I obtained my PhD degree in 2006 at National Astronomical Observatories, CAS (NAOC), and spent one year at Max-Planck Institute for Radioastronomy as a postdoc working for SKADS. Since 2007, I have been working at NAOC as a staff member until I moved to Australia in 2011.
_ Galactic interstellar medium. Our Galaxy hosts both large scale regular magnetic field and small scale turbulent field. The relativistic electrons spiralling the field generate synchrotron emission which is highly polarized. This significantly contaminates the observations of cosmic microwave background emission. The magnetized ionized gas introduces Faraday effect to polarization observations. This on one hand can be used to infer the magnetic field such as for pulsars, on the other hand smears out the polarized emission to a large extent depending on the observation wavelength. The propagation of cosmic ray particles is also influenced by the Galactic magnetic field. What is the configuration of the large-scale field? What is the fluctuation properties of the small scale field? Is it Kolmogorov-like? How it is compared to the regular field? How the field is spatially distributed? What is the scale height of the thermal gas? Is it coupled to the field? The consensus is yet to be reached for the above questions. I endeavor to embark on some aspects. _ Radio continuum survey. The continuum survey is essential to investigate the Galactic interstellar medium. The Sino-German 6 cm polarization of the Galactic plane combining the international effort is being made. I have participated in the project since 2002. Now the survey will be finished soon. Fruitful results have come out from the survey.