hmi helioseismic and magnetic imager for the solar dynamics observatory bao – beijing, july 2006
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Page 1 COSPAR2006-A-01469 HMI
HMIHelioseismic and Magnetic Imager for the
Solar Dynamics Observatory
BAO – Beijing, July 2006
P.H. Scherrer, J. Todd Hoeksema
And the HMI Team
Stanford University
Stanford Lockeed Institute for Astrophysics and Space Research
Page 2 COSPAR2006-A-01469 HMI
Outline
• The SDO Mission
• Instrument Overview
• Calibration Activities
• HMI Science Goals
• Observations & Observables
• Joint Science Operations Center
Page 3 COSPAR2006-A-01469 HMI
The Science of SDO
Page 4 COSPAR2006-A-01469 HMI
SDO Science Requirements
•What mechanisms drive the quasi-periodic 11-year cycle of solar activity?
•How is active region magnetic flux synthesized, concentrated & dispersed across the solar surface?
•How does magnetic reconnection on small scales reorganize the large-scale field topology and current systems?
•How significant is it in heating the corona and accelerating the solar wind?
•Where do the observed variations in the Sun’s total & spectral irradiance arise, how do they relate to the magnetic activity cycle?
•What magnetic field configurations lead to CMEs, filament eruptions and flares which produce energetic particles and radiation?
•Can the structure & dynamics of the solar wind near Earth be determined from the magnetic field configuration & atmospheric structure near the solar surface?
•When will activity occur and is it possible to make accurate and reliable forecasts of space weather and climate?
Page 5 COSPAR2006-A-01469 HMI
Sensing the Sun from Space
• High-resolution Spectroscopy for Helioseismology and Magnetic Fields
– Observe ripples and polarization properties on the surface of the Sun
– Sound waves require long strings of continuous data to interpret—satellites may have no day/night cycle
– Convection zone velocities and magnetic fields require high spatial resolution
• Coronal Imaging
– Observe bright plasma in the corona at ultraviolet wavelengths —can’t be seen from ground
– Temperatures of the plasma range from 50,000 K to >3 million K
– High spatial resolution to see the detailed interaction of the magnetic field and the plasma
– High time resolution is required to see how those features develop
• Spectral Irradiance
– Measure the total energy in narrow wavelength bands
– Measure from space to avoid the twinkling and absorption of atmosphere
– Essential for models of the ionosphere
• Coronagraphs
– Light scattered from the corona and solar wind
– Track material as it exits the Sun and moves through the solar system
• Energetic Particles and Fields
– Point measurements from many platforms to resolve structure
Page 6 COSPAR2006-A-01469 HMI
The SDO MissionNASA/LWS Cornerstone Solar Mission
• NASA and three Instrument Teams are building SDO
– NASA/ Goddard Space Flight Center: build spacecraft, integrate the instruments, provide launch and mission operations
– Lockheed Martin & Stanford University: AIA & HMI
– LASP/University of Colorado: EVE
– Launch is planned for August 2008 on an Atlas V EELV from Cape Canaveral
– SDO will be placed into an inclined geosynchronous orbit ~36,000 km (21,000 mi) over New Mexico for a 5-year mission
– Data downlink rate is 150 Mbps, 24 hours/day, 7 days/week (1 CD of data every 36 seconds)
– Data is sent to the instrument teams and served to the public from there
• The primary goal of the SDO mission is to understand, driving towards a predictive capability, the solar variations that influence life on Earth and humanity’s technological systems by determining:
– How the Sun’s magnetic field is generated and structured
– How this stored magnetic energy is converted and released into the heliosphere and geospace in the form of solar wind, energetic particles, and variations in the solar irradiance.
Atlas V carries Rainbow 1 into orbit, July 2003.
Page 7 COSPAR2006-A-01469 HMI
The SDO SpacecraftThe SDO Spacecraft
The total mass of the spacecraft at launch is 3200 kg (payload 270 kg; fuel 1400 kg).
Its overall length along the sun-pointing axis is 4.5 m, and each side is 2.22 m.
The span of the extended solar panels is 6.25 m.
Total available power is 1450 W from 6.5 m2 of solar arrays (efficiency of 16%).
The high-gain antennas rotate once each orbit to follow the Earth.
AIA (1 of 4 telescopes)
EVE (looking at CCD radiator and front)
HMI (looking down from top)
High-gain antennas (1 of 2)
Page 8 COSPAR2006-A-01469 HMI
EUV Variability Experiment
• EVE is the Extreme ultraviolet Variability Experiment
• Built by the Laboratory for Atmospheric and Space Physics at the University of Colorado in Boulder, CO
• Data will include– Spectral irradiance of the Sun
• Wavelength coverage 0.1-105 nm
• Photodiodes to give activity indices
• Full spectrum every 20 s
– Information needed to drive models of the ionosphere
– Cause of this radiation
– Effects on planetary atmospheres
Page 9 COSPAR2006-A-01469 HMI
Page 10 COSPAR2006-A-01469 HMI
SDO Operations
• Mission operations for SDO are at NASA's Goddard Space Flight Center near Washington, DC.
• Communications with the spacecraft are via two radio dishes at NASA's site in the White Sands Missile Range in New Mexico.
• The main tasks of the controllers are to keep SDO pointing at the Sun, maintain its inclined geosynchronous orbit, and keep the data flowing.
• A scientific team, led by NASA and instrument project scientists, plans and executes programs of observations with SDO’s 3 instruments suites, and analyzes the data.
• Unique Operations Mode
– Few observing modes: turn it on and let the data flow!
– Raw images are sent to the ground for processing
– Data is made available soon after downlink; people can use the data in near-real-time
– Campaigns and collaborations are coordinated where convenient, but the data is always available
TDRSS antennae in White Sands Missile Range
Page 11 COSPAR2006-A-01469 HMI
Mission Orbit Overview
• The SDO geosynchronous orbit will result in two eclipse seasons with a variable daily eclipse each day
– The two eclipse seasons will occur each year
– During each eclipse season, SDO will move through the earth’s shadow- this shadow period will grow to a maximum of ~72 minutes per day, then subside accordingly as the earth-sun geometry moves out of the SDO eclipse season
• Eclipse season effects:
– Instrument• Interruption to SDO science collection
• Thermal impacts to instrument optical system due to eclipse
– Power • Temporary reduction or loss of power from solar arrays
• Battery sizing includes eclipse impact
– Thermal• S/C thermal design considerations due to bi-annual eclipses
Page 12 COSPAR2006-A-01469 HMI
HMI Instrument Overview
Page 13 COSPAR2006-A-01469 HMI
Helioseismic & Magnetic Imager
• HMI is the Helioseismic and Magnetic Imager
• Built at Stanford University and Lockheed
Martin in Palo Alto, CA
• Two 4096 x 4096 CCDs
• Instrument is designed to observe polarized
light to measure the magnetic field
Page 14 COSPAR2006-A-01469 HMI
HMI Overview
• The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to study the origin of solar variability and to characterize and understand the Sun’s interior and the various components of magnetic activity.
• HMI makes measurements of several quantities
– Doppler Velocity (13m/s rms.).
– Line-of-sight (10G rms.) and vector magnetic field.
– Intensity
– All variables all the time with 0.5” pixels.
– Most at 50s or better cadence.
– Variables are made from filtergrams, all of which are downlinked.
• Higher level products will be made as part of the investigation.
• All data available to all.
• Launch in August 2008. 5 Year nominal mission.
• Education and Public Outreach program included!
Page 15 COSPAR2006-A-01469 HMI
Instrument Overview
• Optics package
– Telescope section
– Polarization selectors – 3 rotating waveplates for redundancy
– Focus blocks
– Image stabilization system
– 5 element Lyot filter. One element tuned by rotating waveplate
– 2 Michelson interferometers. Tunable with 2 waveplates and 1 polarizer for redundancy
– Reimaging optics and beam distribution system
– Shutters
– 2 functionally identical CCD cameras
• Electronics package
• Cable harness
Page 16 COSPAR2006-A-01469 HMI
Image stabilization mirror
CCD fold mirror
CCD fold mirrorFold mirror
¼ Waveplate ½ Waveplates
Telescope lens set Telecentric
lens
Calibration lensesand focus blocks
Front window filter
Relay lens set
Blocking filter
BDS beamsplitter
NarrowbandMichelson
Polarizer
ISS beamsplitterand limb tracker assembly
Tuningwaveplates
Beam control lens
Lyot
WidebandMichelson
CCD
CCD
Shutter assemblies
Aperture stop
Instrument Overview – Optical Path
Optical characteristics:Focal length: 495 cmFocal ratio: f/35.2Final image scale: 24m/arcsec = 0.5”/pixelPrimary to secondary image magnification: 2Focus adjustment aange: 16 steps of 0.4 mm
Filter characteristics:Central wavelength: 613.7 nm FeIFront window rejects 99% solar heat loadFinal filter bandwidth: 0.0076 nmTuning range: 0.069 nmAll polarization states measurable
Page 17 COSPAR2006-A-01469 HMI
Ray trace
Page 18 COSPAR2006-A-01469 HMI
Instrument Overview – HMI Optics Package (HOP)
OP Structure
Telescope
Front Window
Front Door
Vents
Support Legs (6)
Polarization Selector
Focus/Calibration Wheels
Active Mirror
Limb B/S
Alignment Mech
Oven Structure
Michelson Interf.
Lyot Filter
Shutters
Connector Panel
CEBs
Detector
Fold MirrorFocal Plane B/S
Mechanical Characteristics:Box: 0.84 x 0.55 x 0.16 mOver All: 1.19 x 0.83 x 0.29 mMass: 39.25 kgFirst Mode: 63 Hz
YX
Detector
Limb Sensor
Z
Page 19 COSPAR2006-A-01469 HMI
HMI Assembly Status
Optics Package Assembly
Detector Assembly(Non-Flight)
CEB (Non-Flight, DM1)
Flex-Cables(Eng Model)
Telescope(Flight)
Front Window(Flight)
Primary work after Sun testing:• Bond optics in place• Replace painted parts (including the oven)• Replace one HCM and focus/cal optical mounts
ISS Mirror(Flight)
Polarization Selector(Flight)
Focus/Cal Wheels(Flight)
Limb Sensor(Non-Flight)
ISS Beam Splitter(Flight)
Oven Assembly(non-flight)Parts to replace:E1 and E2 in LyotNB MichelsonPainted housing
BDS Beamsplitter(Flight, hidden by shutter)
Shutters(Flight)
BDS Fold Mirror(Flight)
CCD Fold Mirror(Flight, hidden by detector)
Alignment Mechanism(Flight, hidden in view)
Internal Harness(Flight, not complete)
Limb Pre-amp Box(Flight, not complete)
StructureW/ legs and heaters(Flight)
Oven Controller(ETU)
Page 20 COSPAR2006-A-01469 HMI
Status - Michelsons
Michelson ETU
Page 21 COSPAR2006-A-01469 HMI
HMI Assembly Status
Structural model testing completed ETU oven testing completed BB HEB fabrication completedSUROM acceptance test completed
mission CDR
Received flight MichelsonsAll flight optics in house
Received flight metering tubeCompleted telescope alignment
Received flight structureStart alignment on GSE bench
Hollow core motors completedReceived DM cameras
Received 4 grade zero CCDs
Alignment mechanism completedStarted optical alignment of HOP
BB HEB and EGSE readyShutter & F/C wheels completed
Internal harness completed
Lyot completedInternal mechanisms tested
Focal plane completedOven completed
First image
Page 22 COSPAR2006-A-01469 HMI
Status - Cameras
Image of CCD Image with CCD
Page 23 COSPAR2006-A-01469 HMI
HMI Testing Progress
12/22/06 02/01/0601/30/0601/25/0601/11/06
Tests Performed:
Initial set up w/ lampFocus test w/ lampDistortion, field curvature and MTF w/ lampFocus test w/ SunFilter wavelength dependence w/ Sun
Filter wavelength dependence w/ laserField curvature and MTF w/ SunPolarization calibration w/ Sun
Tests In Progress:
Laser dotBefore holidayNo relay lensNo Lyot No frt Window
Special targetLamp - stim telLyot installedTemp mnt for relay lensNot fully aligned stim tel
Air Force targetLamp - stim telAll together
Laser intensity improved
“HMI is Alive”First Image “Special Target”
First Lamp Image “Ready to Test”Instrument All Together “No More Moon”
Better Laser Image “It’s a Beautiful Day”First Sun Image
Just sunlightWith air/vac corrector
Page 24 COSPAR2006-A-01469 HMI
HMI Calibration Activities
Page 25 COSPAR2006-A-01469 HMI
Status
• Instrument is almost complete
– Only one non-flight Camera installed
– No CIF and DCHRI boards installed
– No radiators
– No heaters and thermistors
– No vents
– No front door
– Non flight cover
– ISS still being worked
– Many items need to be mounted permanently
– Except, perhaps, for one of the Michelson all optics are flight
• In-Air and vacuum calibrations later this summer
• Delivery in March 2007
• Launch in August 2008
Page 26 COSPAR2006-A-01469 HMI
Upcoming Tests
• Suntest2
– Mostly repeat what was done in first suntest
• Verify that instrument has been properly reassembled
– Check for gross errors
– Check that earlier problems have been corrected
• Eg. Birefringence in focus block
– Provide data to adjust various components
• Eg. Calmode lenses, waveplate rotation, CCDs, …
– Check software
• Must be in good shape before actual calibrations
• In-air calibration
– Gather actual calibration data
• Some, such as part of polarization may not be doable in vacuum
• Vacuum calibration
– Repeat most in-air calibrations with lower noise
– Some items only doable in vacuum (E.g. Noise tests)
Page 27 COSPAR2006-A-01469 HMI
Sun Test Objectives
• Learn how to operate the HMI optics package.
• Learn how to characterize/calibrate the instrument.
• Discover gross errors in design or workmanship of the HMI optics package.
• Determine position of focus to set the final shim on the secondary lens.
• Determine position of waveplates in polarization selector to set the final orientation relative to hollow core motor step locations.
• 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.
• The Sun test does not provide final calibration data.
• The instrument had not been finally assembled during first Sun test.
– Several components were missing.
– Several components have since been changed.
– Test setup was under development.
– Test procedures and analysis software were under development.
Page 28 COSPAR2006-A-01469 HMI
Calibration Matrix
123456789
1013141617181920212223
24
252628
30
31
32333435363839
A B C F G N O P QTest Group Property First
SunLight Source Status
1 Image quality Distortion Yes Lamp Not yet finished2 Image scale Yes Sun All OK
3a MTF Yes Lamp Minor problem3b MTF Yes Sun Taken Bad4a Focus Yes Lamp Really bad4b Field curvature Yes Lamp4c Focus Yes Sun4d Field curvature Yes Sun Taken*7 Ghost images Yes? All? ?????*8 Scattered light Yes? All? ?????10 CCD and Camera Flat field Yes Lamp11 Linearity Yes Lamp
*12a Quadrant crosstalk No? Lamp ?????*12b Quadrant crosstalk No? Laser ?????13a Contamination Yes Lamp13b Contamination Yes Sun13c Contamination Yes Laser14 Image motions Offset and distortion Yes Lamp15 Filter transmission Wavelength and
spatial dependenceYes Laser + Sun
16 Angular dependence Yes Laser + Sun
17 Stability No? Laser or Sun? ?????19 Throughput Yes Sun
21a Polarization All sorts of stuff Yes Lamp
21b Polarization All sorts of stuff Yes Sun
22 Observables performance
Doppler Yes Sun
23 Line of sight Yes Sun24 Vector Yes Sun
*25 Thermal effects Pointing No? Lamp ?????*26 Focus No? Lamp ?????28 Alignment legs Range and step size Yes Lamp29 Repeatability Yes Lamp
Page 29 COSPAR2006-A-01469 HMI
Image Quality
• Distortion
• Image scale
• MTF
• Focus and field curvature
• Ghost images and scattered light
• Contamination
• Image motions
Page 30 COSPAR2006-A-01469 HMI
Image Wobble
Page 31 COSPAR2006-A-01469 HMI
Image focus
Page 32 COSPAR2006-A-01469 HMI
HMI Testing Progress
First Magnetogram First Dopplergram
Page 33 COSPAR2006-A-01469 HMI
HMI Science Goals
Page 34 COSPAR2006-A-01469 HMI
Primary goal: origin of solar variability
• The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to study the origin of solar variability and to characterize and understand the Sun’s interior and the various components of magnetic activity.
• HMI produces data to determine the interior sources and mechanisms of solar variability and how the physical processes inside the Sun are related to surface and coronal magnetic fields and activity.
Page 35 COSPAR2006-A-01469 HMI
HMI Science Objectives
• HMI science objectives are grouped into five broad categories:
– Convection-zone dynamics
• How does the solar cycle work?
– Origin and evolution of sunspots, active regions and complexes of activity
• What drives the evolution of spots and active regions?
– Sources and drivers of solar activity and disturbances
• How and why is magnetic complexity expressed as activity?
– Links between the internal processes and dynamics of the corona and heliosphere
• What are the large scale links between the important domains?
– Precursors of solar disturbances for space-weather forecasts
• What are the prospects for prediction?
• These objectives are divided into 18 sub-objectives each of which needs data from multiple HMI data products.
Page 36 COSPAR2006-A-01469 HMI
A. Sound speed variations relative to a standard solar model.
B. Solar cycle variations in the sub-photospheric rotation rate.
C. Solar meridional circulation and differential rotation.
D. Sunspots and plage contribute to solar irradiance variation.
E. MHD model of the magnetic structure of the corona.
F. Synoptic map of the subsurface flows at a depth of 7 Mm.
G. EIT image and magnetic field lines computed from the photospheric field.
H. Active regions on the far side of the sun detected with helioseismology.
I. Vector field image showing the magnetic connectivity in sunspots.
J. Sound speed variations and flows in an emerging active region.
B – Rotation VariationsC – Global Circulation
D – Irradiance Sources
H – Far-side Imaging
F – Solar Subsurface Weather
E – Coronal Magnetic Field
I – Magnetic Connectivity
J – Subsurface flows
G – Magnetic Fields
A – Interior Structure
HMI Data Product Examples
Page 37 COSPAR2006-A-01469 HMI
HMI Science Objectives
• Convection-zone dynamics and the solar dynamo
• Structure and dynamics of the tachocline
• Variations in differential rotation
• Evolution of meridional circulation
• Dynamics in the near surface shear layer
• Origin and evolution of sunspots, active regions and complexes of activity
• Formation and deep structure of magnetic complexes of activity
• Active region source and evolution
• Magnetic flux concentration in sunspots
• Sources and mechanisms of solar irradiance variations
• Sources and drivers of solar activity and disturbances
• Origin and dynamics of magnetic sheared structures and d-type sunspots
• Magnetic configuration and mechanisms of solar flares
• Emergence of magnetic flux and solar transient events
• Evolution of small-scale structures and magnetic carpet
• Links between the internal processes and dynamics of the corona and heliosphere
• Complexity and energetics of the solar corona
• Large-scale coronal field estimates
• Coronal magnetic structure and solar wind
• Precursors of solar disturbances for space-weather forecasts
• Far-side imaging and activity index
• Predicting emergence of active regions by helioseismic imaging
• Determination of magnetic cloud Bs events
Page 38 COSPAR2006-A-01469 HMI
HMI Science Analysis Plan
Magnetic Shear
Tachocline
Differential Rotation
Meridional Circulation
Near-Surface Shear Layer
Activity Complexes
Active Regions
Sunspots
Irradiance Variations
Flare Magnetic Configuration
Flux Emergence
Magnetic Carpet
Coronal energetics
Large-scale Coronal Fields
Solar Wind
Far-side Activity Evolution
Predicting A-R Emergence
IMF Bs Events
Brightness Images
Global Helioseismology
Processing
Local Helioseismology
Processing
Version 1.0w
Filtergrams
Line-of-sightMagnetograms
Vector Magnetograms
DopplerVelocity
ContinuumBrightness
Line-of-SightMagnetic Field Maps
Coronal magneticField Extrapolations
Coronal andSolar wind models
Far-side activity index
Deep-focus v and cs
maps (0-200Mm)
High-resolution v and cs
maps (0-30Mm)
Carrington synoptic v and cs
maps (0-30Mm)
Full-disk velocity, v(r,Θ,Φ),And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Internal sound speed,cs(r,Θ) (0<r<R)
Internal rotation Ω(r,Θ)(0<r<R)
Vector MagneticField Maps
Science ObjectiveData ProductProcessing
Observables
HMI Data
Page 39 COSPAR2006-A-01469 HMI
Solar Domain of HMI Helioseismology
rota
tion
2
3
4
5
6
7
Sun
Log
Siz
e (k
m)
Zonal flow
AR
spot
SG
dynamoP
-mod
es
Tim
e-D
ista
nce
Rin
gs
Glo
bal H
S1 2 3 4 5 6 7 8 9
min
5min
hour
day
year
cycl
e
Log Time (s)
10
polar field
Earth
HMI resolution
granule
Page 40 COSPAR2006-A-01469 HMI
Solar Domain of HMI Magnetic Field
2
3
4
5
6
7
Sun
Log
Siz
e (k
m)
Large-Scale
AR
spot
SG
dynamoP
-mod
es
1 2 3 4 5 6 7 8 9
min
5min
hour
day
rota
tion
year
cycl
e
Log Time (s)
10
polar field
Earth
HMI resolution
Granule
Coronal field estimates
Vector
Line-of-sight
Page 41 COSPAR2006-A-01469 HMI
Key Features of HMI Science Plan
• Data analysis pipeline: standard helioseismology and magnetic field analyses
• Development of new approaches to data analysis
• Targeted theoretical and numerical modeling
• Focused data analysis and science working groups
• Joint investigations with AIA and EVE
• Cooperation with other space- and ground-based projects (SOHO, Solar-B, PICARD, STEREO, RHESSI, GONG+, SOLIS, etc)
Page 42 COSPAR2006-A-01469 HMI
HMI Observing Scheme
Page 43 COSPAR2006-A-01469 HMI
Observing Scheme
• Observables
– Dopplergrams
– Magnetograms, vector and line-of-sight
– Others: Intensity, line depth, etc.
• Observables made from filtergrams described by framelists
• Filtergram properties
– Wavelength – selected by rotating waveplates (polarizer for redundancy only)
– Polarization state – selected by rotating waveplates
– Exposure time
– Camera ID
– Compression parameters, …
– Determined by subsystem settings
• E.g. motor positions
• Framelists
– List of filtergrams repeated at fixed cadence during normal operations
– Entirely specified in software – Highly flexible
Page 44 COSPAR2006-A-01469 HMI
Framelist Example
• Time: Time of first exposure at given wavelength since start of framelist execution
• Tuning: I1, I2, … specify the tuning position
• Doppler pol.: Polarization of image taken with Doppler camera
– L and R indicate left and right circular polarization
– Used for Doppler and line of sight field
• Vector pol.: Polarization of image taken with vector camera
– 1, 2, 3, 4: Mixed polarizations needed to make vector magnetograms
– Used for vector field reconstruction
• Note that the data from the two cameras may be combined
Page 45 COSPAR2006-A-01469 HMI
Observables Calculation
• Make I, Q, U, V, LCP, RCP
– Linear combinations of filtergrams
– Correct for flat field, exposure time and polarization leakage
– Correct for solar rotation and jitter (spatial interpolation)• Sun rotates by 0.3 pixels in 50s, so interpolation necessary
• Fast and accurate algorithm exists
– Correct for acceleration effects (temporal interpolation)• Nyquist criterion almost fulfilled for Doppler and LOS but is violated for vector measurements
• Significant improvement from interpolation and averaging
– Fill gaps• Data loss budget gives missing data in every filtergram, various algorithms exist
• May do nothing for vector field
• Calculate observables
– MDI-like and/or least squares for Doppler and LOS
– Fast and/or full inversion for vector field
• Many challenges remain
– Calibration, code development, lists of dataproducts etc.
– Community input needed!
Page 46 COSPAR2006-A-01469 HMI
HMI Data Processing and Products
HMI Data Analysis Pipeline
DopplerVelocity
HeliographicDoppler velocity
maps
Tracked TilesOf Dopplergrams
StokesI,V
Filtergrams
ContinuumBrightness
Tracked full-disk1-hour averagedContinuum maps
Brightness featuremaps
Solar limb parameters
StokesI,Q,U,V
Full-disk 10-minAveraged maps
Tracked Tiles
Line-of-sightMagnetograms
Vector MagnetogramsFast algorithm
Vector MagnetogramsInversion algorithm
Egression andIngression maps
Time-distanceCross-covariance
function
Ring diagrams
Wave phase shift maps
Wave travel times
Local wave frequency shifts
SphericalHarmonic
Time seriesTo l=1000
Mode frequenciesAnd splitting
Brightness Images
Line-of-SightMagnetic Field Maps
Coronal magneticField Extrapolations
Coronal andSolar wind models
Far-side activity index
Deep-focus v and cs
maps (0-200Mm)
High-resolution v and cs
maps (0-30Mm)
Carrington synoptic v and cs
maps (0-30Mm)
Full-disk velocity, v(r,Θ,Φ),And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Internal sound speed,cs(r,Θ) (0<r<R)
Internal rotation Ω(r,Θ)(0<r<R)
Vector MagneticField Maps
HMI DataData ProductProcessing
Level-0
Level-1
Page 47 COSPAR2006-A-01469 HMI
Joint Science Operations CenterJSOC – HMI & AIA
Page 48 COSPAR2006-A-01469 HMI
Joint HMI/AIA SOC
• Common aspects– Instrument commanding
– Telemetry data capture (MOC to JSOC and DDS to JSOC interfaces)
– Pipeline generation of Level-1 data
– Distribution of data to co-investigator teams and beyond
– Location of facilities
• Unique requirements– HMI Higher Level Helioseismology Data Products
– AIA Visualization and Solar Event Catalog
Page 49 COSPAR2006-A-01469 HMI
JSOC Scope
• The HMI/AIA Joint SOC consists of two parts:– Science Data Processing (SDP) – at Stanford and LMSAL
– Joint Operations Center (JOC) – at LMSAL
• JSOC JOC includes:
– HMI and AIA Commanding and Health Monitoring
– HMI and AIA Engineering support as needed
• JSOC SDP includes:
– HMI and AIA Telemetry Data capture (from DDS) and archive
– HMI and AIA Level-0 processing and archive
– HMI processing through to level-2 with archiving of end products
– AIA processing through level-1a with online archive at Stanford
– AIA level-2 processing at LMSAL
– Data export of the above and other HMI and AIA products as needed
• JSOC does not include tasks such as:
– Science analysis beyond level-2 products
– HMI and AIA EPO
– HMI & AIA Co-I science support
Page 50 COSPAR2006-A-01469 HMI
SDO Ground System Architecture
10/21/03
Telemetry & Command System
ASIST / FEDSTelemetry Monitoring
Command Management
HK Data ArchivalHK Level-0 Processing
Ground Station Control
DDS ControlAutomated Operations
Anomaly detection
Flight DynamicsSystem
Maneuver PlanningProduct Generation
R/T Attitude Determination
Sensor/Actuator Calibration
SDO Mission Operations Center
EVE SOC
Acquisition Data
Observatory Commands
Observatory HK Telemetry
Tracking Data
Integrated Trending& Plotting System
Mission Planning& Scheduling
Plan daily/periodic eventsCreate engineering planGenerate Daily Loads
HMI Science Data (55Mbps)
Ka-Band:150 Mbps
Science Data
Instrument Commands/Loads
Data DistributionSystem
(Incl. 30-Day Science Data Storage)
Ka Science Data
AIA R/T HK Telemetry/ Science Planning and FDS Products
EVE R/T HK Telemetry Science Planning and FDS Products
Universal Space Network
S-Band HK Tlm
CMD, Acquisition
Data
Station/DDS Control
Station/DDS Status
SDO Ground StationWSGT
Ka-Band:150 Mbps
Science Data
S-Band: TRK, Cmd & HK Tlm
S-Band: TRK,Cmd & HK Tlm
Alert NotificationSystem
Flight Software Maintenance Lab
Flight software loadsSimulated housekeeping telemetry
S/C Memory dumpsSimulated commands
Same Interfaces
as WSGT Ground Station
HMI AIA JSOC
Stanford Univ.
Science Data Capture
LMSAL
Instrument Monitoring& Control Instrument Commands/Loads
SDO Ground StationSTGT Flight Dynamics
FacilityOrbit DeterminationProduct Generation
Tracking Data
OD Products
Space Network(L&EO only)
S-Band: TRK,Cmd & HK Tlm
S-Band HK Tlm
Tracking Data
CMD
Acquisition DataS-Band: TRK & HK Tlm
DDS & Ground Station Control
AIA Science Data (67Mbps) EVE Science Data (7Mbps)
(Palo Alto, CA)
(Stanford, CA)
Tracking Data
Ka Science Data
Status and
Control
LASP(Boulder, CO)
Science Data CaptureInstrument Monitoring
& Control
Data Ack. & Retrans. RequestsData Ack. & Retrans. Requests
FLATSAT
Instrument Commands/LoadsHMI R/T HK Telemetry/ Science Planning and FDS Products
SDO
WSC
FSW SupportTool Suite
DDS & SDOGSIntegrated Manager
GSFC
S-Band RF &FEP system
Ka-Band RF system
(Includes 72-hr storage)
DDS FEP(Incl. 120-hr
storage)
S-Band RF &FEP system
Ka-Band RF system
(Includes 72-hr storage)
DDS FEP(Incl. 120-hr
storage)
Status and
Control
Mini MOC
Page 51 COSPAR2006-A-01469 HMI
HMI & AIA JSOC Architecture
Redundant
Data Capture System
Redundant Data Capture System
AIA HMI
30-DayArchive
Science TeamForecast Centers
EPOPublic
Catalog
Primary Archive
HMI & AIAOperations
House-keeping
Database
OffsiteArchiv
e
OfflineArchiv
e
JSOC Pipeline Processing System
HMI/AIA Level-0, 1, HMI-level2
DataExport& WebService
Stanford
LMSAL
High-LevelData Import
AIA Analysis System
Local Archive
QuicklookViewing
MOCDDShousekeeping
GSFCWhite Sands
World
Page 52 COSPAR2006-A-01469 HMI
JSOC Data Export System
DRMS
Pa
cka
ge
Format
Custom Keywords
Utilities
Selected
DataRecords
API
Dril
ldo
wn
OverviewNew/AvailStatistics
KeywordsRange
Se
arc
hB
row
se
Researcher A
General Public
Grid AdaptorGrid
VSO AdaptorVSO
CoSEC CoSEC Adaptor
Researcher B
Script Access
Space Weather
VSO – Virtual Solar ObservatoryDRMS – Data Record Mgmt Sys
Page 53 COSPAR2006-A-01469 HMI
JSOC SDP Development Milestones
• HMI and AIA Data EGSE installed
– Prototype for I/F testing with GS March 2005
– Version 2 to support flight inst. June 2005
• JSOC Capture System
– Purchase computers Fall 2006
– Final system installed Spring 2007
– Support DDS testing Summer 2007
• JSOC SDP Infrastructure, SUMS, DRMS, PUI
– Prototype testing of core system June 2005
– Fully functional Jan, 2006
• Purchase computers for JSOC Spring, 2007
• Infrastructure Operational Summer, 2007
• Data Product Modules Spring, 2008
• Test in I&T and with DDS,MOC as called for in SDO Ground System schedule
Page 54 COSPAR2006-A-01469 HMI
Summary
•HMI/SDO Will Provide Excellent New Data
•The Instrument Development is On Track
•Much Science Can Be Accomplished
•All Data are Available to Any Researcher
•The Team Very Much Wants Your Participation
Page 55 COSPAR2006-A-01469 HMI
Backup slides
Page 56 COSPAR2006-A-01469 HMI
• The AIA team will stimulate joint observing and analysis.– Coordinated observing increases the coverage of the global Sun-Earth system (e.g., STEREO, coronagraph,
wind monitors, …), provides complementary observations for the solar field (e.g., vector field, H filament data) and its atmosphere (Solar-B/EIS spectral information). And it increases interest in analysis of AIA data.
– The AIA team includes PI’s and Co-I’s from several other space and ground based instruments committed to coordination (perhaps “whole fleet months”):
• EVE and HMI needs have been carefully taken into account in setting plate scale, field of view, cadence, and channel selections, and in science themes.
Science Coordination
HVMI GBO coronagr.
SOLIS
SOLAR B EIS
SOLAR B FPP
SOLAR B XRT
AIA
Soft X-ray images for complementary T-coverage in corona
Full-Disk:Vector Field Convection
Flows (spectra) for 3-D velocities & geometry
Densities + Calibration
Vector Field small scales
H
EVECalibration
STEREO SECCHI2D 3D
GOES
CME propagationHigh Field Wind structure
Energetic Particles
RHESSIACESTEREO -WAVES
Flows (spectra) for 3-D velocities and geometry
FASRVLA
OVRO
Full-Disk Chromosphere Surface Vector Field for field extrapolation
(Non) Thermal ParticlesCoronal Field
Other
AIA Co-I’s
On SDOLegend:
Page 57 COSPAR2006-A-01469 HMI
The EVE Instrument on SDO
Page 58 COSPAR2006-A-01469 HMI
EUV Variability Experiment
• EVE is the Extreme ultraviolet Variability Experiment
• Built by the Laboratory for Atmospheric and Space Physics at the University of Colorado in Boulder, CO
• Data will include– Spectral irradiance of the Sun
• Wavelength coverage 0.1-105 nm
• Photodiodes to give activity indices
• Full spectrum every 20 s
– Information needed to drive models of the ionosphere
– Cause of this radiation
– Effects on planetary atmospheres
Page 59 COSPAR2006-A-01469 HMI
EVE Data & Research
• One spectrum every 20 seconds is the primary product
• Driver of real-time models of the upper atmosphere of the Earth and other planets
• Identify sources of EUV irradiance (with AIA)
• Predict the future of EUV irradiance (with HMI)
Below (left): Example spectrum from EVE. The elements emitting some of the lines and where the lines are formed in the solar atmosphere is noted at the top.
(right) Absorption of radiation as it enters the Earth’s atmosphere. Red areas are altitudes that do not absorb a wavelength, black means complete absorption. The layers of the atmosphere are also listed. All of the radiation measured by EVE is absorbed above 75 km, most above 100 km.
Page 60 COSPAR2006-A-01469 HMI
Page 61 COSPAR2006-A-01469 HMI
JSOC Data Requirements
this version modified to show the links to the hardware plan
img size channels
cadence
compress
HMI: 55,000,000 bps ** SU 553 30 16 200% 395 90
AIA: 67,000,000 bps ** SU 674 30 20 200% 482 90
HMI: 4k*4k*2 bytes/2-seconds*(pi/4) 3.4E+07 2 4 0.39 SU 530 100 52 100% 189 180
AIA: 4k*4k*2 bytes * 8 imgs per 10 seconds 3.4E+07 8 10 0.50 SU 1,080 30 32 100% 386 1,900
HMI: V,M,Ic @ 45s & B, ld, ff @ 90s*(pi/4) 3.4E+07 5.5 45 0.39 SU 130 0 0 46 0
AIA: Level 1.0 same as level-0 3.4E+07 8 10 0.50 tbd 1,080 90 95 10% 39
HMI: See below 7.5E+10 1 86400 1.00 SU 70 0 0 25 100% 25 0
AIA (lev1a): movies & extracted regions. @ 20% 6.7E+06 8 10 0.50 LM 216 0 0 77 100% 77 0
HMI: Magnetograms (M, B) 3.4E+07 5 90 0.39 na 59 100 6 0
AIA: Full Level-0 data+lev1_extract 3.5E+07 8 10 0.50 na 1,134 100 111 0
HMI: 2 * Higher Level products + 5*10 min B SU 149 60 1 0
AIA: 3* higher Level products (TRACE < 1) SU 648 60 6 0
HMI: tlm SU 553 100% 198
AIA: tlm SU 674 100% 241
HMI: Lev0, Lev-1, All Higher SU 730 412
AIA: Lev0, Lev1a SU 1,296 743
HMI Totals 68 71 610
AIA Totals 146 77 984
Combined (TB) 214 148 1,594
Tape shelf size (TB) 7,968
Tape shelf number of tapes - mixed density 11,257
Export
Near-line retain days
Tape Archive Fraction
Totals
2,026Local tape
LMSAL Link 1,193
1,227Offsite tape
Higher level 286
Level-1
Data Path Assumptions Combined (GB/day)
Fixed Disk cache (TB)
Online disk cache days
Perm disk per year (TB)
Level-01,610
Volume (GB/day)
Processed at
In from DDS
Tape per year (TB)
1,227
1,210
797
TotalsCapture System Offsite Archive SUMS Archive Transient, 10 day
Page 62 COSPAR2006-A-01469 HMI
JSOC Pipeline Processing System Components
Database Server
SUMSStorage Unit
Management System
DRMSData Record
Management SystemSUMS Tape Farm
SUMS Disks
Pipeline Program, “module”
Record Manage
ment
Keyword Access
Data Access
DRMS Library
Link Manage
ment
Utility LibrariesJSOC Science
Libraries
Record Cache
PUIPipeline User
Interface
Pipeline processing
plan
Processing script, “mapfile”
List of pipeline modules with needed datasets for input, output
Pipeline Operato
r
Processing History Log
Page 63 COSPAR2006-A-01469 HMI
Illustration of solar dynamo
Page 64 COSPAR2006-A-01469 HMI
Page 65 COSPAR2006-A-01469 HMI
Calibration Status as of Feb. 12, 2006
• White – Not yet finished
– Taken: Data taken but not yet analyzed
– ?????: May not be doable with current configuration (eg. high camera dark current)
• Green – Test done, all is OK
• Yellow – Minor problems
– Incomplete or buggy analysis software.
– Fixable test setup problem or apparent test glitch (eg. clouds)
– Problem is understood and is easy to correct
– Problem is understood and can’t be fixed, but does not impact full science objectives
• Red – Instrument problem potentially impacting science objectives, but
– Not yet fully understood
– Has known likely solution with modest modest schedule and cost impacts
• Black – Fatal problem found
– Problem understood and science objectives can’t be met
– Solution is unknown or has severe cost or schedule impacts
• Surgeon General’s warning: Preliminary results may cause severe upsets!
Page 66 COSPAR2006-A-01469 HMI
Image Quality
• Distortion– Procedure works, but problems with stimulus telescope illumination. Difficult to do with Sun.
• Image scale– All OK. 0.5025”/pixel
• MTF– Astigmatism seen, but problems with stimulus telescope illumination
– Sun data not yet analyzed
• Focus and field curvature– Right on for lamp. Bad seeing during Sun test
– Field curvature analysis not complete
• Ghost images and scattered light– Difficult to do with high camera noise. May have to be deferred to vacuum test
• Contamination– Still needs to be done
• Image motions– Saw problems with test setup. Probably has been solved
– Some displacements seen with focus blocks
Page 67 COSPAR2006-A-01469 HMI
Special target continued
Page 68 COSPAR2006-A-01469 HMI
Observables and Miscellaneous
• Observables
– Still to be done. May wait for some instrument upgrades
• Thermal effects
– Probably not doable in air
• Alignment legs
– Range and step size determined. Meets spec.
– Repeatability. Looks adequate, but more tests planned
Page 69 COSPAR2006-A-01469 HMI
Status - Mechanisms
Page 70 COSPAR2006-A-01469 HMI
Conclusion
• Tests progressing– Some tests done
– Some not
• Some problems found– Some fixed
– Some still need work
– No showstoppers!
• Lots of data to analyze– Over 10000 images so far
– Need people
• Stay tuned!
• Ask not what HMI can do for you!
• Ask what you can do for HMI!
Page 71 COSPAR2006-A-01469 HMI
CCD and Camera
• Flat Field
– Details still to be worked out
• Linearity and gain
– Still to be done.
– Difficult due to thermal noise and camera drifts
– Drifts believed due to known problem with this particular camera
• Quadrant crosstalk
– Probably has to await vacuum test due to high thermal noise in air
Page 72 COSPAR2006-A-01469 HMI
Filter transmission
• Wavelength and spatial dependence
– Phase maps have been made with laser and Sun
– Test equipment problems for wavelength dependence. Believed fixable.
– Elements will be replaced (decided before this test)
• Angular (as seen from detector) dependence
– Still to be done
• Stability
– Will try, but oven stability in air likely insufficient
• Throughput
– Looks good
– But gain drifts make things difficult
Page 73 COSPAR2006-A-01469 HMI
Phase Maps
Page 74 COSPAR2006-A-01469 HMI
Polarization
• Some data taken, but much analysis still to be done
• Significant problem found. – Linear polarization into instrument gives circular polarization of up to +/- 0.4!
Page 75 COSPAR2006-A-01469 HMI
Schedule Summary (As of February)
• Complete initial testing Feb 06
• Complete instrument integration April 06– Except flight camera electronics box
• Pre-Environmental Review April 06
• Instrument calibration April – July 06– In air April – May 06
• Need brassboard camera interface board
• Use demonstration camera electronics box
– In vacuum June – July 06• Mid-stream install flight camera electronics box
• HOP vibration & acoustic test July 06
• Comprehensive performance test Aug 06– With flight HMI electronics box
• Instrument EMI/EMC test Sept 06
• HMI electronics box vibration test Oct 06
• Thermal vacuum cycling and balance test Nov – Dec 06
• Comprehensive performance test Dec 06
• Alignment with instrument module panel Jan 07
• Pre-Ship Review Jan 07
• Ship to Goddard Feb 07
Page 76 COSPAR2006-A-01469 HMI
Ray trace – Obsmode and Calmode
Page 77 COSPAR2006-A-01469 HMI
Calibration Matrix
123456789
10
11
121314
151617181920212223
24
2526
2728
29
30
31
3233343536373839
A B C F GTest Group Property Sun
TestsLight Source
1 Image quality Distortion Yes Lamp2 Image scale Yes Sun
3a MTF Yes Lamp3b MTF Yes Sun4a Focus Yes Lamp4b Field curvature Yes Lamp4c Focus Yes Sun4d Field curvature Yes Sun
5 Relative alignment of cameras
No Lamp
6 Relative focus of cameras
No Lamp
*7 Ghost images No TBD*8 Scattered light No TBD9 CCD and Camera Noise No Dark
10 CCD and Camera Flat field Yes Lamp+Sun11 Linearity Yes Lamp
*12a Quadrant crosstalk No TBD*12b Quadrant crosstalk No TBD13a Contamination Yes Lamp13b Contamination Yes Sun13c Contamination No Laser14 Image motions Offset and distortion Yes Lamp15 Filter transmission Wavelength and
spatial dependenceYes All
16 Angular dependence Yes Laser + Sun
17 Stability No Laser or Sun18 Turn-on transients No Laser or Sun?
19 Throughput Yes Sun20 Contrast Yes Laser + Sun
21a Polarization All sorts of stuff Yes Lamp
21b Polarization All sorts of stuff Yes Sun
22 Observables performance
Doppler Yes Sun
23 Line of sight Yes Sun24 Vector Yes Sun
*25 Thermal effects Pointing No Lamp*26 Focus (Yes) Lamp+Sun27 ISS Range and stability No Lamp28 Alignment legs Range and step size Yes Lamp29 Repeatability Yes Lamp
Page 78 COSPAR2006-A-01469 HMI
Test Setup – Stimulus telescope with white light lamp
Stim tel w/ lamp
SpacecraftSimulator
HEB
Inside cleanroom
Outside cleanroom
HOP
PC
U
Line of Sight
Work area
Ent
ran
ce to
cle
anr
oom
Entrance to gowning area
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