MUSE observations of the blue compact dwarf galaxy Haro 14. Data
  analysis and first results on morphology and stellar populations
  (Abriged) Blue compact galaxies (BCGs) are low-luminosity, metal-poor,
gas-rich objects that form stars at high rates, excellent analogs to the
high-redshift star-forming galaxy population. Being low-mass starbursts, they
also constitute ideal laboratories for investigating star formation and massive
stellar feedback. This work presents results from integral field spectroscopic
observations of the BCG Haro 14 taken with the Multi Unit Spectroscopic
Explorer (MUSE). The large MUSE field of view enables simultaneous observations
of the starburst and the host galaxy. We built galaxy maps in continuum and in
emission lines and generated synthetic VRI images, from which we produced color
index maps and surface brightness profiles. We detected numerous clumps spread
throughout the galaxy, both in continuum and in emission lines, and produced a
catalog with their position, size, and photometry. This analysis allowed us to
study the morphology and stellar populations of Haro 14 in detail. The stellar
distribution shows a pronounced asymmetry; the intensity peak in continuum is
not centered with respect to the stellar host but is displaced by about 500 pc
southwest. At the position of the continuum peak we find a bright stellar
cluster that with M$_{V}=-12.18$ appears as a strong super stellar cluster
candidate. We also find a highly asymmetric, blue, but nonionizing stellar
component that occupies almost the whole eastern part of the galaxy. We
conclude that there are at least three different stellar populations in Haro
14: the current starburst of about 6 Myr; an intermediate-age component of
between ten and several hundred million years; and a red and regular host of
several gigayears. The pronounced lopsidedness in the continuum and also in the
color maps, and the presence of numerous stellar clusters, are consistent with
a scenario of mergers or interactions acting in Haro 14.
