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Jim Lovell - 26 May 2016

Kashima 34m

  • We are working for exchanging  1.6m dish with 2.4m Cassegrain optics of MARBLE1 station at NMIJ(Tsukuba).
  • Our station is still single linear (V) polarization. Planning to enable dual (VH) polarization at Kashima 34m in near future.
  • Broadband 24h experiment has been conducted about 10 times between MBL1-MBL2-Kashima34 network. After replacement of 1.5m->2.4m dish at MBL2 station, Performance has been improved more than 4 times. Collecting are of the dish is factor 2. Efficiency was  aslo improved by modification from prime focus optics with QRFH(Rindgren) to Cassegrain focus optics with NINJA(NICT) feed. Image Removed  This is correlation amplitude between Kashima34(O)-MBL2(B) baseline for scans of 3C84 at Eleveation angle above 80 deg. Four of each symbol of the plot indicated as A, B, C, D are frequency band from lower side, though they are not constant for all the sessions. Center frequency of the frequency array were [3.7, 5.3, 10.1, and 13.3GHz] for 26th Jan., [5.9, 7.1, 8.7, and 10.6GHz] from 12th Feb. to 25th Nov., and [3.8, 5.9, 8.7, and 10.6GHz] for 9th Dec.
  • We are going to replace the dish and feed at MBL1 too in March.Broadband observation sessions conducted in 2016 were performed with 2048Msps-1bit-4ch mode. Frequency array was:
       
    Lower_edge　(　Center　Freq)=
    3188MHz(3700),　4788MHz(5300),　9588MHz(10100),　12788MHz(13300)
    5388MHz(5900),　6588MHz(7100),　8188MHz(8700),　10088MHz(10600)
    3288MHz(3800),　5388MHz(5900),　8188MHz(8700),　10088MHz(10600)

  • If any station can do broadband fringe test observation (1GHz bandwidth for single channel), we are pleased to be a counterpart of the experiment. We will make correlation and provide the results. Frequency array can be arranged  flexibly.

Mamoru Sekido - 26 Jan23 Mar. 2017

Yebes

 We are taking part in the biweekly 24 hour VGOS tests. For those observations we use 4 RDBE-G units, 500 MHz bandwidth each band and polarization. We do not plan to make any hardware update in the near term. Our next mid-term goal is installing a combination of filters that will filter out frequencies below 3 GHz but will allow the passage of the legacy S band. That should allow us to install two amplifiers per polarization and not saturate the optical fiber amplifiers.

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 G. Tuccari - 26 May 2016

 

We are working for exchanging 1.6m dish with 2.4m dish of MARBLE1 station at NMIJ(Tsukuba).