1. Photometric Analysis with TAOS Zipper Mode Data Wang, Tanya T.-Y. Supervisor : King, Sun-Kun

2. TAOS Part 1 － Zipper-Mode image row block 2048*32pixel Our real image 2048*2048 Time interval : 0.3 sec Steady state 2048*7200 pixel

3. Part 2 － Dealing with the Data ( IDL ) Setup the file of each star which includes the information of it’s coordinates and magnitude in our interesting region of sky. Whole zipper-mode image row blocks. Use Source Extractor to determine the magnitudes of stars in all row blocks. Use sky-list to collate the coordinates of stars in each row block and put the same coordinates of stars into a file. TAOS

4. Find special data point in our star files Standard deviation. curve(ΔX, ΔY, magnitude) ： x-axis is the time sequence which means the same star in different time and y-axis is the value of Δx (x-mx), Δy (y-my), magnitude. TAOS 0 20 40 60 80 100 MAGNITUDEMAGNITUDE MAGNITUDEMAGNITUDE

5. TAOS Zipper-mode imageRow blocks Using Source Extractor Get a file including x, y and magnitudes of all stars in a row block. x y mag 1.1 1.2 13 1.3 4.5 9.0... 2031 29.1 16 Star_1 Star_2 Star_3 Star_n row x y mag 0 9.1 4.2 13 1 9.09 4.1 12.9..... n 9.12 4.15 13.1 File of star_5 Curve of x, y, mag

6. Part 3 － example 010719_zipperc_a020.fit Starc20_52 TAOS ΔX ΔY M A G N I T U D E

7. 010719_zipperc_a020.fit Starc20_60 TAOS ΔX ΔY M A G N I T U D E

8. 010719_zipperc_a020.fit Starc20_155 TAOS ΔX ΔY M A G N I T U D E

9. 010719_zipperc_a020.fit Starc20_186 TAOS ΔX ΔY M A G N I T U D E

10. 010719_zipperc_a020.fit Starc20_231 TAOS ΔX ΔY M A G N I T U D E

11. 010719_zipperc_a020.fit Starc20_239 TAOS ΔX ΔY M A G N I T U D E

12. 010719_zipperc_a025.fit Starc25_30 TAOS ΔX ΔY M A G N I T U D E

13. 010719_zipperc_a025.fit Starc25_190 TAOS ΔX ΔY M A G N I T U D E

14. 010719_zipperc_a030.fit Starc30_36 TAOS ΔX ΔY M A G N I T U D E

15. Four zipper-mode images TAOS Total star Possible Data point 010719_zipperc_a020192*957 010719_zipperc_a021178*950 010719_zipperc_a025190*954 010719_zipperc_a030192*951

16. Part 4 － Future Use another tool to determine the magnitude. Eliminate background from our image – black frame. Calibration Improve the ability of tracking. 2-D cross correlation An photometric analysis program in real-time. TAOS