Big Bear Solar Observatory Some ground-based technology developments that will propel solar physics Phil Goode for Jeff Kuhn Big Bear Solar Observatory New Jersey Institute of Technology

Big Bear Solar Observatory Light to Instruments – Aperture Matters ATST 4 m off-axis PM –Null Corrector CGH(?) Pentaprism scan AO –Note rolloff away from isoplanatic patch –Even for NST DM faceplate matter because of heat Hinode (0.5m) & NST (1.6 m)

Big Bear Solar Observatory Full FOV AO correction for flare and CME studies. Residual Motion with 3-4 guide regions Measure C n 2 GPUs vs. DSPs Multiconjugate Adaptive Optics 3-4 Guide Region Residual Image Motion

Big Bear Solar Observatory Light to Instruments: Hyperspectral Imaging Need 2D spectroscopy to get simultaneous measurements of FOV at a wide range of wavelengths – 2 nd generation fiber bundling. Bundles feed light from focal plane to spectrograph Develop large format fiber bundle arrays that operate in the visible and NIR wavelengths is important for solar spectropolarimetry This capability will allow magnetic field measurements with temporal, spatial and spectral resolution that match the next generation of optical telescopes

Big Bear Solar Observatory Rapid Polarization Multiplexors and Analyzers Need to overcome seeing limitations for polarimetry in new ground-based telescopes. Typically one stacks several field measurements to improve S/N Need C 3 (caching-charge CMOS) camera to stack, say I, Q, U and V, single pixel voltages while atmosphere is frozen since we have technology for camera multiplexing. Need development of rapid polarization multiplexors and analyzers, with broad-band optical performance and rapid (faster than kHz) switching times. Advancements in swift liquid crystal detectors (Meadowlark) seem to be moving in the right direction.

Big Bear Solar Observatory Large Diameter Fabry-Perot Interferometers Need for high throughput optical and IR Fabry-Perot development for polarimetry in large aperture telescopes. There is a growing need for large etendue tunable Fabry- Perots. The most fruitful development here is for large diameter interferometers. Need /200 flatness (gravity deformation) can make mm, FPIs, but need 300 mm for ATST Progress?

Big Bear Solar Observatory Mid-IR Large Format Detector Weak field measurements utilizing large Zeeman splitting Development of 12  m wavelength region large format detector

Big Bear Solar Observatory Development of Custom Gratings Development of generalized gratings with the possibility of arbitrary ruling direction and groove density in optical/IR gratings will open new opportunities High resolution spectral imaging that minimize and simplify both thermal IR and UV instrumentation for solar spectropolarimetry.

Big Bear Solar Observatory High speed parallel computation For real-time image analysis and reconstruction 32 cluster in BB can do “only” 1k by 1k pixel image reconstruction per minute.

Big Bear Solar Observatory Fin!Fin!