2015MNRAS.454L..41B

Recent observations have discovered a number of extremely gas-rich very faint dwarf galaxies possibly embedded in low-mass dark matter haloes. We investigate star formation histories of these gas-rich dwarf (`almost dark') galaxies both for isolated and interacting/merging cases. We find that although star formation rates (SFRs) are very low (<10-5M<sub>☉</sub>/yr) in the simulated dwarfs in isolation for the total halo masses (Mh) of 10<sup>8</sup>-10<sup>9</sup>M<sub>☉</sub>, they can be dramatically increased to be ∼ 10<sup>–4</sup> M<sub>☉</sub>/yr when they interact or merge with other dwarfs. These interacting faint dwarfs with central compact H II regions can be identified as isolated emission line dots (`ELdots') owing to their very low surface brightness envelopes of old stars. The remnant of these interacting and merging dwarfs can finally develop central compact stellar systems with very low metallicities (Z/Z_☉ < 0.1), which can be identified as extremely metal-deficient (`XMD') dwarfs. These results imply that although there would exist many faint dwarfs that can be hardly detected in the current optical observations, they can be detected as isolated ELdots or XMD dwarfs, when they interact with other galaxies and their host environments. We predict that nucleated ultrafaint dwarfs formed from the darkest dwarf merging can be identified as low-mass globular clusters owing to the very low surface brightness stellar envelopes.