COVER INFORMATION Station: SHANGHAI (Code Sh ) Experiment: Fringe Tape - Session 1 2001 Exp. Code: f01C1 Schedule Version: 1.00 Processed by SCHED version: Release of 12 Jan. 2001 PI: Antonis Polatidis Address: Onsala Space Observatory Onsala S-439 92 SWEDEN Phone: +46 31 772 5505 EMAIL: apolatid@oso.chalmers.se Fax: +46 31 772 5590 Phone during observation: +46 31 772 5550 Observing mode: Notes: The Fringe Test will be correlated at JIVE Please send the tape as soon as possible to the JIVE correlator Thank you for your efforts COVER LETTER: This is the Fringe Tape experiment for session 1, 2001 The Fringe Tape will be correlated at JIVE It uses 1 THICK tape per station. MEDICINA uses 1 THIN tape To enable quick feedback, please send the tape as soon as possible to the JIVE correlator. Thank you for your efforts Schedule for SHANGHAI (Code Sh ) Page 2 Fringe Tape - Session 1 2001 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. TPStart: Tape motion start time. ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Tapes TPStart Stop UT LST EL AZ HA UP ParA Dwell (see above) ---------------------------------------------------------------------------------------- --- Mon 5 Feb 2001 Day 36 --- Next scan frequencies: 4982.49 4982.49 4990.49 4990.49 Next BBC frequencies: 782.49 782.49 790.49 790.49 Next scan bandwidths: 8.00 8.00 8.00 8.00 10 00 00 0059+581 03 07 17 55.5 331.5 2.1 128.6 0 1 1 0 10 00 00 10 13 00 --- 03 20 20 54.1 329.7 2.3 124.4 780 F 1 8775 10 16 00 0059+581 03 23 20 53.8 329.3 2.3 123.5 177 1 2 8775 10 16 00 10 29 00 --- 03 36 22 52.3 327.8 2.6 119.5 780 R 1 0 10 32 00 0059+581 03 39 23 52.0 327.5 2.6 118.6 177 1 3 0 10 32 00 10 45 00 --- 03 52 25 50.5 326.3 2.8 114.9 780 F 1 8775 10 46 00 0059+581 03 53 25 50.3 326.2 2.8 114.6 58 1 4 8775 10 46 00 10 59 00 --- 04 06 27 48.8 325.2 3.1 111.1 780 R 1 0 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. Setup file: 128-4-2.set Matches group sh6cm in /home/apolatid/sched/catalogs/freq.dat from Huang Xinyong 170300, change in LO Setup group: 8 Station: SHANGHAI Total bit rate: 128 Format: MKIV1:4 Bits per sample: 2 Sample rate: 16.000 Number of channels: 4 Passes/head pos: 1 Speedup factor: 2.00 Tape speeds: Low density - 135.000 ips, High density - 80.00 ips Time per pass for 8820 ft, Low density tapes is: 00:13:04 1st LO= 4200.00 4200.00 4200.00 4200.00 Net SB= U U U U Pol. = RCP LCP RCP LCP BBC = 1 2 3 4 BBC SB= U U U U IF = C A C A The following frequency sets based on this setup were used. Frequency Set: 8 Setup file default. Used pcal sets: 1 LO sum= 4982.49 4982.49 4990.49 4990.49 BBC fr= 782.49 782.49 790.49 790.49 Bandwd= 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 S1 S3 S1 S2 S3 S4 PCALXB2= S2 S4 S2 S4 M1 M2 M3 M4 PCALFR1= 510 510 6510 6510 0 0 0 0 PCALFR2= 510 510 6510 6510 0 0 0 0 Track assignments are: track1= 2, 18, 3, 19 barrel=roll_off SOURCE LIST -- Fringe Tape - Session 1 2001 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). Source Source position (RA/Dec) (B1950) (J2000) (Date) J0102+5824 00 59 43.470978 * 01 02 45.762386 01 02 47.699021 * 0059+581 58 08 04.84745 * 58 24 11.13660 58 24 37.66263 J0102+58 /home/apolatid/sched/catalogs/sources.vlba USNO - Ref Frame 1998-6, Eubanks June 1998 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) 0059+581 87.4 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