Caltech: Marka, Shawhan, Zweizig
     Hobart-Smith: Penn
     LHO: Landry, Matone, Raab, Savage, Schofield, Sigg
     LLO: Coles, Gonzalez, Zotov
     LSU: Daw, Johnson
     Michigan: Riles
     Oregon: Frey, Rahkola
     Penn State: Sutton
     Wisconsin: Brown

S1 Reports: (S1 Web Page )

• Calibration Status (M. Landry)

Results from a number of calibrations performed before, during and after S1 have been posted on the calibration web page . The page also has links to a document on calibration drift correction by Gaby Gonzalez,  and sample plots by Patrick Sutton and Sergey Klimenko from tracking the injected calibration lines. Mike is working with Rana to finalize L1 computed sensitivities and is working with Patrick Brady and others on providing time-dependent parameters to allow correction in astrophysical search engines for calibration drift. Presently the inspiral group uses raw frequency series information, and the burst group uses the results of pole/zero fits. Patrick Sutton is rerunning his new version of SenseMonitor over the entire data for the three interferometes and will post the results and archive them in the DCC. Mike will give an update on calibrations at the October 18 detector characterization teleconference.

• Data Quality (J. Zweizig, E.Daw)

John has compiled a large number of plots of band-limited RMS and of glitch rates from the three interferometers during S1. His plan is to define objective criteria for vetoing "bad data". Auxiliary channels will be sought with which pathologies in AS_Q  can be correlated without biasing, for example, searches for astrophysical bursts. John's plots (1-minute binning) show clearly some periods of increased glitch rates in the H1 AS_Q channel he is investigating. John is rerunning the glitch monitoring with power line filtering included to reduce overall rms. Preliminary results show the expected  average ~1 Hz rate, given Gaussian noise and a low threshold setting. John mentioned that the saiph DMT workstation at Caltech has completed its task of  S1 tape copying and is now available for running DMT jobs. saiph can see all of the data from both sites. Anyone with a Caltech general computing account should be able to access saiph.  In order to help the upper limits analysis groups pre-filter data for the pre-Nov 1 analysis, John will finalize in the next two weeks the criteria to use in defining new segment tables in the database (more refined version of what his online SegGener DMT monitor creates). KR offered to query the detector characterization group for any favorite data stretch veto criteria people have found.
Ed has been reworking his PeakMon DMT monitor plots into the form of 2-dimensional histograms   (jpeg and png formats) with time as one axis. He finds that with a high-pass filter, he sees periods of quite clean tails in the histograms, with occasional pathological periods. He finds the 2-d histogram bin contents to give better resolution than his former contour plots. The histograms are produced by a matlab script that reads in summary data produced by PeakMon and have 16-second binning of filtered (140Hz high-pass) AS_Q.  Duncan has looked at some of the glitchy periods Ed sees and finds them correlated with periods of increased inspiral candidate rates. For example, an average of 20-30 candidates / 256 seconds jumps occasionally to about 400 / 256 seconds for L1. These candidates are characterized by high signal-to-noise but (fortunately) also high chi-square for looking like true inspirals (binning by frequency band. John will give an update on the data quality work at the October 18 detector characterization teleconference.

• The S2 run is nominally slated to begin February 14, 2003 and last for about eight weeks. KR brought up a number of issues to work on between now and then:
• Fixing and refining DMT monitors - Although great progress was made between E7 and S1, there were still many start-up troubles with DMT monitors in S1. A number of new and useful features had been added to monitors in the weeks leading up to S1, but the features hadn't been shaken down thoroughly. Config files were out of data, and so on. We need to start S2 in better shape.
• Figures of merit to watch in the control rooms  - A number of new DMT viewer plots were used in S1 to keep track of interferometer performance, some of which worked well and others of which were flaky or at times misleading. The known problems need to be fixed, and new figures of merit (e.g., time histories of many AS_Q bands) commissioned.
• Alarms  - We chose not to enable audible DMT alarms in S1 for fear of swamping operators and scimons with false alarms that would soon be ignored. But we should be aiming for reliable alarm generation (occurring rarely but correctly).  We need a mechanism for deciding which DMT alarms we trust and choose to enable.
• Graphical real estate in control rooms - KR felt strongly that more wall space could have been profitably used during S1 for displaying DMT monitor outputs and asked whether more could be made available for S2. Fred and Mark said that projection display area could be increased by about a factor of two. Peter Shawhan stressed the need for standardized plots where one knows what to expect at a glance and can quickly spot deviations. The standardization would include pre-set axis limits, placement, etc..
• Shakedown engineering run E9  - After some lengthy discussion a consensus emerged that before the S2 run there should be a set of "mini-runs" scheduled during convenient weekends in the late fall at the sites. These runs would not necessarily be held simultaneously at LHO and LLO, being somewhat opportunistic w.r.t. ongoing commissioning work, and they would be short, perhaps no longer than several hours, just long enough to collect representative IFO data and to test DMT monitor improvements/fixes.A more formal E9 engineering run would then be held sometime in the month preceding S2, in order to shake down the DMT monitors for primetime science running. This would be different from E8 during which DMT authors were strongly encouraged to add new features to monitors. Only bug fixes and config file tuning are envisioned for E9. Fred Raab pointed out that despite a 2 1/2 month interval between E8 and S1, new, improved monitors that were nominally declared ready for primetime weren't and argued for holding E9 sooner rather than later, with a formal DMT code freeze well before the start of  S2.  KR volunteered to query the detchar group for suggestions and come up with a specific run schedule proposal.

DMT (or other) Software Status Review:

Since time was running short after the above discussions, KR asked DMT authors to report only significant code changes since S1:

• Patrick Sutton reported having fixed up and tested SenseMonitor to use the 973 Hz injected calibration lines to correct the raw computed inspiral ranges (see above). Calibration line tracking seems to be working well.
• Duncan Brown has written a new tool based on xmgr graphics for displaying the results of inspiral search engine results in real-time. This tool will soon become part of LigoTools and be available in the control room.
  

• KR inquired on behalf of Albert Lazzarini as to who from outside LIGO Lab would be attending the GWDAW meeting in December in Kyoto. Of those on the line, only Patrick Sutton planned to attend.
  
• Next  meeting: October 18 telecon at 1:30 p.m. EDT. In order to support the ongoing upper limits analysis of S1 data in a timely way, KR proposed to hold detchar telecons more frequently than once per month during the fall and to schedule reports from the S1 investigation teams, with more urgent investigations reporting first.  Proposed telecon dates were Oct 18, Nov 8, Nov 22, and Dec 13. KR will propose a report schedule to S1 team leaders.