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Jim Lovell - 26 May 2016

Kashima 34m

  • We are working for exchanging  replaced 1.6m dish with 2.4m Cassegrain optics of MARBLE1 station at NMIJ(Tsukuba) in March. Now we have two 2.4m dish at NICT(Koganei in Tokyo) and NMIJ( Tsukuba)

     

     
    Marble1
    (Tsukuba)    		Marble2
    (Koganei)
    Image AddedImage Added
     

     

  • 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 - 23 Mar26 Apr. 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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