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EESSI: A cross‐platform ready‐to‐use optimised scientific software stack
Software: Practice and Experience, Volume 53, Issue 1, Page 176-210, January 2023., 2023 Abstract Getting scientific software installed correctly and ensuring it performs well has been a ubiquitous problem for several decades now, which is compounded currently by the changing landscape of computational science with the (re‐)emergence of different microprocessor families, and the expansion to additional scientific domains like artificial ...
Bob Dröge +5 more
wiley +1 more source
X-ray luminosities of galaxies in groups [PDF]
Mon.Not.Roy.Astron.Soc. 325 (2001) 693, 2001 We have derived the X-ray luminosities of a sample of galaxies in groups, making careful allowance for contaminating intragroup emission. The L_X:L_B and L_X:L_{FIR} relations of spiral galaxies in groups appear to be indistinguishable from those in other environments, however the elliptical galaxies fall into two distinct classes.
arxiv +1 more source
The Fastest Galaxy Evolution in an Unbiased Compact Group Sample with WISE [PDF]
, 2017 We study the mid-infrared (MIR) properties of galaxies in compact groups and their environmental dependence using the \textit{Wide-field Infrared Survey Explorer (WISE)} data. We use a volume-limited sample of 670 compact groups and their 2175 member galaxies with $M_r< -19.77$ and $0.01
arxiv +1 more source
Comparing galaxy populations in compact and loose groups of galaxies III. Effects of environment on star formation [PDF]
A&A 573, A96 (2015), 2014 This paper is part of a series in which we perform a systematic comparison of the galaxy properties inhabiting compact groups, loose groups and the field. In this paper we focus our study to the age and the star formation in galaxies. For galaxies in selected samples of compact groups, loose groups and field, we compare the distributions of the ...
arxiv +1 more source
Galaxy groups in the 2dF galaxy redshift survey: Large Scale Structure with Groups
, 2003 We use the 2dF Galaxy Group Catalogue constructed by Merch\'an & Zandivarez to study the large scale structure of the Universe traced by galaxy groups. We concentrate on the computation of the power spectrum and the two point correlation function.
Abadi +45 more
core +2 more sources
THE ROLE OF POOR GALAXY CLUSTERS FOR STUDYING SUPERCLUSTER STRUCTURE
Odessa Astronomical Publications, 2008 The distribution of galaxy clusters is analyzed in regions of 6 galaxy superclusters with both measured and estimated redshifts. The positions of ACO and APM galaxy clusters in the regions are compared with the positions of galaxy clusters and groups ...
E. A. Panko
doaj +1 more source
Comparing galaxy populations in compact and loose groups of galaxies [PDF]
, 2012 We perform a comparison of the properties of galaxies in compact groups, loose groups and in the field to deepen our understanding of the physical mechanisms acting upon galaxy evolution in different environments. We select samples of galaxies in compact groups identified by McConnachie et al., loose groups identified by Zandivarez and Martinez, and ...
arxiv +1 more source
Satellite Luminosities in Galaxy Groups
, 2007 Halo model interpretations of the luminosity dependence of galaxy clustering assume that there is a central galaxy in every sufficiently massive halo, and that this central galaxy is very different from all the others in the halo.
Martino, Matthew C. +2 more
core +3 more sources
The Properties of Poor Groups of Galaxies: I. Spectroscopic Survey and Results [PDF]
Astrophys.J. 496 (1998) 39, 1997 We use multi-fiber spectroscopy of 12 nearby, poor groups of galaxies to address whether the groups are bound systems or chance projections of galaxies along the line-of-sight, why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for ...
arxiv +1 more source
Correlation Function of Galaxy Groups
, 2000 We use the Updated Zwicky Catalog of galaxies (Falco et al. 1999) to generate a catalog of groups, by means of a friend-of-friend algorithm. The correlation length of the total sample is well fitted with a power law $ \xi(r)=(r/r_0)^\gamma $ with ...
Barrow J. D. +7 more
core +1 more source