Greenland Telescope: Single-Dish Science, Instrumentation Requirements Nimesh a Patel Satoki Matsushita Center for Astrophysics | Harvard & Smithsonian ASIAA
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Greenland Telescope: Single-dish science, instrumentation requirements Nimesh A Patel Satoki Matsushita Center for Astrophysics | Harvard & Smithsonian ASIAA Nimesh Patel October 2018, Thule AFB 23 May 2019, EAO Futures meeting, Nanjing !1 Outline: • Current status • Single dish science goals • Summit Station • Future receivers development Nimesh Patel October 2018, Thule AFB 23 May 2019, EAO Futures meeting, Nanjing !2 Completion of mechanical assembly of the Greenland Telescope 10 August 2017 !3 Thule Phase 1 Activities 2017-2019 • Antenna assembly (mechanical + electrical) completed at Thule Air Base, Greenland - September 2017 • Hydrogen maser installed in September 2017 • Servo tuning and tests in progress - October 2017 • Fringes demonstrated at Maunakea, with SMA + JCMT, using 230 GHz receivers and VLBI backend • 86 & 230 GHz receivers installed in late November 2017 • Pointing calibration in November 2017 • Joined the EHT run in April 2018 October 2017 First fringes on ALMA-Thule baseline, 28 January 2018 Mk4/DiFX fourfit 3.19 rev 2292 3C279.0166CV, 028-0843_b4, AG ALMA - THULE, fgroup B, pol XL Fringe quality 9 SNR 10.8 Int time 239.889 Amp 0.136 Phase 134.4 PFD 1.6e-17 Delays (us) SBD -0.000661 MBD 0.006959 Fringe rate (Hz) -0.000040 Ion TEC 0.000 Ref freq (MHz) 228221.3906 AP (sec) 0.205 Exp. e18j28 Exper # 3635 Yr:day 2018:028 Start 084300.00 Stop 084700.03 FRT 084500.00 Corr/FF/build 2018:079:230135 2018:080:102304 2018:080:065037 RA & Dec (J2000) 12h56m11.1666s Amp. and Phase vs. time for each freq., 7 segs, 195 APs / seg (39.94 sec / seg.), time ticks 60 sec -5˚47’21.525" U Validity !5 L A G 228221.39228279.98228338.58228397.17228455.77228514.36228572.95228631.55228690.14228748.73228807.33228865.92228924.52228983.11229041.70229100.30229158.89229217.48229276.08229334.67229393.27229451.86229510.45229569.05229627.64229686.23229744.83229803.42229862.02229920.61229979.20Freq (MHz) All 59.5 129.3 52.2 113.7 178.3 155.5 156.7 85.4 164.5 145.9 133.9 159.8 148.7 109.4 122.6 152.2 162.2 151.0 -158.7 162.0 135.5 126.4 134.4 137.8 123.9 133.3 116.4 98.1 139.7 52.7 95.7 Phase 134.4 0.3 0.1 0.1 0.1 0.2 0.2 0.1 0.1 0.2 0.2 0.1 0.2 0.2 0.2 0.1 0.2 0.2 0.2 0.1 0.2 0.2 0.1 0.1 0.2 0.3 0.1 0.2 0.2 0.2 0.0 0.1 Ampl. 0.1 893.0 527.3 478.9 415.5 53.8 781.4 278.3 111.5 309.4 497.0 894.5 735.7 128.2 348.1 773.5 690.3 568.2 808.7 449.6 86.1 322.2 383.1 703.2 250.8 464.5 300.5 713.9 458.8 777.4 896.6 477.0 Sbd box 464.8 U/L 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 1172/0 APs used A 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 PC freqs G 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 PC freqs A:G 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 PC phase A:G 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 0:0 Manl PC A 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 PC amp G 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 1000 B00UX B01UX B02UX B03UX B04UX B05UX B06UX B07UX B08UX B09UX B10UX B11UX B12UX B13UX B14UX B15UX B16UX B17UX B18UX B19UX B20UX B21UX B22UX B23UX B24UX B25UX B26UX B27UX B28UX B29UX B30UX Chan ids A Tracks B00UL B01UL B02UL B03UL B04UL B05UL B06UL B07UL B08UL B09UL B10UL B11UL B12UL B13UL B14UL B15UL B16UL B17UL B18UL B19UL B20UL B21UL B22UL B23UL B24UL B25UL B26UL B27UL B28UL B29UL B30UL Chan ids G Tracks Group delay (usec)(model) 1.53950718118E+04 Apriori delay (usec) 1.53950648530E+04 Resid mbdelay (usec) 6.95887E-03 +/- 2.8E-05 Sband delay (usec) 1.53950641917E+04 Apriori clock (usec) -2.1089119E+03 Resid sbdelay (usec) -6.61241E-04 +/- 8.8E-04 Phase delay (usec) 1.53950648546E+04 Apriori clockrate (us/s) -6.6459997E-06 Resid phdelay (usec) 1.63576E-06 +/- 1.3E-07 Delay rate (us/s) 5.37017872807E-02 Apriori rate (us/s) 5.37017874558E-02 Resid rate (us/s) -1.75172E-10 +/- 9.3E-10 Total phase (deg) 317.6 Apriori accel (us/s/s) -7.73193107321E-05 Resid phase (deg) 134.4 +/- 10.6 RMS Theor. Amplitude 0.136 +/- 0.013 Pcal mode: MANUAL, MANUAL PC period (AP’s) 5, 5 ph/seg (deg) 15.5 14.0 Search (4096X128) 0.136 Pcal rate: 0.000E+00, 0.000E+00 (us/s) sb window (us) -2.000 2.000 amp/seg (%) 14.8 24.4 Interp. 0.000 Bits/sample: 2x2 SampCntNorm: disabled mb window (us) -0.009 0.009 ph/frq (deg) 35.9 29.5 Inc. seg. avg. 0.137 Sample rate(MSamp/s): 116 dr window (ns/s) -0.011 0.011 amp/frq (%) 43.9 51.4 Inc. frq. avg. 0.140 Data rate(Mb/s): 7192 nlags: 464 t_cohere infinite ion window (TEC) 0.00 0.00 A: az 13.2 el 72.4 pa -167.9 G: az 175.1 el 7.5 pa -1.5 u,v (fr/asec) -1044.494 -30143.124 simultaneous interpolator Control file: cf_3601 Input file: /data-sc05/mike/e18j28/3635/028-0843_b4/AG..0166CV Output file: /data-sc05/mike/e18j28/3635/028-0843_b4/AG.B.1.0166CV EHT observing run April 2018 Keiichi Asada (ASIAA) Hiroaki Nishioka (ASIAA) ChenYu Yu (ASIAA) Nimesh Patel (CfA) !6 31 March - 9 April 2019, Global Millimeter-wave VLBI Array observations at 86 GHz !7 Hydrogen maser house Control room, weather station !8 Current Instrumentation !9 Johnson Han (ASIAA) 2SB !10 !11 Johnson Han (ASIAA) !12 Two ROACH2 spectrometers, each with two IF inputs of 2.048 GHz b/w, 32768 channels CASPER ROACH2, dual 5 Gsps ADCs, Octal 10 Gbps Ethernet !13 Summit Station !14 Thule Air Base Position: 76.5° North, 68.7° West Altitude: 77 m Temperature: 5 C to – 25 C (average) Summit Station Position: 72.5° North, 38.5° West Altitude: 3,200 m Temperature: - 10 C to - 50 C (average) !15 View from level-2 platform Beginning of Ice sheet (traverse) !16 Publications of the Astronomical Society of the Pacific, 129:025001 (11pp), 2017 February Matsushita et al. Publications of the Astronomical Society of the Pacific, 129:025001 (11pp), 2017 February Matsushita et al. Publications of the Astronomical Society of the Pacific, 129:025001 (11pp), 2017 February doi:10.1088/1538-3873/129/972/025001 © 2016. The Astronomical Society of the Pacific. All rights reserved. Printed in the U.S.A. 3.5 Year Monitoring of 225GHz Opacity at the Summit of Greenland Satoki Matsushita1, Keiichi Asada1, Pierre L. Martin-Cocher1, Ming-Tang Chen1, Paul T. P. Ho1, Makoto Inoue1, Patrick M. Koch1, Scott N. Paine2, and David D. Turner3 1 Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan, Republic of China 2 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-78, Cambridge, MA 02138, USA 3 Global Systems Division, Earth System Research Laboratory, National Oceanic and Atmospheric Administration, 325 Broadway, Boulder, CO, 80305, USA Figure 2. Time variationReceived 2016 plot September of 19; 225 accepted GHz 2016 opacity October 28; at published the summit 2016 December of 21 Greenland ice sheet. The measurement has been startedAbstract from 2011 August 17, which is Figure 3. Monthly quartile variation of 225 GHz opacity. Solid, dashed, and deWefined present as the the 3.5 day years 1monitoring in this results diagram. of 225 GHz opacity at the summit of the Greenland ice sheet (Greenland dotted lines are 25%, 50%, and 75% quartiles, respectively. The first and the Summit Camp) at an altitude of 3200 m using a tipping radiometer. We chose this site as our submillimeter telescope last months of this measurement, namely 2011 August and 2015 February, (Greenland Telescope) site, because conditions are expected to have low submillimeter opacity and because its fi location offers favorable baselines to existing submillimeter telescopes for global-scale Very Long Baseline have fewer data than the other months, so that the statistical signi cance is low.