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Observational facilities allow now the detection of optical and IR spectra ofyoung M- and L-dwarfs. This enables empirical comparisons with old M- and L-dwarfs, and detailed studies in comparison with synthetic spectra. Whileclassical stellar atmosphere physics seems perfectly appropriate for oldM-dwarfs, more physical and chemical processes, cloud formation in particular,needs to be modelled in the substellar regime to allow a detailed spectralinterpretation.  Not much is known so far about the details of the inset of cloud formation atthe spectral transition region between M and L dwarfs. Furthermore there isobservational evidence for diversity in the dust properties of objects havingthe same spectral type. Do we understand these differences? The question isalso how young M- and L-dwarfs need to be classified, which stellar parameterdo they have and whether degenerations in the stellar parameter space due tothe changing atmosphere physics are present, like in the L-T transition region.  The Splinter was driven by these questions which we will use to encourageinteractions between observation and theory. Given the recent advances, both inobservations and spectral modelling, an intensive discussion between observersand theoreticians will create new synergies in our field.

Observation and modelling of dusty, low gravity L, and M dwarfs