COVER INFORMATION Station: HART (Code Hh ) Experiment: Fringe Tape - Session 2 2003 Exp. Code: f03l2 Schedule Version: 1.00 Processed by SCHED version: Release of 02 July 2002 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: +49 228 525 229 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 Thanks to D. Graham for advice and contirbuting the schedule Thank you for your efforts COVER LETTER: This is the Fringe Tape experiment for session 2, 2003 The experiment will be observed at 18cm. It uses 1 THIN tape per station + 1 disc pack The 2 min scans are scheduled to make Mk5 disk files small enough for transfer over the internet. Schedule for HART (Code Hh ) Page 2 Fringe Tape - Session 2 2003 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 19 May 2003 Day 139 --- Next scan frequencies: 1650.49 1650.49 1658.49 1658.49 Next BBC frequencies: 140.49 140.49 148.49 148.49 Next scan bandwidths: 8.00 8.00 8.00 8.00 09 00 00 0420-014 02 37 15 54.6 50.4 -1.8 0.0 0 1 1 0 09 00 00 09 08 00 --- 02 45 16 55.9 47.8 -1.6 0.0 480 F 1 3200 09 10 00 0420-014 02 47 16 56.3 47.1 -1.6 0.0 117 1 1 3200 09 10 00 09 18 00 --- 02 55 18 57.6 44.3 -1.5 0.0 480 F 1 6400 09 18 40 0420-014 02 55 58 57.7 44.1 -1.5 0.0 38 1 1 6400 09 18 40 09 20 40 --- 02 57 58 58.0 43.4 -1.4 0.0 120 F 1 7200 09 21 20 0420-014 02 58 38 58.1 43.1 -1.4 0.0 38 1 1 7200 09 21 20 09 23 20 --- 03 00 39 58.4 42.4 -1.4 0.0 120 F 1 8000 09 28 20 0552+398 03 05 39 13.3 32.2 -2.8 0.0 216 1 1 8000 09 28 20 09 30 20 --- 03 07 40 13.5 31.9 -2.8 0.0 120 F 1 8800 09 31 00 0552+398 03 08 20 13.6 31.8 -2.8 0.0 38 1 1 8800 09 31 00 09 33 00 --- 03 10 20 13.8 31.5 -2.8 0.0 120 F 1 9600 09 33 40 0552+398 03 11 00 13.9 31.4 -2.7 0.0 38 1 1 9600 09 33 40 09 35 40 --- 03 13 01 14.2 31.1 -2.7 0.0 120 F 1 10400 09 37 40 0552+398 03 15 01 14.4 30.8 -2.7 0.0 117 1 1 10400 09 37 40 09 45 40 --- 03 23 02 15.3 29.5 -2.5 0.0 480 F 1 13600 09 47 40 0552+398 03 25 03 15.5 29.1 -2.5 0.0 117 1 2 13600 09 47 40 09 55 40 --- 03 33 04 16.4 27.8 -2.4 0.0 480 R 1 10400 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 hh18cm in /homes/antonios/sched/catalogs/freq.dat Values confirmed by E-mail Jonathan Quick 291100 (CR) Setup group: 11 Station: HART 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= 1510.00 1510.00 1510.00 1510.00 Net SB= U U U U Pol. = RCP LCP RCP LCP BBC = 2 1 4 3 BBC SB= U U U U IF = 2N 1N 2N 1N The following frequency sets based on this setup were used. Frequency Set: 11 Setup file default. No pcal detection. LO sum= 1650.49 1650.49 1658.49 1658.49 BBC fr= 140.49 140.49 148.49 148.49 Bandwd= 8.000 8.000 8.000 8.000 Track assignments are: track1= 2, 18, 3, 19 barrel=roll_off SOURCE LIST -- Fringe Tape - Session 2 2003 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) J0423-0120 04 20 43.539850 * 04 23 15.800727 04 23 23.841122 * 0420-014 -01 27 28.70002 *-01 20 33.06531 -01 20 08.35457 J0423-01 /homes/antonios/sched/catalogs/sources.vlba ICRF - Ext.1 Source - 1998 IERS Annual Report J0555+3948 05 52 01.407166 * 05 55 30.805609 05 55 42.159991 * 0552+398 39 48 21.94585 * 39 48 49.16500 39 48 57.54657 DA193 /homes/antonios/sched/catalogs/sources.vlba J0555+39 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) 0420-014 23.3 0552+398 34.8 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