COVER INFORMATION Station: PUSH (Code Pu ) Experiment: RadioAstron sat. tracking Exp. Code: el053j Schedule Version: 1.00 Processed by SCHED version: 11.40 Release 11.4. March 14, 2015 PI: Dmitry Litvinov Address: Sternberg Astronomical Institute Moscow State University Russia Phone: +7 495 9395327 EMAIL: litvda@yandex.ru Fax: Phone during observation: +7 495 9395327 Observing mode: 8 GHz, RadioAstron sat. tracking Notes: Mk5 raw data should be e-transferred to ASC/Moscow Single pol RCP Schedule for PUSH (Code Pu ) Page 2 RadioAstron sat. tracking 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 ---------------------------------------------------------------------------------------- --- Wed 15 Jun 2016 Day 167 --- ---------- The following is to control the PUSH tracking station recorder ---------- Next scan frequencies: 4836.00 4836.00 4836.00 4836.00 Next BBC frequencies: 336.00 336.00 336.00 336.00 Next scan bandwidths: 16.00 16.00 16.00 16.00 14 20 00 EL053J 10 27 42 59.4 3.9 -1.6 -153.4 0 0 14 20 00 14 29 30 --- 10 37 14 59.5 3.6 -1.4 -156.1 570 18 14 20 01 14 30 00 EL053J 10 37 44 59.5 3.6 -1.4 -156.3 10 18 14 30 00 14 39 30 --- 10 47 15 59.6 3.2 -1.2 -159.0 570 37 14 30 01 14 40 00 EL053J 10 47 45 59.6 3.1 -1.2 -159.1 10 37 14 40 00 14 49 30 --- 10 57 17 59.7 2.8 -1.1 -161.8 570 55 14 40 01 14 50 00 EL053J 10 57 47 59.7 2.7 -1.0 -162.0 10 55 14 50 00 14 59 30 --- 11 07 19 59.7 2.3 -0.9 -164.7 570 73 14 50 01 15 00 00 EL053J 11 07 49 59.8 2.3 -0.9 -164.8 10 73 15 00 00 15 09 30 --- 11 17 20 59.8 1.9 -0.7 -167.5 570 91 15 00 01 15 10 00 EL053J 11 17 50 59.8 1.9 -0.7 -167.7 10 91 15 10 00 15 20 00 --- 11 27 52 59.8 1.4 -0.5 -170.6 600 111 15 10 01 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. ======== Setup file: ra6cm2.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: 7 Station: PUSH 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= 4500.00 4500.00 4500.00 4500.00 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: 7 Setup file default. Used with PCAL = 1MHz LO sum= 4836.00 4836.00 4836.00 4836.00 BBC fr= 336.00 336.00 336.00 336.00 Bandwd= 16.00 16.00 16.00 16.00 Matching frequency sets: 7 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) * EL053J 11 57 21.769299 * 12 00 00.000000 12 00 44.054034 0.00 85 16 41.77889 * 85 00 00.00000 84 54 51.93202 0.00 From catalog imbedded in main SCHED input file. fake circumpolar target for a TS to look at 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 EL053J raxevn.set 1 2 3 4 5 1.000 15.000 ra6cm2.set 7 0.958 0.000 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) EL053J 67.3 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