COVER INFORMATION Station: SVETLOE (Code Sv ) Experiment: RadioAstron sat. tracking Exp. Code: el053c Schedule Version: 2.00 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 transferred to JIVE first, from JIVE data should be e-transferred to ASC/Moscow Single pol RCP Schedule for SVETLOE (Code Sv ) 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 ---------------------------------------------------------------------------------------- --- Sat 31 Oct 2015 Day 304 --- ---------- X-band scans ---------- Next scan frequencies: 8398.75 8398.50 8398.25 8398.00 Next BBC frequencies: 318.75 318.50 318.25 318.00 Next scan bandwidths: 4.00 4.00 4.00 4.00 22 00 00 FAKERA 02 38 40 56.5 365.9 -9.4 -34.5 0 0 22 00 00 23 00 00 --- 03 38 50 57.3 367.7 -8.4 -48.0 3600 29 22 00 01 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. ======== Setup file: raxevn.set Matching groups in ./el053c_freq.dat: kvzr_x Added by Des Small, 24 February 2012 Setup group: 1 Station: SVETLOE Total bit rate: 64 Format: MARK5B Bits per sample: 2 Sample rate: 8.000 Number of channels: 4 DBE type: Speedup factor: 1.00 Disk used to record data. 1st LO= 8080.00 8080.00 8080.00 8080.00 Net SB= U U U U IF SB = U U U U Pol. = RCP RCP RCP RCP BBC = 1 2 3 4 BBC SB= U U U U IF = A A A A The following frequency sets based on these setups were used. Frequency Set: 2 Setup file default. Used with PCAL = off LO sum= 8398.75 8398.50 8398.25 8398.00 BBC fr= 318.75 318.50 318.25 318.00 Bandwd= 4.00 4.00 4.00 4.00 Matching frequency sets: 2 3 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 00 30.151922 0.00 85 16 41.77889 * 85 00 00.00000 84 54 31.09650 0.00 From catalog imbedded in main SCHED input file. fake circumpolar target for a TS to look at * FAKERA01 11 57 21.769299 * 12 00 00.000000 12 00 30.151922 0.00 85 16 41.77889 * 85 00 00.00000 84 54 31.09650 0.00 From catalog imbedded in main SCHED input file. fake circumpolar target for a TS to look at * FAKERA02 11 57 21.769299 * 12 00 00.000000 12 00 30.151922 0.00 85 16 41.77889 * 85 00 00.00000 84 54 31.09650 0.00 From catalog imbedded in main SCHED input file. fake circumpolar target for a TS to look at * FAKERA03 11 57 21.769299 * 12 00 00.000000 12 00 30.151922 0.00 85 16 41.77889 * 85 00 00.00000 84 54 31.09650 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 FAKERA raxevn.set 1 2 4 1.000 6.000 ra6cm2.set 7 0.958 0.000 FAKERA01 raxevn.set 5 6 0.329 0.329 FAKERA02 raxevn.set 5 6 0.329 0.329 FAKERA03 raxevn.set 5 6 0.333 0.333 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 100.1 FAKERA01 100.1 FAKERA02 100.1 FAKERA03 100.1 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