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Collaboration

Single-dish Test Observations of the KVN Yonsei telescope at 22/43 GHz - Performance of KVN Yonsei telescope at 22/43GHz Sang-Sung Lee March 18, 2009 2009 East Asia VLBI Workshop. Collaboration. Do-Young Byun – Field System management Do-Heung Je – Receiver System management

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Collaboration

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  1. Single-dish Test Observations of the KVN Yonsei telescope at 22/43 GHz - Performance of KVN Yonsei telescope at 22/43GHz Sang-Sung Lee March 18, 2009 2009 East Asia VLBI Workshop

  2. Collaboration • Do-Young Byun – Field System management • Do-Heung Je – Receiver System management • Seog-Tae Han – Quasi Optics management • Tomoharu Kurayama – DAS management • Se-Jin Oh – DAS and Clock System management • Kee-Tae Kim, Bong Won Sohn – Observation plan • Advisors: Hyunsoo Chung, Se-Hyung Cho, Duk-Gyoo Roh, Chang Hoon Lee, Bong Gyu Kim

  3. Outline • Introduction • Test observations of KVN • Goals of single-dish test observations • Observations and results • System setup • First light and Simultaneous observations • Pointing model at 22GHz • Beam alignment measurements • Aperture Efficiencies • Discussion • Outlook

  4. Introduction • Test observations of KVN in 2007-2009 • 100-GHz Acceptance observations (K. T. Kim’s talk) • Single-dish test observations at 22/43GHz (This talk) • VLBI test observations btw KVN-VERA (B. W. Sohn’s talk) • Goals of single-dish test observations • Performance test of KVN telescopes at 22, 43, 86 and 129GHz • Pointing model • Aperture efficiencies • Feasibility test of multi-frequency simultaneous observations • Beam alignment measurements (S. T. Han’s talk) • Instrumental phase stability measurements (D. H. Je’s poster)

  5. 100 MHz 1.4 GHz H-maser GPS 10 MHz 10 MHz Distributor 5 MHz 1 pps ClockSystem 100 MHz Distributor 10 MHz Distributor 1 pps Distributor 1 pps Distributor Control PC GUI System setup Receiver system DAS Clock Field system DigitalE/O Digital O/E Digital Filters Digital Spectro-meter Down Converter Sampler 22 GHz FE Down Converter Sampler WDM Optical MUX WDM Optical DMUX Down Converter Sampler 43 GHz FE Mark5B Down Converter Sampler DIR-1000 Receiver Cabin Observation Building

  6. First lights of KVN Yonsei telescope First light from H2O masers in W49N at 22GHz on Aug. 30 2008 Digital spectrometer with wideband mode BW = 512MHz

  7. First lights of KVN Yonsei telescope First light from SiO masers in Orion KL at 43GHz on Aug. 31 2008 Digital spectrometer with narrow band mode 1 BW = 256MHz

  8. Simultaneous observations at 22/43 GHzof KVN Yonsei telescope Simultaneous observations at 22/43GHz for thermal emission (Venus) on Oct. 6 2008 Two power-streams at 22 and 43 GHz while OTF scanning Venus

  9. Simultaneous observations at 22/43 GHzof KVN Yonsei telescope Simultaneous observations at 22/43GHz for maser emission (Orion KL) on Oct. 8 2008

  10. Pointing model at 22 GHz Six maser sources : W49N, OrionKL, VY CMa, WB755, W3OH, Cep A Observations on Sep. 10-17 2008 RMS error of the pointing model : 4” in AZ, 5” in EL

  11. 22/43GHz beam alignment measurements • Goals: 7" of beam offsets btw 22/43GHz • 10% of FWHM (70") at 129GHz • Beam alignment measurements @ K/Q bands • Beam offset from 1st measurement (Jupiter): • (∆AZ, ΔEL)=(1.6", 22") @ 30° in EL • No dependency on EL (found by observing Orion KL with FIVE Points) • Adjusting Rx-direction by 2 degrees on the Rx plate • Beam offset from 2nd measurement (Jupiter): • (ΔAZ, ΔEL)=(1.6", -2.9") @ 30° in EL • Within pointing accuracy of 5" and our goal of 7 " • Beam offsets from 3rd measurement (Orion KL): • at various ELs of 14 ° ~ 47 ° • with the optimized sub-reflector model • (<ΔAZ>, <ΔEL>)=(4.2", -0.6")

  12. Beam offsets from • 3rd measurement (Orion KL): • H2O masers (at 22 GHz) and SiO maser (at 43GHz) • at various ELs of 14 ° ~ 47 ° and various AZs of 90 ° ~ 210 ° • with the optimized sub-reflector model • (<ΔAZ>, <ΔEL>)=(4.2", -0.6")

  13. Aperture efficiencies * : Page et al. 2003 ApJS 148, 39** : Butler et al. 2001 Icarus 154, 226*** : Greve et al. 1994 A&A 286, 654 Sub-reflector was optimized in position.Aperture efficiencies are values of single measurements.

  14. Discussion and Outlook • Discussion • Why is the beam offsets btw K/Q dependant in AZ of observations? • Position difference of H2O and SiO masers in Orion KL? • (05 35 14.1 -05 22 37.5) , (05 35 14.5 -05 22 30.5) • System deformation in AZ but not in EL? • Uncertainty of position of Orion KL?

  15. Discussion and Outlook • Outlook • Receivers at 22/43GHz taken down after the observations. • 100-GHz acceptance tests done for KVN YS. • Receivers at 22/43GHz set up again on Feb. 2009 need to confirm the results from the previous observations Beam alignment test for planet revisited (S. T. Han’s talk) Beam alignment test for Orion KL to be revisited Double check of pointing model to be done • Polarization characteristic should be measured • Gain curve measurements • After confirming all the characteristics, we will start single-dish observations of KVN Yonsei.

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