  In this study we combine the multiwavelength ultraviolet -- optical (Solar
Dynamics Observatory, SDO) and radio (Nobeyama Radioheliograph, NoRH)
observations to get further insight into space-frequency distribution of
oscillations at different atmospheric levels of the Sun. We processed the
observational data on NOAA 11711 active region and found oscillations
propagating from the photospheric level through the transition region upward
into the corona. The power maps of low-frequency (1--2 mHz) oscillations
reproduce well the fan-like coronal structures visible in the Fe ix 171A line.
High frequency oscillations (5--7 mHz) propagate along the vertical magnetic
field lines and concentrate inside small-scale elements in the umbra and at the
umbra-penumbra boundary. We investigated the dependence of the dominant
oscillation frequency upon the distance from the sunspot barycentre to estimate
inclination of magnetic tubes in higher levels of sunspots where it cannot be
measured directly, and found that this angle is close to 40 degrees above the
umbra boundaries in the transition region.
