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The physical mechanisms for starburst or quenching in less massive ($M_* <10^{10} M_{\odot}$) galaxies are unclear. The merger is one of the inescapableprocesses referred to as both starburst and quenching in massive galaxies.However, the effects of the merger on star formation in dwarf galaxies andtheir evolution results are still uncertain. We aim to explore how to triggerand quench star formation in dwarf galaxies by studying the metal-poor gas-richdwarf 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 mapCO($J=$1-0), [CI]($^3$P$_1 - ^3$P$_0$), and H$\alpha$ emission in one of themost extreme starburst merging dwarf galaxies, Haro 11. We find the moleculargas is assembled around the central two star-forming regions. Themolecular/ionized gas and stellar components show complex kinematics,indicating that the gas is probably at a combined stage of collision of cloudsand feedback from star formation. The peak location and distribution of[CI](1-0) strongly resemble the CO(1-0) emission, meaning that it might tracethe same molecular gas as CO in such a dwarf merger starburst galaxy. Theenhancement of line ratios ($\sim 0.5$) of [CI]/CO around knot C is probablygenerated by the dissociation of CO molecules by cosmic rays andfar-ultraviolet photons. Globally, Haro 11 and its star-forming regions sharesimilar SFEs as the high-$z$ starburst galaxies or the clumps in nearby(U)LIRGs. Given the high SFE, sSFR, small stellar mass, low metallicity, anddeficient HI gas, Haro 11 could be an analog of high-$z$ dwarf starburst andthe potential progenitor of the nearby less massive elliptical galaxies. Thesignificantly smaller turbulent pressure and viral parameter will probablytrigger the intense starbursts. We also predict that it will quench at $M_* <8.5 \times 10^9 M_{\odot}$.

The molecular gas resolved by ALMA in the low-metallicity dwarf merging galaxy Haro 11