C211D

General information

• Session info: http://www3.mpifr-bonn.mpg.de/div/vlbi/globalmm/
• Station feedback: http://www3.mpifr-bonn.mpg.de/div/vlbi/globalmm/sessions/apr21/feedback_apr21.asc

Current Status

Preliminary correlations and tests in progress.

Preliminary Correlation Info and Fringes

Continuum correlation 1: includes only a subset of stations, Aa, Ef, Pv and two of VLBA: Br and Fd. For technical reasons the correlation performed for all antennas only in two 58MHz bands: starting at 86209.703125 MHz and at 86268.296875 MHz (where Aa, Ef and VLBA bands overlap). For VLBA and ALMA only two additional 58MHz bands are added below and above (they don't work for Ef with its 64Mhz x 8 configurations).

At the moment we are not concerned with the linear polarization of ALMA, its "R" and "L" are arbitrarily reassigned X and Y, and the strength of its parralel and cross-hands fringes is roughly the same, as it should be.

Fringes detected from all stations (except Pico, its data for this experiment is useless, it was recording while stowed) only to ALMA and only for calibrators: 1055+018, OJ287, 4C39.25. There is a significant non-linear behavior in fringe rate: being fully compensated in scan 1 it increases to a significant value in scan 22 (130+ mHz or in d-rate units 1600 fs/s). It is not a real cause for concern (if we compensate it in the middle of the experiment, it won't lead to large single-band delays because this is a short experiment), but should be noted.

Map of the currently detected ALMA fringes in the context of the whole experiment:

c211d_FRINGE_RfAnt_Aa_LLRR_AllSrc.pdf

Full fringe plot sets (to ALMA only) for a few scans with the brightest fringes (including autocorrelations and antennas with no fringes):

No0001_A.pdf     (1055+018)

No0003_A.pdf     (OJ287)

No0014_A.pdf     (4C39.25)

No0017_A.pdf     (1055+018)

No0022_A.pdf     (OJ287)

Production Correlation Fringes

Notes

Post-Correlation checks