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Normal, dust-obscured galaxies in the epoch of reionization
Inami, H.; Bowler, R. A. A.; De Looze, I. +26 more
Over the past decades, rest-frame ultraviolet (UV) observations have provided large samples of UV luminous galaxies at redshift (z) greater than 6 (refs. 1-3), during the so-called epoch of reionization. While a few of these UV-identified galaxies revealed substantial dust reservoirs4-7, very heavily dust-obscured sources at …
Large metallicity variations in the Galactic interstellar medium
Jenkins, Edward B.; Petitjean, Patrick; Fox, Andrew J. +5 more
The interstellar medium (ISM) comprises gases at different temperatures and densities, including ionized, atomic and molecular species, and dust particles1. The neutral ISM is dominated by neutral hydrogen2 and has ionization fractions of up to eight per cent3. The concentration of chemical elements heavier than he…
The diffuse γ-ray background is dominated by star-forming galaxies
Krumholz, Mark R.; Crocker, Roland M.; Roth, Matt A. +1 more
The Fermi Gamma-ray Space Telescope has revealed a diffuse γ-ray background at energies from 0.1 gigaelectronvolt to 1 teraelectronvolt, which can be separated into emission from our Galaxy and an isotropic, extragalactic component1. Previous efforts to understand the latter have been hampered by the lack of physical models capable of p…
Quenching of star formation from a lack of inflowing gas to galaxies
Richard, Johan; van Dokkum, Pieter G.; Mowla, Lamiya +16 more
Star formation in half of massive galaxies was quenched by the time the Universe was 3 billion years old1. Very low amounts of molecular gas seem to be responsible for this, at least in some cases2-7, although morphological gas stabilization, shock heating or activity associated with accretion onto a central supermassive blac…
Measuring the density structure of an accretion hot spot
Reynolds, M.; Romanova, M. M.; Calvet, N. +5 more
Magnetospheric accretion models predict that matter from protoplanetary disks accretes onto stars via funnel flows, which follow stellar magnetic field lines and shock on the stellar surfaces1-3, leaving hot spots with density gradients4-6. Previous work has provided observational evidence of varying density in hot spots…