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VERA project

VERA project. H.Kobayashi NAOJ,VERA project VLBA 10 th Anniversary Conference (Socorro, June 12, 2003). Project members. 13 scientists (NAOJ, Kagoshima Univ.)

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VERA project

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  1. VERAproject H.Kobayashi NAOJ,VERA project VLBA 10th Anniversary Conference (Socorro, June 12, 2003)

  2. Project members • 13 scientists (NAOJ, Kagoshima Univ.) • H.Kobayashi, S.Manabe, N.Kawaguchi, T.Omodaka, K.Shibata, O.Kameya, Y.Tamura, M.Honma, K.Hirota, Y.Kanya, T.Jike, H. Ishituka, M.Rijoha • 7 technicians • T.Miyaji, K.Horiai, S.Kuji, K.Iwadate, K.Satou, H.Sakai, T.Bushimata • 8 graduate students • T.Oyama, T.Kurayama, R.Kamohara, H.Suda, S.Sakakibara, K.Nakashima, R.Shimizu, Y.Che

  3. Scientific goal • Astrometry with 10μarcsec. accuracy between background object and galactic object within 2.2 degree separation • Proper motion and parallax measurements • 3D map and velocity field of the Galaxy • Detailed 3D velocity structure of molecular gas around evolved stars and star forming regions • Phase referencing to improve sensitivity with long integration

  4. Expected distance accuracy of VERA Sun 10% error at the G.C 20% error at opposite side

  5. Array configuration

  6. Specifications • Antenna diameter ; 20m • Observing bands ; 2GHz, 8GHz, 22GHz、43GHz • Tape recording rate ; 1Gbps • 2 beam system for phase referencing • Path error between 2 beam; 100μm

  7. Antenna（Mizusawa station)

  8. Construction of the antenna • Panel adjustment • Surface accuracy • 0.15mm rms • Panel; 0.1 mm rms • Panel adjustment; 0.1 mm rms • Sub ref.: 0.03mm rms

  9. Cooled HEMT receiver Trx = 60 K @ 22GHz  40K@22GHz Trx=130K ＠43GHz  70K@43GHz Discrete HEMT  MMIC HEMT

  10. Receiver platform for 2 beam

  11. Antenna upper cabin

  12. Radiator on the antenna surface • Noise source on the dish • Symmetric distribution of 4 noise sources • Instrumental phase error is estimated by the average of 4.

  13. Antenna（Mizusawa station)

  14. Instrumentalphase correction • Phase difference of surface radiator between 2 beams • Less than 1degreemeasurement accuracy is achieved 2B phase response from surface radiator depend on beam separation

  15. First phase variations between 2 beams Fringe phase of W49N,OH43 and difference Allan variance of them

  16. Coherence improvement Coherence drop of 1B and 2B fringe Fringe detection with 20 min. integration, GRB030329

  17. Digital backend • 2.4Gbps transmit for each beam • Digital filter is used for frequency selection

  18. Spiral array feed for ＳＸ

  19. Fringe detection by SX mode Nov. 19th, 2002 between VERA mizusawa- Gifu

  20. Geodesy observations • Combine with the world coordinate by SX observations • Combined with Tsukuba 32m of Japanese GSI • Baseline determination • Required accuracy2mm • 22GHz wideband observations • SX conventional observations

  21. VERA first fringe on Feb. 20th, 2002 Orion-KL H2O maser

  22. １Ｇｂｐｓ recorder & correlation • SONYDIR20001024Mbps • 80 min/tape • Mitaka FX correlator • 5 station correlation with 1Gbps • Output to CODA system • Convert correlation data to FITS

  23. First 1Gbps fringe among VERA 4 stations, Sep. 18th, 2002 IrーIs OgーIs Mz-Is Mz-Ir

  24. Test observations • Phase referencing check • 22GHz • SgrB2-SgrA*, W51N, W49N, Orion-KL, W3OH • VX-Sgr, VY-CMa, etc • 43GHz • Orion-KL • Fringe check and calibrators • Strong H2O masers (>20Jy), • Calibrator candidates

  25. Antenna（Mizusawa station)

  26. Improvement of sensitivity ２２ＧＨｚ

  27. Improvement of sensitivity 43ＧＨｚ

  28. Expected sensitivity 1 * Measured value

  29. Expected Sensitivity 2

  30. VERA Mizusawa met a strong earthquake (Sanriku-minami jishin) Vertical 0.2G, Horizontal 0.3G

  31. Plan of VERA 2002：　Fringedetection / 2B fringe test 2003: Feasibility check of 2B interferometer Test observations for astrometry 2004: Test observations for astrometry Improvement of system sensitivity 2005: Complete

  32. VERA & KVN Network Mizusawa KVN VERA Iriki Ogasawara Ishigakijima

  33. 16 VLBI stations in east Asia Under operation Under construction

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