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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 A recent diffraction-limited image obtained at BBSO on April 29, 2005 with the AO-76 system and speckle reconstruction.}}{4}}
\newlabel{FIG03}{{A.1.2}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\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).}}{5}}
\newlabel{FIG04}{{4}{5}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.2.1}High Cadence, High Resolution Studies of Solar Flares}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Top panels: (a) IRIM magnetogram taken at 16:02 UT, on July 1, 2005 with AO-76; (b) MDI magnetogram taken at 16:00 UT. Bottom Panel: an example of observed and fitted Stokes V profile from the data set shown in (a) (Cao et al, 2005).}}{6}}
\newlabel{FIG05}{{A.2}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.2.2}Structure and Evolution of Magnetic Fields and Flow Fields in Flaring Active Regions}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\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 integrations. 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.}}{7}}
\newlabel{FIG06}{{A.2.1}{7}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.2.3}Dynamics of Kilogauss Flux Tubes}{8}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.3}The Technical Detail of the AO project for the 1.6-m NST}{8}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.1}Evaluation of the Strehl Ratio}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\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{FIG07}{{7}{9}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.2}Overview of the AO Development Effort}{9}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.3}Optical Design}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces  Comparison of the schematic conceptual optical lay-outs of two possible designs for the NST AO system. Left is the side view of an all-refractive system that is modified slightly from the working AO system of the current 65-cm telescope: the 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 another lens, which could be fed to science instruments. Right is a new design, i.e., a largely reflective system. Lenses after L2 are now replaced by mirrors. }}{11}}
\newlabel{FIG08}{{8}{11}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.4}Electronic, Computing and Mechanics Systems}{12}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.3.5}Setup, Testing and Observations of the New AO System}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces example}}{13}}
\newlabel{fig09}{{9}{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}{16}}