COVER INFORMATION Station: SHANGHAI (Code Sh ) Experiment: VSOP observation of J2052+36 at 1.6 GHz Exp. Code: w330v Schedule Version: 1.00 Processed by SCHED version: Release of 28 April 2000 PI: Seiji Kameno Address: National Astronomical Observatory 2-21-1 Osawa, Mitaka, Tokyo 181-8588 Japan Phone: +81-422-34-3607 EMAIL: kameno@hotaka.mtk.nao.ac.jp Fax: +81-422-34-3869 Phone during observation: Observing mode: VSOP, 1.6 GHz continuum, 128-2-2 Notes: Fringe finder : J1800+78 Schedule for SHANGHAI (Code Sh ) Page 2 VSOP observation of J2052+36 at 1.6 GHz 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) ---------------------------------------------------------------------------------------- --- Sat 18 Nov 2000 Day 323 --- Next scan frequencies: 1634.00 1650.00 Next BBC frequencies: 566.00 550.00 Next scan bandwidths: 16.00 16.00 10 00 00 J2052+36 21 55 50 75.8 297.1 1.0 108.3 0 1 1 0 10 00 00 10 22 00 --- 22 17 53 71.6 293.1 1.4 101.1 1320 F 1 17600 10 25 00 J2052+36 22 20 54 71.0 292.7 1.5 100.4 176 1 2 17600 10 25 00 10 47 00 --- 22 42 57 66.6 291.1 1.8 95.5 1320 R 1 0 10 47 40 J2052+36 22 43 37 66.4 291.0 1.8 95.4 38 1 1 0 10 47 40 11 09 40 --- 23 05 41 62.0 290.4 2.2 91.5 1320 F 2 17600 11 10 20 J2052+36 23 06 21 61.9 290.4 2.2 91.4 38 1 2 17600 11 10 20 11 32 20 --- 23 28 25 57.5 290.4 2.6 88.2 1320 R 2 0 11 33 00 J2052+36 23 29 05 57.3 290.4 2.6 88.1 38 1 3 0 11 33 00 11 55 00 --- 23 51 08 52.9 290.9 3.0 85.2 1320 F 1 17600 11 55 40 J2052+36 23 51 49 52.8 290.9 3.0 85.1 38 1 4 17600 11 55 40 12 17 40 --- 00 13 52 48.4 291.7 3.3 82.4 1320 R 1 0 12 18 20 J2052+36 00 14 32 48.2 291.7 3.4 82.3 38 1 3 0 12 18 20 12 40 20 --- 00 36 36 43.9 292.7 3.7 79.7 1320 F 2 17600 12 50 20 J1800+78 00 46 38 28.2 347.2 6.8 72.1 489 1 4 17600 12 50 20 12 57 20 --- 00 53 39 27.8 347.3 6.9 70.5 420 R 2 12000 13 07 20 J2052+36 01 03 40 38.6 294.2 4.2 76.7 492 1 4 12000 13 07 20 13 22 20 --- 01 18 43 35.6 295.1 4.4 75.0 900 R 2 0 13 23 00 J2052+36 01 19 23 35.5 295.2 4.4 74.9 38 1 5 0 13 23 00 13 45 00 --- 01 41 27 31.3 296.6 4.8 72.4 1320 F 1 17600 13 45 40 J2052+36 01 42 07 31.1 296.7 4.8 72.4 38 1 6 17600 13 45 40 14 07 40 --- 02 04 10 26.9 298.3 5.2 69.9 1320 R 1 0 14 08 20 J2052+36 02 04 50 26.8 298.4 5.2 69.8 38 1 5 0 14 08 20 14 30 20 --- 02 26 54 22.7 300.2 5.6 67.2 1320 F 2 17600 14 31 00 J2052+36 02 27 34 22.6 300.2 5.6 67.2 38 1 6 17600 14 31 00 14 53 00 --- 02 49 38 18.5 302.2 5.9 64.6 1320 R 2 0 Schedule for SHANGHAI (Code Sh ) Page 3 VSOP observation of J2052+36 at 1.6 GHz 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) ---------------------------------------------------------------------------------------- --- Sat 18 Nov 2000 Day 323 --- 14 53 40 J2052+36 02 50 18 18.4 302.2 6.0 64.5 38 1 7 0 14 53 40 15 15 40 --- 03 12 21 14.5 304.3 6.3 61.8 1320 F 1 17600 15 16 20 J2052+36 03 13 02 14.3 304.4 6.3 61.7 38 1 8 17600 15 16 20 15 38 20 --- 03 35 05 10.5 306.6 6.7 58.9 1320 R 1 0 15 39 00 J2052+36 03 35 45 10.4 306.7 6.7 58.8 38 1 7 0 15 39 00 15 50 00 --- 03 46 47 8.5 307.9 6.9 57.3 660 F 2 8800 15 50 40 J2052+36 03 47 27 8.4 307.9 6.9 57.3 38 1 7 8800 15 50 40 16 01 40 --- 03 58 29 6.5 309.2 7.1 55.8 660 F 2 17600 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. Setup file: /home/sched/short-term/progs/current/setups/vsop1634.set Matches group sh18cm in /home/sched/short-term/progs/current/catalogs/freq.dat Huang Xinyong 170300, dual pol but narrow(?) Setup group: 1 Station: SHANGHAI Total bit rate: 128 Format: MKIV1:4 Bits per sample: 2 Sample rate: 32.000 Number of channels: 2 Passes/head pos: 2 Speedup factor: 1.00 Tape speeds: Low density - 270.000 ips, High density - 160.00 ips Time per pass for 17600 ft, High density tapes is: 00:22:00 1st LO= 2200.00 2200.00 Net SB= U U Pol. = LCP LCP BBC = 1 2 BBC SB= L L IF = A A The following frequency sets based on this setup were used. Frequency Set: 1 Setup file default. Used pcal sets: 1 LO sum= 1634.00 1650.00 BBC fr= 566.00 550.00 Bandwd= 16.000 16.000 The following pulse cal sets were used with this setup: Pulse cal detection set: 1 PCAL = 1MHZ PCALXB1= S1 S1 S1 S2 S1 OFF OFF OFF PCALXB2= S2 S2 M1 M2 S2 OFF OFF OFF PCALFR1= 1000 13000 0 0 2000 0 0 0 PCALFR2= 1000 13000 0 0 2000 0 0 0 Track assignments are: track1= 2, 18 track2= 3, 19 barrel=roll_off SOURCE LIST -- VSOP observation of J2052+36 at 1.6 GHz Catalog positions marked with *. Position of date is for stop time of first scan. Names used in schedule marked with *. Short names used in VLA and SNAP files marked with +. Source Source position (RA/Dec) (B1950) (J2000) (Date) J1800+7828 18 03 39.193553 * 18 00 45.683929 18 00 38.043461 1803+784 78 27 54.29752 * 78 28 04.01847 78 28 18.12700 * J1800+78 /home/sched/short-term/progs/current/catalogs/sources.vlba USNO - Ref Frame 1998-6, Eubanks June 1998 J2052+3635 20 50 54.437441 * 20 52 52.057400 20 52 52.946675 2050+364 36 24 12.28891 * 36 35 35.29900 36 35 59.99039 * J2052+36 /home/sched/short-term/progs/current/catalogs/sources.vlba JVAS - Patnaik et al. 1992, mnras, 254, 655; S8.4GHz= 1972 mJy 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) J1800+78 99.9 J2052+36 93.0 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