\relax 
\@writefile{toc}{\contentsline {section}{\numberline {1}Converting the SKY CCD coordinate to the FPI XY coordinate}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces  The relation between the sky camera CCD coordinate, the FPI XY coordinate, and the cerestial coordinate. It should be noted that the SKY camera Y coordinate is flipped on the data and the Echidna GUI window). }}{2}}
\newlabel{FPI_coordinate}{{1}{2}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces  The measured sky-camera to FPI coordinate converstion factors. Between 200712 and 200805, the sky-camera was re-installed. }}{3}}
\@writefile{lot}{\contentsline {table}{\numberline {2}{\ignorespaces  The measured FPI coordinates of the rotator axis. Echidna re-installations happen between 200712 and 200801 and between 200805 and 200801. The shifts of the FPI coordinates reflect the shift of the Echidna against the rotator axis. }}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {2}Rotator axis on the FPI coordinate}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Measuring the center of the distortion pattern}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces  The measured distortion of the corrector lens in 20071224 with rotator angle of $-97$deg. Horizontal axis is the distance from the FPI (0,0) position in arcmin. Vertical axis is the offset from the $0.01240$ (or $0.01237$) arcsec/$\mu $m in arcsec. Left) in Y (or Dec) direction, MAP2-Y and MAP3 results are shown in red and blue, respectively. Ray trace model is shown in green. The model is offsetted by $-0.39$arcmin ($-1.9$mm) to match the observed distortion curve. Right) in X (or RA) direction, MAP2-X and MAP4 results are shown in red and blue, respectively. Ray trace model is shown in green. The model is offsetted by $-0.95$ arcmin ($-4.6$mm). }}{4}}
\newlabel{FPI_coo_distortion}{{2}{4}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Summary of 1st pass telescope model with sky camera}{4}}
\@writefile{lot}{\contentsline {table}{\numberline {3}{\ignorespaces  Summary of the results of the distortion center measurements. }}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces  Summary of the results of the distortion center measurements. The numbers in the figure indicate the ROTATOR\_REAL\_ANGLE during the measurements. The cross mark indicates the measured position of the rotator center. The measured distortion centers circles arount the rotator center with radius of 4.3mm. The direction of the ROTATOR\_REAL\_ANGLE is different from the OFFSET\_ANGLE.}}{5}}
\newlabel{plot_dist_cen}{{3}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces  The position of the distortion center and the rotator axis, and the relation between the CMM coordinate and the FPI XY coordinate, evaluated based on the CMM position (($+3.7$mm, $-3.8$mm) in the CMM coordinate) of the measurements, the rotator angle ($\sim 0$deg), and the distortion center results. The zeropoint of the CMM coordinate is estimated to be ($-2.1$mm, $-0.6$mm) on the FPI XY coordinate, thus the offset between the CMM center and the rotation center is ($-1.4$mm, $+0.1$mm), which is roughly consistent with the measured offset between the CMM center and the rotation center ($\sim $1mm, $\sim $1mm). (!!! It need to be confirmed that the CMM coordinate is aligned with FPI coordinate !!!). }}{6}}
\newlabel{FPI_coordinate3}{{4}{6}}
\@writefile{toc}{\contentsline {section}{\numberline {5}Acquiring guide stars with guide bandles}{6}}
\@writefile{toc}{\contentsline {section}{\numberline {6}Appendix}{6}}
\@writefile{lot}{\contentsline {table}{\numberline {4}{\ignorespaces  The results of the 1st pass telescope model with the sky-camera. Angle, Dist1, Dist2, Dist3, OffsetX, and OffsetY are the fitting results. For field2, field3, and field4, the distortion parameters were fixed because the number of available stars were small. The field7 and field8 were observed after appling the telescope model determined in field5. The resulting RMS values and the number of the stars are shown in the last two columns. OffsetX and OffsetY are offsets of the distortion pattern from the center of the pointing (the axis of the rotator). The best OffsetX,Y for field5-7 look not consistent with the measured offset shown in Figure 3. The results for field8,9 are roughly consistent (it shold be noted that the CMM positions were ($+4.7,-4.2$) for 20080514). }}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces  The measured offsets (left panels) and the residuals after fit for the measured offsets (right panels). The top panels are for field5 and the bottm panels are for field9. The measurements for field9 were done after appling the telescope model determined in the field5. FPI X+ is to the right, and FPI Y+ is to the top. }}{7}}
\newlabel{fields_all}{{5}{7}}
\@writefile{lot}{\contentsline {table}{\numberline {5}{\ignorespaces  Summary of the required offsets to acquire guide stars in several fields. After slewing telescope, the telescope needed to be moved in the above amount in order to acquire guide stars. The last line indicates the required corrections for the XERR and YERR, i.e. XERR and YERR needs to be 1939 and 939, respectively (NEED TO BE CHECKED!) }}{8}}
\newlabel{offsets}{{5}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces  The relation between the Echidna unit and the PIR/CMM unit at rotator angle of 0 degree. !!! INCONSISTENT WITH FIGURE 3, NEED TO BE CHECKED FURTHER !!! }}{8}}
\newlabel{FPI_coordinate2}{{6}{8}}