Physical properties of Lyman-alpha emitters at $z\sim 0.3$ from
  UV-to-FIR measurements
  The analysis of the physical properties of low-redshift Ly$\alpha$ emitters
(LAEs) can provide clues in the study of their high-redshift analogues. At $z
\sim 0.3$, LAEs are bright enough to be detected over almost the entire
electromagnetic spectrum and it is possible to carry out a more precise and
complete study than at higher redshifts. In this study, we examine the UV and
IR emission, dust attenuation, SFR and morphology of a sample of 23
GALEX-discovered star-forming (SF) LAEs at $z \sim 0.3$ with direct UV (GALEX),
optical (ACS) and FIR (PACS and MIPS) data. Using the same UV and IR limiting
luminosities, we find that LAEs at $z\sim 0.3$ tend to be less dusty, have
slightly higher total SFRs, have bluer UV continuum slopes, and are much
smaller than other galaxies that do not exhibit Ly$\alpha$ emission in their
spectrum (non-LAEs). These results suggest that at $z \sim 0.3$ Ly$\alpha$
photons tend to escape from small galaxies with low dust attenuation. Regarding
their morphology, LAEs belong to Irr/merger classes, unlike non-LAEs. Size and
morphology represent the most noticeable difference between LAEs and non-LAEs
at $z \sim 0.3$. Furthermore, the comparison of our results with those obtained
at higher redshifts indicates that either the Ly$\alpha$ technique picks up
different kind of galaxies at different redshifts or that the physical
properties of LAEs are evolving with redshift.
