To: Moscadelli Subject: EM099A Dear PI, We have examined your project (EM099A,03/11/2012) 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. If your experiment included the phased array Westerbork, it may be possible to 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: EfWbJbOnMcNtTrYs. The correlation had two passes, using: 1s integration time 2 polarizations per IF CONTINUUM: 8 2MHz IFs (Upper/Lower sidebands; DC edges = 6665.63, 6669.63, 6673.63, 6677.63) 128 frequency points per IF/pol LINE: 1 2MHz IFs (Lower sideband; 6667.63-6669.63 = AIPS IF3 from continuum) 1024 frequency points per IF/pol You can download the FITS files directly from the Data Archive as described below (you can arrange a password through me), or we can make DATs/DVDs and mail them to you. Each individual FITS file is ~1.8GB, and the different passes contain: continuum: 9 files 15.8 GB em099a_1_1.IDI line: 9 files 15.8 GB em099a_2_1.IDI The em099a.README file on the archive also contains this information. 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 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/select-experiment (or via the menu items of the main jive page www.jive.nl). Once in this portal to the EVN data archive, you can 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. You will then see a new window for your experiment, from which you can select from the various sorts of data available from the menu row along the top: *) Station Feedback = information provided by the stations' VLBI friends about the conduct of the experiment *) Station Logfiles = sched-based files you uploaded to VLBEER, observing log-files from the stations, other unprocessed station-generated files. *) Standard plots = the plots described below in a variety of formats, a copy of this cover letter *) Pipeline = pipeline plots; the ANTAB & UVFLG files used in pipelining *) Fitsfiles = FITS files, plus an associated README in case there are multiple correlator passes each with its own set of FITS files. The proprietary period for data on the EVN archive is 1 year (6 months for target-of-opportunity observations) -- the raw FITS files and pipeline results relating to sources you identified as "private" receive password protection during the proprietary period. For more details, see www.evlbi.org/user_guide/archive_policy.html Financial assistance may be available to some projects (i.e., those meeting RadioNet trans-national access eligibility criteria) for visiting JIVE or other EVN institutes. 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. ------------- o --------------- 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 description can be found in your experiment's standard plots section of 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 0.4. 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. To get CVEL to correctly compensate for Earth rotation for EVN data correlated on the EVN software correlator at JIVE (SFXC), you will need to: (1) use the 31DEC10 or later version of AIPS (2) set APARM(10) = 1 when running CVEL Remarks on plots or individual stations: Ef: In the continuum pass, the first scan of the fringe finder had IF1-2/RCP apparently dead. This can be seen in the ampphase amp(t) or cross-1 amp(freq) standard plots on the archive, and also the auto-1 amp(freq) plot shows exceedingly high DC power in those subbands. Wb: Jb: On: Mc: Nt: Tr: Ys: Further remarks: