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Meeting Notes: Monday, November 21, 2011

In Attendance: Emma, Jake, Paul, Sarah, Zoe

• FPA Temperatures
• We noted the step function in ATA 4 on 26-Aug-2011, which happened when we increased the ATA 4 aft telescope temperature by 5 degrees in preparation for the ATA 4 bakeout.
• HOPA Temperatures
• We noted that the temperatures of ATAs 1 and 3 continue to climb. The current yellow high limit is 70 for ATAs 2 and 4, and 75 for ATAs 1 and 3. Jake says "Dave and I probably took one HOPA to about 85 when trying ot break it."
• We should definitely keep an eye on this trend, and we may have to raise the limits again sometime in January if the upward trend continues.
• Spider Temperatures
• The ATA 4 temperature increased on 17-October-2011 because we raised the front telescope temperatures slightly at this time in order to keep them under deadband control.
• Bus Voltage
• Jake noted that eventually we should expect to see the eclipse season dips in voltage drop even lower as the battery wears out. Hopefully this will not be for a long time.
• Secondary voltages (15 and -15 V Monitors)
• It looks a little bit like the 15 V (blue) monitor is trending downward, but it is hard to tell for sure. This could be related to the temperatrue of the electronics box.
• The jump in the 15 V Mech monitor (red) in May corresponds with when we first started running the sequencer (and using the motors).
• Secondary voltages (78 V Monitor)
• We speculated that the shift in rage in mid-May 2010 corresponded to when we closed the ISS loop. Emma checked, and it turns out we closed the loop April 8, so we are still unsure what caused this shift.
• Bus current
• The jumps in bus current are likely due to binning errors. Emma will bug Rock to look into this, because he wrote the IDL code for the websites initially.
• Exposure Quality
• We decided the exposure quality plots had the potential to be useful. Jake noted that the drop in ATA 4 (304 and 94 channels) corresponds to the ATA 4 telescope bakeout. We also thought it was odd that the quality has increased over the mission in nearly every channel, and speculated that this was due to "wear-in".
• NPACKETS
• We thought this plot seemed funny because it dropped to zero at times and did not fall in the expected range around 6000.
• Emma looked into the issue afterwards and discovered a bug in her code that plotted NSPIKES instead of NPACKETS, which explains why the NPACKETs plots looked eerily similar to the NSPIKES plots. NPACKETS is only available in level 0 data as it turns out, so we will need to find another way to trend this if we want to do so.
• Data Mean
• The UV channels show an annual variation do to the changing size of the Sun on the CCD. This variation should be on the order of about a 7% (min to max) difference.
• Camera Gains
• The camera gains all briefly went to zero on May 18, 2010 due to a flight software load and reboot.
• The camera 4 gains went to zero briefly on 3-Dec-2010, and again on 26-Aug-2011, due to steps taken to recover from the "Invalid data from camera 4" anomaly.
• Telescope Pointing Plots
• Paul will show Emma how to create these using Solarsoft. (Dick Shine made them in the past).
• Filter Health Plots
• The Focal Plane Filter Ratio v. Intensity plots are not exactly trending plots, but we will leave them up for now because they contain useful information.
• Corrupt Images
• We noted that so far there have been no corrupt images from camera 1. We speculated that perhaps this lended support to the theory that AIA's observing sequence order has something to do with corrupt images. We concluded that it was not worth investigating further at this time.