We present the first successful CVN (Chinese VLBI Network) phase-referencing observation of the pulsar B0329+54 on October 16, 2008 in S band. A new background source, J0347+5557, 2.5 • away from the pulsar was employed as a position reference, which is closer to the pulsar and better for the 'nodding' mode than that used in previous observations. The position by fitting image of the pulsar relative to the calibrator is accurately determined at the level of tens of μas, which is comparable with the present differential VLBI astrometric accuracy, proving that CVN will be a potential powerful tool for astrometry and astrophysics. PSR B0329+54, VLBI, CVN, phase reference PACS: 95.75Kk, 95.85Bh Proper motion and trigonometric parallax of pulsars can be obtained with Very Long Baseline Interferometry (VLBI) phase-referencing observations. These parameters through such observations can provide the only model-independent distances and velocities of pulsars and also can be exploited to address a variety of scientific questions such as making associations with Supernova Remnants, improving the accuracy of kinematic and distance information for use in timing, luminosity, and Galactic electron distribution models, making reference frame ties, pulsar auto-navigation techniques and so on [1][2][3].PSR B0329+54 with the period of 0.7 s is one of the strongest pulsars in the sky. So it has been extensively studied on the proper motion, distance and interstellar scintillation by single dish, and VLBI by many authors [4][5][6][7]. Though severely punishing observations were made at higher frequencies [5], observations of the pulsar are always set in lower frequencies (including L band) due to weak flux and its steep power-law spectra. Since 2000 January, the timing observations of PSR B0329+54 have been carried out by *Corresponding author (email: kent-gl@shao.ac.cn) using Nanshan 25-m radio telescope at the frequency of 1540 MHz with two polarizations fed to a filter-bank consisting of 2×128 contiguous channels and each of the width 2.5 MHz [8]. The timing position published by using the Nanshan data from 2000 January to 2004 August is α(J2000.0) = 03 h 32 m 59 s .391(7) and δ(J2000.0) = 54 • 34 43 .40(8) at epoch MJD 52337.0 [8]. Brisken et al. measured the parallax and proper motion of the pulsar B0329+54 using Very Long Baseline Array (VLBA). The parallax was 0.94 ± 0.11 mas and the proper motions were μ α = 17.0 ± 0.27 mas yr −1 and μ δ = −9.48 ± 0.37 mas yr −1 , respectively. Positions of the pulsar were α(J2000.0) = 03 h 32 m 59 s .3862 and δ(J2000.0) = 54 • 34 43 .5051 calibrated with J0302+5331, 4 • .37 away [5]from the pulsar. The VLBA Observations were set in L band, and antennas nodded back and forth between the pulsar and the calibrator with a cycle time of 5 min. And the 338 MHz wide band available from VLBA receivers was Nyquist sampled in eight 8 MHz spectral windows ranging from 1410 to 1730 MHz. Pulsar gating employed in the correlator is an important technique in such observations, which increases sensiti...