RV134 (Astrometric/Geodetic VLBA-134) 2019 APR297 17:00 DOY 119 Notes prepared by David Gordon, Ed Himwich and John Gipson NVI/GSFC Special notes for this experiment ================================= This session will use the RDBE/DDC/Mark5C system at the VLBA sites, as in previous RV sessions. The X-band frequencies are: 8365.75, 8445.75, 8805.75, and 8925.75 MHz, and spans 560 MHz. We are trying a slighly different set of S-band frequencies to avoid RFI in the third S-band channel (2352.75). The S-band frequencies for this session will be: 2232.75, 2262.75, 2372.75 and 2392.75 MHz. The ending in .75 MHz is necessary at the VLBA stations. Therefore it will not be possible to monitor phase cals using the 10 kHz filters. This session will record 8 8-MHz bandwidth channels using 2-bit sampling, as in previous RDV's. The bit rate will be 256 Mbits/sec. The data will be correlated at the VLBA using the VLBA DiFX software correlator. There are 4 non-VLBA stations scheduled - HARTRAO, NYALES20, ONSALA60 and WETTZELL. These stations should see the "Special operations notes for non-VLBA stations" section below for special instructions. The SC-VLBA antenna will not observe due to repairs in progress. To facilitate fringe-finding, there are some long scans on fairly strong sources with most antennas at the beginning and near the end of the schedule. All stations please try to be onsource and recording data for these scans. These scans are: Source Start DURATIONS name yyddd-hhmmss Br Fd Hh Hn Kp La Mk Nl Ny On Ov Pt Wz 0133+476 19119-170000| 300 329 300 321 316 336 311 372 372 325 318 332| 0458-020 19119-170729| 453 351 446 454 454 452 427 454 454| 2000+472 19120-164152| 300 319 326 321 316 325 300 334 326 300 318 334| 0458-020 19120-164915| 341 374 343 340 332 354 341 374| We are again using the new 'Fill' scheduling option. 'Fill' is run after a schedule is finished in the normal manner. It increases the scan times at stations, when possible, based on how much idle time each station has before its next scan. We used a 'FILL_OFF' margin of 5 seconds. Using 'Fill' on the original schedule the average observing time increased from 46% to 62%, and the average idle time decreased from 25% to 10%. The observing time increases most at the faster antennas and least at the slower antennas. Purpose ======= This is the second of six coordinated astrometric/geodetic sessions in 2019 that use the full 10-station VLBA plus several geodetic stations capable of recording VLBA modes. This year's series is a continuation of the highly successful RDV series begun in 1997. These are now being run under the USNO's VLBA time allocation. The RV sessions are now being run on Mondays, concurrently with the R1 sessions for comparison purposes. These experiments are being coordinated by the geodetic/astrometric VLBI programs of 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 and Bordeaux Observatory will perform 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 and USNO will analyze this data to determine and maintain high accuracy terrestrial reference and celestial reference frames. 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. This data will also produce highly accurate Earth orientation results and possibly the best nutation results ever produced. NASA and NRAO will use these sessions to provide a service to users who require high quality positions for a small number of sources. While the quality of these results will be high, the observing and data reduction overhead required will be minimal because a small number of 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 ~60 sources from the pool of geodetic, astrometric, and monitoring sources. About 20-30 of these will remain the same from experiment to experiment and will be chosen to optimize the goals of the three groups. A number of poorly observed and/or new requested sources will also be included to obtain or improve their positions. Schedule information ==================== This is a new schedule generated by David Gordon at GSFC using sked. Schedule file name: rv134.skd At the IVS Data Center (ftp://cddisa.gsfc.nasa.gov/vlbi/ivsdata/aux/2019/rv134): Sked file: rv134.skd Text file: rv134.txt At the NRAO/VLBA: VLBA Pointing files: rv134crd.br rv134crd.fd rv134crd.hn rv134crd.kp rv134crd.la rv134crd.mk rv134crd.nl rv134crd.ov rv134crd.pt Summary file: rv134.sksum Sked file: rv134.skd Text file: rv134.txt Vex file: rv134.vex This experiment uses 9 of the VLBA stations and 4 IVS stations. The IVS stations are: HARTRAO, NYALES20, ONSALA60 and WETTZELL. Below is the sked summary. Key: Br=BR-VLBA Fd=FD-VLBA Hh=HARTRAO Hn=HN-VLBA Kp=KP-VLBA La=LA-VLBA Mk=MK-VLBA Nl=NL-VLBA Ny=NYALES20 On=ONSALA60 Ov=OV-VLBA Pt=PIETOWN Wz=WETTZELL Br Fd Hh Hn Kp La Mk Nl Ny On Ov Pt Wz Avg % obs. time: 61 62 36 59 63 61 62 61 71 72 63 62 71 62 % cal. time: 4 4 1 4 4 4 3 4 4 3 4 4 3 4 % slew time: 28 29 23 30 28 29 19 30 18 19 27 29 10 25 % idle time: 6 4 39 6 4 4 15 4 7 5 5 4 15 10 total # scans: 348 346 115 353 341 351 279 359 303 265 329 347 280 308 # scans/hour : 15 14 5 15 14 15 12 15 13 11 14 14 12 13 # OF OBSERVATIONS BY BASELINE | Br Fd Hh Hn Kp La Mk Nl Ny On Ov Pt Wz Total --------------------------------------------------------------------------- Br| 320 40 320 322 328 269 328 241 185 317 325 202 3197 Fd| 55 330 329 343 252 338 230 194 309 342 205 3247 Hh| 66 41 57 0 65 79 97 20 52 97 669 Hn| 315 335 245 348 245 199 299 329 215 3246 Kp| 330 261 326 223 186 317 332 199 3181 La| 255 346 235 198 312 345 210 3294 Mk| 253 180 134 272 257 144 2522 Nl| 246 204 307 340 219 3320 Ny| 238 216 231 241 2605 On| 167 194 239 2235 Ov| 314 183 3033 Pt| 207 3268 Wz| 2361 Number of 2-station scans: 0 Number of 3-station scans: 38 Number of 4-station scans: 42 Number of 5-station scans: 11 Number of 6-station scans: 7 Number of 7-station scans: 12 Number of 8-station scans: 21 Number of 9-station scans: 78 Number of 10-station scans: 55 Number of 11-station scans: 63 Number of 12-station scans: 120 Number of 13-station scans: 0 Total number of scans: 447 Total number of obs: 18089 INTENSIVE BREAKS ================ There is an IVS INT01 Intensive session scheduled during RV134. Wettzell will drop out from ~18:15 - 19:45 on DOY 119 for this Intensive. There will also be a USNO/NRAO UT1 Intensive session, scheduled to start at ~06:30 UTC (+/- 4 hrs) on DOY 008, using Pietown and MK-VLBA, so these stations will drop out for about 100 minutes. The exact time is not fixed, so it is not scheduled in, but the loss of these two antennas for a short period should have only a minimal effect. SOURCE SELECTION ================ There are a total of 77 sources in this session, though not all were scheduled. Among them, 60 are from the geodetic source list, and 17 are sources with few or no previous observions in IVS sessions. SCHEDULING ALGORITHMS ===================== This schedule uses the "SRCEVN SQRT" mode of Sked. In the absence 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. RECORDING MODE and FREQUENCIES ============================== The data will be recorded using the following setup: 8 channels 1:2 fan-out 16 MHz sample rate 2-bit sampling This recording mode is designated 256-8(RDV). There is no correlator speed-up factor. The frequency sequence covers 560 MHz at X-band and 160 MHz at S-band using 4 channels in each band. At the VLBA, the X-band uses two LO's in order to fit into the VLBA 512 MHz passband. At the Mark4 stations, the X-band uses both the high and low parts of the geodetic receivers. Because only 8 channels are available when observing with the VLBA/RDBE/DDC systems, a wider spanned bandwidth is not advisable. The following tables list the setup for the VLBA stations and the geodetic stations with DBBC, Mark IV, Mark 5, and VLBA5 back ends. VLBA | HARTRAO Chan Sky Tracks LO IF BBC | LO IF BBC BBC# 1 X 8365.75 2, 4, 6, 8 7600 B 765.75| 8080.0 A1 285.75 3 2 X 8445.75 10,12,14,16 7600 B 845.75| 8080.0 A1 365.75 4 3 X 8805.75 18,20,22,24 9600 D 794.25| 8080.0 B2 725.75 5 4 X 8925.75 26,28,30,32 9600 D 674.25| 8080.0 B2 845.75 6 5 S 2232.75 3, 5, 7, 9 3100 A 867.25| 2020.0 C1 212.75 9 6 S 2262.75 11,13,15,17 3100 A 837.25| 2020.0 C1 242.75 10 7 S 2372.75 19,21,23,25 3100 A 727.25| 2020.0 C1 352.75 13 8 S 2392.75 27,29,31,33 3100 A 707.25| 2020.0 C1 372.75 14 VLBA | NYALES20 Chan Sky Tracks LO IF BBC | LO IF BBC BBC# 1 X 8365.75 2, 4, 6, 8 7600 B 765.75| 8080.0 1N 285.75 3 2 X 8445.75 10,12,14,16 7600 B 845.75| 8080.0 1N 365.75 4 3 X 8805.75 18,20,22,24 9600 D 794.25| 8580.1 3N 225.65 5 4 X 8925.75 26,28,30,32 9600 D 674.25| 8580.1 3N 345.65 6 5 S 2232.75 3, 5, 7, 9 3100 A 867.25| 2020.0 2N 212.75 9 6 S 2262.75 11,13,15,17 3100 A 837.25| 2020.0 2N 242.75 10 7 S 2372.75 19,21,23,25 3100 A 727.25| 2020.0 2N 352.75 13 8 S 2392.75 27,29,31,33 3100 A 707.25| 2020.0 2N 372.75 14 VLBA | ONSALA60, WETTZELL Chan Sky Tracks LO IF BBC | LO IF BBC BBC# 1 X 8365.75 2, 4, 6, 8 7600 B 765.75| 8080.0 A1 285.75 3 2 X 8445.75 10,12,14,16 7600 B 845.75| 8080.0 A1 365.75 4 3 X 8805.75 18,20,22,24 9600 D 794.25| 8080.0 B1 725.75 5 4 X 8925.75 26,28,30,32 9600 D 674.25| 8080.0 B1 845.75 6 5 S 2232.75 3, 5, 7, 9 3100 A 867.25| 2020.0 C1 212.75 9 6 S 2262.75 11,13,15,17 3100 A 837.25| 2020.0 C1 242.75 10 7 S 2372.75 19,21,23,25 3100 A 727.25| 2020.0 D1 352.75 13 8 S 2392.75 27,29,31,33 3100 A 707.25| 2020.0 D1 372.75 14 Special operations for non-VLBA stations: ========================================= All non-VLBA stations: Please note that due to the frequency sequence, phase-cal will not be visible with a 10 kHz viewing filter in the USB channels. If you have another means to verify phase-cal, please use it. If you have a Mark IV Decoder, please contact Ed.Himwich@nasa.gov if you would like advice on how to set it up to check phase-cal for this frequency sequence. HARTRAO: This station uses a DBBC rack. Please use the procedures generated by DRUDG. BBCs 3 & 4 are used at X-band with IF A, input 1. BBCs 5 & 6 are used at X-band with IF B, input 2. BBCs 9, 10, 13 & 14 are used for S-band with IF C, input 1. NYALES20 and WETTZELL: These stations have Mark IV or Mark 5 racks. Please use the procedures generated by DRUDG. VCs 3 & 4 are used at X-band with IF 1. VCs 5 & 6 are used at X-band with IF 3. VCs 9, 10, 13 & 14 are used at S-band with IF 2. ONSALA60: This station uses a DBBC rack. Please use the procedures generated by DRUDG. BBCs 3 & 4 are used at X-band with IF A, input 1. BBCs 5 & 6 are used at X-band with IF B, input 1. BBCs 9 & 10 are used for S-band with IF C, input 1. BBCs 13 & 14 are used at S-band with IF D, input 1. The IF3 command in the procedure IFDSX assumes that VC3 and VC10 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. The standard wiring is described in "help=if3". If you have questions about the wiring, please contact Brian Corey at Haystack. If you wish to record back-up channels, please add appropriate valo=..., va=... vblo=... and vb=... commands in the VCSX8 procedure. 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 the last RV session. Check out parity check procedures. 2. Make the .snp file with DRUDG. 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. 7. Transfer your log file to your normal IVS data center. The directories for the IVS servers are listed below: ftp cddisin.gsfc.nasa.gov/ivsincoming ftp ivsopar.obspm.fr/ivsincoming ftp ivs.bkg.bund.de/ivsincoming Correlation =========== This experiment will be correlated at the NRAO/VLBA on the VLBA DiFX software correlator. Most of the Mark4 stations are now E-transfering their data to Haystack, where it will be copied and shipped to the VLBA in Socorro, New Mexico. These stations will need to coordinate this with Haystack Observatory (contact: Jason SooHoo at jsoohoo@haystack.mit.edu). The VLBA needs to process the session at their correlator as soon as possible because of limited media. So please try to set up the E-transfer as soon as possible after the session ends. If you need to ship the media instead, please ship it to Socorro as soon after the experiment as is practical. It should be shipped to the following address: Socorro address for media shipping: VLBA Array Operations Center National Radio Astronomy Observatory Attn: Juan Cordova 1003 Lopezville Road Socorro, NM 87801 U.S.A. Phone: 575-835-7000 Shipping and VLBA contact information is also given at: https://science.nrao.edu/facilities/vlba/contact/shipping_information. Please use one of the recommended shipping companies (FedEx, UPS, DHL, TNT). Please ship your media to the VLBA the same day the session ends or the next business day (just like the R1/R4 media is shipped). If you know that there is going to be a problem sending your media to the VLBA the same day the session ends or the next business day, please let us (David.Gordon-1@nasa.gov) know as soon as possible so that we, along with the VLBA, can determine the best course of action. If you have any questions or comments, please let us know.