Dear PI, We have examined the data for project RDV22 on 06 Jul. 2000. The contact person for this project was Craig Walker. Here's a summary: 1. Tape weights vs. time plots have been generated for the entire time range of your experiment. These are a measure of tape record/playback quality, representing the fraction of valid data samples. Data with weights below 70-75% should be flagged. However, you may want to be more cautious when dealing with non-VLBA stations. The easiest way to estimate the best weight threshold is by looking at the tape weights vs. time plots generated here. You can find the weights plots at /home/aspen6/astronomy/jul00/rdv22/sniffer/final/wtsfile.ps. If your experiment involves more than one distribution tape then there will be a tape# subdirectory between /final and wtsfile.ps. See /home/aspen6/README.sniffer for instructions on how to interpret this plot. 2. Delay, rate, phase, and amplitude plots were made for the observation. 3. Autocorrelation bandpass plots were generated for all antennas for scans on all sources. 4. Cross-correlation bandpass plots were generated for all baselines to HN for scans on all sources. 5. Gzipped PostScript plots of Tsys and other monitor data for each available VLBA antenna can be found at /home/aspen6/astronomy/jul00/rdv22. 6. The jobs associated with the correlation of RDV22 can be found at: /home/aspen6/astronomy/jul00/rdv22/jobs. These files provided the correlator with all ancillary data needed for VLBI, including: correlation parameters and telescopes correlated in the final production. The job numbers are: 2020-2051 7. Operations staff have devised a web browser to navigate the file server aspen, as well as view and retrieve its text and PostScript files, gzipped or not. This browser can be reached through the VLBA homepage http://www.aoc.nrao.edu/vlba/html/VLBA.hmtl, initially under What's New but eventually under Observing. All of the files mentioned above can be accessed either with this browser or by FTPing to the vlbiobs account on aspen. Automated Calibration Transfer for VLBA Correlator Output --------------------------------------------------------- The first phase of automated calibration transfer for data from the VLBA correlator has been completed, and was used for your observation. This transfer of calibration information includes data from the 10 VLBA antennas, as well as selected information from the VLA and Effelsberg, which currently provide VLBA-style monitor data. Significant changes to AIPS have been required to introduce calibration transfer, so users must have the patched version of 15OCT98 AIPS, or any later version, beginning with 15APR99. Help files for a number of AIPS tasks have been updated to reflect the new calibration procedures. There also is a new version of the VLBI chapter of the AIPS cookbook, available from http://www.cv.nrao.edu/aips/aipsdoc.html, that includes more details on how to cope with the calibration transfer process. The calibration-transfer process relieves observers of the burden of creating and inputting calibration files for VLBA antennas. Instead, this information is now provided as tables attached to the FITS data sets output by the VLBA correlator. The ancillary data include antenna gain (GC table), system temperature (TY table), pulse calibration (PC table), flags (FG table), and weather (WX table). The wise observer will not modify these original tables; processing errors might then force the data to be reloaded using FITLD. See the description of MERGECAL in Section 9.2.1.7 of the new cookbook chapter for more detail. Of course, skeptical users can simply delete the appropriate tables created by FITLD and generate their tables in the old manner. Phase 2 of calibration transfer will include supply of data from more external telescopes, and probably will proceed incrementally, depending on both the availability of the external information and the implementation of new software in Socorro. At present, ancillary data from most external telescopes must still be loaded in the old manner, and observations of strong sources may be needed for manual pulse calibration at those telescopes. Up-to-date instructions on coping with observations including external telescopes can be found at http://www.nrao.edu/vlba/html/OBSERVING/cal-transfer/cal-transfer.html. Please send comments on calibration transfer to julvesta@nrao.edu, and send bug reports to daip@nrao.edu, with a copy to julvesta@nrao.edu. NOTES: VLBA Stations: SC: OK HN: RFI spikes seen in IF channels 5. NL: Pcal phase jump at ~ 19:30 UT during power shutdown. FD: Slight pcal jump at ~ 4:45 UT. RFI seen in IF channel 5. LA: OK PT: RFI seen in all S-band channels. KP: RFI seen in all S-band channels. OV: OK BR: Rained during observation. RFI seen in IF channel 5. MK: Rained during observation. Non-VLBA stations: GC: No fringes from 7:00 - 12:00 UT due to hydro failure at the site. GG: Tape footages at ~20:10 - 1:13 UT are not logical. Log seems to state many scans when the tape wasn't moving when it should have been. Tape would have just stayed in SEARCH, so I cut the station out of the jobs during that time range to minimize stress on the tape and playback drive. HH: Variable weights at ~0:30 - 4:15 UT; tape was moved with no improvement; track # 10 appeared weak; weights vary between 80% - 100%. Variable weights at 12:00 - 19:07 UT; weights vary between 50% - 100%; track #17 was reported poor. KK: Broke away from RDV22 at 20:26 - 22:40 UT to help with i00188. MA: RFI seen in all S-band channels in the autocorrelation and some cross- correlation plots. NY: Variable weights at 10:00 - 11:00 UT; weights vary between 0% - 100%; all track were reported weak. The weights were good for the rest of the observation. TS: OK WF: No fringes at 19:30 - 20:00 UT at the beginning. Probably due to the receiver still cooling. Small RFI spikes were seen in all S-band channels of the autocorrelation plots. WZ: Out for intensive at ~20:40 - 22:30 UT. General Notes: RFI in channel 6 (S-band) at most stations.