We describe the formation of baryonic remnants in the halo along with hot in-tergalactic gas. In this scenario, the mass and metallicity of hot gas in the Local Group relates directly to the production of baryonic remnants during the collapse of galactic halos. We construct a schematic but self-consistent model in which early bursts of star formation lead to a large remnant population in the halo. These bursts also produce an outflow of stellar ejecta into the halo, Local Group, and ultimately, the intergalactic medium. This study suggests that an optimum value of 40% (and a 2σ upper limit of 77%) of the halo mass could be in the form of O.5M_⊙ white dwarfs without violating any observational constraint. Thus, the microlensing objects in the halo may predominantly be white dwarfs. However, this model requires an initial mass function for early star formation which favors the formation of intermediate mass stars.
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