Large and less-biased samples of star-forming galaxies are essential to
investigate galaxy evolution. H{\alpha} emission line is one of the most
reliable tracers of star-forming galaxies because its strength is directly
related to recent star formation. However, it is observationally expensive to
construct large samples of H{\alpha} emitters by spectroscopic or narrow-band
imaging survey at high-redshifts. In this work, we demonstrate a method to
extract H{\alpha} fluxes of galaxies at z = 2.1-2.5 from Ks broad-band
photometry of ZFOURGE catalog. Combined with 25-39 other filters, we estimate
the emission line fluxes by SED fitting with stellar population models that
incorporate emission-line strengths. 2005 galaxies are selected as H{\alpha}
emitters by our method and their fluxes show good agreement with previous
measurements in the literature. On the other hand, there are more H{\alpha}
luminous galaxies than previously reported. The discrepancy can be explained by
extended H{\alpha} profiles of massive galaxies and a luminosity dependence of
dust attenuation, which are not taken into account in the previous work. We
also find that there are a large number of low-mass galaxies with much higher
specific star formation rate (sSFR) than expected from the extrapolated star
formation main sequence. Such low-mass galaxies exhibit larger ratios between
H{\alpha} and UV fluxes compared to more massive high sSFR galaxies. This
result implies that a "starburst" mode may differ among galaxies: low-mass
galaxies appear to assemble their stellar mass via short-duration bursts while
more massive galaxies tend to experience longer-duration (> 10 Myr) bursts.Comment: 18 pages, 19 figures, Resubmitted to ApJ after addressing reviewer's
comment