH & Comissioning July-Dec 2015 FAH December 2015 Survey

27 (Novembre 10, Nice) GYES project & timelines Phase A (GEPI +Oxford ) January - Sept 2010 Delta-Phase A November March 2011 Phase B March April 2013 kickoff for Phase B march 2011 PDR May 2012 FDR April 2013 PAE July 2015 PAH & Comissioning July-Dec 2015 FAH December 2015 Survey

28 (Novembre 10, Nice) GYES System Team (Phase B) P. Bonifacio (PI) P. François (Co-PI) V. Hill (PS) F. Royer (IS) P. Jagourel (PM) +OCAS. Mignot (SE)M. Cohen, D. Horville + OCA (optics) J.-M. Huet (Mechanics) I. Guinouard (fibres)G. Fasola (detectors & electronics) + LAB (ICE)P. Laporte (thermal control) G. Dalton, I. Lewis (positioner) ICS: OCA (JM Clausse) AIT : OCA (F. Henault)

29 (Novembre 10, Nice) Contribution OCA Actuel FIZEAU: ICS: 3.7 FTE 0.6 FTE en phase B; 3FTE en phase C AIT: 4.4 FTE 1 FTE en phase B; 2 personnes en phase C + salle grise Optique (en discussion: correcteur de champ ?) FODR phasé avec PDR (ie mai 2012) Actuel Cassiopée: Survey: ~4 FTE sur 5 ans Spectral analysis (pipeline development & operations)

30 (Novembre 10, Nice) GYES project & timelines Phase A (GEPI +Oxford ) January - Sept 2010 Delta-Phase A November March 2011 Recommandation SAC (nov 2011) - Board (dec 2011) Phase B March April 2013 PAE July 2015 PAH & Comissioning July-Dec 2015 FAH December 2015 Survey

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32 Status of study Report status of study – 9-month study – still work in progress – HW cost 4.6 M€ (with contigencies) – Consolidated cost 13.8M€ – Timeline: on sky Dec 2015 Active developments – refinements of the baseline – need to loop back to science requirements and tradeoffs – need for input as regards options (impact on timescale) – need for input from CFHT (eg. guiding, software) → active work on transmission: many improvements possible active reaction to VPH issue

33 (Novembre 10, Nice) Type Only the fibres from Polymicro have been investigated (commonly used in astronomy).

34 (Novembre 10, Nice) For Phase B some novelties P. Bonifacio (PI) P. François (co-PI) V. Hill (PS) F. Royer (IS) P. Jagourel (PM) + Participation of OCA (ICS + AIT) LAB (ICE+ Detectors) + ????


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