  Dwarf highly star-forming galaxies (SFGs) dominated the early Universe and
are considered the main driver of its reionization. However, direct
observations of these distant galaxies are mainly confined to rest-frame
ultraviolet and visible light, limiting our understanding of their complete
properties. Therefore, it is still paramount to study their local analogs, the
green pea (GP) and blueberry (BB) galaxies. This work aims to expand our
knowledge of BBs by identifying a new sample that is closer and in the southern
sky. In addition to the already known BBs, this new sample will allow for a
statistically significant study of their properties probed by visible and
infrared (IR) light. By utilizing the HECATE catalog, which provides photometry
and characterization of galaxies, along with data from Pan-STARSS and SDSS,
this study selects and analyzes a new sample of BBs. We employed spectral
energy distribution fitting to derive homogeneous measurements of
star-formation rates and stellar masses. Additionally, we measured
emission-line fluxes, including $\rm HeII~\lambda 4686$, through spectral
fitting. Through this work, we identified 48 BBs, of which 40 were first
recognized as such, with the nearest at 19~Mpc. 14 of the BBs are in the south
sky. The BBs tend to be extremely IR red in both WISE $W1-W2$ and $W2-W3$
colors, distinguishing them from typical SFGs. Dwarf SFGs with higher specific
star-formation rates tend to have redder IR colors. Blueberry galaxies stand
out as the most intensely star-forming sources in the local Universe among
dwarf galaxies. They exhibit unique characteristics, such as being
intrinsically bluer in visible light, redder in the infrared, and less massive.
They also have higher specific star-formation rates, equivalent widths, lower
metallicities, and the most strongly ionized interstellar medium compared to
typical SFGs and GPs.
