COVER INFORMATION Station: HART (Code Hh ) Experiment: Network Monitoring Experiment Exp. Code: N19K3 Schedule Version: 1.00 Processed by SCHED version: 11.50 Development version 11.5. Started Apr. 2 PI: Olga Bayandina Address: JIVE Oude Hoogeveensedijk 4 7991PD Dwingeloo The Netherlands Phone: +31-521-596508 EMAIL: bayandina@jive.eu Fax: Phone during observation: +31-521-596508 Observing mode: Notes: K-Band NME and ftp fringe test for session 3/2019 (1024 Mbps, L+R, 2-bit sampling, 16 MHz filters) Please send the disk pack by express to JIVE Please DO NOT use the phase cal signal. COVER LETTER: This is the schedule for the K-band NME and ftp fringe-test on 17 October 2019 involving antennas: Jb2, Ef, Mc, On60, T6, Ur, Tr, Ys, Hh, Sv, Zc, Bd, Sr, Mh, Kt, Ky, Ku The NME uses a standard setup with 1024 Mbps. The schedule consists of long integrations on calibrators J1751+0939, J1801+4404, and J2148+0657 for ftp-fringe tests; The following ftp-fringe tests are scheduled throughout the experiment (1024 Mbps): 12:15:00 (scan 2, 4 sec, J1751+0939) 12:45:00 (scan 4, 4 sec, J1751+0939) 13:15:00 (scan 6, 4 sec, J1751+0939) 13:45:00 (scan 8, 4 sec, J1751+0939) 14:15:00 (scan 10, 4 sec, J1801+4404) -- the source is expected to be resolved on long baselines; Zc is down for this one. 14:45:00 (scan 12, 4 sec, J2148+0657) -- check of long baseline fringes; Ef is down. Good luck with the session! Olga Bayandina Mattermost: coms.evlbi.org Schedule for HART (Code Hh ) 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 17 Oct 2019 Day 290 --- ---------- N19K3 ---------- Next scan frequencies: 22187.49 22187.49 22187.49 22187.49 22219.49 22219.49 22219.49 22219.49 22251.49 22251.49 22251.49 22251.49 22283.49 22283.49 22283.49 22283.49 Next BBC frequencies: 187.49 187.49 187.49 187.49 219.49 219.49 219.49 219.49 251.49 251.49 251.49 251.49 283.49 283.49 283.49 283.49 Next scan bandwidths: 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 12 00 00 J1751+0939 15 33 34 41.0 48.1 -2.3 0.0 0 0 12 00 00 12 04 00 =1749+096 15 37 34 41.6 47.1 -2.2 0.0 240 31 12 00 01 12 07 00 J1751+0939 15 40 35 42.1 46.3 -2.2 0.0 159 31 12 07 00 12 17 00 =1749+096 15 50 37 43.7 43.8 -2.0 0.0 600 108 12 07 01 12 20 00 J1751+0939 15 53 37 44.2 43.0 -2.0 0.0 159 108 12 20 00 12 32 00 =1749+096 16 05 39 46.0 39.6 -1.8 0.0 720 201 12 20 01 12 35 00 J1751+0939 16 08 40 46.4 38.7 -1.7 0.0 159 201 12 35 00 12 47 00 =1749+096 16 20 42 48.0 35.1 -1.5 0.0 720 294 12 35 01 12 50 00 J1751+0939 16 23 42 48.4 34.1 -1.5 0.0 159 294 12 50 00 13 02 00 =1749+096 16 35 44 49.9 30.2 -1.3 0.0 720 386 12 50 01 13 05 00 J1751+0939 16 38 44 50.2 29.1 -1.2 0.0 159 386 13 05 00 13 17 00 =1749+096 16 50 46 51.4 24.9 -1.0 0.0 720 479 13 05 01 13 20 00 J1751+0939 16 53 47 51.7 23.8 -1.0 0.0 159 479 13 20 00 13 32 00 =1749+096 17 05 49 52.7 19.2 -0.8 0.0 720 572 13 20 01 13 35 00 J1751+0939 17 08 49 52.9 18.0 -0.7 0.0 159 572 13 35 00 13 47 00 =1749+096 17 20 51 53.6 13.2 -0.5 0.0 720 665 13 35 01 13 52 00 J1801+4404 17 25 52 19.5 6.9 -0.6 0.0 204 665 13 52 00 14 02 00 =1800+440 17 35 54 19.8 5.0 -0.4 0.0 600 742 13 52 01 14 05 00 J1801+4404 17 38 54 19.8 4.4 -0.4 0.0 159 742 14 05 00 14 17 00 =1800+440 17 50 56 20.0 2.1 -0.2 0.0 720 835 14 05 01 14 20 00 J1801+4404 17 53 57 20.0 1.6 -0.1 0.0 159 835 14 20 00 14 32 00 =1800+440 18 05 59 20.0 359.3 0.1 0.0 720 927 14 20 01 14 37 00 J2148+0657 18 11 00 27.7 65.9 -3.6 0.0 160 927 14 37 00 14 47 00 =2145+067 18 21 01 29.7 64.3 -3.5 0.0 600 1005 14 37 01 Schedule for HART (Code Hh ) Page 3 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 17 Oct 2019 Day 290 --- 14 50 00 J2148+0657 18 24 02 30.3 63.8 -3.4 0.0 159 1005 14 50 00 15 02 00 =2145+067 18 36 04 32.7 61.7 -3.2 0.0 720 1098 14 50 01 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. ======== Setup file: sess319.K1024 --- 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: 7 Station: HART Total bit rate: 1024 Format: VDIF Bits per sample: 2 Sample rate: 32.000 Number of channels: 16 DBE type: DBBC_DDC Speedup factor: 1.00 Disk used to record data. 1st LO= 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 22000.00 Net SB= L L U U L L U U L L U U L L U U IF SB = U U U U U U U U U U U U U U U U Pol. = RCP LCP RCP LCP RCP LCP RCP LCP RCP LCP RCP LCP RCP LCP RCP LCP BBC = 1 9 1 9 2 10 2 10 3 11 3 11 4 12 4 12 BBC SB= L L U U L L U U L L U U L L U U IF = A1 C1 A1 C1 A1 C1 A1 C1 A1 C1 A1 C1 A1 C1 A1 C1 The following frequency sets based on these setups were used. Frequency Set: 9 Setup file default. Used with PCAL = off LO sum= 22187.49 22187.49 22187.49 22187.49 22219.49 22219.49 22219.49 22219.49 22251.49 22251.49 22251.49 22251.49 22283.49 22283.49 22283.49 22283.49 BBC fr= 187.49 187.49 187.49 187.49 219.49 219.49 219.49 219.49 251.49 251.49 251.49 251.49 283.49 283.49 283.49 283.49 Bandwd= 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 16.00 Matching frequency sets: 9 Track assignments are: track1= 1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15, 16 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 27.525083 0.00 * J1751+0939 09 39 42.82586 * 09 39 00.72841 09 38 58.84204 0.00 J1751+09 /home/guest/rmc/SCHED/sched11.5/catalogs/sources.gsfc GSFC 2016a X/S astro solution, 192391 observations. 1800+440 18 00 03.197729 * 18 01 32.314823 18 02 06.138809 0.01 * J1801+4404 44 04 18.35296 * 44 04 21.90026 44 04 43.85419 0.01 J1801+44 /home/guest/rmc/SCHED/sched11.5/catalogs/sources.gsfc GSFC 2016a X/S astro solution, 6631 observations. 2145+067 21 45 36.078473 * 21 48 05.458671 21 49 04.130820 0.26 * J2148+0657 06 43 40.90456 * 06 57 38.60416 07 03 15.90594 0.25 J2148+06 /home/guest/rmc/SCHED/sched11.5/catalogs/sources.gsfc GSFC 2016a X/S astro solution, 110505 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 sess319.K1024 1 2 3 4 5 6 7 8 9 10 14 15 1.433 185.933 J1801+4404 sess319.K1024 1 2 3 4 5 6 7 8 9 10 14 15 0.567 68.000 J2148+0657 sess319.K1024 1 2 3 4 5 6 7 8 9 10 14 15 0.367 47.200 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 68.4 J1801+4404 81.4 J2148+0657 125.7 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