Results 61 to 70 of about 1,023,991 (216)

The Shocking Features in the Closest Rich Galaxy Cluster Norma

open access: yesThe Astrophysical Journal
The merger shocks generated by the collision of galaxy clusters elevate the pressure within the intracluster medium, significantly influencing the evolution of embedded cluster galaxies.
Chong Ge   +4 more
doaj   +1 more source

Visual Icons

open access: yesPhilosophy and Phenomenological Research, Volume 113, Issue 2, Page 327-345, September 2026.
ABSTRACT Philosophers often characterize perception as image‐like. There is little agreement, however, about what constitutes an imagistic or iconic representation. This article identifies five signature properties of iconic representations endorsed in the philosophical and scientific literature: item‐richness, feature‐richness, spatiotemporal ...
Jake Quilty‐Dunn
wiley   +1 more source

AGN outflows and the cluster cooling flow conundrum

open access: yes, 2011
Temperature distributions within cores of galaxy clusters indicate gas in the core should cool down rapidly and contract. The cooling flow problem involves the hypothesis that the rapidly cooling gas should eventually condensate into unobserved molecular
Klees, Ilja
core   +1 more source

Turbulent heating in galaxy clusters brightest in X-rays [PDF]

open access: yesNature, 2014
published in ...
I. Zhuravleva   +11 more
openaire   +11 more sources

Detailed Shapes of the Line-of-sight Velocity Distributions in Massive Early-type Galaxies from Nonparametric Spectral Models

open access: yesThe Astrophysical Journal, 2023
We present the first systematic study of the detailed shapes of the line-of-sight velocity distributions (LOSVDs) in nine massive early-type galaxies (ETGs) using the novel nonparametric modeling code WINGFIT.
Kianusch Mehrgan   +4 more
doaj   +1 more source

Solvent‐Guided Chiral Assemblies and Chemical Doping of OEG‐Functionalized Conjugated Polymers

open access: yesAdvanced Materials, Volume 38, Issue 45, 13 August 2026.
Solvent‐dependent aggregation pathways dictate whether conjugated polymers form chiral lyotropic liquid‐crystalline assemblies or achiral packed aggregates. Mapping solvent‐controlled β₁ and β2 states reveals that weaker backbone association favors β₁ aggregates and reorganizable twisted mesophases, whereas stronger backbone association favors β2 ...
Sanghyun Jeon   +10 more
wiley   +1 more source

The Photometric Properties of Brightest Cluster Galaxies [PDF]

open access: yes, 1980
NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document. Photometry of a large sample of first-ranked cluster galaxies, obtained with SIT and CCD area photometers, is discussed.
Hoessel, John Greg
core   +1 more source

Brightest Cluster Galaxy Alignments in Merging Clusters [PDF]

open access: yesThe Astrophysical Journal, 2019
Abstract The orientations of brightest cluster galaxies (BCGs) and their host clusters tend to be aligned, but the mechanism driving this is not clear. To probe the role of cluster mergers in this process, we quantify alignments of 38 BCGs in 22 clusters undergoing major mergers (up to ∼1 Gyr after first pericenter).
David Wittman   +2 more
openaire   +4 more sources

A Catalog of 1.58 Million Clusters of Galaxies Identified from the DESI Legacy Imaging Surveys

open access: yesThe Astrophysical Journal Supplement Series
Based on the DESI Legacy Imaging Surveys released data and available spectroscopic redshifts, we identify 1.58 million clusters of galaxies by searching for the overdensity of the stellar mass distribution of galaxies within redshift slices around ...
Z. L. Wen, J. L. Han
doaj   +1 more source

Comparing Globular Cluster System Properties with Host Galaxy Environment

open access: yesThe Astrophysical Journal, 2023
We present Hubble Space Telescope photometry in the optical (F475X) and near-infrared (F110W) bands of the globular cluster (GC) systems of the inner halos of a sample of 15 massive elliptical galaxies.
Kate Hartman   +4 more
doaj   +1 more source

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