Fig. 10.

Upper panels: LAEV physical properties with respect to the environment in the VANDELS fields. The LAEVs located in the identified overdensities and with EW(Lyα) > 20 Å are shown as red stars, the ones with EW(Lyα) < 20 Å are shown as green stars, the ones located in transition regions are shown as cyan circles and in the field as black circles. Dashed lines indicate the median values of sSFR, stellar mass, and EW(Lyα) = 20 Å of the entire LAEV sample. The physical properties we investigate are sSFR versus EW(Lyα) (upper left), stellar mass versus EW(Lyα) (upper right), dust reddening, Av, versus rest-frame optical magnitude (lower left), rest-frame NIR magnitude versus rest-frame UV magnitude (lower right). The squares with error bars represent the typical parameter uncertainties coming from the SED fitting (see the upcoming work on SED fitting parameters). Lower panels: median physical properties of the LAEVs and of all the galaxies in the input catalog located in overdensities (red symbols) and in the field (black symbols). The medians are presented as diamonds for all the galaxies in the input catalog and stars for the LAEVs. The error bars on the medians correspond to the uncertainties due to SED fitting. The physical properties we investigate are sSFR versus stellar mass (upper left), stellar mass versus distance to the highest-density peak (upper right) of the identified overdensities, dust reddening, Av, versus rest-frame optical magnitude (lower left), rest-frame NIR magnitude versus rest-frame UV magnitude (lower right).
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