by the code by examining simple properties of our sample of detected WLFs. The aim of the second goal is to show that the code returns data product suitable for a further investigation of the physics of WLFs.

In a future we believe that the systematic research of WLFs from synoptic instruments such as SDO/HMI may answer questions regarding the WLF’s morphology, which was studied only scarcely. For instance, some recent studies indicate that there might be two classes of WLFs, “type I” (the brightest events showing increase in contrast towards blue end of the spectrum) and “type II” (with flatter spectra, kernels appear often as faint and diffuse wave-like features). claimed that these two types must have a different origin of heating, e.g. the observable properties of type II WLFs are not consistent with the heating flux coming down from the corona, but are rather consistent with a local heating in the lower atmospheric layers [e.g. @1999ApJ...512..454D; @2001ChJAA...1..176C]. A large catalogue of WLFs from synoptic instruments is a necessary starting point for such studies.

Data
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The routine availability of synoptic solar observations by Solar Dynamics Observatory (SDO), especially from Helioseismic and Magnetic Imager [HMI; @2012SoPh..275..229S] in the range 