1. Solar-B Mission Preparation Len Culhane – UK EIS Principal Investigator Louise Harra – UK Project Scientist David Williams – UK EIS Chief Observer Mullard Space Science Laboratory University College London

2. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B Solar-B Spacecraft and Mission EIS Team Roles and Responsibilities UK (MSSL (PI), Birmingham, RAL):  CCD cameras, Structure, On-board Processor, Filter Housing, Calibration USA (NRL, GSFC, Columbia):  Optics, Coatings, Mechanisms, Filters, Japan (NAOJ, ISAS):  Testing, Integration with Spacecraft Norway (UiO):  EGSE and Quick-look Software All participants are involved in Post-launch Mission Operations and Data Analysis

3. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B  Solar Optical Telescope (SOT) Largest optical telescope (d = 0.5m) to observe Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in range 388 – 668 nm Vector magnetic field and velocity measurement at the photosphere  X-Ray Telescope (XRT) High angular resolution ( < 2 arc sec) coronal imaging Wide temperature coverage: 1 MK < T e < 30 MK  EUV Imaging Spectrometer (EIS) Coronal raster imaging at 2 arc sec Plasma diagnostics (T e, n e, v) in 170 – 210Å and 250 – 290Å ranges Solar-B Mission Instruments

4. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B Large Effective Area in two EUV bands: 170-210 Å and 250-290 Å –Multi-layer Mirror (15 cm dia ) and Grating; both with optimized Mo/Si Coatings –CCD camera; Two 2048 x 1024 high QE back illuminated CCDs Spatial resolution: 1 arc sec pixels/2 arc sec resolution Line spectroscopy with ~ 25 km/s per pixel sampling and ~ 3 – 5 km/s Doppler velocity estimates for ≥ 100 photons per line Field of View ： –Raster: 6 arc min×8.5 arc min; –FOV centre moveable E – W by ± 15 arc min Wide temperature coverage: log T = 4.7, 5.4, 6.0 - 7.3 K Simultaneous observation of up to 25 lines/spectral windows EIS - Instrument Features

5. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B EIS Optical Diagram Grating Front Baffle Entrance Filter Primary Mirror CCD Camera

6. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B EIS Field-of-View 360  512  EIS Slit: 1 or 2 arc sec Maximum FOV for raster observation 512  900  Raster-scan range Shift of FOV center with coarse-mirror motion 250  slot 40  slot 512 

7. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B 2Mbps max  1.3 Mbps EIS Data Flow CCD Readout Electronics EIS ICU Large hardware CCD window S/C MDP Small spectral window (25 max) Data compression DPCM(loss less) or 12bit-JPEG  250 kbps max for short duration,  40 kbps average Telemetry data format Average rate depends on number of downlink station. 1  slit obs. 40  slot obs. 250  slot obs. Spec.width 16 40 250 Spatial width 256" 512" 256" No. of lines 8 4 4 Compression 20% 20 % 20% Cadence 2 sec 5 sec 15 sec Rate 38.4 kbps 38.4 kbps 40 kbps 10 min cadence for 4  4 rastering Observation table control

8. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B EIS Instrument Pre-Calibration EIS Instrument Completed

9. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B SOT/FPP Data a) b) c) Solar-B Mission Data Acquisition Data are stored on-board in an 8 Gbit mass memory Baseline instrument memory allocations are: - SOT/FPP → 70% - EIS/XRT → 15% each Data downlinked to Svalbard ground station (ESA/Norway) on 15 orbits/day - memory dumped once per orbit EIS average data rate → 45 kbps - x 5 -7 greater with lossy compression Command uplinks only from Kagoshima Quick-look data at ISAS and Kagoshima

10. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B Mission operations will be conducted from the ISAS Spacecraft Operations Centre in Fuchinobe, Japan Solar-B team observing plans and community proposals will be discussed at monthly meetings Each instrument team will have a Scientific Schedule Coordinator who will organize the preparation of instrument proposals and their integration in the overall mission observing plan Weekly and daily planning meetings allow flexibility to respond to changing solar conditions Solar-B Mission Operations

11. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B Level-0 and Cal Data Level-2 Data (FPP) Level-0 Reformat Solar-B Database in Japan Solar- B Database in US Solar- B Database in UK FPP Level-1and-2 Reformat at Lockheed Solar-B Mission Data Distribution Data distributed to UK and US in compressed level – 0 form Because of complexity, FPP vector magnetogram data are transmitted in level – 0 form to Lockheed Palo Alto They are processed to level – 2; vector magnetograms are then sent to the UK and Japan

12. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B Data Handling and Observation Planning

13. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B UK Data Processing, Storage and Availability

14. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B UK Solar-B Proposal Handling

15. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B UK Solar-B Data Centre (SDC) at MSSL The SDC will maintain:  analysis guides on-line for users of all three software sets  an email helpdesk and web discussion site for community support  a record of Solar-B observing plans and schedules on the centre web site A software tool will be made available for preparation of observing proposals The UK SSC will help in this process by assisting the UK community in making contact with members of the other Solar-B instrument teams All Solar-B mission data will be archived at the SDC, stored at the Atlas Data Centre and made available through Grid networks e.g. Astrogrid Anticipated data volume for the three year mission life is ~ 25 Tbyte Relevant Solar-B software will be held at the SDC and periodically updated to reflect developments in the UK, US and in Japan

16. Solar-B Mission Timeline Pre-launch period will include planning, commanding and data acquisition rehearsals Observing with Solar-B, using any or all of EIS, XRT and SOT/FPP, will require the preparation of proposals These will be presented by the UK Scientific Schedule Coordinator (SSC) to the Solar-B team at the monthly planning meetings in Japan Review of operations will take place 18 months after mission start  Possibility for more remote operation for Solar-B from US and UK

17. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B SUMMARY Following SOHO CDS, the EIS instrument will provide the next steps in EUV spectral imaging of the corona: –x 10 enhancement in A eff from use of multilayers and CCDs –x 5 enhancement in spectral resolution –x 3 enhancement in spatial resolution –Like CDS; absolute calibration performed to ± 20% EIS will: –Address a broad range of coronal science topics –Enable major goals of Solar-B mission by relating coronal response to magnetic flux emergence and material flows

18. Astrogrid Solar/STP Planning Meeting, UCL, 22 Feb, 2006. Preparing for Solar-B END OF TALK