COVER INFORMATION Station: DARNHALL (Code Da ) 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 DARNHALL (Code Da ) 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 45 35 24.4 107.4 -4.1 -35.5 0 0 12 00 00 12 02 00 =1749+096 13 47 35 24.7 107.9 -4.1 -35.4 120 8 12 00 01 12 07 00 J1751+0939 13 52 36 25.4 109.0 -4.0 -35.1 294 8 12 07 00 12 12 00 =1749+096 13 57 37 26.2 110.1 -3.9 -34.8 300 27 12 07 01 12 17 00 J1751+0939 14 02 38 26.9 111.3 -3.8 -34.5 294 27 12 17 00 12 27 00 =1749+096 14 12 40 28.2 113.6 -3.7 -33.9 600 66 12 17 01 12 32 00 J1751+0939 14 17 40 28.9 114.7 -3.6 -33.5 294 66 12 32 00 12 42 00 =1749+096 14 27 42 30.3 117.1 -3.4 -32.8 600 104 12 32 01 12 47 00 J1751+0939 14 32 43 31.0 118.3 -3.3 -32.4 294 104 12 47 00 12 57 00 =1749+096 14 42 44 32.3 120.8 -3.2 -31.5 600 143 12 47 01 13 02 00 J1751+0939 14 47 45 32.9 122.0 -3.1 -31.0 294 143 13 02 00 13 12 00 =1749+096 14 57 47 34.2 124.6 -2.9 -30.0 600 182 13 02 01 13 17 00 J2031+1219 15 02 48 14.4 88.4 -5.5 -37.9 167 182 13 17 00 13 27 00 =2029+121 15 12 49 15.9 90.4 -5.3 -37.9 600 220 13 17 01 13 32 00 J2031+1219 15 17 50 16.6 91.4 -5.3 -37.9 294 220 13 32 00 13 42 00 =2029+121 15 27 52 18.1 93.4 -5.1 -37.8 600 259 13 32 01 13 47 00 J2031+1219 15 32 53 18.9 94.4 -5.0 -37.7 294 259 13 47 00 13 57 00 =2029+121 15 42 54 20.4 96.5 -4.8 -37.6 600 298 13 47 01 14 02 00 J2031+1219 15 47 55 21.1 97.5 -4.8 -37.5 294 298 14 02 00 14 12 00 =2029+121 15 57 57 22.6 99.6 -4.6 -37.3 600 336 14 02 01 14 17 00 J2031+1219 16 02 58 23.3 100.7 -4.5 -37.1 294 336 14 17 00 14 27 00 =2029+121 16 12 59 24.8 102.8 -4.3 -36.8 600 375 14 17 01 14 32 00 J2031+1219 16 18 00 25.5 103.9 -4.2 -36.6 294 375 14 32 00 14 42 00 =2029+121 16 28 02 27.0 106.1 -4.1 -36.1 600 414 14 32 01 14 47 00 J2031+1219 16 33 03 27.7 107.2 -4.0 -35.9 294 414 14 47 00 14 52 00 =2029+121 16 38 03 28.4 108.3 -3.9 -35.6 300 433 14 47 01 14 57 00 J2031+1219 16 43 04 29.1 109.5 -3.8 -35.4 294 433 14 57 00 15 00 00 =2029+121 16 46 05 29.6 110.2 -3.8 -35.2 180 444 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: 15 Station: DARNHALL 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