The molecular gas resolved by ALMA in the low-metallicity dwarf merging
  galaxy Haro 11
  The physical mechanisms for starburst or quenching in less massive ($M_* <
10^{10} M_{\odot}$) galaxies are unclear. The merger is one of the inescapable
processes referred to as both starburst and quenching in massive galaxies.
However, the effects of the merger on star formation in dwarf galaxies and
their evolution results are still uncertain. We aim to explore how to trigger
and quench star formation in dwarf galaxies by studying the metal-poor gas-rich
dwarf mergers based on the multi-band observations at a spatial resolution of
$\sim$ 460 pc. We use the archival data of ALMA (band 3, 8) and VLT/MUSE to map
CO($J=$1-0), [CI]($^3$P$_1 - ^3$P$_0$), and H$\alpha$ emission in one of the
most extreme starburst merging dwarf galaxies, Haro 11. We find the molecular
gas is assembled around the central two star-forming regions. The
molecular/ionized gas and stellar components show complex kinematics,
indicating that the gas is probably at a combined stage of collision of clouds
and feedback from star formation. The peak location and distribution of
[CI](1-0) strongly resemble the CO(1-0) emission, meaning that it might trace
the same molecular gas as CO in such a dwarf merger starburst galaxy. The
enhancement of line ratios ($\sim 0.5$) of [CI]/CO around knot C is probably
generated by the dissociation of CO molecules by cosmic rays and
far-ultraviolet photons. Globally, Haro 11 and its star-forming regions share
similar SFEs as the high-$z$ starburst galaxies or the clumps in nearby
(U)LIRGs. Given the high SFE, sSFR, small stellar mass, low metallicity, and
deficient HI gas, Haro 11 could be an analog of high-$z$ dwarf starburst and
the potential progenitor of the nearby less massive elliptical galaxies. The
significantly smaller turbulent pressure and viral parameter will probably
trigger the intense starbursts. We also predict that it will quench at $M_* <
8.5 \times 10^9 M_{\odot}$.
