2017/04/12 by Luz Ángela García, L. A. García, E. Tescari +5
Engineering · Physics and Astronomy · #Absorption (acoustics) #Astrophysics #CCD and CMOS Imaging Sensors #Context (archaeology) #Dwarf galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Optics #Physics #Stellar, planetary, and galactic studies #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1093/mnrasl/slx053
5 pages, 4 figures. Accepted April 10, 2017 in MNRAS
openalex publication_date 2017/04/12 · openalex created_date 2017/04/28 · arxiv created 2017/05/23 · arxiv updated 2017/05/24 · openalex updated_date 2026/08/05
Abstract We present a theoretical model to predict the properties of an observed z = 5.72 Lyman α emitter galaxy–C iv absorption pair separated by 1384 comoving kpc h−1. We use the separation of the pair and an outflow velocity/time travelling argument to demonstrate that the observed galaxy cannot be the source of metals for the C iv absorber. We find a plausible explanation for the metal enrichment in the context of our simulations: a dwarf galaxy with M⋆ = 1.87 × 109 M⊙ located 119 comoving kpc h−1 away with a wind velocity of ∼100 km s−1 launched at z ∼ 7. Such a dwarf (MUV = −20.5) is fainter than the detection limit of the observed example. In a general analysis of galaxy–C iv absorbers, we find galaxies with − 20.5 <MUV < −18.8 are responsible for the observed metal signatures. In addition, we find no correlation between the mass of the closest galaxy to the absorber and the distance between them, but a weak anti-correlation between the strength of the absorption and the separation of galaxy–absorber pairs.