COVER INFORMATION Station: GBTS (Code Gt ) Experiment: RadioAstron AGN polarization imaging Exp. Code: gr039 Schedule Version: 1.00 Processed by SCHED version: 11.40 Release 11.4. March 14, 2015 PI: E.Ros Address: Max Planck Institute for Radio Astronomy Auf dem Hugel 69 D-53121 Bonn Phone: +79165452842 EMAIL: eros@mpifr-bonn.mpg.de Fax: Phone during observation: +79165452842 Observing mode: L-K-Q-band, dual-pol Notes: L-band, Radioastron-compatible frequency setup P-CAL is ON Tsys is ON auto-level (AGC) is ON Schedule for GBTS (Code Gt ) Page 2 RadioAstron AGN polarization imaging UP: D => Below limits; H => Below horizon mask; W => still slewing at end; blank => Up. Early: Seconds between end of slew and start. Dwell: On source seconds. Disk: GBytes recorded to this point. TPStart: Recording start time. Frequencies are LO sum (band edge). SYNC: Time correlator is expected to sync up. ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Disk TPStart Stop UT LST EL AZ HA UP ParA Dwell GBytes SYNC ---------------------------------------------------------------------------------------- --- Mon 20 Mar 2017 Day 79 --- ---------- The following is to control the GB tracking station recorder ---------- Next scan frequencies: 1668.00 1668.00 1668.00 1668.00 Next BBC frequencies: 178.00 178.00 178.00 178.00 Next scan bandwidths: 16.00 16.00 16.00 16.00 18 40 00 FAKERA 01 14 36 33.6 1.9-10.8 -17.3 0 0 18 40 00 19 00 00 --- 01 34 39 33.7 2.4-10.4 -22.0 1200 38 18 40 01 19 00 30 FAKERA 01 35 09 33.7 2.4-10.4 -22.1 10 38 19 00 30 19 20 00 --- 01 54 42 33.9 2.9-10.1 -26.7 1170 76 19 00 31 ---------- The following is to control the GB tracking station recorder ---------- 22 10 00 FAKERA 04 45 10 36.6 6.0 -7.3 -67.4 10180 76 22 10 00 22 30 00 --- 05 05 14 37.0 6.2 -6.9 -72.3 1200 114 22 10 01 22 30 30 FAKERA 05 05 44 37.1 6.2 -6.9 -72.4 10 114 22 30 30 22 50 00 --- 05 25 17 37.5 6.3 -6.6 -77.2 1170 152 22 30 31 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. ======== Setup file: ra18cm2.set --- WARNING --- This group does not match an entry in the frequency catalog. This might be ok because the catalog is not complete. But be very careful to be sure that the setup is correct. Setup group: 24 Station: GBTS Total bit rate: 256 Format: MARK5B Bits per sample: 2 Sample rate: 32.000 Number of channels: 4 DBE type: Speedup factor: 1.00 Disk used to record data. 1st LO= 1490.00 1490.00 1490.00 1490.00 Net SB= U L U L IF SB = U U U U Pol. = LCP LCP RCP RCP BBC = 1 1 2 2 BBC SB= U L U L IF = A A B B The following frequency sets based on these setups were used. Frequency Set: 23 Setup file default. Used with PCAL = 1MHz LO sum= 1668.00 1668.00 1668.00 1668.00 BBC fr= 178.00 178.00 178.00 178.00 Bandwd= 16.00 16.00 16.00 16.00 Matching frequency sets: 23 57 Track assignments are: track1= 2, 4, 6, 8 barrel=roll_off POSITIONS OF SOURCES USED IN RECORDING SCANS Source Source position (RA/Dec) Error (B1950) (J2000) (Date) (mas) * FAKERA 11 57 21.769299 * 12 00 00.000000 12 01 00.367264 0.00 85 16 41.77889 * 85 00 00.00000 84 54 17.22708 0.00 From catalog imbedded in main SCHED input file. fake circumpolar target for a TS to look at * 0615+820 06 15 32.765101 * 06 26 03.006221 06 29 37.890984 0.00 J0626+8202 82 03 56.43135 * 82 02 25.56790 82 01 53.90638 0.00 ./gr039_sources.radioastron AGN, rfc_2013d Petrov, 201d, RA-AO4-09 * 2007+777 20 07 20.430168 * 20 05 30.998496 20 04 50.658051 0.00 J2005+7752 77 43 58.12300 * 77 52 43.24753 77 55 30.00114 0.00 ./gr039_sources.radioastron AGN, rfc_2013d Petrov, 2013, unpublished 16338 observations, RA-AO3-04, RA-AO2-1 SOURCE SCAN SUMMARY FOR SOURCES LISTED ABOVE Scan hours are for recording scans only. Baseline hours are only counted for scans above horizon at both ends. Source Setup file Frequency sets Observing hours (duplicates not shown) Scan Baseline FAKERA ra18cm2.set 23 4.600 0.000 0615+820 ra18cm2.set 1 2 3 4 5 6 7 8 9 10 13 17.992 1564.327 ra1cm2.set 24 25 26 27 30 35 36 28.325 631.950 ra7mm2.set 31 34 46 56 7.350 595.039 2007+777 ra18cm2.set 1 2 3 4 6 7 8 9 10 0.867 34.039 ra1cm2.set 24 25 26 27 30 35 36 1.831 77.044 ra7mm2.set 31 34 46 56 0.856 82.328 EFFECT OF SOLAR CORONA The solar corona can cause unstable phases for sources too close to the Sun. SCHED provides warnings at individual scans for distances less than 10 degrees. The distance from the Sun to each source in this schedule is: Source Sun distance (deg) FAKERA 94.8 0615+820 90.6 2007+777 83.6 Barry Clark estimates from predictions by Ketan Desai of IPM scattering sizes that the Sun will cause amplitude reductions on the longest VLBA baselines at a solar distance of 60deg F^(-0.6) where F is in GHz. For common VLBI bands, this is: 327 MHz 117. deg 610 MHz 81. deg 1.6 GHz 45. deg 2.3 GHz 36. deg 5.0 GHz 23. deg 8.4 GHz 17. deg 15.0 GHz 12. deg 22.0 GHz 9. deg 43.0 GHz 6. deg