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 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 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 ) 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 IRIM = Fabry-Perot + Birefringent Lyot Filter + Interference Filter Infrared Imaging Magnetograph of BBSO 12 oct 2005

Diffraction Limited Polarimetry 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 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 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 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

Summary (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

Collaboration of BBSO/NST and SOT