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Focal Plane Instrumentation at Big Bear Solar Observatory. Wenda Cao. Big Bear Solar Observatory New Jersey Institute of Technology. Why ?. How are magnetic fields generated and how are they destroyed?

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focal plane instrumentation at big bear solar observatory

Focal Plane Instrumentation at Big Bear Solar Observatory

Wenda Cao

Big Bear Solar Observatory

New Jersey Institute of Technology

slide2
Why ?
  • How are magnetic fields generated and how are they destroyed?
  • What role do magnetic fields play in the organization of plasma structures and the impulsive releases of energy?
  • What are the mechanisms responsible for solar variability (that ultimately affects the Earth)?

NST

NST

NST

  • An angular resolution of 0.1 arcsec or better to resolve the pressure scale height and the photon mean free path
  • A high photon flux at the critical spatial resolution for precise magnetic and velocity field measurements
  • Access to a broad set of diagnostics, VIR to IR

NST

Why ?

2 Nov 2007

slide3
What ?
  • An angular resolution of 0.1 arcsec or better to resolve the pressure scale height and the photon mean free path
  • A high photon flux at the critical spatial resolution for precise magnetic and velocity field measurements
  • Access to a broad set of diagnostics, VIR to IR
  • Adaptive Optics: diffraction limited image;
  • InfraRed Imaging Magnetograph (IRIM): infrared high precision polarimetry and spectrometry;
  • Visible Imaging Magnetograph (VIM): visible spectrometry and polarimetry;
  • Real-time Speckle Image Processor: high resolution dynamics monitor;

What ?

2 Nov 2007

slide4
Where ?

Adaptive Optics

2 Nov 2007

slide5
Adaptive Optics System

Tutelary to Obtain High Spatial Resolution

2 Nov 2007

slide6
How ?

Principle of Adaptive Optics

2 Nov 2007

slide7
Scientific Results

Adaptive Optics

2 Nov 2007

slide8
InfraRed Imaging Magnetograph

Infrared Imaging Magnetograph -- IRIM

2 Nov 2007

slide9
How ?

Wavelength Range: 1 ~ 1.6 m ( Fe I 1.5648 m and Fe I 1.5651 m )

Field of View: ~ 80” × 80”

Four Operation Modes:

► Polarimetry: Stokes I, Q, U, V

►Spectrometry: spectral line profile

► Dopplergram: a few selected spectral points

► Photometry: narrow (~0.1Å), medium(~2.5Å), broad(~50Å)

High Spatial Resolution: close to diffraction limit

High Temporal Resolution: < 1 min

Moderate Spectral Resolution: λ/δλ~ 105

High Throughput: > 35 % for polarized light

High Zeeman Sensitivity: V / I ~ 10-4

λ

X

Y

Infrared Imaging Magnetograph – IRIM

2 Nov 2007

slide10
How?

IRIM = Fabry-Perot + Birefringent Lyot Filter + Interference Filter

Infrared Imaging Magnetograph – IRIM

2 Nov 2007

slide11
Observation

IRIM and MDI:

Observation I – IRIM Polarimetry

2 Nov 2007

slide12
Visible Imaging Magnetograph

Visible Imaging Magnetograph -- VIM

2 Nov 2007

slide13
How ?

Wavelength Range: 400 ~ 700 nm ( G-band, Fe I 630.2 nm and H 656.3 nm)

Field of View: ~ 80” × 80”

Four Operation Modes:

► Polarimetry: Stokes I, Q, U, V

►Spectrometry: spectral line profile

► Dopplergram: a few selected spectral points

► Photometry: narrow (~0.08Å)

High Spatial Resolution

High Temporal Resolution: < 1 min

Moderate Spectral Resolution: λ/δλ~ 105

High Throughput: > 65 %

λ

X

Y

VIM

2 Nov 2007

slide14
Observation

Observation II – IRIM Photometry

2 Nov 2007

slide15
Next …
  • Adaptive Optics:
    • AO-76 transfer to NST
    • NST high order AO system
    • MCAO
  • Infrared Imaging Magnetograph:
    • Upgrade to NST
    • Dual Infrared Fabry-Perot System
  • Visible Imaging Magnetograph:
    • Upgrade to NST
  • Real-time Speckle Processor:
    • Phase Diversity Processor

The future of BBSO focal plane instrument

2 Nov 2007

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