FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2132575702> ?p ?o ?g. }

• W2132575702 endingPage "206" @default.
• W2132575702 startingPage "188" @default.
• W2132575702 abstract "We introduce a new technique for following the formation and evolution of galaxies in cosmological N-body simulations. Dissipationless simulations are used to track the formation and merging of dark matter haloes as a function of redshift. Simple prescriptions, taken directly from semi-analytic models of galaxy formation, are adopted for gas cooling, star formation, supernova feedback and the merging of galaxies within the haloes. This scheme enables us to explore the clustering properties of galaxies, and to investigate how selection by luminosity, colour or type influences the results. In this paper we study the properties of the galaxy distribution at z=0. These include B- and K-band luminosity functions, two-point correlation functions, pairwise peculiar velocities, cluster mass-to-light ratios, B-V colours, and star formation rates. We focus on two variants of a cold dark matter (CDM) cosmology: a high-density (Ω =1) model with shape-parameter Γ =0.21 (τ CDM), and a low-density model with Ω =0.3 and λ =0.7 (λ CDM). Both models are normalized to reproduce the I-band Tully--Fisher relation of Giovanelli et al. near a circular velocity of 220 km s−1. Our results depend strongly both on this normalization and on the adopted prescriptions for star formation and feedback. Very different assumptions are required to obtain an acceptable model in the two cases. For τ CDM, efficient feedback is required to suppress the growth of galaxies, particularly in low-mass field haloes. Without it, there are too many galaxies and the correlation function exhibits a strong turnover on scales below 1 Mpc. For λ CDM, feedback must be weaker, otherwise too few L* galaxies are produced and the correlation function is too steep. Although neither model is perfect, both come close to reproducing most of the data. Given the uncertainties in modelling some of the critical physical processes, we conclude that it is not yet possible to draw firm conclusions about the values of cosmological parameters from studies of this kind. Further observational work on global star formation and feedback effects is required to narrow the range of possibilities." @default.
• W2132575702 created "2016-06-24" @default.
• W2132575702 creator A5005885259 @default.
• W2132575702 creator A5015259782 @default.
• W2132575702 creator A5052111945 @default.
• W2132575702 creator A5079556845 @default.
• W2132575702 date "1999-02-11" @default.
• W2132575702 modified "2023-10-03" @default.
• W2132575702 title "Clustering of galaxies in a hierarchical universe -- I. Methods and results at z = 0" @default.
• W2132575702 cites W1575728940 @default.
• W2132575702 cites W1681070356 @default.
• W2132575702 cites W1786331656 @default.
• W2132575702 cites W1835404664 @default.
• W2132575702 cites W1964055719 @default.
• W2132575702 cites W1964072764 @default.
• W2132575702 cites W1964357829 @default.
• W2132575702 cites W1972346442 @default.
• W2132575702 cites W1974159111 @default.
• W2132575702 cites W1981057084 @default.
• W2132575702 cites W1982364216 @default.
• W2132575702 cites W1983751127 @default.
• W2132575702 cites W1994905665 @default.
• W2132575702 cites W1998577648 @default.
• W2132575702 cites W2001621694 @default.
• W2132575702 cites W2002142654 @default.
• W2132575702 cites W2005609165 @default.
• W2132575702 cites W2007116814 @default.
• W2132575702 cites W2007978190 @default.
• W2132575702 cites W2008258224 @default.
• W2132575702 cites W2021571115 @default.
• W2132575702 cites W2025165550 @default.
• W2132575702 cites W2026263995 @default.
• W2132575702 cites W2029724930 @default.
• W2132575702 cites W2030571512 @default.
• W2132575702 cites W2031990986 @default.
• W2132575702 cites W2033362295 @default.
• W2132575702 cites W2034055090 @default.
• W2132575702 cites W2040405503 @default.
• W2132575702 cites W2043685494 @default.
• W2132575702 cites W2056903171 @default.
• W2132575702 cites W2058028423 @default.
• W2132575702 cites W2058935714 @default.
• W2132575702 cites W2059039109 @default.
• W2132575702 cites W2061593633 @default.
• W2132575702 cites W2064847672 @default.
• W2132575702 cites W2071208690 @default.
• W2132575702 cites W2071864147 @default.
• W2132575702 cites W2074005806 @default.
• W2132575702 cites W2076626779 @default.
• W2132575702 cites W2079726379 @default.
• W2132575702 cites W2087425736 @default.
• W2132575702 cites W2091162092 @default.
• W2132575702 cites W2094993922 @default.
• W2132575702 cites W2095511138 @default.
• W2132575702 cites W2108191436 @default.
• W2132575702 cites W2116466430 @default.
• W2132575702 cites W2119275317 @default.
• W2132575702 cites W2126435753 @default.
• W2132575702 cites W2127896663 @default.
• W2132575702 cites W2128886095 @default.
• W2132575702 cites W2135561086 @default.
• W2132575702 cites W2152878210 @default.
• W2132575702 cites W2167635287 @default.
• W2132575702 cites W2170924363 @default.
• W2132575702 cites W3022439517 @default.
• W2132575702 cites W3036191520 @default.
• W2132575702 cites W3098632302 @default.
• W2132575702 cites W3099122631 @default.
• W2132575702 cites W3101590468 @default.
• W2132575702 cites W3102288935 @default.
• W2132575702 cites W3103795774 @default.
• W2132575702 cites W3105302330 @default.
• W2132575702 cites W3105556382 @default.
• W2132575702 cites W4252384811 @default.
• W2132575702 doi "https://doi.org/10.1046/j.1365-8711.1999.02202.x" @default.
• W2132575702 hasPublicationYear "1999" @default.
• W2132575702 type Work @default.
• W2132575702 sameAs 2132575702 @default.
• W2132575702 citedByCount "803" @default.
• W2132575702 countsByYear W21325757022012 @default.
• W2132575702 countsByYear W21325757022013 @default.
• W2132575702 countsByYear W21325757022014 @default.
• W2132575702 countsByYear W21325757022015 @default.
• W2132575702 countsByYear W21325757022016 @default.
• W2132575702 countsByYear W21325757022017 @default.
• W2132575702 countsByYear W21325757022018 @default.
• W2132575702 countsByYear W21325757022019 @default.
• W2132575702 countsByYear W21325757022020 @default.
• W2132575702 countsByYear W21325757022021 @default.
• W2132575702 countsByYear W21325757022022 @default.
• W2132575702 countsByYear W21325757022023 @default.
• W2132575702 crossrefType "journal-article" @default.
• W2132575702 hasAuthorship W2132575702A5005885259 @default.
• W2132575702 hasAuthorship W2132575702A5015259782 @default.
• W2132575702 hasAuthorship W2132575702A5052111945 @default.
• W2132575702 hasAuthorship W2132575702A5079556845 @default.
• W2132575702 hasBestOaLocation W21325757022 @default.
• W2132575702 hasConcept C121332964 @default.

• next