1. EUV Imaging Spectrometer (EIS): Instrument Checkout, Performance Verification and Initial 90 Day Observing Plan Extended Solar Optical Telescope Meeting 17 th – 20 th April, 2006 at NAOJ Len Culhane for the EIS Team

2. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 2 SUMMARY EIS Instrument Outline Instrument Performance Tests Post-launch activities –Spacecraft –EIS Engineering –EIS Calibration EIS Initial Science Plan EIS Planning Tool Software Conclusions

3. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 3 EIS Optical Diagram Grating Front Baffle Entrance Filter Primary Mirror CCD Camera

4. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 4 EIS Effective Area Primary and Grating: Measured- flight model data used Filters: Measured- flight entrance and rear filters CCD QE: Measured- engineering model data used Following the instrument end-to-end calibration, analysis suggests that the above data are representative of the flight instrument

5. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 5 EIS Sensitivity IonWavelength (A) logTN photons ARM2-Flare Fe X184.546.001536 Fe XII186.85 / 186.886.1113/21105/130 Fe XXI187.897.00-346 Fe XI188.23 / 188.306.1141 / 15110/47 Fe XXIV192.047.30- 4.0  10 4 Fe XII192.396.1146120 Ca XVII192.826.7031 1.8  10 3 Fe XII193.526.11135305 Fe XII195.12 / 195.136.11241/16538/133 Fe XIII200.026.2020113 Fe XIII202.046.203582 Fe XIII203.80 / 203.836.207/2038/114 Detected photons per 1  1  area of the Sun per 1 sec exposure. IonWavelength (A) logTN photons ARM2-Flare Fe XVI251.076.40-108 Fe XXII253.167.11-71 Fe XVII254.876.60-109 Fe XXVI255.107.30- 3.3  10 3 He II256.324.7016 3.6  10 3 Si X258.376.111462 Fe XVI262.986.4015437 Fe XXIII263.767.20- 1.2  10 3 Fe XIV264.786.3020217 Fe XIV270.516.3017104 Fe XIV274.206.301476 Fe XV284.166.35111 1.5  10 3

6. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 6 Principal EIS Subsystems for Commissioning Primary Mirror Grating Dual CCD Camera Filter Holder Installed Instrument Control Unit Slit/Slot Wheel Shutter

7. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 7 Optical Performance Primary mirror: Coarse mirror motion Fine mirror motion Slit/slot: Slit width Repeatability of slit position Position of slits with respect to slots Grating: Focus check post-launch Detector Slit curvature and orientation Magnification vs. wavelength Plate scale Variation of above around orbit Pointing: Short-term stability Around orbit variation Instrument Performance Tests

8. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 8 Instrument Performance Tests Photometric Assess throughput/ photometric calibration:Compare with pre-launch – T e, n e insensitive line ratios in QS Detector:Full well Linearity Flat field Dark current Charge Transfer Efficiency (CTE) Co-alignment:SOT – He II 256Å slot images with magnetograms and chromospheric images XRT – Fe XV 284Å slot images with XRT images Spectral lines:Spectral resolution Dispersion Monitor average count rates for QS, AR, CH and Flares

9. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 9 Post-Launch Activities 1.Spacecraft –Systems commissioning (~ 21 days; tbc) 2.EIS Engineering –Pre-filter enclosure opening (6 days) –Post-filter enclosure opening (4 days) 3.EIS Calibration –EIS specific observations (~ 5 days) –Trial synoptic observations (2 days) 4.EIS Initial Science –90 day initial observing plan (90 days) 5.EIS Planning Tool Software

10. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 10 1. Spacecraft Launch sequence t = X – Liftoff t = X + 77 min – begin array deployment t = X + 80 min – complete array deployment t = X + 83 min – begin Sun acquisition t = X + 94 min – complete Sun acquisition Spacecraft systems commissioning t = X + 21 days (TBC) – complete systems commissioning Note: Useful to have some instrument testing enabled during this interval e.g. QCM readings, CCD bakeout Allow minimum of 24 hrs for out-gassing before first turn on

11. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 11 2. EIS Engineering Tests COMENG01ICU on - software checks (memory) [1 / 2]  Day 1 is Day 21 COMENG02MHC on – load code, QCMs on [2 / 1] COMENG20Initial QCM readings [2 / 2] REGENG00QCM1/2; readings once per day [2 / 2] COMENG03Op. heaters on for temp. stabilisation [2 / 3] COMENG04 Mechanism tests for Slit/Slot selection [4 / 1] COMENG05 Mechanism tests for Shutter [4 / 2] COMENG10CCDs on - load/initiate test sequence [5 / 1] - start Camera data assessment [5 / 2] Note: X days elapsed time allowed for complete EIS out-gassing and camera data assessment before front filter doors opened [Day/Orbit] Pre-Clamshell Opening Study Activity

12. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 12 COMENG99Opening of filter enclosure doors [1 / 1]  Day 1 is Day (21 + X) COMCAL00Test sequences of full CCD [1 / 2] COMENG07 Mechanism tests for Fine Mirror [2 / 1] COMENG08 Mechanism tests for Grating – grating focus [3 / 1] COMENG06 Mechanism tests for Coarse Mirror [5 / 1] 2. EIS Engineering Tests [Day/Orbit Post-Clamshell Opening Study Activity

13. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 13 3. EIS Calibration and Performance Verification COMCAL00Test sequences of full CCD – top-half then bottom-half to establish solar image position; assign 512 pixel y-range COMCAL01Test sequences with 512 pixel hardware window for range of exposure times to check wavelength range, QE, solar response COMCAL02Wavelength calibration; execute full spectral scans in different solar regions e.g. AR, QS, CH – compare with lab calibration COMCAL03Intensity calibration; QS observations to determine detector efficiency - T e, n e insensitive line ratios; compare with pre-launch QE COMCAL04CCD dark current; confirm stable CCD operating temperature in nominal orbit so that dark current can be estimated Study Activity

14. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 14 COMCAL05Measure CCD flat-fields using EIS LEDs COMCAL06Establish EIS pointing and alignment - network and limb observations with SOT; EIS 40” slot/He II 256Å - AR and limb observations with XRT; EIS 40” slot/Fe XV 284Å COMCAL07 Determine CCD particle background; measure as f (orbit position) COMCAL08Sit and stare with changing slit/slot; - establish mechanism repeatability - determine line profiles for different slit/slot selections - identify any variation with orbit position - measure EIS plate scale; compare with XRT - determine slit curvature - determine magnification as f ( ) COMCAL09Scattered light estimate; off-pointing from bright AR 3. EIS Calibration and Performance Verification Study Activity

15. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 15 3. EIS Calibration and Performance Verification Study Activity COMCAL10Trial synoptic observation – full spectral survey - Observe structure-free quiet Sun and network - Observe a suitable AR if one is available - Complete spectral coverage, field of view and observing time TBD COMCAL11 Trial synoptic observation - solar equator survey - Use EIS coarse pointing mechanism - Observe four 10 arc min x 8 arc min fields of view - Raster each field with 40” slot and 2 minute cadence - Approximately two hours for complete limb-to-limb survey Following their development, these synoptic observations should be undertaken routinely at a frequency to be agreed

16. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 16 Aim of outline observing plan is to achieve critical science goals in the first three months after commissioning Goals identified but not yet prioritized: - Sun’s status in the period after launch will influence EIS and mission observing strategy on a weekly/daily basis Plan will need to be detailed and further enhanced 4. Initial Science Plan Background

17. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 17 Include three lines in ALL studies for a consistent dataset throughout the mission – core lines Core line list is: - He II → 256 Å, Fe XII → 195 Å, Ca XVII → 192.8 Å Selection based on line strength and temperature range Additional lines included as appropriate for each separate science objective Line Lists 4. Initial Science Plan

18. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 18 Flare trigger and dynamics: - Spatial determination of evaporation and turbulence in a flare Active region heating: - Spatial determination of v, T e and n e in active region structures Quiet Sun and coronal hole boundary: - Establish relationship between different types of quiet Sun event Boundary Conditions If solar conditions permit, observing time will be split evenly between topics An active region will be tracked if possible For AR with highly sheared magnetic field, EIS will be in flare mode to respond to XRT's trigger Otherwise observe quiet Sun and coronal holes for long periods (> 12 hrs) If no active regions but a quiet prominence, concentrate on this 4. Initial Science Plan Principal Topics

19. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 19 Spatial determination of evaporation and turbulence in a flare - Fast raster on pre-selected AR with a complex magnetic topology - Spectral imaging mode with 40” slot for a flare-productive AR - Flare trigger response from 250” slot to observe early velocity shifts - Line selection: core line list and Fe XXIV - 192 Å, Fe XV - 284 Å - FOV 200" X 200" with 2" slit - Cadence for 1 raster: 2.5 min with 1 s exposure - Windows to be wide enough for velocities of ~ 400 km/s (> 30 pixels) 4. Initial Science Plan Flare Trigger and Dynamics

20. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 20 Spatial determination of v and n e in AR loops for range of T e values  High time cadence sit and stare observations - - Spectral imaging with 40” slot/2s cadence to observe new dynamic phenomena - Alternate with 1” slit/2s cadence - Line selection: core lines and Fe XIII – 202 Å, - 203 Å  Spatial variation raster observations - Large raster (256” x 256”)/2” slit/20 sec cadence to observe AR global changes over several hours - Alternate with smaller raster (128” x 128”)/1” slit/40 sec cadence for detailed velocity measurements (± 3 km/s) - Line selection: core lines and Si VII – 275 Å, Mg VI – 269 Å, Fe X – 190 Å, Fe XI – 180 Å, Fe XIII – 202 Å, - 203 Å, Fe XIV – 274 Å, Fe XV – 284 Å, Fe XVI – 263 Å, Ca XIV - 193.8 Å, Si X – 258 Å  For suitable AR, follow from disc centre to limb comparing disc/limb structures 4. Initial Science Plan Active Region Heating:

21. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 21 4. Initial Science Plan Quiet Sun Studies: Correlate coronal T e, n e and v with magnetic topology inferred from SOT  Detailed study of corona above two supergranule cells; - Alternate 60” x 512” rasters with slot (40”) and slit (1”) - Spectral imaging (40” slot) for 50s cadence study of changes in morphology - Spectral imaging (1” slit) for high resolution 50s cadence spectra at fixed QS locations; insert 40” images for context - Line selection: core lines and Si VII – 275 Å, Mg VI – 269 Å, Fe X – 190 Å, Fe XI – 188 Å, Fe XIII – 202 Å, - 203 Å, Si X – 258 Å, - 261Å  Detailed study of corona above bright point or explosive event; - Raster, slot and field of view selections as above - Also run sit and stare mode - Line selection as above  Detailed study above a coronal hole boundary - Raster, slot and field of view selections as above - Also run sit and stare mode - Line selection as above

22. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 22 5. EIS Planning Tool Software Planning tool software is in SSW –Users will need to install the EIS SolarSoft tree Study Definition –Line Lists –Raster Definition –Study Definition Planners then export studies to ASCII format E-mail a formatted file and a science case to a dedicated account at MSSL

23. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 23 5. Planning Tool - line list interface

24. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 24 5. Planning Tool – make/edit raster

25. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 25 5. Planning Tool – make/edit study

26. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 26 EIS Core Science Programme AR Heating → dynamic phenomena in loops Coronal/Photospheric velocity field comparison in AR Coronal Seismology → waves in AR structures AR Helicity content → CMEs, magnetic clouds Evolution of trans-equatorial Loops Flare produced plasma → source, location and triggering Flare reconnection → inflow and outflow Quiet Sun transient events → network, network boundaries, CH boundaries, size scales CME Onsets → dimming, filaments, flux-ropes, flaring AR, trans- equatorial Loops Evolution of large coronal structures → streamers, large-scale reconnection, slow Solar Wind

27. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 27 Some Possible Joint Observations Solar-B Instruments: –Active Region study campaign (SOT/EIS/XRT) –Emission measure distributions in AR structures (EIS/XRT) –AR helicity content and CME launches (SOT/EIS/XRT) –Magnetic topologies in small events (SOT/EIS/XRT) –Network and intra-network small event energies and velocities (EIS/SOT) –Plasma and magnetic structures above Coronal Hole boundaries (EIS/SOT) –Reconnection flows in flares (EIS/XRT) Other Missions: –CME launching, topology and magnetic clouds (Solar-B, STEREO, ACE) –CME dimming outflow velocities; their relation to CMEs (Solar-B/EIS, STEREO) –Trans-equatorial loop and filament eruptions (Solar-B/EIS, XRT, STEREO) –Coronal (EIT) waves and their relation to CMEs (Solar-B/EIS, XRT, STEREO) –Intensity and velocity studies of waves in AR structures (Solar-B, TRACE, SDO) –Impulsive flares and sub-surface wave propagation (Solar-B, TRACE, SDO)

28. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 28 After an instrument outline, necessary EIS performance tests were described Following the spacecraft commissioning of ~ 20 days, EIS checkout should begin Useful to have some overlap of EIS and spacecraft work Three major science areas are described as suitable for the first 90 days of observation – subject to Sun’s status EIS planning tool programmes – line list, raster and study construction codes, are described EIS core mission science programme is listed along with some possible joint observations Conclusions

29. Extended SOT Meeting, NAOJ, 17 th – 20 th April, 2006 29 END OF TALK