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Oscillation properties in two sunspots and two facular regions are studiedusing Solar Dynamics Observatory (SDO) data and ground-based observations inthe SiI 10827 and HeI 10830 lines. The aim is to study different-frequencyspatial distribution characteristics above sunspots and faculae and theirdependence on magnetic-field features and to detect the oscillations that reachthe corona from the deep photosphere most effectively. We usedFast-Fourier-Transform and frequency filtration of the intensity andDoppler-velocity variations with Morlet wavelet to trace the wave propagatingfrom the photosphere to the chromosphere and corona. Spatial distribution oflow-frequency (1-2 mHz) oscillations outlines well the fan-loop structures inthe corona (the Fe IX 171 line) above sunspots and faculae. High-frequencyoscillations (5-7 mHz) are concentrated in fragments inside the photosphericumbra boundaries and close to facular-region centers. This implies that theupper parts of most coronal loops, which transfer low-frequency oscillationsfrom the photosphere, sit in the Fe IX 171 line-formation layer. We useddominant frequency vs. distance from barycenter relations to estimatemagnetic-tube inclination angle in the higher layers, which poses difficultiesfor direct magnetic-field measurements. According to our calculations, thisangle is about 40 degrees in the transition region around umbra borders. Phasevelocities measured in the coronal loops' upper parts in the Fe IX 171line-formation layer reach 100-150 km/s for sunspots and 50-100 km/s forfaculae.

Oscillations Above Sunspots and Faculae: Height Stratification and Relation to Coronal Fan Structure