The WireObs program finds or calculations frame by frame quantities and presents them in tables divided by hexadecimal day-of-year number and observation segment (see data reports ). These table includes raw telemetry ACS data (APID #62), computed image statistics, and computed ACS statistics (such as "dither time"). See here, for descriptions of the table quantities.

For the following analyses, we ignore the image statistics and show only the ACS statistics. We used all the segments for the following days (with the following exclusions): Observation Days Used:

Hex Day::: GMT Date ::: Day of Year ::: # of Frames
    51 ::: 99/03/22 :::     081     ::: 2899
    52 ::: 99/03/23 :::     082     ::: 4618
    57 ::: 99/03/28 :::     087     ::: 2353
    58 ::: 99/03/29 :::     088     ::: 3030
    5e ::: 99/04/04 :::     094     ::: 5358
    61 ::: 99/04/07 :::     097     ::: 3534
    65 ::: 99/04/11 :::     101     ::: 3728
    6f ::: 99/04/21 :::     111     ::: 3797
    71 ::: 99/04/23 :::     113     ::: 1169
    74 ::: 99/04/26 :::     116     ::: 3204
    76 ::: 99/04/28 :::     118     ::: 1162
    78 ::: 99/04/30 :::     120     ::: 3487
    7b ::: 99/05/03 :::     123     ::: 3396
    7f ::: 99/05/07 :::     127     ::: 3727
    82 ::: 99/05/10 :::     130     ::: 2577
    86 ::: 99/05/14 :::     134     :::  756
    89 ::: 99/05/17 :::     137     ::: 1103

  Exclude all frames with:
 - The first frame in all segments.
 - Commanded dither amplitudes less than 1 arcminute or greater than 30 arcminutes.
 - Actual dither amplitudes less than 1 arcminute or greater than 30 arcminutes.
 - Actual dither times less than 1 second or greater than 300 seconds.
 - Frames not in steller pointing mode (non-STP ACS mode).
 - Frames with an average number of guide stars less than 1.3.
 - All frames in a segment where the image count is out of order (missing frame).

The "dither time" for a frame is defined here as the time at the end of the exposure minus the time at the end of the previous exposure. The "dither amplitude" for a frame is defined here as the separation between the telescope position at the end of an exposure and the end of the previous exposure.

Many of the following plots are in the form of histograms of frequency. The frequency value is computed by dividing the number of values in a given histogram bin by the total number of values used. The total number and median and average values are given at the top of each of these plots.

Frame based (all three pages, 8 plots per page). . (PS)

Individual plot pages: #1. . (PS) ::::: #2. . (PS) ::::: #3. . (PS) .

In the case of the RMS and maximum pointing deviations, plots are shown separated by the average number of guide stars ("AGS").