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Collaboration of BBSO/NST and SOT. Haimin Wang Big Bear Solar Observatory 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

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Collaboration of bbso nst and sot

Collaboration of BBSO/NST and SOT

Haimin Wang

Big Bear Solar Observatory

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


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.


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 pressFuture: Combining core field studies by SOT and large scale studies of Halpha


Coronal dimming and halpha remote brightening
Coronal Dimming and Halpha remote brightening the 2003 October 29 X10 Flare

Very similar dimming areas in EUV and SXR

The Hα remote brightenings are co-spatial with the large-scale dimmings


Infrared imaging magnetograph irim of bbso

InfraRed Imaging Magnetograph the 2003 October 29 X10 Flare (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 the 2003 October 29 X10 Flare

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

Field of View: ~ 170” × 170”

Main components:

► Fabry-Perot Etalon

►Birefringent Lyot Filter

► 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

λ

X

Y

Infrared Imaging Magnetograph of BBSO

12 oct 2005


Principle the 2003 October 29 X10 Flare

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

Infrared Imaging Magnetograph of BBSO

12 oct 2005


Diffraction Limited Polarimetry the 2003 October 29 X10 Flare

Infrared Imaging Magnetograph of BBSO

12 oct 2005




The 1 6 m nst
The 1.6 m NST of 1 minute

  • World’s largest aperture solar 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
Some NST Details of 1 minute

  • 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 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


Nst 1 7 primary surface error on 1 6 06
NST 1.7 primary surface error on 1/6/06 of 1 minute

nm surface

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.


Adaptive optics currently ao 96 proposed ao 349
Adaptive Optics, of 1 minuteCurrently AO-96, proposed: AO-349


Summary collaboration with sot

Summary of 1 minute(Collaboration with SOT)

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


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