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\@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{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 {subsubsection}{\numberline {A.1.1}New Solar Telescope at BBSO}{2}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.1.2}Adaptive Optics}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Schematic of the 1.6 m off-axis, open NST and its optical layout.}}{4}}
\newlabel{FIG02}{{A.1.1}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.2}Science Drivers for the AO Equipped NST}{4}}
\@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.}}{5}}
\newlabel{FIG03}{{A.1.2}{5}}
\@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).}}{6}}
\newlabel{FIG04}{{4}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Left panels: (a) IRIM magnetogram taken at 16:02 UT, on July 1, 2005 with AO-76 at BBSO; (b) MDI magnetogram taken at 16:00 UT. Right: an example of observed and fitted Stokes V profile from the data set shown in (a) (Cao et al, 2005).}}{6}}
\newlabel{FIG05}{{5}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.2.1}High Cadence, High Resolution Studies of Solar Flares}{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, observed with the AO-76 at NSO/SP. 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.}}{7}}
\newlabel{FIG06}{{A.2.1}{7}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A.2.2}Structure and Evolution of Magnetic Fields and Flow Fields in Flaring Active Regions}{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}{14}}
\@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}}