HMI Helioseismic and Magnetic Imager for the Solar Dynamics Observatory BAO Beijing, July 2006

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HMIHelioseismic and Magnetic Imager for
theSolar Dynamics ObservatoryBAO Beijing,
July 2006
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Outline

• The SDO Mission
• Instrument Overview
• Calibration Activities
• HMI Science Goals
• Observations Observables
• Joint Science Operations Center

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The Science of SDO
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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 Suns
  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?

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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 interpretsatellites 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 cant be seen from
  ground
• Temperatures of the plasma range from 50,000 K to
  gt3 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

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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 humanitys technological
  systems by determining
• How the Suns 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.
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The SDO Spacecraft
EVE (looking at CCD radiator and front)
AIA (1 of 4 telescopes)
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.
High-gain antennas (1 of 2)
HMI (looking down from top)
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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

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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 SDOs 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
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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 earths 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

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HMI Instrument Overview
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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

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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 Suns 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!

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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

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Instrument Overview Optical Path
Optical characteristics Focal length 495
cm Focal ratio f/35.2 Final image scale
24?m/arcsec 0.5/pixel Primary to secondary
image magnification 2 Focus adjustment aange 16
steps of 0.4 mm
Filter characteristics Central wavelength 613.7
nm FeI Front window rejects 99 solar heat
load Final filter bandwidth 0.0076 nm Tuning
range 0.069 nm All polarization states
measurable
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Ray trace
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Instrument Overview HMI Optics Package (HOP)
Connector Panel
Z
Focal Plane B/S
Fold Mirror
Shutters
Alignment Mech
X
Limb Sensor
Y
Oven Structure
Detector
Michelson Interf.
Lyot Filter
CEBs
Detector
Vents
Limb B/S
Front Window
Active Mirror
Polarization Selector
Focus/Calibration Wheels
OP Structure
Mechanical Characteristics Box 0.84 x 0.55 x
0.16 m Over All 1.19 x 0.83 x 0.29 m Mass 39.25
kg First Mode 63 Hz
Telescope
Support Legs (6)
Front Door
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HMI Assembly Status
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Status - Michelsons
Michelson ETU
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HMI Assembly Status
Feb
Apr
Mar
May
Structural model testing completed
Received flight Michelsons All flight optics in
house
ETU oven testing completed
BB HEB fabrication completed SUROM acceptance
test completed mission CDR
Jun
Aug
Jul
Hollow core motors completed Received DM
cameras Received 4 grade zero CCDs
Received flight metering tube Completed telescope
alignment
Received flight structure Start alignment on GSE
bench
Nov
Sep
Oct
Dec
Alignment mechanism completed Started optical
alignment of HOP
BB HEB and EGSE ready Shutter F/C wheels
completed Internal harness completed
Lyot completed Internal mechanisms tested
Focal plane completed Oven completed First image
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Status - Cameras
Image of CCD
Image with CCD
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HMI Testing Progress
Tests Performed
Initial set up w/ lamp Focus test w/
lamp Distortion, field curvature and MTF w/
lamp Focus test w/ Sun Filter wavelength
dependence w/ Sun
Tests In Progress
Filter wavelength dependence w/ laser Field
curvature and MTF w/ Sun Polarization calibration
w/ Sun
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HMI Calibration Activities
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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

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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)

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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.

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Calibration Matrix
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Image Quality

• Distortion
• Image scale
• MTF
• Focus and field curvature
• Ghost images and scattered light
• Contamination
• Image motions

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Image Wobble
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Image focus
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HMI Testing Progress
First Dopplergram
First Magnetogram
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HMI Science Goals
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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 Suns 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.

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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.

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HMI Data Product Examples

• Sound speed variations relative to a standard
  solar model.
• Solar cycle variations in the sub-photospheric
  rotation rate.
• Solar meridional circulation and differential
  rotation.
• Sunspots and plage contribute to solar irradiance
  variation.
• MHD model of the magnetic structure of the
  corona.
• Synoptic map of the subsurface flows at a depth
  of 7 Mm.
• EIT image and magnetic field lines computed from
  the photospheric field.
• Active regions on the far side of the sun
  detected with helioseismology.
• Vector field image showing the magnetic
  connectivity in sunspots.
• Sound speed variations and flows in an emerging
  active region.

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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

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HMI Science Analysis Plan
Data Product
Processing
HMI Data
Science Objective
Tachocline
Global Helioseismology Processing
Internal rotation O(r,T) (0ltrltR)
Meridional Circulation
Filtergrams
Internal sound speed, cs(r,T) (0ltrltR)
Differential Rotation
Near-Surface Shear Layer
Full-disk velocity, v(r,T,F), And sound speed,
cs(r,T,F), Maps (0-30Mm)
Local Helioseismology Processing
Activity Complexes
Active Regions
Carrington synoptic v and cs maps (0-30Mm)
Sunspots
Irradiance Variations
High-resolution v and cs maps (0-30Mm)
Observables
Magnetic Shear
Deep-focus v and cs maps (0-200Mm)
Flare Magnetic Configuration
Flux Emergence
Far-side activity index
Magnetic Carpet
Line-of-Sight Magnetic Field Maps
Coronal energetics
Large-scale Coronal Fields
Vector Magnetic Field Maps
Solar Wind
Coronal magnetic Field Extrapolations
Far-side Activity Evolution
Predicting A-R Emergence
Coronal and Solar wind models
IMF Bs Events
Version 1.0w
Brightness Images
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Solar Domain of HMI Helioseismology
rotation
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Solar Domain of HMI Magnetic Field
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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)

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HMI Observing Scheme
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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

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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

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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!

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HMI Data Processing and Products
Level-0
Level-1
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Joint Science Operations CenterJSOC HMI AIA
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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

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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

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SDO Ground System Architecture
10/21/03
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HMI AIA JSOC Architecture
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JSOC Data Export System
VSO Virtual Solar Observatory DRMS Data
Record Mgmt Sys
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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 IT and with DDS,MOC as called for in SDO
  Ground System schedule

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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

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Backup slides
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Science Coordination

• 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 PIs and Co-Is 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.

SOLAR B XRT
HVMI
GBO coronagr.
STEREO SECCHI
2D
Full-Disk Vector Field Convection
3D
Soft X-ray images for complementary T-coverage
in corona
CME propagation High Field Wind structure
Flows (spectra) for 3-D velocities and geometry
EVE
Vector Field small scales H?
SOLAR B FPP
AIA
Calibration
Legend
Full-Disk Chromosphere Surface Vector Field
for field extrapolation
On SDO
Densities Calibration
SOLIS
Energetic Particles
AIA Co-Is
Flows (spectra) for 3-D velocities geometry
(Non) Thermal Particles Coronal Field
Other
FASR VLA OVRO
GOES
RHESSI
ACE
SOLAR B EIS
STEREO -WAVES
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The EVE Instrument on SDO
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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

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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 Earths 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.
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JSOC Data Requirements
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JSOC Pipeline Processing System Components
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Illustration of solar dynamo
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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 cant 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 cant
  be met
• Solution is unknown or has severe cost or
  schedule impacts
• Surgeon Generals warning Preliminary results
  may cause severe upsets!

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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

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Special target continued
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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

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Status - Mechanisms
70
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!

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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

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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

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Phase Maps
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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!

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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

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Ray trace Obsmode and Calmode
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Calibration Matrix
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Test Setup Stimulus telescope with white light
lamp