Apr 17-22, NAOJ SOT Initial Operation in Commissioning Phase Y. Katsukawa (NAOJ) SOT team

Apr 17-22, NAOJ2 SOT initial operation overview Y+ ISpacecraft verification and checkout phase 7-20Before installation to the nominal orbit FPP on, initial status check CCD decontamination IISOT instrument checkout phase (1) Instrument verification (TBD)Before OTA top door opening Basic function check Obtain dark images IIISOT instrument checkout phase (2) First light phase (TBD)After OTA top door opening Optical performance checkout Correlation tracker In-flight calibration IVPerformance verification phase (TBD) Run all the kinds of observables with combination In-flight calibration (continued) VInitial Science Phase for SOT core team 60d – 6months Used for dedicated scientific purpose In-flight calibration (continued)

Apr 17-22, NAOJ3 (I) Spacecraft verification and checkout phase Period: Launch  Y+20 Orbit control maneuvers are carried out several times to install the S/C to the sun-synchronous orbit. Check-out of S/C attitude control system is also performed during this period. No Event Perigee (km) Apogee (km) Inclination (  ) Date 0 Launch Test maneuver Y+3 2 Perigee-up maneuver # Y+6 3 Perigee-up maneuver # Y+11 4 Perigee-up maneuver # Y+14 5 Out-of-plane maneuver # Y+17 6 Final orbit controlY+20

Apr 17-22, NAOJ4 (I) Spacecraft verification and checkout phase

Apr 17-22, NAOJ5 (I) Spacecraft verification and checkout phase After  a#1 (Y+6), the altitude of S/C becomes high enough, and the attitude of S/C is controlled by MWs. During the period between Y+7 and Y+20, we plan to do initial status check (temperatures) and CCD heater operation. Primary objective is to decontaminate the CCDs.  a#2  a#3 MDP and FPP ON FPP and MDP OFF CCD decontamination heater ON CCD decontamination heater OFF 3days 1.5 days

Apr 17-22, NAOJ6 (II) SOT instrument checkout phase (1) Period: Y+21  Y+28 (TBD) (  1 week) From the installation to the sun-synchronous polar orbit To opening the SOT top door The primary objectives are (1) decontamination of M1, M2, and HDM, and (2) initial functional checkout without sunlight into the telescope. The test items of this phases are the following –Verify function of operational heaters for OTA and FPP –Open the telescope side door –Decontamination of M1, M2, and HDM –Verify function of mechanisms (shutters, filter wheels etc.) –FG, SP, and CT image acquisition –Automatic observation by MDP table control Obtaining dark images is also important items especially for SP because there is no shutter in the SP optical path.

Apr 17-22, NAOJ7 (II) SOT instrument checkout phase (1) Y+OTA / CTMFPP 20CTM ON, check OTA heaters 21OTA side-door opening Decontamination heaters ON FPP ON / operational heaters ON 22CCD heaters ON / Cameras ON 23PMU ON / Mechanisms check 24Tip-tilt mirror ON / PZT voltage testCheckout FG table observations 25Checkout SP table observations 26Dark images 27Dark images / Camera noise 28Dark images 29Preparation for door operationVerify obs. table for door operation 30OTA top-door opening Decontami heaters OFF Operational heaters ON

Apr 17-22, NAOJ8 (II) SOT instrument checkout phase (1) Obtaining dark images –Obtain the images with some camera setting (gain, amplifier) –Orbital variation, temperature dependence –Effect of cosmic radiation on the images All the data taken during this period is to be down- linked at the Uchinoura station (USC). Some of them will be down-linked at the Svalvard station (SVA) in order to test data transfer system from SVA to Japan.

Apr 17-22, NAOJ9 (III) SOT instrument checkout phase (2) Period: Y+30  Y+45 (TBD) (  2 weeks) First light phase after the telescope door is opened The primary purpose of this period is verification of optical performance –Alignment with respect to sun-sensor, XRT, and EIS –Image quality and focus stability –Correlation tracker performance –Function of FG and SP observables, etc. In-flight calibration of the instruments –Darks and flat fields –Polarization –TF wavelength tuning etc.

Apr 17-22, NAOJ10 (III) SOT instrument checkout phase (2) Y+S/C major eventFGSPCT 30OTA top-door openingInitial optical check Coarse focus scan Initial optical check Coarse focus scan Initial optical check Coarse focus scan 31XRT door opening(background obs) (CT jitter data) 32EIS clamshell opening(background obs) (CT jitter data) 33Update pointing offsets (background obs) CT servo-on /off 34(background obs) CT servo-on (ready for running) 35Tracking start (around DC) Fine focus scan (adjust focus) Fine focus scan (adjust focus) Fine focus scan 36(Flat fields) Continuous obs (Flat fields) Continuous obs 37TF wavelength scan (adjust tuning) (background obs) 38TF wavelength scan(background obs)CT wedge check 39NFI observables(background obs)

Apr 17-22, NAOJ11 (III) SOT instrument checkout phase (2) Y+S/C major eventFGSPCT 40Pointing to limbImage quality stability CT wedge check 41Limb optic check 42TF wavelength scan(background obs) 43NFI observables(background obs) 44Go back to DCImage quality stability 45NFI observables(background obs)

Apr 17-22, NAOJ12 (1) Top-door opening / Initial optical check One of the most critical event in the initial operation Make the satellite pointing to the disk center Light level is continuously monitored by CT live images when the door opening operation. After the top-door is successfully opened, we plan to switch observation tables to carry out the initial optical checkout. –Light level check for FG (all the wavelengths), SP, and CT –SP / spectrum line positions and profiles –Alignment check to the sun-sensor (chromospheric features may provide pointing information even in QS) Quick focus scan and adjustment are planned to be done in real- time operation half a day after the door operation.

Apr 17-22, NAOJ13 (2) Background observations during the operation of the other telescopes SOT commanding operation cannot be done during the door opening operation of the other telescopes. We plan to run some observation tables in background with low cadence in order to verify the following items. –Data transfer from Svalvard station –Image compression efficiency –Dark images, flat fielding (by averaging many images) –Camera noise (light transfer measurement) –Alignment with respect to XRT and EIS –CT diagnostic data to get S/C jitter information –SP full FOV scanning (to check vignetting and alignment) BFI observations (e.g. G-band) with shorter exposure can be possibly carried out without correlation tracker. Such observations with longer duration may provide information on orbital variation of image quality.

Apr 17-22, NAOJ14 (3) Correlation tracker servo-on / Detailed verification of optical performance After CT servo is turned on, we can go to detailed verification and calibration of optical performance. Fine focus scan –Image quality evaluation –Co-focus among different channels –Adjust focus position if necessary Continuous observations for several hours with a few wavelengths –Orbital variation of image quality –Inter-channel alignment –Image quality degradation by disturbance from FPP, XRT and EIS Flat fielding –Flat fielding by intentionally move the tip-tilt mirror Tunable filter (TF) wavelength scan/ NFI observables –TF spectroscopic performance –Update tuning parameters if necessary –Verification of MDP Doppler velocity compensation

Apr 17-22, NAOJ15 (4) Limb observation After optical performance verification is done near the disk center, we like to go to limb observation. The verification items in the limb observation are –S/C pointing check –Image quality and focus change between DC obs and limb obs –Scattered light –TF wavelength tuning, MDP Doppler compensation –Function of the correlation tracker in limb obs.

Apr 17-22, NAOJ16 Pointing and target selection in the first light phase We have to know misalignment with respect to the sun sensor (ACS), XRT, and EIS as fast as possible for the secure operation. After the satellite pointing is established, we like to track a suitable active region near the disk center if we have for verification of the optical performance (as well as scientific interest). When the verification near the disk center is done, the limb observation is necessary to verify performance of SOT at the limb. We may go to the limb observation automatically by tracking an active region in the first light phase. After the limb observation, we can make SOT pointing to any region.

Apr 17-22, NAOJ17 (IV) Performance verification (PV) phase Period: Y+46  Y+60 (TBD) (  2 weeks) After the first light phase The primary purpose in this phase is verification of scientific performance of the SOT observables Background: –SOT has a capability to observe various scientific targets. –Wavelength coverage BFI 6 channels, NFI 6 channels, and SP 6302A –Many types of observables Single image, LOS magnetograms, Stokes IQUV, and Dopplergrams –Temporal and spatial sampling Knowledge obtained in this phase shall be used for following scientific operation.

Apr 17-22, NAOJ18 (IV) Performance verification (PV) phase Phase-I –At first, we verify performance of high-priority observables with a typical wavelength to verify basic scientific performance of SOT –Only one observable or simple combination are used for long duration (several hours  half a day). –SP observations can be carried out simultaneous with FG. Phase-II –After the verification of each observable is completed, we make combined observations with multiple wavelengths and observables. –SP observations can be carried out simultaneous with FG.

Apr 17-22, NAOJ19 (IV) PV Phase-I Make observations with some observables with typical wavelength for long duration to verify long-term stability. Some of them can be carried out in the first light phase as background observation ObservablesWavelengt h FOVCadenceDuration 1FiltergramsG-band / H-alpha 4K x 2K1 min0.5 day 2Dopplergrams (with continuum obs.) Fe I 5576A2K x 1K1 min0.5 day 3Shuttered Stokes IQUV (with continuum obs.) Fe I 6302A2K x 1K4 min0.5 day 4LOS magnetogram (with continuum obs.) Fe I 6302A2K x 1K1 min0.5 day Examples of FG observation sequences

Apr 17-22, NAOJ20 (IV) PV Phase-I ObservablesFOVCadenceDuration 1Normal mapping320”x160”160 min1 day 2Fast mapping320”x160”60 min0.5 day 3Dynamics16” x 32”3 min0.5 day 4Deep magnetogram32” x 160”30 min0.5 day Examples of SP observation sequences Some FG observables, especially magnetograms and Dopplergrams, shall be carried out simultaneous with SP in order check their performance.

Apr 17-22, NAOJ21 (IV) PV Phase-II Make combined observations with multiple wavelengths and observables. ObservablesWavelengthFOVCadenceDuration 1FiltergramsAll wav for BFI and NFI 4K x 2K12 min0.5 day 2Dopplergrams (with continuum obs.) Fe I 5576A Mg I 5173A 2K x 1K2 min0.5 day 3LOS magnetogram (with continuum obs.) Fe I 6302A Fe I 5250A Na D 5896A 2K x 1K2 min0.5 day 4Shuttered Stokes IQUV (with continuum obs.) Fe I 6302A Fe I 5250A Mg I 5173A 2K x 1K12 min0.5 day 5Shutterless Stokes IQUV (with continuum obs.) Fe I 6302A Fe I 5250A Mg I 5173A 64 x 1K1 min0.5 day Examples of FG observation sequences (multiple wavelength combination)

Apr 17-22, NAOJ22 Target region selection in PV phase  In general, we track one active region for several days - one week.  When there is no active region on the sun, we observe quiet regions, dark filaments etc. with science priority.