Most studies rely on stacked photometry and are able to derive only average properties (e.g. Finkelstein et al. 2007, Nilsson et al. 2007, Lai et al. 2008). Furthermore until recently, most LAEs samples, lacked (deep) data in the mid-IR range which are crucial to constrain stellar mass at redshift $>$ 4, where the 4000 Å break is shifted beyond the K-band. A good coverage of the near-IR was also often missing, and this is important to reduce the model degeneracies (e.g old/dust-free vs young/dusty population). For this reason, we took a slightly different approach and decided to study the properties of Ly$\alpha$ emitting galaxies selected as LBGs. In this way, we select galaxies that are bright enough in the continuum to be detected at other wavelengths (so their SEDs can be modelled) and show Ly$\alpha$ in emission: we can then study the dependence of physical properties on the emission line strength and characteristics, on individual galaxies, rather than relying on the stacking technique. Clearly this is only possible with a survey that has both deep multi-band data on a relatively large area, as well as excellent spectroscopic coverage. The GOODS survey (e.g., Dickinson et al. 2004, Giavalisco et al. 2004) 