***************************************************************************
REVISED 001122
Last observation was changed for some stations. Number of scans per station
and tape usage is changed. The schedule is different from 0h UT onwards.
***************************************************************************
RDV24 (Astrometric/Geodetic VLBA-24)
2000 December 4
Notes prepared by
Nancy Vandenberg, NVI/GSFC
Schedule name: rdv24.skd
Pointing files: rdv24crd.br, rdv24crd.fd, rdv24crd.hn, rdv24crd.kp,
rdv24crd.la, rdv24crd.mk, rdv24crd.nl, rdv24crd.ov,
rdv24crd.pt, rdv24crd.sc
ftp://aspen.nrao.edu/home/aspen6/astronomy/dec00/rdv24
Summary file for correlator: rdv24.sksum on aspen
PCFS file: vlbigeo@cddisa.gsfc.nasa.gov/vlbigeo/dec00/rdv24.skd
http://lupus.gsfc.nasa.gov/sess/2000/sesshtml/rdv24.html
Nominal Start: 14:00 U.T. on December 4 (day 339)
first observation at 13:45 U.T. on 4C39.25 for Br-Fd-Gc-Hn-
La-Nl-Ov-Pt-Sc-Wf-Gg
first observation at 14:00 U.T. on 2145+067 for Hh-Ma-Mc-Wz
first observation at 14:00 U.T. on 4C39.25 for Kk-Kp-Mk-Ny-Ts
Duration: 24 hours + 1 hour extra for Br-Fd-Gc-Hn-La-Nl-Ov-Pt-Sc-Gg-Wf
Nominal Stop: 14:00 U.T. on December 5 (day 340)
last observation at 13:41 U.T. on 2234+282 for Hh
last observation at 13:42 U.T. on 1045-188 for Kk
last observation at 13:59 U.T. on 1357+769 for Ma-Mc-Wz-Ny-Ts-Mk
last observation at 14:10 U.T. on NRAO512 for Br-Fd-Gc-Hn-Kp-La
Nl-Gg-Ov-Pt-Sc-Wf
Correlator: VLBA at Socorro
Station Codes # of tapes # of obs Occupation Code
Brewster B Br 2.4 (TT) 283 76149901
Fort Davis D Fd 2.4 (TT) 303 76139801
Gilcreek A Al 2.2 (TT) 263 40476601
HartRAO J Hh 2.0 (TT) 148 72326201
Hancock H Hn 2.4 (TT) 263 76185001
Kokee K Kk 2.0 (TT) 246 72983001
Kitt Peak L Kp 2.4 (TT) 293 76109401
Los Alamos M La 2.4 (TT) 301 76119601
Matera I Ma 2.2 (TT) 235 72435701
Mauna Kea N Mk 2.1 (TT) 211 76175501
Medicina C Mc 2.4 (TT) 283 72308801
North Liberty O Nl 2.5 (TT) 284 76129701
Ny Alesund Q Ny 2.1 (TT) 231 73313301
GGAO (MV3) Z Gg 2.1 (TT) 254 71085301
Owens Valley R Ov 2.4 (TT) 290 76165401
Pie Town S Pt 2.4 (TT) 301 72348601
St. Croix E Sc 2.4 (TT) 263 76159001
Tsukuba U Ts 2.1 (TT) 258 73452301
Westford F Wf 2.2 (TT) 274 72097301
Wettzell V Wz 2.0 (TT) 197 72247801
Total number of observations (delay measurements): 31658
Total number of scans in the schedule: 553
Special notes for this session:
- The VLBA stations will use automatic tape allocation and automatic
tape reversal.
- Most VLBA stations record two initial fringe finding scans along
with geodetic stations Fairbanks and Westford. These stations also
record two final long (5-min) scans.
- GGAO (MV3) will participate in this session in order to maintain
the VLBI position determination for this fundamental station.
This station is tagged along so that its small size does not
make the scan lengths too long.
- Onsala will not participate in this session.
- The Green Bank geodetic station has been shut down and will not
participate in any future sessions.
- Wettzell and Kokee will leave the schedule on day 339 to observe
intensive schedule i00339 which starts at 18:30. They will rejoin
the RDV schedule at about 20:00 at pass 7F.
Purpose
=======
This is the last of six bi-monthly coordinated astrometric/geodetic
experiments in 2000 that use the full 10-station VLBA plus up to 10
geodetic stations capable of recording VLBA modes. This year's series
is a continuation of the highly successful RDV series begun in 1997.
These experiments are being coordinated by the geodetic VLBI programs
of three agencies: USNO, NASA, and NRAO. The experiments have been
designed so that the same data set may be used by each agency for
its particular goals.
USNO will perform repeated imaging and correction for source structure.
These sources will establish a set of core reference sources with known
structure and precisely known positions. These data will provide the
basis for evaluating the long term stability of the radio reference
frame and the ultimate accuracy of wide angle astrometric measurements
of extragalactic radio sources using VLBI.
NASA will analyze this data to determine a high accuracy terrestrial
reference frame. The data will incorporate the VLBA stations into
the VLBI reference frame through the inclusion of other geodetic
stations for which we have long histories. The data will also produce
the most accurate Earth rotation results ever produced. We will use
these data to make accurate absolute measurements of UT1.
NRAO will use these sessions to provide a service to users who
require high quality positions for small numbers of sources. While
the quality of these results will be high, the observing and data
reduction overhead required will be minimal because such sources
can be incorporated into a session of the regular geodetic
observations, instead of requiring special observations.
Sources for this series of experiments will be selected using the
proposed approach. For each experiment we will select a set of 70-80
sources out of the pool of ~400 Northern Hemisphere ICRF sources.
About 40-50 of these will remain the same from experiment to experiment
and will be chosen to optimize the goals of the three groups.
Schedule
========
This is a new schedule generated by Nancy Vandenberg using sked.
"Requested" Sources in rdv24 :
Leonid Petrov requested that 0839+187 and nearby sources be observed
so that reference positions are available for observations when
Jupiter passes close to the quasar. The target source and first two
reference sources were observed in RDV23. The other two reference
sources are observed in this session.
1) J0839+1802 08h39m30.7209 18d02'47.141 0.17 Jy distance: 49 arcmin!
2) J0854+2006 08h54m48.8749 20d06'30.642 0.13 Jy distance: 3d21'
3) J0856+2111 08h56m57.2445 21d11'43.644 0.18 Jy distance: 4d21'
4) J0825+1332 08h25m11.8915 13d32'32.541 0.21 Jy distance: 5d03'
I would like to ask for an accurate position measures for the sources listed
below. These sources will be used for phase referencing in my recently proposed
VLBA observations because of the low flux densities of the target sources.
Emmanuel Momjian requested accurate positions for the following sources
for a phase referencing experiment with the VLBA.
__________________________________________________________________________
| Source Name | RA | DEC | Flux Density(mJy) |
| | (2000) | (2000) | ------------------------ |
| | | | 2.3GHz | 8.4GHz |
|______________|_______________|______________|______________|_____________|
| | | | | |
| J0837+2454 | 08:37:40.2467 | 24:54:23.123 | 400 | 350 |
| | | | | |
| J1329+3154 | 13:29:52.8650 | 31:54:11.047 | 1500 | 833 |
| | | | | |
| J1453+2648 | 14:53:53.6061 | 26:48:33.472 | 600 | 400 |
|______________|_______________|______________|______________|_____________|
Yearly (Y), ROTATING ( ), NEW (N) SOURCES FOR RDV24 :
| 0237-027
| 0406-127
N | 0422-380
| 0458+138
| 0736+017
| 0808+019
| 0912+297
Y | 1004+141
| 1045-188
| 1147+245
| 1237-101
N | 1244-255
| 1342+662
| 1427+543
| 1511-100
| 1622-297
| 1717+178
| 1826+796
Y | 2136+141
| 2144+092
| 2328+107
With this session we continue rotating through the large list of
candidate ICRF sources. The method was as follows:
- Remove sources from the core list of 80 sources used last year.
- Add up to 20 sources from the list of candidates that already have
some NEOS or VLBA data available (rotating sources).
- Add 2 sources from the list of sources to be observed yearly.
- Add 2 sources from the list of candidates that have never been
observed with the VLBA (new sources).
The same criteria were used for generating this schedule as were
used during the first year of these sessions. The criteria for
sources to be mapped are a minimum of 3 scans and 135 observations.
These criteria are relaxed for sources below -25 degrees declination.
Most of the sources in this schedule meet the mapping criteria.
The schedule was made using a combination of automatic selection
plus manual scheduling to improve the coverage of the sources.
Automatically scheduled scans were selected first on their improvement
of sky coverage in the previous 1 hour, and then the best 60% were
evaluated for the minor options: minimize idle time, minimize slewing
time, and maximize the number of observations. An individual source
was not observed more often than every 90 minutes. An early start
of 30 seconds was used for the first scan on a tape pass. The minimum
scan length was 40 seconds.
NEW: RDV21 was the first schedule made with a new version of sked that
takes advantage of the automatic tape allocation at the VLBA stations.
For these stations sked assumes that any scan will fit on the tape
pass and there is no need to run the tape to the end of a pass if
the scan is too long to fit in the remaining tape.
Recording Mode and Frequencies: same as previous experiment
===========================================================
The data will be recorded using the following setup:
8 channels
1:4 fan-out
16 MHz sample rate
1-bit sampling
This recording mode is designated 128-8-1. The correlator speed-up
factor is 2.
The frequency sequence covers 490 MHz in 8 channels. This span fits in
one VLBA receiver passband but it uses both the high and low parts of the
geodetic receivers. Because only 8 channels are available when observing
with the VLBA stations, a wider spanned bandwidth is not advisable. With
the 1:4 fanout at 16 MHz sample rate, all 32 tracks are recorded in one
pass, so there will be 14 passes on a tape.
These tables list the setup for the VLBA stations, the geodetic stations
with VLBA back ends, and the geodetic stations with Mark IV back ends.
These are the SAME frequencies used in all the standard RDV sessions.
Geodetic stations: please read the special procedures in the next section!
VLBA | Fairbanks | Kokee
Chan Sky Tracks LO IF BBC | LO IF BBC #| LO IF BBC #
1 X 8405.99 2, 4, 6, 8 7900 B 505.99| 7600.1 A 805.89 3| 7600 A 805.99 3
2 X 8475.99 10,12,14,16 7900 B 575.99| 7600.1 A 875.89 4| 7600 A 875.99 4
3 X 8790.99 18,20,22,24 7900 B 890.99| 8080.0 C 710.99 5| 8100 C 690.99 5
4 X 8895.99 26,28,30,32 7900 B 995.99| 8080.0 C 815.99 6| 8100 C 795.99 6
5 S 2220.99 3, 5, 7, 9 2900 A 679.01| 1540.1 B 680.89 9| 1500 B 720.99 9
6 S 2240.99 11,13,15,17 2900 A 659.01| 1540.1 B 700.89 10| 1500 B 740.99 10
7 S 2330.99 19,21,23,25 2900 A 569.01| 1540.1 B 790.89 13| 1500 B 830.99 13
8 S 2360.99 27,29,31,33 2900 A 539.01| 1540.1 B 820.89 14| 1500 B 860.99 14
VLBA | Tsukuba
Chan Sky Tracks LO IF BBC | LO IF BBC #
1 X 8405.99 2, 4, 6, 8 7900 B 505.99| 7680 A 725.99 3
2 X 8475.99 10,12,14,16 7900 B 575.99| 7680 A 795.99 4
3 X 8790.99 18,20,22,24 7900 B 890.99| 8080 A 710.99 5
4 X 8895.99 26,28,30,32 7900 B 995.99| 8080 A 815.99 6
5 S 2220.99 3, 5, 7, 9 2900 A 679.01| 1600 B 620.99 9
6 S 2240.99 11,13,15,17 2900 A 659.01| 1600 B 640.99 10
7 S 2330.99 19,21,23,25 2900 A 569.01| 1600 B 730.99 13
8 S 2360.99 27,29,31,33 2900 A 539.01| 1600 B 760.99 14
Medicina, Wettzell, Matera, GGAO
VLBA | Westford, Ny Alesund, HartRAO
Chan Sky Tracks LO IF BBC | LO IF VC VC# Patch
1 X 8405.99 2, 4, 6, 8 7900 B 505.99| 8080.0 1 325.99 3 H
2 X 8475.99 10,12,14,16 7900 B 575.99| 8080.0 1 395.99 4 H
3 X 8790.99 18,20,22,24 7900 B 890.99| 8580.1 3 210.89 5 L
4 X 8895.99 26,28,30,32 7900 B 995.99| 8580.1 3 315.89 6 H
5 S 2220.99 3, 5, 7, 9 2900 A 679.01| 2020.0 2 200.99 9 L
6 S 2240.99 11,13,15,17 2900 A 659.01| 2020.0 2 220.99 10 L
7 S 2330.99 19,21,23,25 2900 A 569.01| 2020.0 2 310.99 13 H
8 S 2360.99 27,29,31,33 2900 A 539.01| 2020.0 2 340.99 14 H
Procedures
==========
With continuous tape motion, the tape starts moving and recording
at the beginning of the first scan of a pass. The tape runs and records
continuously thereafter to the end of the tape (EOT or BOT). A parity
check is done after the tape reaches this point. The tape starts moving
in the opposite direction at the early start time (30 seconds) before
the next scan. There will be a variable length of time between tape
passes. For the VLBA stations, there will normally be a long enough
time gap between passes for playback.
Special procedures for non-VLBA stations
========================================
The tape motion in this experiment is different from normal
start&stop schedules. At the time the antenna gets on source, you
should see the command "data_valid=on" from the SNAP schedule. This
is the signal that the VLBA correlator will use to determine when
to start correlating this scan.
At the time the antenna begins slewing to the next source, you will
see the command "data_valid=off" from the schedule. This is the signal
the correlator will use to stop correlating that scan. There will
be no "et" command at the end of a scan.
The DRUDG listing has a column that lists the time that the tape
will stop. Note the "Start Tape" and "Stop Tape" columns list
times only when the tape will start or stop, otherwise the time is
blanked out because the tape is moving. For each scan, the "Start
Data" column will be the time when the antenna is expected to be
on source. The "Stop Data" column is the time when the antenna
starts slewing to the next source.
After the setup procedure, the tape is started at the beginning of
each pass and will continue to move, at record speed, until it reaches
the end of the pass. There are no fast tape motions in this schedule.
The tape is continuously recording from the initial "st" command at
the start of the pass. There are no other "st" commands during a
pass and there are no other setup procedures called.
If you have to re-start the schedule for a problem or emergency, you
will be able to do it either 1) at the beginning of a pass or 2)
in the middle of a pass by entering the setup and start tape commands
manually. The problem is that the heads cannot be positioned reliably
when the tape is moving if there is recorded data on the tape. If the
tape is moving the reproduce power level can cause cross-talk with
the head positioner and give false indications of position. Another
problem is that the data disappears on tape while the formatter
resets itself, thus largely eiliminating the benefits of continuous
motion.
At the end of each pass a parity check is done. You will need
procedures named "checkf80" and "checkr80". Check and adjust the timing
of this procedure and then make sure it can complete in the 100 seconds
that the schedule allows.
Special procedures for Medicina, Westford, GGAO
Ny Alesund, Wettzell, HartRAO, Tsukuba, Matera
==================================================================
These stations have Mark IV formatters.
Use the procedures generated by DRUDG. These should be the same
as the ones used in previous RDV sessions, starting with RDV13.
This is a non-standard setup. There are 8 video converters used:
3, 4, 5, 6, 9, 10, 13, and 14. These were selected so that you
will NOT have to change the standard geodetic IF patching. The 6
unused VCs 1, 2, 7, 8, 11, and 12 should be set to frequencies which
do not occur in any of the passbands. Any value in the 100-200 MHz
range is OK.
The Mark IV formatters currently have no barrel roll capability, so
please verify that your FORM command has no specification for barrel
roll.
The IF3 command in the procedure IFDSX assumes that VC3 will be
patched to High. Please verify that the switches for your IF3
module are wired this way, and if they are not please edit the
IF3 command to change the switches. If you have questions about
the wiring, please contact Brian Corey at Haystack.
Special procedures for Fairbanks, Kokee
=======================================
These stations have VLBA back ends.
Use the procedures generated by DRUDG. BBCs 3,4,5,6 are used at
X-band with IFs A and C. BBCs 9,10,13,14 are used at S-band with IF B.
The unused BBCs 1,2,7,8,11,12 should be set to frequencies
which do not occur in any of the passbands. Any value in the range
500-600 MHz is OK.
The formatter should be set up to use barrel roll. Please verify that
you are using the same barrel roll as you used in previous sessions
correlated at the VLBA.
CHECKLIST for non-VLBA stations
===============================
Please follow the checklist below to ensure you have done all the
necessary steps for this experiment:
1. Make .prc file with DRUDG and check them out, or use the procedures
from last session. Check out parity check procedures.
2. Make .snp file and listings using DRUDG options 3 and 5.
3. Set up your system to monitor the clocks with the "gps-fmout" or
"fmout-gps" commands. If you have questions about this, please
contact Ed Himwich as soon as possible.
4. Send a "ready" message an hour or so before the experiment to the
ivs-ops mail list. Copy analysts@nrao.edu on your ready message.
5. Send a "start" message soon after you have started recording.
Copy analysts@nrao.edu on the message.
6. At the end of the experiment, send a "finish" message summarizing
how the experiment was conducted. Copy analysts@nrao.edu on
your message.
8. Transfer your log files to your normal log file data center.
The directories for three possible servers are listed below:
directory on cddisa: dec00
directory on vlbeer: dec00
directory on aspen: /home/aspen6/astronomy/dec00/rdv24
NOTE: If you don't normally use aspen, you should not put
your log file on that server. The VLBA correlator knows where
to find your log files.
Correlation
===========
This experiment will be correlated at the VLBA Correlator. Tapes should
be shipped to Socorro as soon after the experiment as practical.
Summary
=======
The following listing is a summary of the observations in this schedule.
SKED Summary from file ../schedules/rdv24.skd for experiment RDV24
(all scans with at least one subnet station)
SOURCE |0 6 12 18 | #SCANS #OBS #Obs/bl
J0856+21I x x x I 3 126 1.1
J0825+13Ix x x x I 4 132 1.3
J0837+24I x x x x x I 5 293 2.6
J1329+31I x x x x x x x I 7 519 4.4
J1453+26I x x x I 3 259 2.3
0237-027I x x x x I 4 195 2.3
0406-127I x x x x x I 5 116 1.6
0422-380Ix x x x I 4 26 .6
0458+138I x x x I 3 170 1.7
0736+017I x x x x x x I 6 365 4.2
0808+019I x x x x x x I 6 265 3.0
0912+297I x x x I 3 206 1.8
1045-188I x x x x x I 5 147 2.4
1147+245I x x x x I 4 338 3.1
1237-101I x x x I 3 115 2.2
1244-255I x x x x x x I 6 175 3.3
1342+662I x x x I 3 276 1.6
1511-100I x x x x x I 5 136 2.8
1622-297I I 0 0 .0
1717+178I x x x xI 4 255 2.4
1826+796I x x x I 3 269 1.5
2144+092I x x x x I 4 230 2.4
2328+107I x x x x I 4 254 2.6
0003-066I x x x x x x x x x I 9 290 3.8
0014+813I x x x x x x x x xI 9 1049 6.0
0048-097I x x x x x x x I 7 210 2.9
0059+581I x x x x x x x x x xI 10 1285 8.3
0104-408I x x x x x x x I 7 94 3.1
0119+115I x x x x x I 5 272 2.8
0119+041I x x x x x x x I 7 259 2.8
0133+476I x x x x x x x x x I 9 831 6.2
0201+113I x xI 2 126 1.3
0202+149I x x x x x x x I 7 413 4.1
0208-512I x x I 2 2 .1
0229+131I x x x xI 4 198 2.0
0234+285I x x x x x x x x xI 9 610 5.3
0235+164I x x x x x x x I 7 349 3.3
NGC1052 I x x x x x x I 6 251 3.8
CTA26 I x x x x x x I 6 195 2.3
0402-362I x x x x x x I 6 105 2.4
3C120 I x x x x x x x I 7 400 4.4
0454-234I x x x x x x x I 7 141 2.4
0458-020Ix x x x I 4 96 1.1
0528+134Ix x x x x x x x I 8 531 5.3
0537-441I x x x x I 4 20 .9
0552+398I x x x x x x x x x x I 10 603 4.7
0642+449Ix x x x x x x x x I 9 931 6.9
0727-115I x x x x x x x I 7 241 3.5
0804+499I x x x x x x x x x I 9 1067 7.8
0823+033I x x I 2 81 .9
OJ287 I x x x x x x x x I 8 518 4.9
0919-260I x x x x x I 5 179 3.3
0920-397I x x I 2 37 1.1
4C39.25 I x x x x x xx x x x I 11 920 7.3
0955+476I x x x x x x x I 7 832 6.3
1034-293I x x I 2 2 .0
1044+719Ix x x x x x x x x x I 10 1407 8.3
1101+384I x x x x I 4 205 1.6
1124-186I x x x x x x I 6 177 2.9
1128+385I x x x x x I 5 591 4.6
1144-379I x x x x x I 5 69 2.0
1145-071I x x x x I 4 73 .9
1156+295I x x x I 3 73 .6
3C274 I x x x x x x x I 7 562 5.7
1308+326I x x x x x x I 6 473 3.9
1313-333I x x x x I 4 63 1.4
1334-127I x x x x x x x xI 8 278 3.9
1357+769I x x x x x x x x I 8 1130 6.5
OQ208 I x x x x x x xI 7 449 3.9
1424-418I x x x x I 4 9 .3
1448+762I x x I 2 272 1.6
1451-375I x x x x xI 5 21 .5
1451-400I x x I 2 37 1.2
1514-241I x x x x x x x I 7 148 2.7
1606+106I x x x x x x x x x xI 10 539 5.6
1611+343I x x x x x x x x I 8 660 5.4
1622-253I I 0 0 .0
NRAO512 Ix x x x x x x x x I 10 817 6.4
1642+690I x x x x x x x x I 8 835 5.0
1657-261I I 0 0 .0
1739+522I x x x x x x x xI 8 577 4.0
1741-038I x x x x x x x x x xI 10 277 3.3
1745+624Ix x x I 3 398 2.5
1749+096Ix x x x x x x I 7 265 2.8
1803+784Ix x x x x x x x x I 9 1245 7.2
1815-553I x x I 2 2 .2
1908-201I x x x x x x x x I 8 220 3.7
1921-293Ix x x x x x x x I 8 175 3.6
1954-388I x x x x x x x I 7 51 1.5
2052-474I x x x x x I 5 7 .3
2145+067I x x x x xx x x I 8 325 3.5
VR422201I x x x x x x x x x x x I 11 628 4.8
3C446 I x x x x x x x I 7 271 3.4
2234+282I x x x x I 4 207 1.8
2243-123Ix x x x x x x x I 8 215 2.8
Total scans, obs: 546 31756
Average number of obs. per baseline per source (normalized by up-time) = 3.2
Min = .0 Max = 22.9 (Baseline Gc-Kp on 1237-101) RMS = 3.0
Total time: 1466 minutes ( 24.4 hours).
Key: Br=BR-VLBA Fd=FD-VLBA Gc=GILCREEK Hh=HARTRAO Hn=HN-VLBA
Kk=KOKEE Kp=KP-VLBA La=LA-VLBA Ma=MATERA Mc=MEDICINA
Mk=MK-VLBA Nl=NL-VLBA Ny=NYALES20 Gg=ORION_5M Ov=OV-VLBA
Pt=PIETOWN Sc=SC-VLBA Ts=TSUKUB32 Wf=WESTFORD Wz=WETTZELL
Br Fd Gc Hh Hn Kk Kp La Ma Mc Mk Nl Ny Gg Ov Pt Sc Ts Wf Wz Avg
% obs. time: 70 69 62 24 72 52 64 65 57 40 55 68 61 57 65 66 63 46 70 58 59
% cal. time: 3 3 3 1 3 2 3 3 2 2 3 3 2 3 3 3 2 2 3 2 2
% slew time: 24 24 17 33 22 12 23 24 16 27 22 24 13 9 23 24 22 12 12 6 19
% idle time: 1 3 17 40 2 32 8 7 23 29 19 4 23 29 7 5 11 37 13 32 17
# of tapes : 2.4 2.4 2.2 2.1 2.4 2.0 2.4 2.4 2.2 2.2 2.4 2.5 2.2 2.1 2.4 2.4 2.4 2.1 2.2 2.2
total # scans: 289 301 265 153 272 244 293 300 230 211 278 287 223 267 290 301 257 256 275 190 259
# scans/hour : 11 12 10 6 11 9 11 12 9 8 11 11 9 10 11 12 10 10 11 7 10.8
Avg scan (sec): 215 201 206 142 234 188 192 190 219 170 175 208 242 190 198 193 216 160 226 269 201
# OF OBSERVATIONS BY BASELINE
| Br Fd Gc Hh Hn Kk Kp La Ma Mc Mk Nl Ny Gg Ov Pt Sc Ts Wf Wz StnTotal
----------------------------------------------------------------------------------------------
Br|289 270 232 20 246 180 267 276 116 134 210 265 177 220 270 276 212 137 244 132 3884
Fd| 301 216 25 251 181 283 294 109 126 213 276 165 231 275 295 230 123 251 126 3940
Gc| 265 12 201 176 215 221 115 132 195 218 185 179 221 221 168 168 203 130 3408
Hh| 153 33 0 21 25 105 73 0 28 37 38 13 25 41 48 35 58 637
Hn| 272 153 240 252 121 138 175 255 170 236 234 252 230 110 261 136 3694
Kk| 244 186 180 69 82 230 170 123 143 189 181 131 147 155 90 2766
Kp| 293 284 107 124 220 265 165 219 272 285 215 128 241 124 3861
La| 300 114 131 213 280 170 230 278 300 228 128 251 129 3984
Ma| 230 192 66 118 149 122 103 114 110 97 124 161 2212
Mc| 211 81 135 165 129 120 131 127 97 136 177 2430
Mk| 278 198 131 160 222 214 152 160 174 83 3097
Nl| 287 174 232 260 280 231 123 257 133 3898
Ny| 223 152 162 170 142 140 169 154 2900
Gg| 267 214 230 215 104 236 125 3415
Ov| 290 279 206 131 233 119 3801
Pt| 301 228 128 251 129 3989
Sc| 257 77 231 122 3296
Ts| 256 112 91 2249
Wf| 275 134 3698
Wz| 190 2353
Number of 2-station scans: 90
Number of 3-station scans: 55
Number of 4-station scans: 43
Number of 5-station scans: 25
Number of 6-station scans: 16
Number of 7-station scans: 10
Number of 8-station scans: 13
Number of 9-station scans: 16
Number of 10-station scans: 22
Number of 11-station scans: 24
Number of 12-station scans: 16
Number of 13-station scans: 25
Number of 14-station scans: 37
Number of 15-station scans: 33
Number of 16-station scans: 35
Number of 17-station scans: 25
Number of 18-station scans: 32
Number of 19-station scans: 29
Number of 20-station scans: 0
Number of 21-station scans: 0
Total # of scans, observations: 546 31756
Average baseline components for all observations
Average XY = 4311.
Average XZ = 3535.
Average YZ = 3037.
Average length = 4633.