The first stars are believed to have formed a few hundred million years after the big bang in
so-called dark matter minihalos with masses∼ 10 6 M⊙ ∼10^6M_⊙. Their radiation lit up …

We present a new model of the extragalactic background light (EBL) and corresponding γγ
opacity for intergalactic gamma-ray absorption from z= 0 up to z= 10, based on a semi …

The ability of metal-free gas to cool by molecular hydrogen in primordial haloes is strongly
associated with the strength of ultraviolet (UV) flux produced by the stellar populations in the …

We present results from three cosmological simulations, only differing in gas metallicity, that
focus on the impact of metal fine-structure line cooling on stellar cluster formation in a high …

We use a simple one-zone model of the thermal and chemical evolution of interstellar gas to
study whether molecular hydrogen (H2) is ever an important coolant of the warm, diffuse …

We investigate the transition from primordial Population III (Pop III) star formation to normal
Pop II star formation in the first galaxies using new cosmological hydrodynamic simulations …

We examine the linear stability and nonlinear growth of the thermal instability in isobarically
contracting background gas with various metallicities and far-UV (FUV) field strengths. Such …

We simulate the formation of a low-metallicity (10− 2 Z⊙) stellar cluster at redshift z∼ 14.
Beginning with cosmological initial conditions, the simulation utilizes adaptive mesh …

The conditions that affect the formation of stars in radiatively and mechanically active
environments are quite different from the conditions that apply to our local interstellar …

Low-metallicity star formation poses a central problem of cosmology, as it determines the
characteristic mass scale and distribution for the first and second generations of stars …