Hi Ylva, Lorant -- The full correlation and FITS preparation for GP051D has finished, and I've just finished reviewing the results and preparing various plots for you to look at. The correlation used: 18 stations (EfWbJbOnNtTrYsScHnNlPtKpLaFdOvBrMkYy) 2 polarizations per IF line pass: 1 16MHz IFs (Upper sideband; DC edge = 6666.25) 8192 frequency points per IF/pol 0.35s integration time geod pass: 2 16MHz IFs (Upper sideband; DC edges = 6620.25, 6690.25) 32 frequency points per IF/pol 2s integration time You can download the FITS files directly from the Data Archive as described below (you can arrange a password through me). Each individual FITS file is ~1.8GB; there are a total of: line pass: 574 files (total 1034.2GB) geo pass: 1 file (total 0.2GB) 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 Pipeline page on the EVN archive. (Note that the unprocessed station- generated *.antabfs files under the Station Logfiles page of the archive are not directly usable.) 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 made 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, and CHFLAG 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 (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 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. For AIPS versions starting with 31DEC13, you should set DIGICOR to -1 in FITLD (previously, it would do that automatically if the array was not VLBA). 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 -----------------o----------------- General comments (see experiment feedback link on Archive): On - missed the whole observation with a problem with the declination motor. Nt - Feedback says that they had the wrong set-up for the first hour; but there are detections in the first geod block. In the transition from the geod to line modes, there aren't any detections in the line mode until after 10:10. Tr - had short-term, quasi-periodic clock bifurcations of ~18.5 ns in RR (see the ampphase-{N}a2 plots for the clearest signature in the fringe-finders -- the "split" ampt traces stem from slightly different delays (phase-slopes across the band) causing loss of amp in the vector-averaging: affected about 1-1.4s out of every ~5-6s. Also visible as extra scatter in RR in the phase(t) plots. Ys - mount/focus type should be right-handed Nasmyth (mount type = 4 in aips). I forgot to fix this in the measurement set stage, but did insert a TABED into its pipeline to correct this prior to the CLCOR/PANG step prior to fringing. To fix this in the raw data, here are the TABED adverbs (after having set indata): inext = 'AN' bcount = 7 ! Ys = antenna 7 in the GP051* fits files ecount = 7 optype = 'REPL' aparm = 5 0 ! MOUNT = 5th column in AN table keyvalue = 4 0 outver = -1 ! to change AN table in place Br - much weaker than the other VLBAs; sickly-looking autocorrelation (behavior continues through all four parts A-D) Yy - much weaker RR response in the first fringe-finder (3C454.3) -----------------o----------------- PLOTS All plots discussed here were made while the data were still in aips++ Measurement Sets prior to conversion to FITS files. The station/IF numbering is 0-based in the aips++ plots, but 1-based in the FITS data (1-based numbering used below). The names of the standard plots are: Line-pass plots: gp051d-weight-[1-2].ps station weight vs. time gp051d-auto-[1-2].ps station autocorrelation vs. freq gp051d-cross-[1-2][a,p].ps Ef-* & Yy-* baseline amp/phs vs. freq gp051d-ampphase-[1-2][a,p].ps Ef-* baseline amp/phs vs. time The plots vs. time are divided into 2 separate parts, each with about 2h20m of data. The ampphase plots show amp [a] and phase [p] separately; there are two variants of the amp(t) plots, as described in more detail below. The auto and cross plots show 1 minute of data from [1] scan 90 (3C84) and [2] scan 170 (3C84). Geod-pass plots: gp051d.geod-weight-[1-2].ps station weight vs. time gp051d.geod-auto-[1-2].ps station autocorrelation vs. freq gp051d.geod-cross-[1-2][a,p].ps Ef-* & Yy-* baseline amp/phs vs. freq gp051d.geod-ampphase-[1-2][a,p].ps Ef-* baseline amp/phs vs. time Here, the two parts correspond to the beginning and ending geo-blocks in the schedule. The auto and cross plots show 1 minute of data from [1] scan 4 (2236+282) and [2] scan 174 (0808+495). Specific points in regard to the various plots are below. (a) WEIGHT plots The plots shows the weights for all IFs/pols per station, with each 0.35s integration plotted (2s for the geod pass) as a separate ".". The IF/pol color-coding is for the line pass: IF1/RR = red, IF1/LL = blue and the geod pass: IF1/RR=red, IF1/LL=blue, IF2/RR=cyan, IF2/LL=green Before making the FITS files, I flagged weights at 0.6 (integrations below this are in the FITS files, but with negative weights). (b) AUTOCORRELATION SPECTRA [*auto*] plots The plots show data from the scans listed above. Since the plots for each station self-scale, y-axes may not go down to zero. For the geod plots, the IFs for each station are separted by the vertical dashed lines. The polarization color-coding is RR=red, LL=blue. The data have already been corrected for the 2-bit van Vleck compensation, so ACCOR shouldn't be run. It should be okay to use autocorrelations for bandpass corrections or to use ACFIT. (c) BASELINE SPECTRA [*cross*] plots The baseline vs. frequency plots show vector-averaged amplitude and phase for all baselines for same the time ranges as the autocorrelation plots, with with amp & phase going to separate plots denoted by the 'a' or 'p' following the scan identifier. For the geod plots, the IFs per baseline are separated by the dashed vertical lines. The polarization color-coding remains RR=red, LL=blue. (d) AMP/PHASE(t) [*ampphase*] plots The baseline vs. time plots show amplitude and phase for non-target scans, with amp & phase going to separate plots, denoted by the 'a' or 'p' following 'ampphase-'. Each 0.35s integration (2s for the geod pass) is plotted as a separate ".", with the middle 80% of the band used for vector-averaging over frequency. The color-coding remains the same as in the weight plots. For each ~2h20m period of the line pass, there are two amp(t) plots (-{N}a, -{N}a2) and one phase(t) plot (-{N}p), where {N} = 1,2,3, such that: -{N}a: amp(t) for only J0038+4137 scans (to avoid the fringe-finders from dominating the y-axis scale -{N}a2: amp(t) for all non-target scans -{N}p: phase(t) for all non-target scans