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Design and Application of Near Infrared Tunable Filter for ATST and NST Doctoral Thesis Proposal

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Design and Application of Near Infrared Tunable Filter for ATST and NST Doctoral Thesis Proposal by Jun Ma February, 2005. Contents. Introduction Related Work Achromatic Waveplate Layered medium Infrared Imaging Magnetograph system (IRIM)

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slide1
Design and Application of Near Infrared Tunable Filter for ATST and NST
  • Doctoral Thesis Proposal
  • by
  • Jun Ma
  • February, 2005
slide2
Contents
  • Introduction
  • Related Work
    • Achromatic Waveplate
    • Layered medium
    • Infrared Imaging Magnetograph system (IRIM)
    • Magnetic structures of light bridges and umbral dots
  • Tasks
  • Timeline
slide5
(1) Infrared Observation
  • Advantages of IR observation
    • Strong Zeeman splitting
      • Detecting weaker fields
    • Optical opacity reaches minimum at 1.6 micron
    • Earth atmosphere
      • Scattering light
      • Disturbance
    • Seeing condition is better
  • Instrumental difficulties in IR
    • Detectors
    • Optical components (for filter)
      • Polarizer, LC, coatings
    • Tunability

FTS Observation of umbral Stokes profiles: I & V.

Field Strength is roughly around 300 Gauss.

Rueedi, et al., 1994

slide6
New Solar Telescope

Big Bear Solar Observatory

1.6-meter

ATST

  • (2) ATST & NST

A substitution of current 65cm telescope. It will be the largest ground based solar telescope before the construction of ATST (2006).

Advanced Technology Solar Telescope (ATST)

National Solar Observatory

Based on the theoretical models, the magnetic features on the Sun have spatial scales about 30km. This corresponds to a 4-meter aperture at 630.2 nm, an important line for most polarimetry studies.

Lift time spans 3~4 decades.

My thesis project is supported by ATST “near infrared tunable filter system” project.

NST

slide7
(4) NIR Narrow band tunable filter and image-based magnetograph

Polarization Modulation (one example):

Baur & Elmore, “Stokes II – A new polarimeter for solar observation”, 1980

  • Design tasks:
  • Match FWHM of Lyot with the FSR of FPI;
  • Suppress the off band transmission – stray light.
slide8
(5) Lyot Filter - Structure
  • Convolve of FPI/Lyot
  • Mention FPI

1.56 m Birefringent filter, designed by Dr. J. Wang.

Bandpass = 2.2 Å ; LC tuning; normal-wavelates.

Used in the observation at SacPeark, in Dec. 2004

Tunable Laser testing of 1.56m birefringent filter.

Proceeded at Cambridge Research Incorporated (CRi),

March, 2004

slide9
Contribution
  • Achromic
  • Calibr
  • Application
slide10
Lyot Filter - Tuning

Tunable Birefringent Filter design in J. Wang’s paper. without achromatism consideration, i.e., working at single wavelength.

Wavelength tuning v.s. rotation angle of waveplate

A linear relation.

Simulated with Jones matrix method in MATLAB.

Voltage count on LC’s v.s. retardation

[Courtesy CRi, Inc.]

Non-linear; oracle function

slide11
Contents
  • Introduction
  • Related Work
    • Achromatic Waveplate
    • Layered medium
    • Infrared Imaging Magnetograph system (IRIM)
    • Magnetic structures of light bridges and umbral dots
  • Tasks
  • Timeline
slide12
Questions needs answer in final thesis
  • Waveplates ( layered birefringent crystals)
    • More layers achromatic waveplate
    • Incident angles
    • Propagation of polarization modes
  • Lyot filter
    • Tuning & Instrumental Errors
    • LC properties
    • Calibration
  • Filter system
    • Synchronization
  • Light bridges and umbral dots
    • Field strength and distribution
    • Motion
    • Energy transport mechanism
slide13
One idea of making achromatic waveplate

?

How about different layers of different birefringent materials?

How many do we need?

slide14
Preliminary numerical simulation (1)

[ Left Panel ] Retardance error plotted from Title’s paper.

1975 – A.M. Title, “Improvement of Birefringent Filters 2: Achromatic Waveplates”, J.O.S.A., 1975

[ Right Panel ] Retardance error plotted from new design.

2004 – J. Ma, J. Wang, W. Cao, C. Denker, H. Wang. “Near Infrared (NIR) Achromatic Phase Retarder”, SPIE, Oct 2004

  • Result shown here is half-waveplate.
  • The achromatic range on the left is around 200 nm ; on the right, achromatic range is 700 nm . Also, it should be noticed that the error tolerance is defined in different sense.
slide15
Testing of three-layer achromatic waveplate

Transmission profile (not retardance profile). Courtesy Nanjing Institution of Astronomical Instrumentation.

Testing cases:

1) Half awp sandwiched by parallel aligned linear polarizers

2) Two quarter awp sandwiched by parallel aligned linear polarizers

Blue curve: achromatic waveplate

Red curve: normal waveplate

Yellow curve: stray light of the two linear polarizers

slide16
Calibration of Lyot filter, December, 2004

Calibration of 1.56 micron Lyot filter from data of December, 2004.

FWHM ~ 2.1 angstrom

CRi calibration

slide17
Calibrations
  • Calibration of achromatic waveplates.
  • Calibration of tunable birefringent fitler.
    • Data analysis of the calibration in Dec 2004, NSO
  • Calibration of high resolution tunable filters
    • Lookup-table for Voltage on LC’s of Lyot filter
    • Lookup-table for FPI bandpass shifting
    • Automatic calibration procedure instead of lookup-tables
    • CLIPS – C Language Integrated Production System
      • The Artificial Intelligence Section at NASA’s Johnson Space Centre
      • Expert system / An Inference Engine of Logics
      • Prototype – 1984; Open to public – 1986
slide18
Data Analysis: Light Bridges and Umbral Dots
  • Field Strength measurement
    • The Zeeman splitting between two circular polarizations
    • The magnitude of the linear polarization gives some hint on the inclination of the field
    • VMG is needed in order to get the true vector field: polarization modulator
  • Field distribution
    • The characteristics of the field strength distribution within interested area: boundaries
    • Comparison between these characteristics with quiet sun granulations
  • Field evolution
    • Is it possible to have velocity map?
  • Time evolution of light bridges and umbral dots
    • High spatial resolution is required
slide19
Quiet sun granular

(6) Light Bridges and Umbral Dots

L.B.

[ Dec. 2, 2004, NSO-SacPeak ]

NOAA 10706

FOV: 120”  120”

Filtergram observed @ 1.56 m

FWHM = 2.2 Å

Processed with flat-field correction. The dynamic process of these two interests me more. How do they evolve?

Umbral dots

pores

umbra

Umbral dots

penumbra

120”

L.B.

120”

slide20
First-light of IRIM of BBSO

Dec. 2004

Lyot + FPI

Centred at 1.56 micron

Bandwidth ~0.15 angstrom

Seeing condition got worse during this period compared with the observation with Lyot filter one day before.

The fringe pattern comes probably from FPI, since it didn’t appear in Lyot observation. However, it could come from other optics as well, since the optical setup were quite different.

Again, a movie might be more interesting. Also, since the filter system was used to scan the neighbouring spectral range, the Zeeman splitting of the FeI line might be derived from this time sequence of images. Data process hasn’t been done yet.

slide21
Contents
  • Introduction
  • Related Work
    • Achromatic Waveplate
    • Layered medium
    • Infrared Imaging Magnetograph system (IRIM)
    • Magnetic structures of light bridges and umbral dots
  • Tasks
  • Timeline
slide23
The End

Newark, NJ

February, 2005

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