To: Moscadelli Subject: EM069E Dear PI, We have examined your project (EM069E,14/03/2009) and the data are ready for distribution to you. You can download the data directly from the EVN Data Archive (see below). Contact your support scientist to arrange a password for your experiment. Let us know whether you would rather have us send you the FITS file(s) on DAT tape(s) or DVDs. If your experiment included the phased array Westerbork, we can provide you the Wb synthesis array data in IDI FITS format, which may prove useful for the amplitude and polarization calibration of the VLBI data set. The experiment scheduled the following telescopes: CmEfWbJbOnMcNtTr. Your experiment was processed with the following parameters: Pass1: 8 Tels, 8 band X 2 pols, each with 128 points, 1 sec int. Comment: Continuum pass Pass2: 8 Tels, 1 band X 2 pols, each with 1024 points, 1 sec int. Comment: Line pass The originally recorded disks from the stations can be released after two weeks. If you have any questions, contact us at jops@jive.nl. EVN and Global VLBI Observations correlated at the EVN MkIV Data Processor at JIVE are now automatically calibrated via a pipeline process. You will receive email notification when the pipeline is complete. In particular, the a priori amplitude calibration table (and the associated, final ANTAB file), plus various other tables and plots will be available to download from the EVN archive (subject to the EVN Data Archive policy as discussed below). A description of the pipelining process can be found at: www.evlbi.org/pipeline/user_expts.html The EVN data archive at JIVE is now a central location for obtaining the information you need in reviewing your project. You can find network feedback from the stations, standard plots from the correlation review done here prior to distribution, pipeline results, and the FITS files themselves. Contact your support scientist to arrange for a password with which you can download your FITS file(s) from the archive directly. See the EVN Users' Guide in www.evlbi.org for a link to the EVN Archive policy -- in short, data from sources you identified as target/private in pre-correlation e-mail will not be made public, nor will pipeline images be available from them, for one year from distribution. The archive can be accessed via: www.jive.nl/archive/scripts/listarch.php (or via the menu items of the main jive page www.jive.nl). Once in the EVN data archive, there are two ways to reach your experiment: 1) click on your experiment in the pull-down menu in the "Select Experiment" window; then click on the link "Show Experiment" that will appear immediately below this. 2) click on "Show Catalogue of Experiments", then click on your experiment in the left-hand column of the new window. Both paths will lead to you a new window for your experiment, from which you can select from the various sorts of data available from the menu in the left-hand column. JIVE also invites PIs to visit Dwingeloo in order to analyze EVN data. Financial assistance may be available to all users located within the EU (and associated states). Contact campbell@jive.nl for more details. Papers that result from your EVN observations should carry the standard EVN acknowledgment: The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. General Remarks: In the process of checking your experiment we have created plots of the weights vs time, auto- and cross-correlation spectra for a few one-minute intervals, and the behavior of amplitude and phase in time. These plots and an explanatory supplement can be found on the EVN data archive. As part of the check-out procedure, we evaluate the quality of all data with low weights and set an appropriate cutoff for flagging. In this experiment the cutoff was set at 0.9. If you observed with 2-bit sampling, your data have been corrected with an improved van Vleck correction to account for the statistics of high/low bits for each BBC's data stream at each station. Thus you shouldn't run ACCOR in AIPS. It should be okay to use autocorrelations for bandpass corrections or to use ACFIT. Remarks on plots or individual stations: Cm: Lost first 20 minute data (scan 1-6) due to problems of recording. Only IF 1-6 were fed into signal. Ef: No known problems. Wb: Used single dish. No known problems. Jb: Used MkII telecope (Jb2). No known problems. On: No known problems. Mc: No known problems. Nt: Low amplitude in IF 5-6 LCP (BBC6 LSB and USB). Tr: RFI impacted IF 3-8, LCP.