COVER INFORMATION Station: GBT_VLBA (Code Gb ) Experiment: Fine-scale imaging of M87 Exp. Code: gs042 Schedule Version: 1.00 Processed by SCHED version: 11.40 Release 11.4. March 14, 2015 PI: Tuomas Savolainen Address: Aalto University Metsahovi Radio Observatory Metsahovintie 114, 02540 Kylmala, Finland Phone: +358505819717 EMAIL: tuomas.k.savolainen@aalto.fi Fax: Phone during observation: +358505819717 Observing mode: K-band dual-pol Notes: K-band, Radioastron-compatible frequency setup P-CAL is ON Tsys is ON auto-level (AGC) is ON Schedule for GBT_VLBA (Code Gb ) Page 2 Fine-scale imaging of M87 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 ---------------------------------------------------------------------------------------- --- Mon 14 May 2018 Day 134 --- ---------- This is an 10-min pointing & focus scan for GBT ---------- Next scan frequencies: 22236.00 22236.00 22236.00 22236.00 Next BBC frequencies: 800.00 800.00 800.00 800.00 Next scan bandwidths: 16.00 16.00 16.00 16.00 20 15 00 1156+295 06 25 44 22.2 69.7 -5.6 -57.2 0 0 Stopped 20 25 00 --- 06 35 45 24.1 70.9 -5.4 -58.0 600 0 ---------- K-band VLBI scans. Ground segment 04: ---------- 20 26 20 1228+126 06 37 06 8.6 81.1 -5.9 -52.4 2 0 20 26 20 20 35 30 --- 06 46 17 10.4 82.5 -5.8 -52.6 550 18 20 26 21 20 36 50 1156+295 06 47 37 26.3 72.4 -5.2 -58.8 1 18 20 36 50 20 40 30 --- 06 51 18 27.0 72.9 -5.2 -59.0 220 25 20 36 51 20 41 50 1228+126 06 52 38 11.7 83.5 -5.7 -52.8 3 25 20 41 50 20 50 30 --- 07 01 20 13.3 84.8 -5.5 -53.0 520 42 20 41 51 20 51 50 1226+023 07 02 40 7.6 93.6 -5.5 -51.5 34 42 20 51 50 20 55 30 --- 07 06 20 8.3 94.1 -5.4 -51.4 220 49 20 51 51 20 56 50 1228+126 07 07 41 14.6 85.7 -5.4 -53.1 34 49 20 56 50 21 05 30 --- 07 16 22 16.3 87.1 -5.3 -53.2 520 65 20 56 51 21 12 00 1228+126 07 22 53 17.6 88.1 -5.1 -53.2 368 65 21 12 00 21 20 30 --- 07 31 24 19.2 89.4 -5.0 -53.3 510 82 21 12 01 21 21 10 1228+126 07 32 05 19.4 89.5 -5.0 -53.3 19 82 21 21 10 21 30 00 --- 07 40 56 21.1 90.8 -4.8 -53.3 530 99 21 21 11 ---------- This is an 8-min pointing & focus scan for EFLSBERG&GBT ---------- 21 31 00 1236+077 07 41 56 16.6 93.8 -5.0 -52.0 19 99 Stopped 21 39 00 --- 07 49 58 18.2 95.0 -4.8 -51.9 480 99 ---------- K-band VLBI scans. Space segment 04: 1228+126 ---------- 21 40 00 1228+126 07 50 58 23.1 92.4 -4.7 -53.2 18 99 21 40 00 21 56 40 --- 08 07 40 26.3 95.1 -4.4 -53.0 1000 131 21 40 01 21 57 20 1228+126 08 08 21 26.5 95.2 -4.4 -53.0 19 131 21 57 20 22 13 20 --- 08 24 23 29.6 97.9 -4.1 -52.6 960 162 21 57 21 Schedule for GBT_VLBA (Code Gb ) Page 3 Fine-scale imaging of M87 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 ---------------------------------------------------------------------------------------- --- Mon 14 May 2018 Day 134 --- 22 14 00 1228+126 08 25 03 29.7 98.0 -4.1 -52.5 19 162 22 14 00 22 30 00 --- 08 41 06 32.8 100.8 -3.8 -51.9 960 193 22 14 01 22 31 20 1253-055 08 42 26 16.4 111.7 -4.2 -47.0 -1 193 22 31 21 22 33 20 --- 08 44 26 16.7 112.0 -4.2 -46.9 119 197 22 31 21 22 35 00 1156+295 08 46 07 49.0 88.0 -3.2 -63.7 -34 197 22 35 34 22 37 00 --- 08 48 07 49.4 88.3 -3.2 -63.7 86 200 22 35 01 22 38 40 1228+126 08 49 47 34.5 102.4 -3.7 -51.5 24 200 22 38 40 22 42 40 --- 08 53 48 35.2 103.2 -3.6 -51.3 240 207 22 38 41 22 43 30 1228+126 08 54 38 35.4 103.3 -3.6 -51.3 29 207 22 43 30 22 52 00 --- 09 03 10 37.0 104.9 -3.5 -50.8 510 224 22 43 31 22 52 40 1228+126 09 03 50 37.1 105.1 -3.5 -50.7 19 224 22 52 40 22 56 40 --- 09 07 50 37.9 105.9 -3.4 -50.5 240 231 22 52 41 22 57 30 1228+126 09 08 40 38.1 106.0 -3.4 -50.4 29 231 22 57 30 23 10 00 --- 09 21 12 40.4 108.6 -3.2 -49.5 750 256 22 57 31 SETUP FILE INFORMATION: NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings. ======== Setup file: ra1cm2.set Matching groups in ./gs042_freq.dat: gbt1cm_a4 LO1=28.868, LO2=16.532, LO3=10.5 Setup group: 3 Station: GBT_VLBA Total bit rate: 256 Format: VDIF Bits per sample: 2 Sample rate: 32.000 Number of channels: 4 DBE type: RDBE_DDC Speedup factor: 1.00 Disk used to record data. 1st LO= 23036.00 23036.00 23036.00 23036.00 Net SB= L L U U IF SB = L L L L Pol. = RCP LCP RCP LCP BBC = 1 2 3 4 BBC SB= U U L L IF = B D B D The following frequency sets based on these setups were used. Frequency Set: 23 Setup file default. Used with PCAL = 1MHz LO sum= 22236.00 22236.00 22236.00 22236.00 BBC fr= 800.00 800.00 800.00 800.00 Bandwd= 16.00 16.00 16.00 16.00 VLBA legacy crd files using 4 channels based on RDBE channels: 1 2 3 4 CRD fr= 799.99 799.99 800.01 800.01 CRD bw= 16.00 16.00 16.00 16.00 Matching frequency sets: 23 Track assignments are: track1= 1, 2, 3, 4 barrel=roll_off POSITIONS OF SOURCES USED IN RECORDING SCANS Source Source position (RA/Dec) Error (B1950) (J2000) (Date) (mas) * FAKERA 11 57 21.769299 * 12 00 00.000000 12 00 58.985352 0.00 85 16 41.77889 * 85 00 00.00000 84 54 13.48772 0.00 From catalog imbedded in main SCHED input file. fake circumpolar target for a TS to look at J1239+0730 12 36 52.308755 * 12 39 24.588327 12 40 20.487542 0.10 * 1236+077 07 46 45.39997 * 07 30 17.18902 07 24 18.52672 0.11 J1239+07 From catalog imbedded in main SCHED input file. rfc_2012b Petrov, 2012, unpublished 1855 observations * 1226+023 12 26 33.245835 * 12 29 06.699731 12 30 03.025117 0.00 J1229+0203 02 19 43.30547 * 02 03 08.59797 01 57 05.87367 0.00 3C273B ./gs042_sources.radioastron 3C273 AGN, rfc_2013d Petrov, 2013, unpublished 32011 observations, RA-AO4-07, RA-AO3-0 * 1253-055 12 53 35.831289 * 12 56 11.166557 12 57 08.371431 0.00 J1256-0547 -05 31 07.99603 *-05 47 21.52489 -05 53 17.34581 0.00 3C279 ./gs042_sources.radioastron AGN, rfc_2013d Petrov, 2013, unpublished 7924 observations, RA-AO4-07, RA-AO3-04 * 1228+126 12 28 17.569280 * 12 30 49.423382 12 31 45.092957 0.00 J1230+1223 12 40 01.74883 * 12 23 28.04365 12 17 28.41095 0.00 3C274 ./gs042_sources.radioastron M87 AGN, rfc_2013d Petrov, 2013, unpublished 55201 observations, RA-AO3-04, RA-AO3-0 VIR-A * 1156+295 11 56 57.786212 * 11 59 31.833913 12 00 28.033628 0.00 J1159+2914 29 31 25.73868 * 29 14 43.82678 29 08 45.29167 0.00 ./gs042_sources.radioastron AGN, MASIV, rfc_2013d Petrov, 2013, unpublished 70591 observations, RA-AO3-04, R 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 FAKERA ra1cm2.set 9 2.783 0.000 1236+077 ra1cm2.set 1 2 3 6 7 8 11 13 14 15 16 + 0.347 16.742 1226+023 ra1cm2.set 1 2 3 6 7 8 11 13 14 15 16 + 0.667 51.411 1253-055 ra1cm2.set 1 2 3 6 7 8 11 13 14 15 16 + 0.597 42.278 1228+126 ra1cm2.set 1 2 3 6 7 8 11 13 14 15 16 + 8.722 862.110 ra7mm2.set 30 31 32 0.350 15.750 1156+295 ra1cm2.set 1 2 3 6 7 8 11 13 14 15 16 + 0.617 51.640 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) FAKERA 74.5 1236+077 131.5 1226+023 132.1 1253-055 141.6 1228+126 127.0 1156+295 111.1 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