HMI First Sun Test Review December 2, 2005

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HMIFirst Sun Test ReviewDecember 2, 2005
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Agenda
Topic Presenter Time
Overview Objectives Miles 15 min
Test Requirements Schou
Lessons Learned Bush
Test Plan Moskal
Test Descriptions Schou, Bush, Tarbell, Hoeksema, Miles
Test Data Processing Schou
Test Readiness Drake, Kirkpatrick, Miles
Concerns and Issues
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Objectives

• Objectives of the sun test review
• Verify that planned tests meet the verification
  requirements appropriate for the sun test.
• Show that all hardware, software, facilities,
  procedures, and personnel are available and
  prepared to support the test.
• Objectives of the sun test
• Learn how to operate the HMI optics package.
• Learn how to characterize/calibrate the
  instrument. In some cases, obtain initial
  calibration parameters.
• Discover gross errors in design or workmanship of
  the HMI optics package.
• Determine position of focus to set the final shim
  on the telescope secondary lens.
• Results of the sun test will directly feed into
  the plans and procedures for the formal test and
  calibration series.
• The sun test does not provide formal verification
  of any requirements.

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HMI Integration and Test Flow
Dec 05
Cnfg I
Cnfg II
Develop SW Accpt Test
Initial Sun Tests
In Air Calibration
HOP w/BB Functional Test
Roll Over
CIF BBHEB
Apr 06
Mar 06
Flight CCD DM Camera Install ISS
BB HEB (no CIF) DM CCD, DM Camera No ISS
Install Flt Cameras
Alignment Thermostats
Sine Vibration
Acoustics
Random Vibration
Quasi-static Loads
HOP w/BB Functional Test
HOP Vibration Prep
May 06
Complete Flight HOP Only - Functional Test w/
BBHEB
Repeated for X-, Y-, and Z-axes
Cnfg Flight
Flight Sftwr Acct Test
CPT
Special Test
EMI/EMC Prep
Aliveness Test
EMI/EMC
HOPHEB Functional Test
HEB FT
Flight HEB
Sine Vibration
Random Vibration
Quasi-static Loads
HEB Vibration Prep
HEB FT
HEB Flight
HEB FT
Jul 06
Aug 06
Conformal Coat
Repeated for X-, Y-, and Z-axes
Delivery to GSFC 40D Slack
Vacuum Calibration
TV/TB Prep
Aliveness Test
Thermal Balance
Thermal Vacuum
CPT
Special Test
Sept 06
Nov 06
Sine signature
Transport HOP
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HMI Instrument Test Configurations

• HMI Instrument Configuration 1
• Brassboard Electronics Box
• Brassboard Cables
• Optics Package Non-flight hardware
• Flight CCD with flight focal plane housing (one
  location)
• DM Camera (one location)
• Optics Package Flight hardware
• Structure with alignment mechanism, legs, and
  mounting brackets
• Telescope assembly front window filter, primary
  lens, secondary lens, mounting bracket
• Polarization selector and wavelength tuner (seven
  HCMs)
• Harness (mechanisms only)
• ISS mirror and beam-splitter
• Oven assembly
• BDS beam-splitter and fold mirror
• CCD fold mirror (two)

• HMI Instrument Configuration 2
• Brassboard Electronics Box
• Brassboard Cables
• Optics Package Install flight items
• Focal plane (two)
• ISS limb sensor and preamp box
• Oven controller electronics box
• More harness
• Finish heater routing
• Install vents
• Oven thermostat
• Replace Lyot elements one and two
• Replace NB Michelson

• Tests
• ISS Testing
• CCD Alignment
• In-air calibration
• HOP Vibration testing

• Tests
• Initial Sun Test
• Initial Functional Tests

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HMI Instrument Test Configurations

• HMI Instrument Flight Configuration
• Fight electronics box
• Flight Harness
• Flight HOP

• HMI HEB Flight Configuration
• Conformal coated boards in HEB
• Flight Harness
• Flight HOP

• Tests
• Software Acceptance Test
• Flight CPT
• EMI/EMC Test

• Tests
• HEB Vibration Test
• Vacuum Calibration
• Thermal Balance and Thermal Vacuum

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Test Article Configuration for Initial Sun Test

• Optics
• All flight optics in place except as noted below.
• Michelsons are likely to be replaced with a
  better set after the sun test.
• Lyot elements 1 and 2 are likely to be replaced
  with better elements after the sun test.
• Telescope not set in final focus final focus
  position to be determined from sun test data.
• No ISS actuation.
• Camera and Detector
• DM camera electronics and flight CCD with forward
  flight focal plane housing and flight-like
  headboard.
• No side camera.
• Thermal
• Flight oven and preamp, ETU oven controller.
• No operational heater thermal control.
• No MLI.

• Mechanisms
• All seven flight hollow core motors with flight
  optics.
• Both flight focus / calibration wheels with
  flight optics
• Flight alignment legs.
• Flight shutters.
• No front door mechanism.
• Mechanical
• Flight structure with legs and mounting brackets
• Non-flight HOP cover non-flight covers in place
  of radiators and vents.
• Cables
• Flight HCM, shutter, and cal/focus wheel
  harnesses non-flight alignment leg harness
• Non-flight CCD flex cable.
• Brassboard intra-instrument harness.
• Brassboard HEB
• No CIF.
• Environment
• Ambient temperature and pressure

8
Setting Final Telescope Focus

• The sun test must provide enough data to
  calculate the proper distance between the primary
  and secondary lenses, and hence, the proper shim
  size at the secondary lens.
• We have already used two tests to determine the
  proper primary-secondary spacing
• Set up primary and secondary lens to form the
  best image, and measured the distance between the
  lenses and the image.
• Set up telescope and spherical mirror centered at
  telescope focus with interferometer to produce
  the best fringes, and measure the distance
  between the lenses and the mirror.
• Using a Zemax model to compensate for the in-air
  measurements and the as-built lens prescriptions,
  a shim size was determined.
• The focus test and image scale measurements will
  provide the data necessary to go back to the
  Zemax model and determine whether any further
  as-built deviations in the optics could be
  optimally compensated in the primary-secondary
  spacing.
• The results of these tests will determine the
  final flight shim for the telescope, and the
  secondary mirror mount with flight shim will be
  potted in place to that position.

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Sun Test Overview
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Sun Test Flow
Distortion
Flat field
Contamination
Focus
Alignment leg range, step size, repeatability
Image scale
Linearity
Ghost images
MTF
Scattered light
Field curvature
Filter spatial / angular dependence
Polarization
Image motions, offset, distortion
Filter wavelength dependence
Doppler observables
Filter throughput
Line of sight observables
Vector observables
Sun
Laser
Lamp
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Sun Test Overview Interdependencies

• At least three tests are prerequisites for other
  tests
• Focus
• Can use either Sun or lamp
• Needed to reduce length of other tests
• Not needed for many tests due to bad seeing or
  spatial averaging
• Wavelength dependence
• Either Sun or laser can be used
• Needed to set tuning positions
• Not needed for lamp or polarization tests
• Polarization calibration
• Lamp or Sun can be used
• Needed to make observing sequences. Especially
  LOS.
• Note that none of these are dependent on each
  other
• Others are needed before analysis can be completed

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Sun Test Overview Other prerequisites

• There are a number of other tests we need to
  perform before starting
• Determine exposure times
• Lamp
• Sun
• Laser
• Test various targets
• Determine spatial power and quality of each
• Alignments
• Stim tel
• Laser
• Heliostat
• Existing focus test procedure may be used for
  these

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Sun Test Go/no go criteria

• Several types of criteria
• Prerequisites done See separate charts
• Equipment available and properly configured
• Laser and wavemeter working
• PCU properly configured
• Targets available/installed
• Sunlight
• Some require long stretches of clear skies
• Others can use shorter stretches and/or light
  clouds
• STOLs working
• Procedural issues resolved
• See overview chart and individual tests for
  details

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Sun Test Pass/fail criteria

• This is not an acceptance test!
• However, we are looking for gross errors
• Note that in many cases all we need is
  characterization NOT pass/fail
• Two levels
• Do we have the required data?
• If no pass/fail then we only need to know when we
  have data of sufficient quality
• Have we analyzed the data?
• If pass/fail needed or if test is prerequisite
  for other tests we need short turn around
• Analysis software for prerequisites is ready
• Preliminary results and decisions will be part of
  calibration meetings
• In case of gross errors high level decisions
  needed
• Abort Sun test and fix problem
• Continue with other parts of test

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Sun Test Priorities

• Several competing criteria for priority
• Make good use of sunlight
• May not get that many days
• Do prerequisites first
• Equipment constraints
• Dont want to fire up laser too often
• Dont want to change PCU configuration too often
• Allow efficient development and testing of STOL
  procedures
• Easy ones first
• Test various types
• Maximize time to develop and run analysis
  procedures
• Data of marginal quality (eg. clouds) may still
  allow for some testing
• May need data from other instruments
• MDI under our control, but keyhole
• May like to have data from ground based. GONG,
  SOLIS, ASP,
• Near real time flexibility will be required to be
  efficient!
• With this in mind

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Sun Test Attack plan

• Get STOLs for prerequisites ready before test
  starts
• Focus done. Wavelength dependence and PCU both
  well defined
• Run all relevant STOLs we have as soon as we can
• Can check for proper functioning may do
  abbreviated versions to save time
• Gives sample data for analysis code development
• POR Dont do extensive real time debugging
• Run STOLs even if ideal source not available
• With luck we can have prerequisites done on day
  one!
• Does depend on PCU operational
• Does depend on Sun shining or laser working
• Dont use laser on day one
• Probably takes too long to get set up
• Can use other sources for initial tests
• But do get it to work soon, especially if
  forecast calls for solid overcast
• Plan further tests depending on weather, people
  and equipment availability
• Try to get prerequisites done as soon as possible
• Do weekly and daily planning

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Lessons Learned from MDI FPP Rock Bush, Ted
Tarbell

• Have several standard stimulus setups, with
  more than one person knowing how to change from
  one to another.
• Keep a log of which setup is used for every test
  and any deviations from standard
• Test and cal procedures evolve by trial and
  error need prompt (not necessarily real time)
  data analysis and STOL/procedure editing.
• Have scientists analyze the data who are not
  involved in collecting the data.
• Decide on measurements for trending and start
  early keep standard, clear tables/web sites of
  results.
• Need quick look (almost real time) viewing of
  images during testing interactive X, Y, I ltIgt,
  etc. measurements

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Sun Test Plan Ryan Moskal

• Ground Support Equipment (GSE)
• Procedures (logs, shop orders, etc.)
• Test Flow
• Facilities
• Provide a description of the required test
  facility, including floorplan.
• Describe the characteristics and capabilities of
  the test facility and required support equipment.
  (lasers, interferometers, stim tel, PCU,
  heliostat, etc.)

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GSE

• Status

• Mechanical
• Targets pinhole, other
• Stimulus telescope with white light lamp and dye
  laser
• PCU
• Interferometer
• Heliostat
• Light meter for light source monitoring
• Wave meter for wavelength tuning verification
• Mechanical hoist
• Electrical
• Spacecraft simulator
• Workstations for running STOL procedures
• Workstations for collecting data from instrument
• RAL EGSE
• Software
• Flight software
• STOLs

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Procedures

• Testing takes place in HMI Cleanroom (Sun Lab,
  Bay 3)
• Shop order for each procedure
• Provides the steps to run one test procedure and
  gather data
• A procedure can gather data for more than one
  test
• STOL modifications necessary during testing are
  captured in STOL development shop order, not test
  procedure shop order
• Test setup log appears in Appendix A of test
  sequence shop orders
• Mate/De-mate log
• Must be updated throughout the testing process
• Step in shop order

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Test Flow
Align HMI with heliostat
Align PCU in optical path
Tests Stim tel with lamp
Tests Stim tel with heliostat
Tests Stim tel with dye laser

• PCU will always be in optical path but PCU optics
  will move out of the optical path when not in use
• Details on dye laser vs. white light lamp setup
  and how to switch between
• Details on GSE cover (Will there be a case where
  we need to remove the cover to adjust/examine?)

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Test Setup Stimulus telescope with white light
lamp
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Test Setup Stimulus telescope with dye laser
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Test Setup - Heliostat
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Individual Test Descriptions
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Image Quality Focus

• Purpose
• Determine the nominal focus position
• Requirements
• Need to take images for other tests near optimal
  focus. Also needed to set secondary shim.
• Description
• Determine spatial power as a function of focus
  setting. Fit model to determine ideal focus.
• Test configuration
• Stimulus telescope with lamp and desired
  target(s) (dots). Sun may also be used to
  illuminate target.
• Also do with direct sunlight from heliostat.
• Test plan
• Take images at all 16 focus positions.
• Data analysis
• For each focus position determine the amount of
  spatial power. Fit parabola to three highest
  points to determine best focus.
• For the Sun it may be possible to use the
  sharpness of the limb.
• Codes are ready.
• Procedure
• STOL status Exists.
• Shop order status Does not exist
• The test timeline 16 images of 10s or 3 minutes.
  Little setup required.

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Image Quality Distortion

• Purpose
• Determine the amount of optical distortion.
• Requirements
• 0.001 (0.02 pixels) based on Korzennik et al.
  (204) 0.01pixels desirable.
• Description
• Determine parameters in distortion model by
  offpointing instrument using alignment legs.
• Test configuration
• Stimulus telescope with lamp and desired
  target(s) (dots). Sun may also be used to
  illuminate target.
• Test plan
• At each of 5x5 leg offsets, take images at a few
  positions around the nominal focus.
• Data analysis
• For each focus position determine the offsets
  between each pair of images for a grid of points
  in the images.
• Fit distortion model to the measured offsets.
• Codes are ready.
• Procedure
• STOL status Does not exist
• Shop order status Does not exist
• The test timeline Each series is 25 offsets
  times 5 focus positions for a total of 125
  images. At 10s per images this will take 20
  minutes. Needs to be run for a few targets plus
  setup so a few hours.
• No particular personnel required.

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Mechanism induced images motions and distortions

• Purpose
• Determine the image motions and distortions
  introduced by rotating the optics in the hollow
  core motors.
• Requirements
• CPS gives 0.1 (0.2 pixels). IPD 4.3 gives a goal
  of 0.1 pixels.
• Description
• Determine offsets by taking images of fixed
  target at various HCM rotation angles.
• Test configuration
• Stimulus telescope with lamp and desired
  target(s) (dots). Sun may also be used to
  illuminate target.
• Test plan
• For each of 7 HCMs and each of 10 or so angles,
  take images at a few positions around the nominal
  focus.
• Data analysis
• At each focus position determine the offsets
  between each pair of images for a grid of points
  in the images..
• Code is ready.
• Procedure
• STOL status Does not exist
• Shop order status Does not exist
• The test timeline About 100 images. At 10s per
  images this will take 20 minutes. Needs to be run
  for a few targets plus setup so a few hours.
• No particular personnel required.

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Image Quality Field curvature

• Purpose
• Determine the amount of field curvature.
• Requirements
• The change of focus as a function of image
  position should be a fraction of a focus step.
• Description
• Determine spatial power as a function of focus
  setting, leg offset and image position. Fit
  model.
• Test configuration
• Stimulus telescope with lamp and desired
  target(s) (dots). Sun may also be used to
  illuminate target.
• Also do with sunlight.
• Test plan
• Same as for distortion. Also use sun focus
  series.
• Data analysis
• At each leg position and image position fit mode
  power as a function of focus position to
  determine best focus.
• For Sun test no additional analysis required.
• For lamp test analyze focus as a function of
  offset and position to separate stim tel and HMI
  curvature.
• Codes are mostly ready.
• Procedure
• STOL status Exists for Sun test. Does not exist
  for lamp test.
• Shop order status Does not exist

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Image Quality MTF

• Purpose
• Determine the MTF variation as a function of
  image position.
• Requirements
• Astigmatism should be a fraction of a focus step.
  The MTF at any k should not be degraded by more
  than that corresponding to a(?) focus step. 10
  or better knowledge is desirable.
• Description
• Determine spatial power as a function of k and
  image position at best focus.
• Test configuration
• Stimulus telescope with lamp and desired
  target(s) (dots). Sun may also be used to
  illuminate target.
• Also do with sunlight.
• Test plan
• Same as for distortion. Also use sun focus
  series.
• Data analysis
• At each leg position and image position fit mode
  power as a function of k at best focus.
• For Sun test no additional analysis required.
• For lamp test analyze power as a function of
  offset and position to separate stim tel and HMI
  MTF.
• Codes are mostly ready.
• Procedure
• STOL status Exists.
• Shop order status Does not exist

31
Image Quality Image scale

• Purpose
• Determine the absolute image scale.
• Requirements
• The image scale should be between 0.494/pixel
  and 0.505/pixel.
• Description
• Take images of Sun. Determine diameter and
  compare to ephemeris.
• Test configuration
• Sun from heliostat.
• Test plan
• Take solar images at each focus position.
• Data analysis
• Determine solar image diameter. Look up diameter
  in in ephemeris. Divide numbers.
• Code exists.
• Procedure
• STOL status Exists.
• Shop order status Does not exist
• The test timeline Data already taken for other
  tests.
• No particular personnel required.

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Contamination

• Purpose
• Determine if any large particles are present in
  the optical path.
• Requirements
• Any contaminants should not be large enough to
  degrade science.
• Description
• Using a pinhole camera mode look for shadows
  from contaminants and determine their position in
  the optical path by determining motion when
  moving pinhole.
• Test configuration
• Stimulus telescope with lamp or Sun and direct
  sunlight. PCU with hole plate.
• Laser in stimulus telescope with leg offsets.
• Test plan
• For each hole position or each leg offset take
  image in obs and cal mode.
• Also rotate each HCM at one or more hole and leg
  positions.
• Data analysis
• Offset images proportional to pinhole offset.
  Look for shadows coming into focus. Determine
  position in optical path from raytrace and
  proportionality constant used for shifting.
• For HCM rotations look for moving shadows.
• Codes exists for MDI.
• Procedure
• STOL status Does not exist
• Shop order status Does not exist

33
Polarization calibration

• Purpose
• Determine intsrument polarization matrix.
• Requirements
• See IPD.
• Description
• Using light with well determined polarization
  determine instrument response.
• Test configuration
• Stimulus telescope with lamp or Sun and sunlight
  from heliostat.
• Test plan
• Using PCU take series of images with various PCU
  and instrument settings.
• Data analysis
• Too complicated to describe here.
• Codes are ready.
• Procedure
• STOL status Does not exist
• Shop order status Does not exist
• The test timeline 50-100 images in obs and
  calmode required for Sun and lamp. Total one day.
• No particular personnel required.

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Image Quality Linearity Light Transfer

• Objective
• Determine the calibration necessary to correct
  for CCD response non-linearities, the exposure
  limit for calibratable response, and the camera
  noise characteristics
• Requirements
• Measure the CCD mean response and noise variance
  as a function of exposure time, from dark to
  full-well
• Description
• Take pairs (or more) of identical images at
  each exposure time in a list, which ranges from
  the shortest possible exposure to long enough to
  saturate the CCD
• Test configuration
• Can be done with lamp or stable sun best
  illumination is smoothly varying but not uniform
• Can be done with dark current useful for
  trending in test setups where no light source
  available
• Test plan
• Set up light source (or block for dark test),
  take list of exposures, quickly look at data to
  verify adequate exposure range, repeat with
  modified exposure times if necessary
• Data analysis
• Plot analyze linearity curve (mean output vs.
  exposure time) and light transfer curve (variance
  of output vs. mean output)
• FPP IDL code exists, mods for HMI are
  straightforward
• Procedure
• STOL status may exist (use a standard exposure
  list STOL)
• Shop order status does not exist
• The test timeline 20-30 images for each source
  desired, lt 5 minutes per set, half an hour for
  entire test
• No special personnel requirements

35
Alignment Mechanism Step Size, Repeatability,
and Range

• Objective
• Determine alignment leg step size, step
  repeatability, and full range of travel in
  arcseconds on the sky.
• Requirements and Description
• Measure step size at center of travel, and at 300
  arcsec from center, to within 0.25 arcsec.
• Measure step repeatability within the vicinity of
  the center of travel to within 0.25 arcsec.
• Measure step repeatability between center of
  travel and 300 arcsec from center to within 0.25
  arcsec.
• Measure full range of travel to within 10 arcsec.
• Test configuration
• Lamp input, Grid target, PCU out.
• HMI focused and image scale measured.
• Procedure
• STOL status hmi_find_center hmi_move_legs_to_cen
  ter hmi_set_leg_position, ral_tp
• Shop order status
• Personnel one test conductor one data analyst.

• Test plan
• Start with both alignment legs at home position.
  Move one leg 3 single steps in one direction,
  then 6 single steps in the opposite direction,
  then 3 single steps back to the nominal start
  position. Take an image of the grid target at
  each position. Repeat with the other leg.
• Repeat the above, but with the starting position
  300 arcseconds from home position (in a direction
  requiring equal actuation of the two legs).
• Calculate step size and step repeatability in
  arcseconds from images, using knowledge of image
  scale.
• Set alignment legs to the four extreme positions
  (which is about 700 arcsec) and take images at
  each position. Measure range of motion in images
  using knowledge of image scale.
• Data analysis
• Find crosshair centroids to within half a pixel
  in HMI images.

36
Observables Doppler Velocity

• Purpose
• Test end-to-end function and performance of the
  instrument with a prime HMI observable.
  Quantitative understanding of the sources,
  levels, and changes in the signal and noise in
  individual Dopplergrams and time series taken in
  different configurations will validate many other
  tests and calibrations. Images and data series
  will be used for testing analysis pipelines as
  well as the instrument and observing sequences.
  Generation of a rudimentary solar k-w diagram
  will demonstrate function of instrument hardware,
  software, and analysis components.
• Requirements
• A repeatable, uniform set of tuned filtergrams
  must be obtained at a rapid, regular cadence to
  generate each Dopplergram. Individual
  Dopplergrams provide a reasonably good end-to-end
  verification that the whole system is working,
  once noise sources are understood. Times series
  of Dopplergrams are required to reduce noise and
  produce a signal that can be analyzed in the
  science pipelines. Analyzable data from at least
  one lengthy (several hour) sequence obtained with
  a reasonable cadence in sunlight must be provided
  in cal mode and in image mode.
• Description
• Single Dopplergrams will be used to characterize
  the instrument performance and noise levels and
  validate instrument simulations. The early tests
  will be dominated by noise and so will provide
  only a gross indication of how things are
  working. Individual Dopplergrams for all sources
  except the imaged Sun should be very uniform and
  highly predictable. Solar observations will
  provide a known signal measured by other
  instruments against which to compare. Solar time
  series will be analyzed to disentangle the
  changes caused by the instrument and the Sun.
  Stim telescope observations may be useful for
  determining instrument noise levels and stability.

• Test Configuration
• Solar target should be centered and focused in
  image mode.
• The instrument should be in as flight-like a
  configuration as possible proper focus and
  alignment, tuning, temperature control, guiding,
  air/vacuum, data collection, etc
• Test Plan
• The test begins and ends with a set of standard
  characterizations and repeats a standard sequence
  in between. This presumes that you can record
  the sequence of filtergrams for a Dopplergram
  every minute or so.
• Start Verify image focus and centeringCollect
  5 darksRun shortest detune sequenceTake 5
  Image-Mode DopplergramsTake 5 Cal-mode
  Dopplergrams
• Prime Dopplergram Sequence (run N times)Repeat
  Desired-Mode Dopplergrams 20-times, maintaining
  image centeringTake one Cal-mode
  DopplergramTake one Image-mode DopplergramTake
  5 darks
• End Verify image focus and centeringRun
  shortest detune sequenceTake 5 darks 
• Data Analysis
• Generate Dopplergrams from filtergrams
• Simulate instrument response under test
  conditions (e.g. noisy CCD)
• Characterize observed signal and noise levels in
  test configurations
• Compare observed data with expected signal and
  noise
• Compare with data from other observatories

37
Observables Line of Site Magnetic Field

• Purpose
• This end-to-end HMI observable test will
  demonstrate that the instrument can measure
  magnetic fields. Sensitivity to noise will be
  somewhat different than Dopplergrams. Depending
  on noise levels, an initial verification of
  magnetic sensitivity will be possible.
  Systematic effects will reveal irregularities
  that are otherwise not apparent. Unlike the
  changing Doppler signal, averaging time series of
  stable magnetic observations should reduce noise.
• Requirements
• Rapid, repeatable sequences of filtergrams are
  required. Remapping of filtergrams will be
  required, at least for time sequences.
  Algorithm for determining magnetic field from
  filtergrams required. Time series of
  magnetograms will be averaged to increase the
  signal to noise ratio. Simultaneous observations
  of magnetic field from other observatories
  required. Understanding of noise sources
  required.
• Description
• The line-of-sight magnetic field observable is
  conceptually the difference of interleaved
  Dopplergrams observed in two circular
  polarizations. Understanding the Dopplergram
  noise is a component of understanding the
  magnetogram signal available during the sun
  tests. The magnetic sequence is significantly
  longer, so filtergrams may need to be registered
  to provide a meaningful signal, though the seeing
  will result in poor resolution. Magnetograms
  will probably require a better flat field than
  the Dopplergrams.

• Test Configuration
• Flight-like solar observations in cal mode and
  image mode. 
• Test Plan
• Know flat field
• Know dark current
• Short detune for solar orientation
• Take one cal and one image magnetogram
• Take one Doppler sequence in each polarization,
  cal image
• Take time series of image magnetograms (10)
• Take time series of cal magnetograms (10)
• Take one Doppler sequence in each polarization
• Take one cal and one image magnetogram
• Short detune for solar orientation
• Know dark current
• Know flat field
• Data Analysis
• Filtergrams will probably need to be registered.
  Magnetograms certainly will.
• Magnetic algorithm will need to be tested and
  verified
• Comparison with simultaneous MDI magnetograms to
  test sensitivity, noise, dynamic range, image
  quality

38
Observables Vector Magnetic Field

• Objective
• Demonstrate that HMI can measure vector magnetic
  fields.
• Demonstrate the proficiency of the polarization
  calibration
• Requirements
• Active region on solar disk is required.
  Polarization calibration tests (item 21) are
  needed in order to analyze data. Algorithm for
  inverting the observations is needed.
  Simultaneous vector magnetic field maps, from
  SOLIS perhaps, would be very beneficial. Hour
  long observations taken with "Mod A" and also in
  "Mod C" are needed.
• Description
• The vector magnetic field is determined using a
  model solar atmosphere and inversion technique
  with full Stokes profile information.
  Polarization modulation in the form of "Mod A" or
  "Mod C" will allow sampling of Stokes I, Q, U and
  V over the spectral line so that we can recover a
  coarse spectral sampling of these Stokes
  profiles. Demodulation of polarization is done
  in combination with a correction of polarization
  introduced by the telescope. The data is then
  inverted using a model solar atmosphere (ME) and
  least squares inversion code. Short term data
  products and ten minute averages will be made.
  For the second sun test with two cameras in
  place, a test for using both cameras for
  obtaining the vector field will be conducted.

• Test configuration
• Flight-like solar observations in cal and obs
  mode.
• Test plan
• Several flats and darks detune seq Take one Mod
  A and one Mod C vector sequence in both cal and
  obs mode.
• Run one hour of Mod A Run one hour of Mod C.
• One Mod A and one Mod C vector sequence in both
  cal and obs mode. Detunes Several flats and
  darks.
• For second sun test that will have in flight
  optics, two cameras and be in vacuum, run an
  additional observation of an hour with only I/-Q
  and I/U observed on vector camera while the
  I/-V is observed on doppler camera.
• Data analysis
• Filtergrams will need to be registered.
  Polarization states will be demodulated including
  correction of telescope matrix. Data will then
  be used with solar model and inversion code to
  recover vector magnetic field data. The signal
  and noise levels will be analyzed. Ideally, data
  will be compared to simultaneous vector data from
  another instrument.
• Procedure
• STOL status may exist (use a standard exposure
  list STOL)
• Shop order status does not exist
• The test timeline 20-30 images for each source
  desired, lt 5 minutes per set, half an hour for
  entire test
• No special personnel requirements

39
Data Processing

• Will use MDI data system (DSDS) for storing data
• Should easily be able to handle data volume
• Will use HMI data system (DRMS) for metadata
• Still in beta test, but alternatives exist
• A few basic utilities will be available
• Data query, selection and export
• Image reconstruction (remove cross)
• Etc.
• Analysis will be done with ad-hoc code
• Mostly IDL
• Observables code may have to be optimized to
  reduce computing time
• Codes for prerequisites exist

40
Hardware Readiness Kirkpatrick

• Alignment status
• Camera
• Safe-to-Mate
• GSE
• PCU
• Air-to-Vac Corrector
• Air-to-vac corrector lens used with either the
  heliostat or the Stim-Tel to produce images in
  focus at the location of the CCD with the
  instrument in ambient pressure.
• Stim-tel
• Heliostat
• Other GSE

41
Software Readiness Drake

• Topics
• Flight Software
• GSE
• Camera
• STOL
• Tables

42
Sun Test Electrical Block Diagram
43
Flight Software

• Mechanism control software and state machines in
  place for
• HCMs (3 Polarization Selector mechanisms and 4
  Wavelength Tuning mechanisms)
• Shutters
• Calibration/filter wheels
• Alignment legs
• Two mechanism control software elements being
  completed
• Front door mechanism
• Not needed for first sun test
• FPGA updated for problem with open/closed
  switches, not yet tested
• Only 1 of 2 FPGAs changed out on HEB brassboard
  system
• Sequencer
• Works with hard-coded framelist
• Framelist table upload in development
• Initial tests will not use sequencer

44
GSE and Camera

• LMSAL EGSE In place and ready
• Release 6.6 development
• RAL GSE Camera Control Interface
• Being modified
• PCU Control
• Stimulus telescope intensity control (not done)
• RAL GSE In place and ready
• Camera
• Development model camera control through RAL GSE
  from LMSAL EGSE STOL
• Work-around for lack of Camera InterFace (CIF)
  board in HMI brassboard
• Images have been taken through this interface and
  provided to Stanford for data analysis/processing
• Header content being updated

45
Sun test STOL list

• Name Status
• hmi_focus Written, not tested
• hmi_leg_focus Higher level STOL invoking
  hmi_focus, not written
• hmi_leg_repeat Higher level STOL invoking
  hmi_focus, not written
• hmi_flatfield Similar to hmi_leg_focus, not
  written
• hmi_pl_wobble Written, not tested
• hmi_wl_wobble Written, not tested
• hmi_find_center Written, needs review/demonstratio
  n
• hmi_set_leg_position Not written
• hmi_pcu_ss_moda Written, not tested
• hmi_pcu_ls_modc Written, not tested
• hmi_move_legs_to_center Use HMI_MC_AL_MOVE
  MECHAL1/2 TARGETX
• hmi_set_known_pos Need known positions
• hmi_set_home_pos Needs home positions

46
Sun test STOL list

• Name Status
• hmi_picture_loop Not written
• hmi_set_all_hcm_zero Needs encoder values to set
  HCM to
• hmi_set_position Not written
• hmi_dop_seq5 Not written, use wl_wobble_10 table
• hmi_detune27 Not written, make table?
• hmi_pcu_fringes Not written
• hmi_pcu_hole Not written
• hmi_linearity Not written
• ral_menu Works, being revised
• ral_tp Works, being revised

47
Tables

• Name Status
• cal_focus Done
• pl_wobble_10 Written, not tested
• wl_wobble_10 Written, not tested
• pcu_ss_moda Reviewed by Jesper, needs updating
• 
  Use equation to convert angle to encoder
• 
  Remove redundant areas
• pcu_ls_modc Reviewed by Jesper, needs updating
• Use equation to convert angle to encoder
• 
  Remove redundant areas

48
Documentation

• Test Plan
• This review chart package, together with a cover
  sheet signature page, constitutes the the Sun
  Test Plan (HMI01567).
• Procedures (shop orders)
• The test procedures are documented in the shop
  orders under which all tests are carried out. No
  test may proceed without a signed shop order.
• Shop orders signed off by Test lead system
  engineer deputy program manager mission
  assurance
• Applicable Documents
• HMI IT Plan, HMI Contract Performance Spec, HMI
  Calibration Plan, HMI IPD
• Test Reports
• Each test lead will prepare a test report and
  attach it to the shop order associated with the
  test.
• Test reports explain results related to
  requirements and identify trended data.
• For any failures, discuss root cause, corrective
  action, and plan for retest.
• All test reports related to in-air calibration
  items are due Feb 06.
• All test reports related to functional test items
  are due Mar 06. (To support pre-environmental
  test review).
• All remaining test reports due Apr 06.

49
Concerns Issues All

• High priority items
• Laser brightness out of the fiber is low.
• Sunlight into stimulus telescope If we can get
  lots of sunlight this will work better than the
  lamp for some purposes. Can also be used instead
  of laser light for a few tests.
• Laser reliability.
• Targets.
• Wavemeter accuracy.
• RAL headers.
• RAL camera interface a lot of coding and testing
  is still needed.
• Flat field determination need to decide what to
  do.
• Availability of people. We are stretched thin.
• Transfer of data from LMSAL to Stanford.

• Lower priority items
• Stimulus telescope brightness.
• We don't know how the solar image rotates during
  the day.
• Fastest cadence.
• Linearity measurement.
• Long term issues
• Monitoring of laser brightness.
• Scattered light in spectrograph.