COVER INFORMATION Station: DARNHALL (Code Da ) Experiment: Network Monitoring Experiment Exp. Code: N24C3 Schedule Version: 1.00 Processed by SCHED version: 11.60 Release 11.6; Feburary 2020 PI: Benito Marcote Address: JIVE Oude Hoogeveensedijk 4 Dwingeloo Netherlands Phone: +31 521 596 508 EMAIL: marcote@jive.eu Fax: Phone during observation: +31 521 596 508 Observing mode: vlbi Notes: C-band (6cm) NME and ftp fringe test for Session 3, 2024. EVN: 4 Gbps, 16 IFs, 32 MHz filters, L+R, 2-bit sampling MER: 512Mbps/2IF/64MHz, UR: 2Gbps/8IF/32MHz, W1: 1 Gbps/4IF/32MHz Please DO NOT use the phase cal signal. COVER LETTER: This is the schedule for the 6cm NME and ftp fringe test on 25 October 2024 involving 11 EVN antennas + eMERLIN: Jb2, Wb, Ef, O8, T6, Ur, Tr, Ys, Hh, Ir, Sr, Cm, Da, Kn, Pi, De. The NME uses a standard setup with a datarate of 4 Gbps, with eMERLIN at 0.5 Gbps, Ur at 2 Gbps, and Wb at 1 Gbps. 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, J2031+1219) 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) Good luck with the session! Benito Marcote 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 ---------------------------------------------------------------------------------------- --- Fri 25 Oct 2024 Day 299 --- 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 14 07 20 27.5 112.3 -3.8 -34.2 0 0 12 00 00 12 02 00 =1749+096 14 09 20 27.8 112.8 -3.7 -34.1 120 8 12 00 01 12 07 00 J1751+0939 14 14 21 28.5 113.9 -3.6 -33.8 294 8 12 07 00 12 12 00 =1749+096 14 19 22 29.1 115.1 -3.6 -33.4 300 27 12 07 01 12 17 00 J1751+0939 14 24 23 29.8 116.3 -3.5 -33.0 294 27 12 17 00 12 27 00 =1749+096 14 34 24 31.2 118.7 -3.3 -32.2 600 66 12 17 01 12 32 00 J1751+0939 14 39 25 31.8 119.9 -3.2 -31.8 294 66 12 32 00 12 42 00 =1749+096 14 49 27 33.1 122.4 -3.1 -30.9 600 104 12 32 01 12 47 00 J2031+1219 14 54 28 13.1 86.7 -5.6 -37.8 168 104 12 47 00 12 57 00 =2029+121 15 04 29 14.6 88.7 -5.5 -37.9 600 143 12 47 01 13 02 00 J2031+1219 15 09 30 15.3 89.7 -5.4 -37.9 294 143 13 02 00 13 12 00 =2029+121 15 19 32 16.9 91.7 -5.2 -37.9 600 182 13 02 01 13 17 00 J2031+1219 15 24 33 17.6 92.7 -5.1 -37.8 294 182 13 17 00 13 27 00 =2029+121 15 34 34 19.1 94.7 -5.0 -37.7 600 220 13 17 01 13 32 00 J2031+1219 15 39 35 19.9 95.8 -4.9 -37.7 294 220 13 32 00 13 42 00 =2029+121 15 49 37 21.3 97.9 -4.7 -37.5 600 259 13 32 01 13 47 00 J2031+1219 15 54 37 22.1 98.9 -4.6 -37.3 294 259 13 47 00 13 57 00 =2029+121 16 04 39 23.6 101.0 -4.5 -37.1 600 298 13 47 01 14 02 00 J2031+1219 16 09 40 24.3 102.1 -4.4 -36.9 294 298 14 02 00 14 12 00 =2029+121 16 19 42 25.8 104.2 -4.2 -36.5 600 336 14 02 01 14 17 00 J2031+1219 16 24 42 26.5 105.3 -4.1 -36.3 294 336 14 17 00 14 27 00 =2029+121 16 34 44 27.9 107.6 -4.0 -35.8 600 375 14 17 01 14 32 00 J2031+1219 16 39 45 28.6 108.7 -3.9 -35.6 294 375 14 32 00 14 42 00 =2029+121 16 49 46 30.1 111.0 -3.7 -35.0 600 414 14 32 01 14 47 00 J2031+1219 16 54 47 30.8 112.2 -3.6 -34.7 294 414 14 47 00 14 52 00 =2029+121 16 59 48 31.5 113.3 -3.6 -34.3 300 433 14 47 01 14 57 00 J2031+1219 17 04 49 32.1 114.5 -3.5 -34.0 294 433 14 57 00 15 00 00 =2029+121 17 07 49 32.6 115.3 -3.4 -33.7 180 444 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: sess324.C4096 Matching groups in /Users/hawky/.pysched/catalogs/freq_RDBE.dat: da6cm_g Generated from sess320C4G.setini Setup group: 13 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: 12 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: 12 13 14 15 16 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 10.387930 * 17 51 32.818574 17 52 42.554513 0.00 * J1751+0939 09 39 42.82586 * 09 39 00.72841 09 38 43.72523 0.00 J1751+09 /Users/hawky/.pysched/catalogs/sources.gsfc GSFC 2016a X/S astro solution, 192391 observations. 2029+121 20 29 32.681260 * 20 31 54.994267 20 33 05.414525 0.01 * J2031+1219 12 09 28.75299 * 12 19 41.34015 12 24 51.31940 0.02 J2031+12 /Users/hawky/.pysched/catalogs/sources.gsfc GSFC 2016a X/S astro solution, 4314 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 sess324.C4096 1 2 3 4 5 6 7 9 10 11 12 0.450 54.000 J2031+1219 sess324.C4096 1 2 3 4 5 6 7 9 10 11 12 1.467 176.000 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 61.4 J2031+1219 100.1 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