COVER INFORMATION Station: CAMBG32M (Code Cm ) Experiment: Network Monitoring Experiment Exp. Code: N22C3 Schedule Version: 2.00 Processed by SCHED version: 11.60 Release 11.6; April 2020 PI: Gabor Orosz Address: JIVE Oude Hoogeveensedijk 4 Dwingeloo Netherlands Phone: +31 686337748 EMAIL: orosz@jive.eu Fax: Phone during observation: +31 521 596 530 Observing mode: vlbi Notes: C-band (6cm) NME and ftp fringe test for Session 3, 2022. EVN: 4 Gbps, 16 IFs, 32 MHz filters, L+R, 2-bit sampling MER: 512Mbps/2IF/64MHz, UR: 2Gbps/8IF/32MHz, W1: 1 Gbps/4IFs/32MHz COVER LETTER: This is the schedule for the 6cm NME and ftp fringe test on October 20, 2022 involving 13 EVN antennas + eMERLIN: Jb2, Wb, Ef, Mc, Nt, O8, T6, Ur, Tr, Ys, Hh, Ir, Km + Cm, Da, Kn, Pi, De. The NME uses a setup with a datarate of 4 Gbps, exc. MER(0.5G), UR(2G), Wb(1G). The NME lasts for 3 hours and consists of long scans on calibrators: J1751+0939 and J2031+1219. with ftp grabs every other scan at the following times (in UT): 12:10:00 (scan 2, 2 sec, J1751+0939) 12:40:00 (scan 4, 2 sec, J1751+0939) 13:10:00 (scan 6, 2 sec, J1751+0939) 13:40:00 (scan 8, 2 sec, J2031+1219) 14:10:00 (scan 10, 2 sec, J2031+1219) 14:40:00 (scan 12, 2 sec, J2031+1219) 14:59:00 (scan 14, 2 sec, J2031+1219) -- Gabor Orosz Mattermost: coms.evlbi.org Schedule for CAMBG32M (Code Cm ) Page 2 Network Monitoring Experiment UP: D => Below limits; H => Below horizon mask; W => still slewing at end; blank => Up. Early: Seconds between end of slew and start. Dwell: On source seconds. Disk: GBytes recorded to this point. TPStart: Recording start time. Frequencies are LO sum (band edge). SYNC: Time correlator is expected to sync up. ---------------------------------------------------------------------------------------- Start UT Source Start / Stop Early Disk TPStart Stop UT LST EL AZ HA UP ParA Dwell GBytes SYNC ---------------------------------------------------------------------------------------- --- Thu 20 Oct 2022 Day 293 --- Next scan frequencies: 4888.00 4888.00 Next BBC frequencies: 736.00 736.00 Next scan bandwidths: 64.00 64.00 12 00 00 J1751+0939 13 55 53 26.2 469.3 -3.9 -36.0 0 0 12 00 00 12 02 00 =1749+096 13 57 53 26.5 469.7 -3.9 -35.8 120 8 12 00 01 12 07 00 J1751+0939 14 02 54 27.3 470.8 -3.8 -35.6 295 8 12 07 00 12 12 00 =1749+096 14 07 55 28.0 472.0 -3.7 -35.2 300 27 12 07 01 12 17 00 J1751+0939 14 12 55 28.7 473.1 -3.7 -34.9 295 27 12 17 00 12 27 00 =1749+096 14 22 57 30.1 475.5 -3.5 -34.2 600 66 12 17 01 12 32 00 J1751+0939 14 27 58 30.8 476.7 -3.4 -33.8 295 66 12 32 00 12 42 00 =1749+096 14 37 59 32.1 479.1 -3.2 -32.9 600 104 12 32 01 12 47 00 J1751+0939 14 43 00 32.8 480.3 -3.2 -32.5 295 104 12 47 00 12 57 00 =1749+096 14 53 02 34.1 482.8 -3.0 -31.5 600 143 12 47 01 13 02 00 J1751+0939 14 58 03 34.7 484.1 -2.9 -31.0 295 143 13 02 00 13 12 00 =1749+096 15 08 04 36.0 486.7 -2.7 -29.9 600 182 13 02 01 13 17 00 J2031+1219 15 13 05 15.9 450.1 -5.3 -38.9 216 182 13 17 00 13 27 00 =2029+121 15 23 07 17.4 452.1 -5.2 -38.9 600 220 13 17 01 13 32 00 J2031+1219 15 28 08 18.2 453.1 -5.1 -38.8 295 220 13 32 00 13 42 00 =2029+121 15 38 09 19.7 455.2 -4.9 -38.7 600 259 13 32 01 13 47 00 J2031+1219 15 43 10 20.5 456.2 -4.8 -38.6 295 259 13 47 00 13 57 00 =2029+121 15 53 12 22.0 458.2 -4.7 -38.4 600 298 13 47 01 14 02 00 J2031+1219 15 58 13 22.8 459.3 -4.6 -38.3 295 298 14 02 00 14 12 00 =2029+121 16 08 14 24.3 461.4 -4.4 -38.0 600 336 14 02 01 14 17 00 J2031+1219 16 13 15 25.1 462.4 -4.3 -37.8 295 336 14 17 00 14 27 00 =2029+121 16 23 17 26.5 464.6 -4.2 -37.4 600 375 14 17 01 14 32 00 J2031+1219 16 28 18 27.3 465.7 -4.1 -37.2 295 375 14 32 00 14 42 00 =2029+121 16 38 19 28.8 467.9 -3.9 -36.7 600 414 14 32 01 14 47 00 J2031+1219 16 43 20 29.5 469.0 -3.8 -36.4 295 414 14 47 00 14 52 00 =2029+121 16 48 21 30.2 470.2 -3.7 -36.1 300 433 14 47 01 14 57 00 J2031+1219 16 53 22 30.9 471.3 -3.7 -35.8 295 433 14 57 00 15 00 00 =2029+121 16 56 22 31.4 472.0 -3.6 -35.6 180 444 14 57 01 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. ======== Setup file: sess322.C4096 --- WARNING --- This group does not match an entry in the frequency catalog. This might be ok because the catalog is not complete. But be very careful to be sure that the setup is correct. Setup group: 14 Station: CAMBG32M Total bit rate: 512 Format: VDIF Bits per sample: 2 Sample rate:128.000 Number of channels: 2 DBE type: Speedup factor: 1.00 Disk used to record data. 1st LO= 5624.00 5624.00 Net SB= U U IF SB = L L Pol. = RCP LCP BBC = 1 9 BBC SB= L L IF = A1 B1 The following frequency sets based on these setups were used. Frequency Set: 14 Setup file default. Used with PCAL = off LO sum= 4888.00 4888.00 BBC fr= 736.00 736.00 Bandwd= 64.00 64.00 Matching frequency sets: 14 15 16 17 18 19 Track assignments are: track1= 1, 2 barrel=roll_off POSITIONS OF SOURCES USED IN RECORDING SCANS Source Source position (RA/Dec) Error (B1950) (J2000) (Date) (mas) 1749+096 17 49 10.387931 * 17 51 32.818574 17 52 36.341459 0.10 * J1751+0939 09 39 42.82585 * 09 39 00.72840 09 38 48.01981 0.10 From catalog imbedded in main SCHED input file. rfc_2022c Petrov and Kovalev, in preparation 274714 observations 2029+121 20 29 32.681262 * 20 31 54.994269 20 32 59.248030 0.10 * J2031+1219 12 09 28.75294 * 12 19 41.34010 12 24 25.90342 0.10 From catalog imbedded in main SCHED input file. rfc_2022c Petrov and Kovalev, in preparation 9885 observations SOURCE SCAN SUMMARY FOR SOURCES LISTED ABOVE Scan hours are for recording scans only. Baseline hours are only counted for scans above horizon at both ends. Source Setup file Frequency sets Observing hours (duplicates not shown) Scan Baseline J1751+0939 sess322.C4096 1 2 3 4 5 6 7 8 9 11 13 14 0.783 133.950 J2031+1219 sess322.C4096 1 2 3 4 5 6 7 8 9 11 13 14 1.133 193.800 EFFECT OF SOLAR CORONA 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) J1751+0939 65.8 J2031+1219 104.8 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