1. Page 1COSPAR2006-A-01469 HMI HMI Helioseismic 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

2. Page 2COSPAR2006-A-01469 HMI Outline The SDO Mission Instrument Overview Calibration Activities HMI Science Goals Observations & Observables Joint Science Operations Center

3. Page 3COSPAR2006-A-01469 HMI The Science of SDO

4. Page 4COSPAR2006-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?

5. Page 5COSPAR2006-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

6. Page 6COSPAR2006-A-01469 HMI The SDO Mission NASA/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.

7. Page 7COSPAR2006-A-01469 HMI The 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 m 2 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)

8. Page 8COSPAR2006-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

9. Page 9COSPAR2006-A-01469 HMI

10. Page 10COSPAR2006-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

11. Page 11COSPAR2006-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

12. Page 12COSPAR2006-A-01469 HMI HMI Instrument Overview

13. Page 13COSPAR2006-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

14. Page 14COSPAR2006-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!

15. Page 15COSPAR2006-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

16. Page 16COSPAR2006-A-01469 HMI Image stabilization mirror CCD fold mirror Fold mirror ¼ Waveplate ½ Waveplates Telescope lens set Telecentric lens Calibration lenses and focus blocks Front window filter Relay lens set Blocking filter BDS beamsplitter Narrowband Michelson Polarizer ISS beamsplitter and limb tracker assembly Tuning waveplates Beam control lens Lyot Wideband Michelson CCD Shutter assemblies Aperture stop 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

17. Page 17COSPAR2006-A-01469 HMI Ray trace

18. Page 18COSPAR2006-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 Mirror Focal Plane B/S 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 Y X Detector Limb Sensor Z

19. Page 19COSPAR2006-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 Lyot NB Michelson Painted 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) Structure W/ legs and heaters (Flight) Oven Controller (ETU)

20. Page 20COSPAR2006-A-01469 HMI Status - Michelsons Michelson ETU

21. Page 21COSPAR2006-A-01469 HMI HMI Assembly Status Structural model testing completed ETU oven testing completed BB HEB fabrication completed SUROM acceptance test completed mission CDR Received flight Michelsons All flight optics in house Received flight metering tube Completed telescope alignment Received flight structure Start alignment on GSE bench Hollow core motors completed Received DM cameras Received 4 grade zero CCDs 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

22. Page 22COSPAR2006-A-01469 HMI Status - Cameras Image of CCDImage with CCD

23. Page 23COSPAR2006-A-01469 HMI HMI Testing Progress 12/22/06 02/01/06 01/30/06 01/25/06 01/11/06 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 Filter wavelength dependence w/ laser Field curvature and MTF w/ Sun Polarization calibration w/ Sun Tests In Progress: Laser dot Before holiday No relay lens No Lyot No frt Window Special target Lamp - stim tel Lyot installed Temp mnt for relay lens Not fully aligned stim tel Air Force target Lamp - stim tel All 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 sunlight With air/vac corrector

24. Page 24COSPAR2006-A-01469 HMI HMI Calibration Activities

25. Page 25COSPAR2006-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

26. Page 26COSPAR2006-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)

27. Page 27COSPAR2006-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.

28. Page 28COSPAR2006-A-01469 HMI Calibration Matrix

29. Page 29COSPAR2006-A-01469 HMI Image Quality Distortion Image scale MTF Focus and field curvature Ghost images and scattered light Contamination Image motions

30. Page 30COSPAR2006-A-01469 HMI Image Wobble

31. Page 31COSPAR2006-A-01469 HMI Image focus

32. Page 32COSPAR2006-A-01469 HMI HMI Testing Progress First Magnetogram First Dopplergram

33. Page 33COSPAR2006-A-01469 HMI HMI Science Goals

34. Page 34COSPAR2006-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.

35. Page 35COSPAR2006-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.

36. Page 36COSPAR2006-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 Variations C – 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

37. Page 37COSPAR2006-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

38. Page 38COSPAR2006-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-sight Magnetograms Vector Magnetograms Doppler Velocity Continuum Brightness Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Far-side activity index Deep-focus v and c s maps (0-200Mm) High-resolution v and c s maps (0-30Mm) Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, c s (r,Θ,Φ), Maps (0-30Mm) Internal sound speed, c s (r,Θ) (0<r<R) Internal rotation Ω(r,Θ) (0<r<R) Vector Magnetic Field Maps Science Objective Data Product Processing Observables HMI Data

39. Page 39COSPAR2006-A-01469 HMI Solar Domain of HMI Helioseismology rotation 2 3 4 5 6 7 Sun Log Size (km) Zonal flow AR spot SG dynamo P-modes Time-Distance Rings Global HS 123 45 6 7 89 min 5min hour day year cycle Log Time (s) 10 polar field Earth HMI resolution granule

40. Page 40COSPAR2006-A-01469 HMI Solar Domain of HMI Magnetic Field 2 3 4 5 6 7 Sun Log Size (km) Large-Scale AR spot SG dynamo P-modes 123 45 6 7 89 min 5min hour day rotation year cycle Log Time (s) 10 polar field Earth HMI resolution Granule Coronal field estimates Vector Line-of-sight

41. Page 41COSPAR2006-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)

42. Page 42COSPAR2006-A-01469 HMI HMI Observing Scheme

43. Page 43COSPAR2006-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

44. Page 44COSPAR2006-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

45. Page 45COSPAR2006-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!

46. Page 46COSPAR2006-A-01469 HMI HMI Data Processing and Products HMI Data Analysis Pipeline Doppler Velocity Heliographic Doppler velocity maps Tracked Tiles Of Dopplergrams Stokes I,V Filtergrams Continuum Brightness Tracked full-disk 1-hour averaged Continuum maps Brightness feature maps Solar limb parameters Stokes I,Q,U,V Full-disk 10-min Averaged maps Tracked Tiles Line-of-sight Magnetograms Vector Magnetograms Fast algorithm Vector Magnetograms Inversion algorithm Egression and Ingression maps Time-distance Cross-covariance function Ring diagrams Wave phase shift maps Wave travel times Local wave frequency shifts Spherical Harmonic Time series To l=1000 Mode frequencies And splitting Brightness Images Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Far-side activity index Deep-focus v and c s maps (0-200Mm) High-resolution v and c s maps (0-30Mm) Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, c s (r,Θ,Φ), Maps (0-30Mm) Internal sound speed, c s (r,Θ) (0<r<R) Internal rotation Ω(r,Θ) (0<r<R) Vector Magnetic Field Maps HMI Data Data ProductProcessing Level-0 Level-1

47. Page 47COSPAR2006-A-01469 HMI Joint Science Operations Center JSOC – HMI & AIA

48. Page 48COSPAR2006-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

49. Page 49COSPAR2006-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

50. Page 50COSPAR2006-A-01469 HMI SDO Ground System Architecture 10/21/03

51. Page 51COSPAR2006-A-01469 HMI HMI & AIA JSOC Architecture Redun dant Data Captur e System AIA HMI 30-Day Archive Science Team Forecast Centers EPO Public Catalog Primary Archive HMI & AIA Operations House- keeping Database Offsite Archiv e Offline Archiv e JSOC Pipeline Processing System HMI/AIA Level-0, 1, HMI-level2 Data Export & Web Service Stanford LMSAL High-Level Data Import AIA Analysis System Local Archive Quicklook Viewing MOC DDS housekeeping GSFC White Sands World

52. Page 52COSPAR2006-A-01469 HMI JSOC Data Export System DRMS Package Format Custom Keywords Utilities Selecte d Data Records API Drilldown Overview New/Avail Statistics Keywords Range Search Browse Researcher A General Public Grid Adaptor Grid VSO Adaptor VSO CoSEC CoSEC Adaptor Researcher B Script Access Space Weather VSO – Virtual Solar Observatory DRMS – Data Record Mgmt Sys

53. Page 53COSPAR2006-A-01469 HMI JSOC SDP Development Milestones HMI and AIA Data EGSE installed –Prototype for I/F testing with GSMarch 2005 –Version 2 to support flight inst.June 2005 JSOC Capture System –Purchase computersFall 2006 –Final system installedSpring 2007 –Support DDS testingSummer 2007 JSOC SDP Infrastructure, SUMS, DRMS, PUI –Prototype testing of core systemJune 2005 –Fully functionalJan, 2006 Purchase computers for JSOC Spring, 2007 Infrastructure OperationalSummer, 2007 Data Product ModulesSpring, 2008 Test in I&T and with DDS,MOC as called for in SDO Ground System schedule

54. Page 54COSPAR2006-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

55. Page 55COSPAR2006-A-01469 HMI Backup slides

56. Page 56COSPAR2006-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  EVE Calibration STEREO SECCHI 2D 3D GOES CME propagation High Field Wind structure Energetic Particles RHESSI ACE STEREO -WAVES Flows (spectra) for 3-D velocities and geometry FASR VLA OVRO Full-Disk Chromosphere Surface Vector Field for field extrapolation (Non) Thermal Particles Coronal Field Other AIA Co-I’s On SDO Legend:

57. Page 57COSPAR2006-A-01469 HMI The EVE Instrument on SDO

58. Page 58COSPAR2006-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

59. Page 59COSPAR2006-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.

60. Page 60COSPAR2006-A-01469 HMI

61. Page 61COSPAR2006-A-01469 HMI JSOC Data Requirements

62. Page 62COSPAR2006-A-01469 HMI JSOC Pipeline Processing System Components Database Server SUMS Storage Unit Management System DRMS Data Record Management System SUMS Tape Farm SUMS Disks Pipeline Program, “module” Record Manage ment Keyword Access Data Access DRMS Library Link Manage ment Utility Libraries JSOC Science Libraries Record Cache PUI Pipeline User Interface Pipeline processing plan Processing script, “mapfile” List of pipeline modules with needed datasets for input, output Pipeline Operato r Processing History Log

63. Page 63COSPAR2006-A-01469 HMI Illustration of solar dynamo

64. Page 64COSPAR2006-A-01469 HMI

65. Page 65COSPAR2006-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!

66. Page 66COSPAR2006-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

67. Page 67COSPAR2006-A-01469 HMI Special target continued

68. Page 68COSPAR2006-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

69. Page 69COSPAR2006-A-01469 HMI Status - Mechanisms

70. Page 70COSPAR2006-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!

71. Page 71COSPAR2006-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

72. Page 72COSPAR2006-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

73. Page 73COSPAR2006-A-01469 HMI Phase Maps

74. Page 74COSPAR2006-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!

75. Page 75COSPAR2006-A-01469 HMI Schedule Summary (As of February) Complete initial testingFeb 06 Complete instrument integrationApril 06 –Except flight camera electronics box Pre-Environmental ReviewApril 06 Instrument calibrationApril – July 06 –In airApril – May 06 Need brassboard camera interface board Use demonstration camera electronics box –In vacuumJune – July 06 Mid-stream install flight camera electronics box HOP vibration & acoustic testJuly 06 Comprehensive performance test Aug 06 –With flight HMI electronics box Instrument EMI/EMC testSept 06 HMI electronics box vibration testOct 06 Thermal vacuum cycling and balance testNov – Dec 06 Comprehensive performance test Dec 06 Alignment with instrument module panelJan 07 Pre-Ship ReviewJan 07 Ship to GoddardFeb 07

76. Page 76COSPAR2006-A-01469 HMI Ray trace – Obsmode and Calmode

77. Page 77COSPAR2006-A-01469 HMI Calibration Matrix

78. Page 78COSPAR2006-A-01469 HMI Test Setup – Stimulus telescope with white light lamp