By V I Abaev; Herbert H Paper; Steven P Hill; Dzaudzhikau (R.S.F.S.R.). Nauchno-issledovatelʹskiĭ institut Severo-Osetinskoĭ ASSR.; Indiana University. Research Center in Anthropology, Folklore, and Linguistics
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Orban et al.  have demonstrated that making star formation less efficient by adding a random component to the normally adopted star formation threshold produces star formation histories for dwarf galaxies which look much more like those observed. Nonetheless, the intense early star formation in the DS86 model produces galactic outflows which appear to be necessary from other observations. For example, Governato et al.  can solve the long standing discrepancy between the observed and modeled shapes of dwarf galaxy rotation curves through high resolution modeling of a central wind.
However, the higher resolution available in most designs comes in the near-infrared. As one moves from the optical to the near infrared, one loses a great deal of diagnostic strength in a classical color-magnitude diagram type of analysis. Thus, preserving as much of the angular resolution at optical wavelengths will be critical for this type of future analysis. 3 Unanswered Questions There are some additional questions concerning morphologies of dwarf galaxies. 1 Transition Galaxies What is the nature of the transition (dSph/dIrr) galaxies?
Hypothesis holds that the difference between dSphs and dIs is due to events during the earliest epochs. This seems at odds with the observation that the star formation histories of dSphs and dIs are not clearly distinguishable except at the current epoch [23, 121]. It also seems at odds with the mechanism proposed by Mayer et al.  – how would a galaxy know early on that it was eventually going to undergo harassment? It is possible that the comparisons of the metallicity–luminosity relationships given by Mateo and Grebel et al.