COVER INFORMATION Station: SHANGHAI (Code Sh ) Experiment: Gamma-ray microquasars: radio pulsars in disguise? Exp. Code: EF018c Schedule Version: 1.00 Processed by SCHED version: 6.05 June 2006 PI: R. Fender Address: School of Physics & Astronomy University of Southampton SO17 1BJ Southampton UK Phone: +44 2380 592076 EMAIL: rpf@phys.soton.ac.uk Fax: +44 2380 593910 Phone during observation: Observing mode: Phase-referencing of LS 5039 at 6cm (512 Mb/s) Notes: Place additional information here (note2-4 available) Schedule for SHANGHAI (Code Sh ) Page 2 Gamma-ray microquasars: radio pulsars in disguise? UP: D => Below limits; H => Below horizon mask. blank => Up. Early: Seconds between end of slew and start. Dwell: On source seconds. Tapes: Drive, Index, Start footage / Direction, Head Group, End footage. For disks, the footages are really the GBytes TPStart: Tape motion start time. Frequencies are LO sum (band edge). SYNC: Time correlator is expected to sync up. ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Tapes TPStart Stop UT LST EL AZ HA UP ParA Dwell (see above) SYNC ---------------------------------------------------------------------------------------- --- Mon 5 Mar 2007 Day 64 --- Next scan frequencies: 4966.49 4966.49 4966.49 4966.49 4982.49 4982.49 4982.49 4982.49 4998.49 4998.49 4998.49 4998.49 5014.49 5014.49 5014.49 5014.49 Next BBC frequencies: 766.49 766.49 766.49 766.49 782.49 782.49 782.49 782.49 798.49 798.49 798.49 798.49 814.49 814.49 814.49 814.49 Next scan bandwidths: 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 8.00 03 00 00 3C345 21 54 45 28.0 -58.3 5.2 71.4 0 1 1 0 03 00 00 03 07 00 --- 22 01 46 26.7 -57.8 5.3 70.5 420 F 1 27 03 00 01 03 12 00 J1825-1718 22 06 47 18.2 235.6 3.7 47.8 5 1 1 27 03 12 00 03 15 00 --- 22 09 47 17.7 236.1 3.7 48.1 180 F 1 39 03 12 01 03 15 00 LS5039 22 09 47 19.5 238.0 3.7 48.7 -5 1 1 39 03 15 00 03 20 00 --- 22 14 48 18.5 238.8 3.8 49.3 295 F 1 58 03 15 01 03 20 00 J1825-1718 22 14 48 16.8 237.0 3.8 48.7 -5 1 1 58 03 20 00 03 23 00 --- 22 17 49 16.3 237.4 3.9 49.1 175 F 1 70 03 20 01 03 23 00 LS5039 22 17 49 18.0 239.3 3.9 49.6 -5 1 1 70 03 23 00 03 28 00 --- 22 22 49 17.1 240.1 3.9 50.2 295 F 1 89 03 23 01 03 29 00 J1825-1718 22 23 50 15.2 238.4 4.0 49.8 55 1 1 89 03 29 00 03 32 00 --- 22 26 50 14.6 238.9 4.0 50.2 180 F 1 101 03 29 01 03 32 00 LS5039 22 26 50 16.3 240.8 4.0 50.6 -5 1 1 101 03 32 00 03 37 00 --- 22 31 51 15.4 241.6 4.1 51.2 295 F 1 120 03 32 01 03 37 00 J1825-1718 22 31 51 13.7 239.7 4.1 50.7 -5 1 1 120 03 37 00 03 40 00 --- 22 34 51 13.1 240.1 4.1 51.1 175 F 1 132 03 37 01 03 40 00 LS5039 22 34 51 14.8 242.0 4.1 51.5 -5 1 1 132 03 40 00 03 45 00 --- 22 39 52 13.9 242.8 4.2 52.0 295 F 1 151 03 40 01 03 46 00 J1743-0350 22 40 52 11.5 258.3 4.9 57.2 42 1 1 151 03 46 00 03 53 00 =1741-038 22 47 54 10.0 259.3 5.1 57.5 420 F 1 178 03 46 01 03 55 00 J1825-1718 22 49 54 10.3 242.4 4.4 52.6 101 1 1 178 03 55 00 03 58 00 --- 22 52 54 9.8 242.9 4.4 52.9 180 F 1 190 03 55 01 Schedule for SHANGHAI (Code Sh ) Page 3 Gamma-ray microquasars: radio pulsars in disguise? UP: D => Below limits; H => Below horizon mask. blank => Up. Early: Seconds between end of slew and start. Dwell: On source seconds. Tapes: Drive, Index, Start footage / Direction, Head Group, End footage. For disks, the footages are really the GBytes TPStart: Tape motion start time. Frequencies are LO sum (band edge). SYNC: Time correlator is expected to sync up. ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Tapes TPStart Stop UT LST EL AZ HA UP ParA Dwell (see above) SYNC ---------------------------------------------------------------------------------------- --- Mon 5 Mar 2007 Day 64 --- 03 58 00 LS5039 22 52 54 11.4 244.8 4.4 53.3 -5 1 1 190 03 58 00 04 03 00 --- 22 57 55 10.4 245.5 4.5 53.7 295 F 1 209 03 58 01 04 03 00 J1825-1718 22 57 55 8.8 243.6 4.5 53.4 -5 1 1 209 04 03 00 04 06 00 --- 23 00 56 8.2 244.0 4.6 53.7 175 F 1 221 04 03 01 04 06 00 LS5039 23 00 56 9.8 245.9 4.6 54.0 -5 1 1 221 04 06 00 04 11 00 --- 23 05 56 8.8 246.7 4.7 54.4 295 F 1 240 04 06 01 04 12 00 J1825-1718 23 06 57 7.1 244.9 4.7 54.3 55 1 1 240 04 12 00 04 15 00 --- 23 09 57 6.5 245.3 4.7 54.6 180 F 1 252 04 12 01 04 15 00 LS5039 23 09 57 8.0 247.2 4.7 54.8 -5 1 1 252 04 15 00 04 20 00 --- 23 14 58 7.0 247.9 4.8 55.2 295 F 1 271 04 15 01 04 20 00 J1825-1718 23 14 58 5.5 246.0 4.8 55.0 -5 1 1 271 04 20 00 04 23 00 --- 23 17 58 4.9 246.4 4.9 D 55.3 0 F 1 283 04 20 01 04 23 00 LS5039 23 17 58 6.4 248.3 4.9 55.4 -4 1 1 283 04 23 00 04 28 00 --- 23 22 59 5.4 249.0 4.9 55.8 296 F 1 302 04 23 01 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. Setup file: ef018c.6cm Matches group sh6cm in /aps3/sched/catalogs/freq.dat Dual-pol available since summer 2005 (CR 051122). Setup group: 10 Station: SHANGHAI Total bit rate: 512 Format: MKIV1:2 Bits per sample: 2 Sample rate: 16.000 Number of channels: 16 Speedup factor: 1.00 Disk used to record data. 1st LO= 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 4200.00 Net SB= L L U U L L U U L L U U L L U U Pol. = RCP LCP RCP LCP RCP LCP RCP LCP RCP LCP RCP LCP RCP LCP RCP LCP BBC = 1 2 1 2 3 4 3 4 5 6 5 6 7 8 7 8 BBC SB= L L U U L L U U L L U U L L U U IF = C A C A C A C A C A C A C A C A The following frequency sets based on this setup were used. Frequency Set: 10 Setup file default. Used pcal sets: 1 LO sum= 4966.49 4966.49 4966.49 4966.49 4982.49 4982.49 4982.49 4982.49 4998.49 4998.49 4998.49 4998.49 5014.49 5014.49 5014.49 5014.49 BBC fr= 766.49 766.49 766.49 766.49 782.49 782.49 782.49 782.49 798.49 798.49 798.49 798.49 814.49 814.49 814.49 814.49 Bandwd= 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 8.000 The following pulse cal sets were used with this setup: Pulse cal detection set: 1 PCAL = 1MHZ PCALXB1= S1 S3 S5 S7 S9 S11 S13 S15 PCALXB2= S2 S4 S6 S8 S10 S12 S14 S16 PCALFR1= 490 510 490 510 490 510 490 510 PCALFR2= 490 510 490 510 490 510 490 510 Track assignments are: track1= 2, 10, 18, 26, 3, 11, 19, 27, 66, 74, 82, 90, 67, 75, 83, 91 barrel=roll_off SOURCE LIST -- Gamma-ray microquasars: radio pulsars in disguise? Catalog positions marked with *. Precession of date coordinates is based on stop time of first scan. Names used in schedule marked with *. Short names used in VLA and SNAP files marked with +. Observation date used in B1950/J2000 coordinate conversion (PRECDATE): 1979.900 No adjustments are made for rates (DRA, DDEC). Scan hours are for recording scans only. Baseline hours are only counted for scans above horizon at both ends. Source Source position (RA/Dec) Error (B1950) (J2000) (Date) (mas) * LS5039 18 23 23.640919 * 18 26 15.056600 18 26 39.431619 0.00 -14 52 42.60801 *-14 50 54.26100 -14 50 50.03872 0.00 From catalog imbedded in main SCHED input file. 1.667 scan hours, 54.567 baseline hours above horizon. J1642+3948 16 41 17.606231 * 16 42 58.809968 16 43 13.723290 0.26 1641+399 39 54 10.81494 * 39 48 36.99400 39 47 21.82974 0.40 * 3C345 /aps3/sched/catalogs/sources.vlba J1642+39 VLBA Calib Survey - GSFC sols. - created L.Petrov 2005f_astro 0.350 scan hours, 13.650 baseline hours above horizon. * J1743-0350 17 41 20.616010 * 17 43 58.856134 17 44 21.540343 0.20 1741-038 -03 48 48.89989 *-03 50 04.61669 -03 50 30.71656 0.30 J1743-03 /aps3/sched/catalogs/sources.vlba VLBA Calib Survey - GSFC sols. - created L.Petrov 2005f_astro 0.350 scan hours, 13.505 baseline hours above horizon. * J1825-1718 18 22 42.013830 * 18 25 36.532282 18 26 01.357293 1.29 -17 20 35.28894 *-17 18 49.84782 -17 18 45.21453 1.99 /aps3/sched/catalogs/sources.vlba VLBA Calib Survey - GSFC sols. - created L.Petrov 2005f_astro 1.000 scan hours, 30.505 baseline hours above horizon. 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) LS5039 68.0 3C345 97.6 J1743-0350 79.1 J1825-1718 68.1 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