COVER INFORMATION Station: VLBA_KP (Code Kp ) Experiment: The Nucleus of the Sombrero Galaxy (M104) Exp. Code: bm283 Schedule Version: 1.00 Processed by SCHED version: 6.05 June 2006 PI: E. Momjian Address: NRAO 1003 Lopezville Rd P. O. Box O Socorro, NM 87801, USA Phone: 575-835-7452 EMAIL: emomjian@nrao.edu Fax: 575-835-7027 Phone during observation: Observing mode: 21cm 128-4-2 Notes: Schedule for VLBA_KP (Code Kp ) Page 2 The Nucleus of the Sombrero Galaxy (M104) 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. Automatic tape allocation specified. Tape positions are just estimates. ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Tapes TPStart Stop UT LST EL AZ HA UP ParA Dwell (see above) SYNC ---------------------------------------------------------------------------------------- --- Sat 26 Apr 2008 Day 117 --- Next scan frequencies: 1422.49 1422.49 1430.49 1430.49 Next BBC frequencies: 977.51 977.51 969.51 969.51 Next scan bandwidths: 8.00 8.00 8.00 8.00 03 54 23 M104 10 46 02 38.5 143.2 -1.9 -31.3 0 1 1 0 03 54 23 04 10 20 --- 11 02 02 40.4 147.6 -1.6 -27.6 957 F 1 15 03 54 46 04 10 50 M104 11 02 32 40.5 147.8 -1.6 -27.5 25 1 1 15 04 10 50 04 26 47 --- 11 18 32 42.2 152.5 -1.4 -23.6 957 F 1 31 04 11 13 04 27 17 M104 11 19 02 42.2 152.6 -1.4 -23.5 25 1 1 31 04 27 17 04 43 15 --- 11 35 02 43.6 157.6 -1.1 -19.3 957 F 1 46 04 27 40 04 43 45 J1239-1023 11 35 32 44.9 157.3 -1.1 -19.5 21 1 1 46 04 43 45 04 46 44 =1237-101 11 38 32 45.1 158.3 -1.0 -18.6 180 F 1 49 04 44 08 04 47 14 M104 11 39 02 44.0 158.9 -1.0 -18.2 22 1 1 49 04 47 14 05 03 11 --- 11 55 02 45.0 164.2 -0.8 -13.7 957 F 1 65 04 47 37 05 03 41 M104 11 55 32 45.1 164.3 -0.7 -13.5 25 1 1 65 05 03 41 05 19 39 --- 12 11 32 45.8 169.8 -0.5 -8.8 957 F 1 80 05 04 04 05 20 09 M104 12 12 02 45.8 170.0 -0.5 -8.7 25 1 1 80 05 20 09 05 36 06 --- 12 28 02 46.3 175.6 -0.2 -3.8 957 F 1 96 05 20 32 05 36 36 J1239-1023 12 28 32 47.5 175.8 -0.2 -3.7 21 1 1 96 05 36 36 05 39 35 =1237-101 12 31 32 47.6 176.8 -0.1 -2.7 180 F 1 98 05 36 59 05 40 05 3C273 12 32 02 60.0 181.2 0.0 1.0 -1 1 1 98 05 40 05 05 44 05 --- 12 36 02 60.0 183.2 0.1 2.7 238 F 1 102 05 40 28 05 44 35 M104 12 36 32 46.4 178.6 -0.1 -1.2 -3 1 1 102 05 44 35 06 00 32 --- 12 52 32 46.3 184.3 0.2 3.7 954 F 1 118 05 44 58 06 01 02 M104 12 53 02 46.3 184.5 0.2 3.9 25 1 1 118 06 01 02 06 16 59 --- 13 09 02 45.8 190.1 0.5 8.7 957 F 1 133 06 01 25 06 17 29 J1239-1023 13 09 32 47.0 190.6 0.5 9.1 22 1 1 133 06 17 29 06 20 29 =1237-101 13 12 32 46.9 191.7 0.5 10.1 180 F 1 136 06 17 52 06 20 59 M104 13 13 02 45.7 191.5 0.5 9.9 21 1 1 136 06 20 59 06 36 56 --- 13 29 02 44.8 196.9 0.8 14.6 957 F 1 152 06 21 22 Schedule for VLBA_KP (Code Kp ) Page 3 The Nucleus of the Sombrero Galaxy (M104) 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. Automatic tape allocation specified. Tape positions are just estimates. ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Tapes TPStart Stop UT LST EL AZ HA UP ParA Dwell (see above) SYNC ---------------------------------------------------------------------------------------- --- Sat 26 Apr 2008 Day 117 --- 06 37 26 M104 13 29 32 44.8 197.1 0.8 14.7 25 1 1 152 06 37 26 06 53 53 --- 13 46 02 43.6 202.5 1.1 19.3 987 F 1 167 06 37 49 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. Setup file: bm283.set Matches group v20cm_2 in /home/filehost/cwalker/sched/catalogs/freq.dat FD filtered above 1760. SC filtered above 1740. Setup group: 2 Station: VLBA_KP Total bit rate: 128 Format: VLBA1:4 Bits per sample: 2 Sample rate: 16.000 Number of channels: 4 Speedup factor: 2.00 Disk used to record data. 1st LO= 2400.00 2400.00 2400.00 2400.00 Net SB= U U U U Pol. = RCP LCP RCP LCP BBC = 1 2 3 4 BBC SB= L L L L IF = A C A C VLBA FE= 20cm omit 20cm omit VLBA Synth= 15.4 2.4 15.4 The following frequency sets based on this setup were used. Frequency Set: 2 Setup file default. Used pcal sets: 1 LO sum= 1422.49 1422.49 1430.49 1430.49 BBC fr= 977.51 977.51 969.51 969.51 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 -- The Nucleus of the Sombrero Galaxy (M104) 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) J1229+0203 12 26 33.245836 * 12 29 06.699732 12 29 33.886484 0.30 1226+023 02 19 43.30565 * 02 03 08.59815 02 00 12.57640 0.20 * 3C273 /home/filehost/cwalker/sched/catalogs/sources.vlba 3C273B VLBA Calib Survey - GSFC sols. - created L.Petrov 2005f_astro J1229+02 0.066 scan hours, 2.981 baseline hours above horizon. * J1239-1023 12 37 07.280404 * 12 39 43.061478 12 40 10.600052 0.21 1237-101 -10 07 00.57793 *-10 23 28.69259 -10 26 25.72933 0.31 J1239-10 /home/filehost/cwalker/sched/catalogs/sources.vlba VLBA Calib Survey - GSFC sols. - created L.Petrov 2005f_astro 0.150 scan hours, 6.732 baseline hours above horizon. J1239-1137 12 37 23.386463 * 12 39 59.431861 12 40 27.011677 0.77 * M104 -11 20 55.07245 *-11 37 22.99629 -11 40 20.16408 2.12 /home/filehost/cwalker/sched/catalogs/sources.vlba VLBA Calib Survey - GSFC sols. - created L.Petrov 2005f_astro 2.668 scan hours, 120.011 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) 3C273 149.3 J1239-1023 156.3 M104 156.6 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