Collaboration of BBSO/NST Collaboration of BBSO/NST and SOTand SOT

Haimin WangHaimin WangBig Bear Solar ObservatoryBig Bear Solar Observatory

1.1. Six-station Global Full Disk Halpha Six-station Global Full Disk Halpha Network –Large scale structure of Network –Large scale structure of flares and CMEsflares and CMEs

2.2. New Near Infrared Imaging New Near Infrared Imaging Magnetograph System—higher Magnetograph System—higher Zeeman Sensitivity and Deeper Zeeman Sensitivity and Deeper atmosphere atmosphere

3.3. 1.6-meter New Solar Telescope—1.6-meter New Solar Telescope—Higher Resolution with Adaptive Higher Resolution with Adaptive OpticsOptics

Global High Resolution H Network

●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.

Yunnan

Huairou

Catania

Big Bear

Meudon

Kanzelhohe

Halpha Image BBSO

Oct. 28, 2003

Example of science: Large-Scale Activities Example of science: Large-Scale Activities Associated with the 2003 October 29 X10 Flare Associated with the 2003 October 29 X10 Flare

Liu et al. 2006, ApJ, in pressLiu et al. 2006, ApJ, in press

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

Coronal Coronal Dimming and Dimming and Halpha Halpha remote remote brighteningbrightening

Very similar Very similar dimming areas dimming areas in EUV and SXRin EUV and SXR

The HThe Hαα remote remote brightenings brightenings are co-spatial are co-spatial with the large-with the large-scale dimmingsscale dimmings

InfraRed Imaging Magnetograph InfraRed Imaging Magnetograph (IRIM) of BBSO(IRIM) of BBSO

Big Bear Solar ObservatoryBig Bear Solar Observatory

New Jersey Institute of TechnologyNew Jersey Institute of Technology

12 Oct 200512 Oct 2005

Why do we need IRIM?

How does IRIM work?

What did IRIM bring us?

Which direction should IRIM go in the next?

SpecificationSpecification

Wavelength Range: 1 ~ 1.6 Wavelength Range: 1 ~ 1.6 m m

( ( Fe I 1.5648 Fe I 1.5648 m and Fe I 1.5651 m and Fe I 1.5651 m m ))

Field of View: ~ 170” Field of View: ~ 170” × × 170”170”

Main components:Main components:

► ► Fabry-Perot EtalonFabry-Perot Etalon

►► Birefringent Lyot FilterBirefringent Lyot Filter

► ► Polarization AnalyzerPolarization Analyzer

► ► Rockwell HgCdTe CMOS CameraRockwell HgCdTe CMOS Camera

High Spatial Resolution: close to diffraction limitHigh Spatial Resolution: close to diffraction limit

High Temporal High Temporal Resolution: < 1 minResolution: < 1 min

Moderate Spectral Resolution: Moderate Spectral Resolution: λλ//δδλλ~ 10~ 1055

High Throughput: > 35 % for polarized lightHigh Throughput: > 35 % for polarized light

High Zeeman Sensitivity: High Zeeman Sensitivity: V / IV / I ~ 10 ~ 10-4-4

XX

YY

λλ

Infrared Imaging Magnetograph of Infrared Imaging Magnetograph of BBSOBBSO

12 oct 200512 oct 2005

PrinciplePrinciple

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

Infrared Imaging Magnetograph of Infrared Imaging Magnetograph of BBSOBBSO

12 oct 200512 oct 2005

Diffraction Limited PolarimetryDiffraction Limited Polarimetry

Analytic solution of transfer equation Analytic solution of transfer equation for polarized radiation of Stokes for polarized radiation of Stokes V V in a Milne-Eddington atmospherein a Milne-Eddington atmospherebased on Unno and Rachkovskybased on Unno and Rachkovsky

Infrared Imaging Magnetograph of Infrared Imaging Magnetograph of BBSOBBSO

12 oct 200512 oct 2005

Science Case: Evolution of Magnetic Science Case: Evolution of Magnetic FieldsFields associated with flaresassociated with flares Before Flare Before Flare After FlareAfter Flare

Very Critical: SOT produces Vector Very Critical: SOT produces Vector magnetograms with cadence of 1 minutemagnetograms with cadence of 1 minute

The 1.6 m NSTThe 1.6 m NST • World’s largest aperture solar World’s largest aperture solar

telescope before ATSTtelescope before ATST

• Off–axis telescopeOff–axis telescope

• BBSO has sustained periods BBSO has sustained periods of good seeing with R0>7cm of good seeing with R0>7cm that AO requires that AO requires

• First light middle 2007 First light middle 2007

• PM –UA Mirror Lab, almost PM –UA Mirror Lab, almost donedone

• Secondary-- SORL, almost Secondary-- SORL, almost donedone

• OSS-- DFM, May 2007OSS-- DFM, May 2007

• New 5/8 dome, MFG Ratech, New 5/8 dome, MFG Ratech, installedinstalled

Some NST DetailsSome NST Details• 1.6 m clear aperture (1.7m blank) 1.6 m clear aperture (1.7m blank) • Gregorian plus two flat mirrorsGregorian plus two flat mirrors• Primary: f/# 2.4, 4.1 m telescope length, Primary: f/# 2.4, 4.1 m telescope length, /30 /30

surface quality, <10 Å μ–roughness, and blank of surface quality, <10 Å μ–roughness, and blank of Zerodur with CTE of 0.0±1.0 Zerodur with CTE of 0.0±1.0 10 10-7-7 per °C per °C

• Adaptive Optics (AO) and active opticsAdaptive Optics (AO) and active optics• 0.39–1.6 μm w/AO and >0.39 w/o AO 0.39–1.6 μm w/AO and >0.39 w/o AO • FOV: 180” in optical labs or 1/2° in prime focusFOV: 180” in optical labs or 1/2° in prime focus• Real–time telescope alignmentReal–time telescope alignment• Polarization and calibration optics after M2Polarization and calibration optics after M2• Thermal control of mirrors (Thermal control of mirrors ( 0.3 °C), incl. airknive 0.3 °C), incl. airknive

use ATST and SOAR studiesuse ATST and SOAR studies• Diffraction limit: 0.06” @ 0.5 μm and 0.2” @ 1.56 Diffraction limit: 0.06” @ 0.5 μm and 0.2” @ 1.56

μmμm

NST 1.7 primary surface NST 1.7 primary surface error on 1/6/06error on 1/6/06

Approximate 1.6 m clear aperture36 nm rms surface error

Full 1.7 m aperture 40 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.

nm

su

rfa

ce

Adaptive Optics, Adaptive Optics,

Currently AO-96, proposed: AO-349Currently AO-96, proposed: AO-349

Summary (Collaboration with SOT)

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