COVER INFORMATION Station: VLBA_MK (Code Mk ) Experiment: Interferometric Radar Observations of Asteroid 2006VV2 Exp. Code: BB243 Schedule Version: 3.00 Processed by SCHED version: 6.05 June 2006 PI: Greg Black Address: 530 McCormick Rd Department of Astronomy University of Virginia Charlottesville, VA 22904 Phone: 434 243-8941 EMAIL: gblack\@virginia.edu Fax: 434 924-3104 Phone during observation: 434 243-8941 Observing mode: Schedule files for near field radar experiment. Notes: Frequency setup intentionally has the same bands recorded on each track. PLEASE run with developmental version of Sched. Ephemeris is from JPL solution #50. Schedule for VLBA_MK (Code Mk ) Page 2 Interferometric Radar Observations of Asteroid 2006VV2 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 ---------------------------------------------------------------------------------------- --- Sun 1 Apr 2007 Day 91 --- Next scan frequencies: 2379.94 2379.94 2379.94 2379.94 2379.94 2379.94 2379.94 2379.94 Next BBC frequencies: 720.06 720.06 720.06 720.06 720.06 720.06 720.06 720.06 Next scan bandwidths: 0.12 0.12 0.12 0.12 0.12 0.12 0.12 0.12 02 25 00 2006VV2 04 39 29 3.0 83.0 -6.0 -70.4 0 1 1 0 02 25 00 02 35 00 --- 04 49 30 5.3 83.8 -5.8 -70.7 600 F 1 2 02 25 35 02 35 00 J1041+0610 04 49 30 3.9 84.9 -5.9 -70.5 -9 1 1 2 02 35 00 02 40 00 =1038+064 04 54 31 5.1 85.3 -5.8 -70.6 291 F 1 4 02 35 00 02 40 00 2006VV2 04 54 31 6.5 84.3 -5.7 -70.8 -9 1 1 4 02 40 00 02 50 00 --- 05 04 33 8.8 85.1 -5.6 -71.0 591 F 1 6 02 40 00 02 50 00 J1041+0610 05 04 33 7.4 86.1 -5.6 -70.8 -9 1 1 6 02 50 00 02 55 00 =1038+064 05 09 34 8.6 86.5 -5.5 -70.8 291 F 1 7 02 50 00 02 55 00 J1041+0610 05 09 34 8.6 86.5 -5.5 -70.8 -4 1 1 7 02 55 00 03 00 00 =1038+064 05 14 35 9.8 87.0 -5.5 -70.9 296 F 1 8 02 55 00 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. Setup file: radarS_nroll.set Matches group v13cm_2 in /home/postdocs2/gb3n/sched/catalogs/freq.dat LA,NL only 2200-2400 Setup group: 10 Station: VLBA_MK Total bit rate: 32 Format: VLBA1:1 Bits per sample: 2 Sample rate: 2.000 Number of channels: 8 Speedup factor: 4.00 Disk used to record data. 1st LO= 3100.00 3100.00 3100.00 3100.00 3100.00 3100.00 3100.00 3100.00 Net SB= U U U U U U U U Pol. = RCP LCP RCP LCP RCP LCP RCP LCP BBC = 1 2 3 4 5 6 7 8 BBC SB= L L L L L L L L IF = A C A C A C A C VLBA FE= 13cm omit 13cm omit VLBA Synth= 15.4 3.1 15.4 The following frequency sets based on this setup were used. Frequency Set: 11 Setup file default. Used pcal sets: 1 LO sum= 2379.94 2379.94 2379.94 2379.94 2379.94 2379.94 2379.94 2379.94 BBC fr= 720.06 720.06 720.06 720.06 720.06 720.06 720.06 720.06 Bandwd= 0.125 0.125 0.125 0.125 0.125 0.125 0.125 0.125 The following pulse cal sets were used with this setup: Pulse cal detection set: 1 PCAL = OFF PCALXB1= S1 S2 S3 S4 S5 S6 S7 S8 PCALXB2= M1 M2 M3 M4 M5 M6 M7 M8 PCALFR1= 0 0 0 0 0 0 0 0 PCALFR2= 0 0 0 0 0 0 0 0 Track assignments are: track1= 2, 6, 10, 14, 18, 22, 26, 30 barrel=roll_off SOURCE LIST -- Interferometric Radar Observations of Asteroid 2006VV2 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) * J1041+0610 10 38 40.885160 * 10 41 17.162506 10 41 41.205729 0.30 1038+064 06 25 58.53255 * 06 10 16.92333 06 07 54.78708 0.21 J1041+06 /home/postdocs2/gb3n/sched/catalogs/sources.vlba VLBA Calib Survey - GSFC sols. - created L.Petrov 2005f_astro 0.833 scan hours, 38.610 baseline hours above horizon. * 2006VV2 10 34 41.868121 * 10 37 18.876731 10 37 43.031923 0.00 07 52 26.62707 * 07 36 51.11576 07 34 30.30866 0.00 Satellite. Position is for scan 1, station 1. 1.167 scan hours, 54.550 baseline hours above horizon. Planetary motion used. Ref. MJD: 54191.0417 Rates: RA = 0.42135E+03 s/day Dec = -0.79459E+05 arcsec/day KERFILE: /home/postdocs2/gb3n/sched/naif0008.tls SATFILE: /home/postdocs2/gb3n/sched/2006VV2/merged_spk.soln50 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) J1041+0610 148.6 2006VV2 147.2 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