COVER INFORMATION Station: SHANGHAI (Code Sh ) Experiment: RadioAstron imaging of Mrk 501 Exp. Code: eg086a Schedule Version: 1.20 Processed by SCHED version: 11.30 Version 11.3 update 1. April 14, 2014 PI: Gabriele Giovannini Address: IRA - INAF via Gobetti 101 40129 Bologna, Italy Phone: +39 0516399415 EMAIL: ggiovann@ira.inaf.it Fax: Phone during observation: +7-903-6614865 Observing mode: C/K-band, dual-pol Notes: C/K-band, Radioastron-compatible frequency setup Mark5C stations should record in Mk5B+ format P-CAL is ON, Tsys is ON auto-level (AGC) is ON Schedule for SHANGHAI (Code Sh ) Page 2 RadioAstron imaging of Mrk 501 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 ---------------------------------------------------------------------------------------- --- Thu 5 Mar 2015 Day 64 --- ---------- Space segment 01: C-band VLBI scans. 3C345 ---------- Next scan frequencies: 4836.00 4836.00 4836.00 4836.00 Next BBC frequencies: 636.00 636.00 636.00 636.00 Next scan bandwidths: 16.00 16.00 16.00 16.00 04 00 00 3C345 22 55 09 17.3 -53.5 6.2 63.6 0 0 04 00 00 04 15 00 --- 23 10 12 14.7 -52.1 6.4 61.6 900 29 04 00 01 ---------- Space segment 01: C-band VLBI scans. MRK501 ---------- 04 20 00 1652+398 23 15 13 15.7 -52.7 6.3 62.3 293 29 04 20 00 04 40 00 --- 23 35 16 12.3 -50.8 6.7 59.6 1200 67 04 20 01 ---------- Ground segment 01: C-band VLBI scans. MRK501 ---------- 04 40 30 1652+398 23 35 46 12.2 -50.7 6.7 59.5 28 67 04 40 30 04 49 30 --- 23 44 48 10.7 -49.8 6.8 58.3 540 85 04 40 31 04 50 00 1652+398 23 45 18 10.7 -49.8 6.8 58.2 28 85 04 50 00 04 59 30 --- 23 54 49 9.1 -48.8 7.0 56.9 570 103 04 50 01 05 00 00 1652+398 23 55 19 9.0 -48.7 7.0 56.8 28 103 05 00 00 05 09 30 --- 00 04 51 7.5 -47.7 7.2 55.4 570 121 05 00 01 05 10 00 1652+398 00 05 21 7.4 -47.6 7.2 55.3 28 121 05 10 00 05 19 30 --- 00 14 53 5.9 -46.6 7.3 53.9 570 139 05 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 Matching groups in ./eg086a_freq.dat: sh6cm Update freq. range AnTao 22Mar08 Setup group: 14 Station: SHANGHAI 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= 4200.00 4200.00 4200.00 4200.00 Net SB= L L U U IF SB = U U U U Pol. = RCP LCP RCP LCP BBC = 1 2 1 2 BBC SB= L L U U IF = C A C A The following frequency sets based on these setups were used. Frequency Set: 16 Setup file default. Used with PCAL = 1MHz LO sum= 4836.00 4836.00 4836.00 4836.00 BBC fr= 636.00 636.00 636.00 636.00 Bandwd= 16.00 16.00 16.00 16.00 Matching frequency sets: 16 Track assignments are: track1= 6, 8, 2, 4 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 53.767689 0.00 85 16 41.77889 * 85 00 00.00000 84 54 47.55670 0.00 From catalog imbedded in main SCHED input file. fake circumpolar target for a TS to look at * 1652+398 16 52 11.729418 * 16 53 52.216683 16 54 22.703114 0.00 J1653+3945 39 50 25.15723 * 39 45 36.60881 39 43 59.85838 0.00 MRK501 ./eg086a_sources.radioastron AGN, rfc_2013d Petrov, 2013, unpublished 6490 observations, RA-AO2-04 1641+399 16 41 17.606226 * 16 42 58.809963 16 43 29.572555 0.00 J1642+3948 39 54 10.81479 * 39 48 36.99385 39 46 46.27832 0.00 * 3C345 ./eg086a_sources.radioastron AGN, rfc_2013d Petrov, 2013, unpublished 51938 observations, RA-AO2-10, 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 ra1cm2.set 21 3.142 0.000 1652+398 ra1cm2.set 1 2 3 4 5 7 8 22 7.900 141.000 ra6cm2.set 11 12 13 14 15 16 17 18 7.892 203.067 3C345 ra1cm2.set 1 2 3 4 5 7 8 0.500 15.000 ra6cm2.set 11 12 13 14 15 16 17 18 0.500 16.500 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 101.0 1652+398 95.5 3C345 97.6 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