Results 81 to 90 of about 147,516 (226)
Reionisation and High-Redshift Galaxies: The View from Quasar Absorption Lines [PDF]
Publications Astronomical Society of Australia, 2015 Determining when and how the first galaxies reionised the intergalactic medium promises to shed light on both the nature of the first objects and the cosmic history of baryons.
G. Becker, J. Bolton, A. Lidz
semanticscholar +1 more source
A New Padé Approach to Modeling Wormholes in Dekel‐Zhao Dark Matter Halos
Annalen der Physik, Volume 538, Issue 3, March 2026.A matter‐first Padé strategy is introduced to build traversable wormholes from prescribed dark‐matter halos. Rational Padé fits approximately the Dekel–Zhao density and are analytically integrated to obtain a shape function that exactly reproduces the intended matter content, avoiding spurious poles of geometry‐first schemes.
Jonathan Alves Rebouças +4 more
wiley +1 more source
High Redshift Radio Galaxies with the VLT [PDF]
, 1997 The study of high-$z$ radio galaxies (HZRGs) has matured considerably during the last decade. Large numbers of $z>2$ radio galaxies have been found and have been studied in considerable detail. In this review we will address the importance of the VLT for studies of samples of distant radio galaxies.
Röttgering, H. J. A., Miley, G. K.
openaire +2 more sources
ON THE [C ii]–SFR RELATION IN HIGH REDSHIFT GALAXIES [PDF]
, 2015 After two Atacama Large Millimeter/submillimeter Array (ALMA) observing cycles, only a handful of [C ii] 158 μm emission line searches in z > 6 galaxies have reported a positive detection, questioning the applicability of the local [C ii]–star formation ...
L. Vallini +4 more
semanticscholar +1 more source
Logarithmic and Strong Coupling Models in Weyl‐Type f(Q,T)$f(Q,T)$ Gravity
Annalen der Physik, Volume 538, Issue 1, January 2026.This work explores Weyl‐type f(Q,T) gravity using recent observational datasets — CC, Pantheon+, Union 3.0, and DESI DR2. Through MCMC analysis of logarithmic and strong coupling models, the study reveals a transition from deceleration to acceleration, quintessence‐to‐phantom dynamics, and late‐time consistency with LCDM, offering a geometry‐driven ...
Rahul Bhagat, S. K. Tripathy, B. Mishra
wiley +1 more source
The visibility of high-redshift galaxies [PDF]
Monthly Notices of the Royal Astronomical Society, 1990 The most visible galaxies (those which have the largest apparent sizes and isophotal luminosities when seen at a given distance) are those with a particular observed surface brightness. Extending this argument to high-redshift galaxies, it is clear that this optimum surface brightness moves progressively to brighter intrinsic surface brightnesses, so ...
S. Phillipps, J. I. Davies, M. J. Disney
openaire +1 more source
Measuring the star formation rate density from CNOC2 [PDF]
, 2006 This thesis charts the evolution of the Universal Star Formation Rate Density (SFRD) across the redshift range 0.2 < z < 0.6, using the 2nd Canadian Network for Observational Cosmology Survey (CN0C2).
Whitaker, Richard James
core
Adsorption of Helium on Cationic or Anionic Tetracene and Pentacene
Small Structures, Volume 7, Issue 1, January 2026.How does the arrangement of helium atoms that are adsorbed on tetracene or pentacene ions change with increasing coverage? When does the adsorption layer change from 1D to 2D, and to 3D? Is the transition abrupt? Are the helium atoms localized? Is the arrangement the same for cations and anions? What changes as the acene grows in length?
Miriam Kappe +6 more
wiley +1 more source
The clustering of dark matter, haloes & galaxies [PDF]
, 2008 In this thesis I study the spatial distribution of galaxies, haloes and dark matter particles using a suite of state-of-art cosmological N-body simulations of the growth structure in the Universe.
Angulo de la Fuente, Raúl Esteban
core
AN INCREASING STELLAR BARYON FRACTION IN BRIGHT GALAXIES AT HIGH REDSHIFT [PDF]
, 2015 Recent observations have shown that the characteristic luminosity of the rest-frame ultraviolet (UV) luminosity function does not significantly evolve at 4 < z < 7 and is approximately M UV * ∼ − 21 .
S. Finkelstein +14 more
semanticscholar +1 more source