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Lyman alpha halos are observed ubiquitously around star-forming galaxies athigh redshift, but their origin is still a matter of debate. We demonstratethat the emission from faint unresolved satellite sources, $M_{\rm UV} \gtrsim-17$, clustered around the central galaxies may play a major role in generatingspatially extended Ly$\alpha$, continuum (${\rm UV + VIS}$) and H$\alpha$halos. We apply the analytic formalism developed in Mas-Ribas & Dijkstra (2016)to model the halos around Lyman Alpha Emitters (LAEs) at $z=3.1$, for severaldifferent satellite clustering prescriptions. In general, our UV and Ly$\alpha$surface brightness profiles match the observations well at $20\lesssim r\lesssim 40$ physical kpc from the centers of LAEs. We discuss how our profilesdepend on various model assumptions and how these can be tested and constrainedwith future H$\alpha$ observations by the James Webb Space Telescope (JWST).Our analysis shows how spatially extended halos constrain (i) the presence ofotherwise undetectable satellite sources, (ii) the integrated, volumetricproduction rates of Ly$\alpha$ and LyC photons, and (iii) theirpopulation-averaged escape fractions. These quantities are all directlyrelevant for understanding galaxy formation and evolution and, for high enoughredshifts, cosmic reionization.

Small-scale Intensity Mapping: Extended Ly$\alpha$, H$\alpha$ and Continuum emission as a Probe of Halo Star Formation in High-redshift Galaxies