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\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces The median value of the $r_0$ (Fried parameter, a rough measure of the diffraction limit, $r_0\ge $ 5.5 cm is required for correction by AO) measurements from the S-DIMM instrument (principal site survey instrument, see \special {color push Blue}\relax $\@@underline {\hbox {\tt  http://atst.nso.edu/site/}}\mathsurround \z@ $\relax \special {color pop} for details) for the three finalists to be the ATST site ({\bf  Big Bear}, \special {color push Red}{\bf  Haleakala}\special {color pop}, and \special {color push Blue}{\bf  La Palma}\special {color pop}) as a function of hour angle (adapted from Figure\nobreakspace  {}10.13 in Hill et al. 2004, ATST Site Survey Report).}}{1}}
\newlabel{FIG01}{{1}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {A}Project Description}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.1}Results from Prior NSF Support Related to this Proposed Research}{1}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.1.1}New Solar Telescope at BBSO}{2}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.1.2}Adaptive Optics}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Schematic of the 1.6 m off-axis, open NST and its optical layout.}}{3}}
\newlabel{FIG02}{{A.1.1}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.2}Science Drivers for the AO equiped NST}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Left Panel: Speckle reconstructed image of active region NOAA 10486 obtained with frame selection and high-order AO system at 16:48\nobreakspace  {}UT on 2003 October 29, at NSO/SP. The annotation of the axes refers to heliographic coordinates corresponding to a FOV of $81'' \times 81''$. Right Panel: NIR image of the same active region during the flare taken on 20:42\nobreakspace  {}UT with a FOV of $91'' \times 91''$. The bright patches marked by white boxes are NIR flare kernels.}}{4}}
\newlabel{FIG03}{{A.1.2}{4}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.2.1}High Cadence, High Resolution Studies of Solar Flares}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces A recent diffraction-limited image obtained at BBSO on April 29, 2005 with the AO-76 system and speckle reconstruction.}}{5}}
\newlabel{FIG04}{{A.1.2}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Comparison of the variance of the Zernike Coefficients for open (asterisks) and closed-loop (carets) data determined from the AO WFS data. The Solid curve represents a fit to Kolmogoroff spectrum of the open-loop data for $D/r_0$=12.10 (Trischler et al., 2005).}}{6}}
\newlabel{FIG05}{{5}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces (a): IRIM magnetogram taken at 16:02 UT, on July 1, 2005 with AO-76. (b) MDI magnetogram taken at 16:00 UT.}}{6}}
\newlabel{FIG06}{{A.2}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces  An example of observed and fitted Stokes V profile from the data set shown in Figure 6 (Cao et al, 2005).}}{7}}
\newlabel{FIG07}{{A.2}{7}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.2.2}Structure and Evolution of Magnetic Fields and Flow Fields in Flaring Active Regions}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces NIR time sequence of the X10 flare from 20:40\nobreakspace  {}UT to 20:47\nobreakspace  {}UT on 2003 October\nobreakspace  {}29. RHESSI HXR contours (blue) correspond to the $50$ - $100$\nobreakspace  {}keV channel with 60 integration. The local NIR intensity maxima are shown in red. Two flare ribbons are correlated with strong HXR kernels. HXR contour levels are drawn at 0.17, 0.25, 0.60, and 0.80 of the maximum intensity, except for the first two frames, where they correspond to 0.7 and 0.8 for the first frame and 0.4, 0.6, and 0.8 for the second, when the HXR kernels were weaker.}}{8}}
\newlabel{FIG08}{{A.2.1}{8}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.2.3}Dynamics of Kilogauss Flux Tubes}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces Theoretical Strehl ratio as a function of the corrected modes at different seeing conditions: r$_0$=6 cm, 14 cm and 24 cm are the BBSO median seeing at 0.5, 1.0 and 1.6$\mu m$ respectively. In addition, a curve for r$_0$=10 cm is included for the discussion in the proposal.}}{9}}
\newlabel{FIG09}{{9}{9}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.3}The Technical Detail of the AO project for the 1.6-m NST}{9}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.1}Evaluation of the Strehl Ratio}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {10}{\ignorespaces The schematic conceptual optical lay-out of one of possible designs for the NST AO system. Left is the side view of the layout: the NST pupil is first imaged onto the tip/tilt mirror by the lens L1. The solar image is then collimated and the telescope pupil is re-imaged again onto the DM by Lenses L2 and L3. Finally, at the AO output, a real solar image is formed by lens L4, which could be fed to science instruments. which is viewed from a vertical direction to that of the side view; Right: the top view of the optical layout. }}{10}}
\newlabel{FIG10}{{10}{10}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.2}Overview of the AO Development Effort}{11}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.3}Optical Design}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {11}{\ignorespaces example}}{12}}
\newlabel{fig11}{{11}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {12}{\ignorespaces example}}{13}}
\newlabel{fig12}{{12}{13}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.4}Electronic, Computing and Mechanics Systems}{13}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.5}Setup, Testing and Observations of the New AO System}{13}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.4}Relationship to Future Work and Night-time Astronomy}{14}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.4.1}Higher Order Solar AO in the Future}{14}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.4.2}Multi-Conjugate AO}{15}}
\@writefile{toc}{\contentsline {section}{\numberline {B}Education and Research Training}{15}}
\@writefile{toc}{\contentsline {section}{\numberline {C}Personnel and Management}{15}}
\@writefile{toc}{\contentsline {section}{\numberline {D}References}{17}}