Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.atnf.csiro.au/pub/people/vlbi/vt02/vt02f/vt02f8/vt02f8sch.pa Дата изменения: Tue Mar 7 04:51:32 2006 Дата индексирования: Mon Jun 28 00:05:44 2010 Кодировка: Поисковые слова: http astrokuban.info astrokuban

COVER INFORMATION

Station: PARKES (Code Pa )
Experiment: real-time fringe-check for v195a
Exp. Code: vt02f8


Schedule Version: 1.00
Processed by SCHED version: 6.02 July 2005

PI: LBA fringe-check

Address: LBA
LBA
LBA


Phone: 02 6790 4032
EMAIL: vlbiobs.csiro.au
Fax:
Phone during observation:

Observing mode: Fringe-check

Notes:




Schedule for PARKES (Code Pa ) Page 2
real-time fringe-check for v195a
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).
SYNC: Time correlator is expected to sync up.
----------------------------------------------------------------------------------------
Start UT Source Start / Stop Early Tapes TPStart
Stop UT LST EL AZ HA UP ParA Dwell (see above) SYNC
----------------------------------------------------------------------------------------

--- Tue 14 Mar 2006 Day 73 ---

Next scan frequencies: 1665.00 1665.00
Next BBC frequencies: 361.00 361.00
Next scan bandwidths: 4.00 4.00

13 00 00 1253-053 10 21 05 44.8 61.7 -2.6 -132.1 0 1 1 52 13 00 00
13 55 00 --- 11 16 14 54.2 46.1 -1.7 -142.6 3300 F 1 1208 13 00 10

13 55 00 340.054-0.24 11 16 14 27.3 128.3 -5.5 D -110.5 -218 1 1 1208 13 55 00
14 05 00 --- 11 26 16 28.9 127.6 -5.4 D -109.0 0 F 1 1418 13 55 10


SETUP FILE INFORMATION:
NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings.


Setup file: oh.set
Matches group pa20cm in /nfs/atapplic/vlbi/sched/catalogs/freq.dat

Setup group: 4 Station: PARKES Total bit rate: 32
Format: S2 Bits per sample: 2 Sample rate: 8.000
Number of channels: 2 Passes/head pos: 4 Speedup factor: 1.00

Tape used at high density at 4.200 ips.
Time per pass is 361.90 minutes.

1st LO= 1304.00 1304.00
Net SB= U U
Pol. = RCP LCP
BBC = 1 2
BBC SB= U U
IF = 1N 2N

The following frequency sets based on this setup were used.

Frequency Set: 4 Based on FREQ, BW, and/or DOPPLER in schedule. No pcal detection.
LO sum= 1665.00 1665.00
BBC fr= 361.00 361.00
Bandwd= 4.000 4.000

Frequency Set: 8 Based on FREQ, BW, and/or DOPPLER in schedule. No pcal detection.
LO sum= 1665.00 1665.00
BBC fr= 361.00 361.00
Bandwd= 4.000 4.000

Track assignments are:
track1= 0, 0
track2= 0, 0
track3= 0, 0
track4= 0, 0
barrel=roll_off
 SOURCE LIST -- real-time fringe-check for v195a
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)

* 1253-053 12 53 35.831233 * 12 56 11.166500 12 56 31.483609 0.00
-05 31 07.99414 *-05 47 21.52300 -05 49 31.39103 0.00
From catalog imbedded in main SCHED input file.
0.917 scan hours, 5.500 baseline hours above horizon.

* 340.054-0.24 16 44 35.982917 * 16 48 13.880000 16 48 40.952805 0.00
-45 16 28.74023 *-45 21 45.10000 -45 22 24.85852 0.00
From catalog imbedded in main SCHED input file.
Doppler based on LSR frame and radio definition. Velocities:
-55.00 -55.00
0.167 scan hours, 0.383 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)
1253-053 158.6
340.054-0.24 96.8

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