Results 1 to 10 of about 2,334,837 (275)
A New Constraint on the Simulation of the Intergalactic Medium through the Evolution of the Neutral Hydrogen Fraction in the Epoch of Reionization [PDF]
arXiv, 2023 The thermal history of the intergalactic medium is full of extremely useful data in the field of astrophysics and cosmology. In other words, by examining this environment in different redshifts, the effects of cosmology and astrophysics can be observed side by side.
S. Mobina Hosseini +3 more
arxiv +2 more sources
The thermal history of the intergalactic medium [PDF]
Monthly Notices of the Royal Astronomical Society, 2000 At redshifts z >~ 2, most of the baryons reside in the smooth intergalactic medium which is responsible for the low column density Lyman-alpha forest. This photoheated gas follows a tight temperature-density relation which introduces a cut-off in the distribution of widths of the Lyman-alpha absorption lines (b-parameters) as a function of column ...
Joop Schaye +4 more
openalex +7 more sources
On the supernova heating of the intergalactic medium [PDF]
Monthly Notices of the Royal Astronomical Society, 2000 submitted to MNRAS, LaTeX, 15 pages, 5 figures, 2 ...
Andrey V. Kravtsov, Gustavo Yepes
openalex +4 more sources
Hydrodynamic Response of the Intergalactic Medium to Reionization [PDF]
The Astrophysical Journal, 2020 Abstract The intergalactic medium is expected to clump on scales down to M ⊙ before the onset of reionization. The impact of these small-scale structures on reionization is poorly understood despite the modern understanding that gas ...
Anson D’Aloisio +4 more
openaire +6 more sources
Enrichment of the Intergalactic Medium by the Milky Way Subgroup [PDF]
arXiv, 2001 I study the effect of the galaxies of the Milky Way subgroup on the chemical enrichment of the diffuse gas within the Local Group. The preferred model predicts that the present-day intergalactic medium mass is 1/22 of the initial baryonic mass and its metallicity is 1/20 $Z_\odot$. Nearly 80 % of intergalactic metals were produced in the Galactic bulge.
Leticia Carigi
arxiv +3 more sources
The growth of structure in the intergalactic medium [PDF]
Monthly Notices of the Royal Astronomical Society, 2002 A {\it stochastic adhesion} model is introduced, with the purpose of describing the formation and evolution of mildly nonlinear structures, such as sheets and filaments, in the intergalactic medium (IGM), after hydrogen reionization. The model is based on replacing the overall force acting on the baryon fluid -- as it results from the composition of ...
S. Matarrese, Roya Mohayaee
openalex +7 more sources
The Evolution of the Intergalactic Medium [PDF]
Annual Review of Astronomy and Astrophysics, 2016 The bulk of cosmic matter resides in a dilute reservoir that fills the space between galaxies, the intergalactic medium (IGM). The history of this reservoir is intimately tied to the cosmic histories of structure formation, star formation, and supermassive black hole accretion.
M. McQuinn
openaire +5 more sources
Lyman-alpha emitters in a cosmological volume II: the impact of the intergalactic medium [PDF]
Monthly notices of the Royal Astronomical Society, 2019 In the near future galaxy surveys will target Lyman alpha emitting galaxies (LAEs) to unveil the nature of the dark energy. It has been suggested that the observability of LAEs is coupled to the large scale properties of the intergalactic medium. Such coupling could introduce distortions into the observed clustering of LAEs, adding a new potential ...
S. Gurung-López +5 more
arxiv +3 more sources
, 2000 About half a million years after the Big Bang, the ever-fading cosmic blackbody radiation cooled below 3000 K and shifted first into the infrared and then into the radio, and the smooth baryonic plasma that filled the Universe became neutral. The Universe then entered a ``dark age'' which persisted until the first cosmic structures collapsed into ...
Piero Madau
openalex +4 more sources
Numerical simulations of the intergalactic medium [PDF]
arXiv, 2002 The intergalactic medium at redshifts 2--6 can be studied observationally through the absorption features it produces in the spectra of background quasars. Most of the UV-absorption lines arise in mildly overdense regions, which can be simulated reliably with current hydrodynamical simulations. Comparison of observed and simulated spectra allows one to
Tom Theuns
arxiv +3 more sources