COVER INFORMATION Station: SHANGHAI (Code Sh ) Experiment: Fringe Tape - Session 1 2002 Exp. Code: f02l1 Schedule Version: 1.00 Processed by SCHED version: 16 Oct. 2001 PI: Antonis Polatidis Address: Max Planck Institut fur Radioastronomie Germany D-51 121 GErmany Phone: +49 228 525 424 EMAIL: apolatid@mpifr-bonn.mpg.de Fax: +49 228 525 329 Phone during observation: +49 228 525 424 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, 2002 The experiment will be observed at 18cm. It uses 1 THIN tape per station. Arecibo takes part for the first time in this FTT experiment. The experiment consists of three 10min scans on 0059+581 in which all EVN antennae participate and one 10 min scan on 1606+106 in which Arecibo is also participating. For this last scan, the source is below the horizon in Sheshan and Urumqi, who can finish the experiment earlier. The Fringe Tape will be correlated at JIVE. To enable quick feedback, please send the tape as soon as possible (with express mail) to the JIVE correlator. Thank you for your efforts. Good luck with the session. Schedule for SHANGHAI (Code Sh ) Page 2 Fringe Tape - Session 1 2002 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. Frequencies are LO sum (band edge). ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Tapes TPStart Stop UT LST EL AZ HA UP ParA Dwell (see above) ---------------------------------------------------------------------------------------- --- Mon 4 Feb 2002 Day 35 --- Next scan frequencies: 1650.49 1650.49 1658.49 1658.49 Next BBC frequencies: 549.51 549.51 541.51 541.51 Next scan bandwidths: 8.00 8.00 8.00 8.00 10 00 00 0059+581 03 02 24 56.0 332.2 2.0 130.3 0 1 1 0 10 00 00 10 10 00 --- 03 12 25 55.0 330.7 2.2 127.0 600 F 1 4000 10 12 00 0059+581 03 14 26 54.7 330.5 2.2 126.3 117 1 1 4000 10 12 00 10 22 00 --- 03 24 27 53.7 329.2 2.4 123.2 600 F 1 8000 10 24 00 0059+581 03 26 28 53.4 329.0 2.4 122.5 117 1 1 8000 10 24 00 10 34 00 --- 03 36 29 52.3 327.8 2.6 119.5 600 F 1 12000 10 50 24 1606+106 03 52 56 -48.2 354.1 11.7 D 5.1 825 1 2 12000 10 50 24 11 00 24 --- 04 02 58 -48.4 357.8 11.9 D 1.9 0 R 1 8000 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 sh18cm in /homes/antonios/sched/catalogs/freq.dat Huang Xinyong 170300, dual pol but narrow(?) 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 15800 ft, High density tapes is: 00:39:30 1st LO= 2200.00 2200.00 2200.00 2200.00 Net SB= U U U U Pol. = RCP LCP RCP LCP BBC = 1 2 3 4 BBC SB= L L L L 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= 1650.49 1650.49 1658.49 1658.49 BBC fr= 549.51 549.51 541.51 541.51 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 2002 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 43.470974 * 01 02 45.762382 01 02 51.032748 * 0059+581 58 08 04.84747 * 58 24 11.13662 58 24 57.87238 0059+581 /homes/antonios/sched/catalogs/sources.vlba J0102+58 ICRF - Ext.1 Source - 1998 IERS Annual Report J1608+1029 16 06 23.396615 * 16 08 46.203178 16 08 50.832999 * 1606+106 10 36 59.80115 * 10 29 07.77585 10 28 41.09237 1606+106 /homes/antonios/sched/catalogs/sources.vlba J1608+10 ICRF - Ext.1 Source - 1998 IERS Annual Report 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 88.3 1606+106 79.5 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