C211D

Continuum correlation 1

It 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)

attempt 1

All 4 line sources were correlated in all scans, that is scans No0002, No0004, No0005, No0008, No0010, No0011, No0012, No0013, No0015, No0016, No0018, No0019, No0020, No0021.

This correlation included ALMA, Ef, Pv (as control, knowing that it has no real signal), and 6 VLBA stations: Br, Fd, Mk, Nl, Ov, Pt.

The correlation frequency window was 86231 - 86236 MHz, fringe search window 86232.5 - 86234 MHz.

The following are some fringe plot examples:

RLEO: No0002_all.pdf, No0021_all.pdf

RLMI: No0013_all.pdf, No0015_all.pdf, No0016_all.pdf (including all stations)

VYCMA: No0019_all.pdf

RCNC: No0020_all.pdf

Unfortunatly, the problem with difx2mark4 / fourfit percists and so not all autocorrelations and baselines are available in these plots.

In general it seems, that ALMA successfully detects the spectral line in some cases, as seen in autocorrelation plots for RLEO and RLMI, howeever the crosscorrelation "fringes" with other stations are just artefacts created by fourfit, as confirmed by low SNR, random values of single-band delay (reliable clocks have already been established in continuum correlation), the shape of the "line" in cross-corr plots (basically just amplified noise spikes) and the fact that they are detected even for Pv, which must have no meaningful signal.

Residuals

FITS completeness (pclist)