QUAK06 (Astrometric/Geodetic QUAK06) 2006 November 08 Notes prepared by John Gipson, NVI/GSFC Schedule name: QUAK06.skd Pointing files: QUAK06crd.br, QUAK06crd.fd, QUAK06crd.hn, QUAK06crd.kp, QUAK06crd.la, QUAK06crd.mk, QUAK06crd.nl, QUAK06crd.ov, QUAK06crd.pt, QUAK06crd.sc ftp://vlbiobs@aspen.nrao.edu/home/aspen6/astronomy/nov06/QUAK06 Summary file for correlator: QUAK06.sksum on aspen PCFS file: ftp://vlbigeo@cddisa.gsfc.nasa.gov/vlbigeo/nov06/QUAK06.skd http://lupus.gsfc.nasa.gov/sess/2006/sesshtml/QUAK06.html This experiment uses the VLBA and the the following 3 stations: HOBART, KOKEE and URUMQI First observations: Source Start DURATIONS name yyddd-hhmmss Br Fd Hn Ho Kk Kp La Mk Nl Ov Pt Sc Ur 0743+259 06312-180000| 300 300 300 300 300 300 300 300 300| 1803+784 06312-180000| 300 300 300 | 1803+784 06312-180648| 300 300| 1424-418 06312-180910| 300 300 300 300 300 300 300 300 300 | Kokee stars observing at 194500 after the intensive: 1357+769 06312-194500| 300 300 300 300 300 300 300 300 300 300 300 300| 0059+581 06312-195137| 40 40 40 40 40 40 40 40 40 40| 1034-293 06312-195157| 55 55 40 | Last observations: 1219+044 06313-174531| 40 40 40 40 40 40 40 40 40 | 1923+210 06313-174820| 40 40 40 40 40 40 40 40 | 1803+784 06313-175019| 300 300 300 | 0743+259 06313-175056| 300 300 300 300 300 300 300 300 300 300| 1739+522 06313-175757| 300 300 300 300 300 300 300 300 300 300 300 300| Observing summary: Key: Br=BR-VLBA Fd=FD-VLBA Hn=HN-VLBA Ho=HOBART26 Kk=KOKEE Kp=KP-VLBA La=LA-VLBA Mk=MK-VLBA Nl=NL-VLBA Ov=OV-VLBA Pt=PIETOWN Sc=SC-VLBA Ur=URUMQI Br Fd Hn Ho Kk Kp La Mk Nl Ov Pt Sc Ur Avg % obs. time: 46 45 41 51 48 47 47 43 45 43 47 46 45 46 % cal. time: 5 5 5 2 3 5 5 4 5 5 5 4 2 4 % slew time: 27 27 28 29 13 27 27 24 27 26 27 25 18 26 % idle time: 22 21 26 16 35 20 20 29 22 25 20 24 34 25 total # scans: 413 454 437 198 288 446 454 324 458 425 455 380 204 379 # scans/hour : 17 19 18 8 12 19 19 13 19 18 19 16 8 16 Avg scan (sec): 96 86 81 224 144 91 89 115 85 88 89 104 191 113 Total GBytes: 939 951 871 906 901 968 972 848 944 904 976 915 810 916 Total GB(M5): 835 846 774 806 801 860 864 754 839 804 867 814 720 814 # of tapes : .1 .1 .1 .1 .1 .1 .1 .1 .1 .1 .1 .1 .1 tape change times (hhmm): Total number of tapes: .9 Total GBytes (M5) recorded: 10582.2 # OF OBSERVATIONS BY BASELINE | Br Fd Hn Ho Kk Kp La Mk Nl Ov Pt Sc Ur StnTotal --------------------------------------------------------------------------- Br| 328 304 69 141 343 344 167 339 351 346 236 122 3090 Fd| 323 77 131 414 433 166 381 364 435 296 82 3430 Hn| 21 87 296 323 108 391 277 315 347 119 2911 Ho| 169 87 75 171 47 85 80 22 62 965 Kk| 145 134 276 111 157 137 76 101 1665 Kp| 417 181 351 388 427 270 85 3404 La| 166 384 374 444 289 90 3473 Mk| 135 194 170 96 101 1931 Nl| 329 374 333 100 3275 Ov| 381 231 90 3221 Pt| 282 90 3481 Sc| 84 2562 Ur| 1126 Number of 2-station scans: 27 Number of 3-station scans: 163 Number of 4-station scans: 76 Number of 5-station scans: 51 Number of 6-station scans: 31 Number of 7-station scans: 49 Number of 8-station scans: 70 Number of 9-station scans: 141 Number of 10-station scans: 61 Number of 11-station scans: 46 Number of 12-station scans: 30 Number of 13-station scans: 0 Total # of scans, observations: 745 17267 Special Notes for this session: - IMPORTANT. In this session ALL stations will record on Mark5. The session will be correlated in 1 pass. Field system version 9.9.0 correctly prepares the snap files. If you have installed this version, please use it to make the snap files on sites. In case you do not have this version installed, I have prepared snap files for HOBART and URUMQI and placed them on CDDIS. - IMPORTANT: The synch time for the VLBA correlator using Mark5 is 25 seconds. Because of this, stations recording with Mark5 disks will start taking data 25 seconds prior to the normal scan time. They will continue to take data between scans if the there is the gap is less than 25 seconds. - Most stations participate in two initial long (5-min) scans and a final 5-min scans. - Kokee is absent until 19:45 because of the intensive. - The fluxes use our most recent models. Purpose ======= This experiment is designed to measure station displacement due to the recent earthquake in Hawaii. The NASA VLBI group submitted a special "Target of Opportunity" proposal to the NRAO which was accepted two days later. This proposal was simultaneously submitted to the IVS OPC. 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. Schedule ======== This is a new schedule generated by John Gipson using sked. SOURCE SELECTION We selected the best 70 geodetic sources. SCHEDULING ALGORITHMS This schedule also uses the "SRCEVN SQRT" mode. In the absense of any constraints, Sked will preferentially observe strong sources that have high visibility. This mode attempts to smooth out the number of observations per source. In this schedule observations involving Hobart were given preference in scheduling. Recording Mode and Frequencies: same as previous experiments ============================================================ 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 500 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 2232.99 3, 5, 7, 9 2900 A 667.01| 1540.1 B 692.89 9|1500 B 732.99 9 6 S 2262.99 11,13,15,17 2900 A 637.01| 1540.1 B 722.89 10|1500 B 762.99 10 7 S 2352.99 19,21,23,25 2900 A 547.01| 1540.1 B 812.89 13|1500 B 852.99 13 8 S 2372.99 27,29,31,33 2900 A 527.01| 1540.1 B 832.89 14|1500 B 872.99 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 2232.99 3, 5, 7, 9 2900 A 667.01| 1600 B 632.99 9 6 S 2262.99 11,13,15,17 2900 A 637.01| 1600 B 662.99 10 7 S 2352.99 19,21,23,25 2900 A 547.01| 1600 B 752.99 13 8 S 2372.99 27,29,31,33 2900 A 527.01| 1600 B 772.99 14 Urumqi Medicina, Wettzell, Matera, GGAO, TIGO VLBA | Westford, NOTO, HartRAO, Onsala 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 2232.99 3, 5, 7, 9 2900 A 667.01| 2020.0 2 212.99 9 H 6 S 2262.99 11,13,15,17 2900 A 637.01| 2020.0 2 242.99 10 H 7 S 2352.99 19,21,23,25 2900 A 547.01| 2020.0 2 332.99 13 H 8 S 2372.99 27,29,31,33 2900 A 527.01| 2020.0 2 352.99 14 H Special procedures for non-VLBA stations ======================================== SEE THE NOTE AT THE START ABOUT MARK5 recording. Special procedures for Urumqi, Medicina, Westford, Onsala, Wettzell, Tsukuba, Matera, GGAO, TIGO ===============================================K=================== These stations have Mark IV formatters. Use the procedures generated by DRUDG. Note that the patching for VC10 must be changed from L to H for this session. 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 now have barrel roll capability, so please verify that your FORM command has 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 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. Use the .snp files provided by GSFC if you don't have FS 9.9.0. 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: nov06 directory on vlbeer: nov06 directory on aspen: /home/aspen6/astronomy/nov06/QUAK06 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. Disks should be shipped to Socorro as soon after the experiment as practical.