4 Summary

We identified about 97 strong pulsars from the NVSS catalog and presented the flux densities at 1.4 GHz. The parameters of linear polarization are independent, but slightly different (see Eqs. (1), and (2) above), measurements from those obtained from normal pulsar observations. Interstellar scintillation both helps and hinders the detection of pulsars. Table 1 presents all known pulsars detected by the NVSS. Well-calibrated VLA measurements of the average polarization angles of 5 strong pulsars can be used for PA calibrations for pulsar observations. By comparing the pulsar positions from the pulsar catalog and those from the NVSS, we got a proper motion upper limit of PSR B0031-07.

Acknowledgements

We thank the anonymous referee for his constructive suggestions which helped to revise the paper significantly, and Drs. Dunc Lorimer, Elly Berkhuijsen, R. Wielebinski and Paul Arendt for their helpful comments. JLH is grateful for the hospitality of Prof. R. Wielebinski and Dr. R. Beck during his stay at the MPIfR, Bonn as an exchange scholar between the Chinese Academy of Sciences (CAS) and Max-Planck-Gesellschaft between 1997 May and 1998 August. He also thanks the National Natural Science Foundation of China and the Astronomical Committee of the CAS for continuous support.