1. Chinese VLBA Programs and Chinese VLBI Network 2011.01.27 Xiaoyu HONG Shanghai Astronomical Observatory ， CAS (xhong@shao.ac.cn)

2. SHAO ： D. R. Jiang ， Z. Q. Shen, A. Tao, Y. Liu, X. Chen, Y. J. Chen, W. Zhao B. Zhang, W. H. Wang, X. Hong et al. PMO: Y. Xu, et al. NJU: X. W. Zheng, et al. NAOC: H. Y. Zhang, C. J. Jin, R. D. Nan, B. Peng et al. XJAO （ Urumq ） : X. Liu et al. … VLBA USERS in China

3. Sgr* A Helical jet in AGNs Radio jet of AGNs with gamma ray emission Studies of red supergiant SiO masers et al.

4. (Shen et al.. 2005, Nature) Z. Q. Shen, K. Y. Lo, M. C. Liang, P. T. P. Ho, J. H. Zhao.

5. A kinematic study of the compact jet in quasar B3 1633+382 Y. Liu, D. R. Jiang, Z.-Q. Shen & M. Karouzos 2010 A&A FS QSO EGRET source z=1.814 OVV 14 epochs of VLBI observations of B3 1633+382 at 22 GHz with the VLBA two different possibilities of component classification two corresponding kinematical models are adopted to explain the tracks of the three components. One is a linear motion, while another is a helical model.

6. VLBA Monitoring of 1633+382 during a Major Millimeter-Flare Y. Liu, T. P. Krichbaum, J. A. Zensus & D. R. Jiang in preparation 1633+382: OVV, z=1.814, core dominated gamma-ray bright AGN major mm flare 2001-2003. 3C345: QSO, z=0.593, well known for its helical motion. 1749+096: BL Lac, z=0.322, also very active QSO, and a very compact mm-source. VLBA monitoring 22 & 37 GHz H.Teräsranta 90, 150 & 230GHz H. Ungerechts

7. Color: Fractional Polarization Left contour: total intensity Right contour: linear intensity Transverse Fractional Polarization (TFP): low in jet spine, high at edges Interpretation in helical magnetic fields: TFP: low in spine, high at edges (Lyutikov et al. 2005); Signature of bifurcation of EVPA at low and top Interpretation in magnetic compression and shear: Bottom and top EVPA: approximately parallel; Undetectable linear polarization in the middle (cancellation of emission from surface and deep magnetic) Multiwaveband VLBA polarimetric observations of NRAO530 Chen, Shen, Feng, 2010,MNRAS

8. 3 VSOP images for high-z GPS OQ172 z=3.522 Multifrequency VLBA Polarimetry of GPS Quasar OQ172 A High-z Laboratory for Studies of the Circumnuclear Environment Y. Liu, D. R. Jiang, L. Gurvits & A. B. Fletcher in preparation High-z GPS (FFA/SSA) the jet suffers a large band at ～ 3 mas the most compact region in the 4 mas map was resolved into two components extremely high rest-frame RM (RM>20,000 rad m -2 ) very steep RM gradient (at 7 mas, RM<100 rad m -2 ) Hβ FWHM 3,700 kms -1 3x10 8 M ⊙ [O III] FWHM 2,200 kms -1 What is the GPS absorption mechanism? (FFA or SSA) Why is the jet strongly bent and curved, and how do physical properties vary along its length? Which is the core? What is the magnetic field topology? And why is the RM extremely high, and the inner jet depolarized? 0642+449 z=3.396 0201+113 z=3.639 multiband VLBA polarimetry observation

9. — VX Sgr ； 3-epoch VLBA data at 1999 1999 Apr. 241999 May. 231999 Apr. 31 Chen, Shen & Xu 2007, ChJAA The estimated distance of 1.57± 0.27 kpc to VX Sgr from the “statistical parallax” analysis to proper motions of SiO masers. Our observations provide the first direct evidence for an inward motion of SiO-maser shell around a red supergiant. Chen, Shen, Imai & Kamohara 2006, ApJ Φ=0.75-0.80 V infall =4.1 km/s Proper motion Studies of red supergiant SiO masers with the VLBA

10. — AH Sco; 2-epoch VLBA data Chen & Shen 2008, ApJ 2004 Mar. 82004 Mar. 20 Proper motion Model fitting: Studies of red supergiant SiO masers with the VLBA Best-fit model for the SiO maser kinematics in AH Sco V 1 =-14 km s -1 and α~0.5 support the presence of a real inward flow in the SiO maser region around AH Sco under the gravitation of the central star. The estimated distance d=2.26 kpc from the model fitting is in a good agreement with its near kinematic distance of about 2.0 kpc.

11. EPOCH 1 EPOCH 2 EPOCH 3 EPOCH 4 EPOCH 5 06,Jul 06,Dec 07,Aug 08,Feb 08,Aug 5 epochs VLBA Observations of SiO Masers around VX Sgr (Su et al. 2011, JAA, in press) VX Sgr: v=1 J=1-0, v=2 J=1-0

13. 4 epochs at 15, 43, and 86GHz Helical jet structure driven by K-H instability : multiple jet bendings in 1156+295 on pc--kpc scales, derived from VLBA observations

14. 1229-021 VLA, VLBA images Hong et al. in preparation

15. Knotty radio jet of 3C48 revealed by the VLBA – indicative of jet-NIR clouds interactions – good case for studying AGN evolution and feedback Nucleus Hot spot Wilkinson et al. 1984; Feng et al. 2004; Worrall et al. 2005; An et al. 2010

16. Major Facilities for RA in China Delingha 13.7m 21CMA L,C,S/X,K S/X L,C(5/6G),S/X,K S/X L,C,S/X:2012 Ku,K,Ka:Q:2015 L,C,S/X:2012 Ku,K,Ka:Q:2015 L,C:2012 K :? L,C:2012 K :? Black:recent status Yellow:plan L,C,X:2014 VLBI in China

17. Sheshan and Urumq are the full members if EVN and IVS

18. CVN --VLBI data processing center Hardware correlator (5 stations)‏ Software correlator (10 stations)‏ Output data: CE-1 format FITS format Software for CE-1 data processing (near real time eVLBI, in 5 min.)‏

19. Digital BBC for 4 stations 4 Processing Boards One for data Selecting 4 Ifs input, 2GHz total BW 16 Ch output / VSI-H 2 VSI-H interface 1 / 2 / 4 bit output Dual redundant system

20. VLBI tracking for Chang’E 1 &2 CE-1 CE -2

21. 1 ）、 VLBI 测站 2 ）、数据传输网络 3 ）、 VLBI 中心 Beijing center VLBI center Network 34 Mbps stations USB data VLBI data in 5 m SH BJ KM UR How VLBI work together with USB?

22. VLBI tracking for Chinese Lunar Project VLBI plays important role for Chinese Lunar project. VLBI is famous to people in China this moment. 2007.12 for CE-1 2010.12 for CE-2

23. e-VLBI 2007 August 28: Shanghai –Australia & Europe (256Mbps) 2008 June 17: Shanghai –Australia & Japan (512Mbps) 2009 January 6: Shanghai-Urumqi (256Mbps) 2009 January 15-16: IYA marathon obs. (Asia, Australia, Europe, America) 2009 February - : Shanghai 25-m participates in the routine eEVN sessions 23

24. CVN (Km+My+Sh+Ur) + Onsala 20-m + Medicina 32-m; 2009 Aug 5-6; 24 hr; X-band; 5 GPS sources JIVE Correlator 0129+560 CVN (An et al. 2010, in prep) 24

25. Shanghai 65m Radio Telescope 65-m in diameter fully steerable radio telescope Active surface system Cover 1.4 – 46 GHz with 8 bands ： –L(1.6GHz) –S/X(2.3/8.4GHz) –C(5GHz) –Ku(15GHz) –K(22GHz) –Ka(30GHz) –Q(43GHz) General-purpose (radio astronomy, geodynamics, single-dish, VLBI, VLBI tracking for Chinese Lunar projects ) 25

26. 2008 ： funded, contract to CETC54 for the antenna construction 2009: complete design, start manufacturing 2010: ground breaking, foundation completed 2011: antenna completed 2012: L/S/C/X band test observations, ready for participation in the Chinese Lunar Mission 2013-14: active surface tested, Ku/K/Ka/Q band test observations 2015: project accomplished, in full operation Project Timeline 26

27. Some photos of the site

28. 天线基础桩基验收准备

32. Active system parts

33. Structure of the antenna CETC54

34. 三、滚轮、齿轮等部件

35. Thank you! By the end of 2012