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Collaboration of BBSO/NST
and SOT
Haimin Wang
Big Bear Solar Observatory
1. Six-station Global Full Disk Halpha
Network –Large scale structure of flares
and CMEs
2. New Near Infrared Imaging
Magnetograph System—higher Zeeman
Sensitivity and Deeper atmosphere
3. 1.6-meter New Solar Telescope—Higher
Resolution with Adaptive Optics
Global High Resolution H
Network
Kanzelhohe
Big Bear
Huairou
Catania
Yunnan
Meudon
The H-alpha (656.3 nm) network utilizes facilities at the Big Bear
Solar Observatory (BBSO/NJIT) in California, the Kanzelhöhe
Solar Observatory (KSO/Graz Univ.) in Austria, the Catania
Astrophysical Observatory of (CAO/INAF) in Italy, Observatoire
de Paris, Meudon in France, the Huairou Solar Observing Station
(HSOS/NAOC) and the Yunnan Astronomical Observatory (YNAO)
in China.
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Halpha Image
BBSO
Oct. 28, 2003
Example of science: Large-Scale Activities Associated with
the 2003 October 29 X10 Flare
Liu et al. 2006, ApJ, in press
Future: Combining core field studies by SOT and large
scale studies of Halpha
Coronal
Dimming and
Halpha remote
brightening
Very similar
dimming areas
in EUV and SXR
The Hα remote
brightenings
are co-spatial
with the largescale dimmings
InfraRed Imaging Magnetograph
(IRIM) of BBSO
Why do we need IRIM?
How does IRIM work?
What did IRIM bring us?
Which direction should IRIM go in the next?
Big Bear Solar Observatory
New Jersey Institute of Technology
12 Oct 2005
Specification
Wavelength Range: 1 ~ 1.6 m
( Fe I 1.5648 m and Fe I 1.5651 m )
λ
Field of View: ~ 170” × 170”
Main components:
► Fabry-Perot Etalon
X
► Birefringent Lyot Filter
Y
► Polarization Analyzer
► Rockwell HgCdTe CMOS Camera
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
Infrared Imaging Magnetograph of BBSO
12 oct 2005
Principle
IRIM = Fabry-Perot + Birefringent Lyot Filter + Interference Filter
Infrared Imaging Magnetograph of BBSO
12 oct 2005
Diffraction Limited Polarimetry
Analytic solution of transfer equation
for polarized radiation of Stokes V
in a Milne-Eddington atmosphere
based on Unno and Rachkovsky
Infrared Imaging Magnetograph of BBSO
12 oct 2005
Science Case: Evolution of Magnetic Fields
associated with flares
Before Flare
After Flare
Very Critical: SOT produces Vector magnetograms
with cadence of 1 minute
The 1.6 m NST
• World’s largest aperture solar
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telescope before ATST
Off–axis telescope
BBSO has sustained periods of
good seeing with R0>7cm that
AO requires
First light middle 2007
PM –UA Mirror Lab, almost
done
Secondary-- SORL, almost
done
OSS-- DFM, May 2007
New 5/8 dome, MFG Ratech,
installed
Some NST Details
• 1.6 m clear aperture (1.7m blank)
• Gregorian plus two flat mirrors
• Primary: f/# 2.4, 4.1 m telescope length, l/30 surface
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quality, <10 Å μ–roughness, and blank of Zerodur with CTE
of 0.0±1.0  10-7 per °C
Adaptive Optics (AO) and active optics
0.39–1.6 μm w/AO and >0.39 w/o AO
FOV: 180” in optical labs or 1/2° in prime focus
Real–time telescope alignment
Polarization and calibration optics after M2
Thermal control of mirrors ( 0.3 °C), incl. airknive use
ATST and SOAR studies
Diffraction limit: 0.06” @ 0.5 μm and 0.2” @ 1.56 μm
nm surface
NST 1.7 primary surface error
on 1/6/06
Full 1.7 m aperture
40 nm rms surface error
Approximate 1.6 m clear aperture
36 nm rms surface error
Alignment aberrations (astigmatism and coma) and flexible bending modes (trefoil and
quadrafoil) have been removed. Full aperture includes spurious data around right half of
perimeter due to imperfect correction of image distortion. Fiducial markers on test optics
that cause artifacts (semi-regular grid of spots) will be removed for final measurements.
Currently AO-96, proposed: AO-349
Summary
(Collaboration with SOT)
1.
2.
3.
Six-station Global Full Disk Halpha Network –
Large scale structure of flares and CMEs
New Near Infrared Imaging Magnetograph
System—Higher Zeeman Sensitivity and
Deeper atmosphere
1.6-meter New Solar Telescope—Higher
Resolution with Adaptive Optics