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From MDI to HMI. Outline. MDI Status HMI Overview Observing scheme Status Schedule Transition. MDI Status. 10 year launch anniversary Dec 2! 100 million exposures Keyhole Broken antenna Flip every 3 months Loose two weeks of high rate data Difficult to get good dynamics runs

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Presentation Transcript
outline
Outline
  • MDI Status
  • HMI
    • Overview
    • Observing scheme
    • Status
    • Schedule
  • Transition
mdi status
MDI Status
  • 10 year launch anniversary Dec 2!
  • 100 million exposures
  • Keyhole
    • Broken antenna
    • Flip every 3 months
    • Loose two weeks of high rate data
    • Difficult to get good dynamics runs
  • Otherwise things are fine
  • Plan to operate for 6-12 months after HMI is operational
    • Other SOHO instruments may be kept running after that
hmi overview
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.
  • The HMI investigation is based on measurements obtained with the HMI instrument as part of the Solar Dynamics Observatory (SDO) mission.
  • 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.
instrument overview
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
instrument overview optical path

¼ Waveplate

½ Waveplates

Image Stabilization Mirror

Beam Control

Lens

Aperture Stop

Blocking Filter

Telescope lens set

Wideband

Michelson

Telecentric

Lens

Lyot

Polarizer

Tuning

Waveplates

Calibration lenses

and Focus Blocks

Narrowband

Michelson

ISS Beamsplitter

and Limb Tracker

Assembly

BDS

Beamsplitter

Front Window Filter

Relay Lens Set

CCD

Shutter

Assemblies

CCD

CCD Fold Mirror

Fold Mirror

CCD Fold Mirror

Instrument Overview – Optical Path

Filter Characteristics:

Central Wave Length: 613.7 nm FeI

Front Window Rejects 99% Solar Heat Load

Bandwidth: 0.0076 nm

Tunable Range: 0.05 nm

Free Spectral Range: 0.0688 nm

Optical Characteristics:

Focal Length: 495 cm

Focal Ration: f/35.2

Final Image Scale: 24m/arcsec

Primary to Secondary Image Magnification: 2

Focus Adjustment Range: 16 steps of 0.4 mm

instrument overview hmi optics package hop
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

observing scheme
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
    • Fixed list of filtergrams repeated at fixed cadence during normal operations
    • Entirely specified in software – highly flexible
observables calculation
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!
      • Interpolation necessary
      • Fast and accurate algorithm exists
    • Correct for acceleration effects (temporal interpolation)
      • Nyquist criterion almost fulfilled for Doppler and LOS
      • Nyquist is grossly violated for vector measurements in case of long framelists
      • Significant improvement from interpolation
      • Clever tricks exist
      • Temporal averaging helps
    • Fill gaps
      • Data loss budget gives missing data in every filtergram!
      • Various algorithms exist
      • May do nothing for vector field
        • What do the users prefer?
observables calculation10
Observables Calculation
  • Average in time, if desired
    • Done for at least some vector field inversions
  • 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, etc.
  • Community input needed!
    • Inversion codes
    • Which dataproducts do you want?
    • Science
status what i hoped to show
Status – What I hoped to show
  • First HMI Dopplergram
status
Status
  • First set of Michelsons in house
  • Optics and filters in house
    • Some spares still to be delivered
  • Several flight 4096x4096 CCD’s in house
  • Instrument being assembled
    • May see first light before Christmas
  • Mechanisms
    • Shutters and HCMs finished life test successfully
  • Electronics at various stages
    • Significant delays expected
  • Instrument software at various stages
  • Ground software at various stages
status integration
Status - Integration

Flight Michelsons

Flight Structure Heater Wiring

Primary & Secondary Lens Assemblies

Telescope Assembly on Alignment Plate

status integration15
Status - Integration

ISS Fold Mirror Assembly

ISS Mirror Assembly

ISS Sensor Assemblies

BDS Fold Mirror Assembly

BDS Fold Mirror Assembly

CCD Fold Mirror Assembly

schedule
Schedule
  • Late 2005: First Sun test
  • Feb 2006: Team meeting
  • Summer 2006: Final instrument tests
  • Feb 2007: Instrument delivery
  • Aug 2008: Launch
  • Nov 2008: Begin science observations
  • Nov 2013: End of science observations
  • Nov 2014: End of mission
  • Stay tuned on http://hmi.stanford.edu !
mdi hmi transition
MDI -> HMI Transition
  • Basically we will get 6-12 months of overlap
  • Any particular things we should do during that period?
  • Anything we need to do now?
summary
Summary
  • 4096x4096 full disk coverage
  • 0.5” pixels
  • Continuous coverage
  • Doppler and LOS at 40s cadence
  • Vector magnetograms at 40s-120s cadence
  • Uniform quality
  • Same observing sequence all the time
  • August 2008 launch
  • 5 year nominal mission
  • Lots of new science possible
  • Need your help!
filter profiles
Filter profiles

Line profile

MDI

Continuum

Continuum