Matches in SemOpenAlex for { <https://semopenalex.org/work/W2085387831> ?p ?o ?g. }
Showing items 1 to 75 of
75
with 100 items per page.
- W2085387831 endingPage "1146" @default.
- W2085387831 startingPage "1127" @default.
- W2085387831 abstract "We have used the Press–Schechter approximation to calculate the abundance and large-scale clustering of dark haloes in the CDM cosmogony. Applying these results to quasars at z = 3−4, we find a wide range of haloes which are both sufficiently massive and sufficiently numerous to host quasars, and the prediction for the clustering strength is correspondingly uncertain. Current estimates of quasar clustering require that the parent haloes lie at the most massive end of the allowed range, with velocity dispersions in the range 550−900 km s−1, and that the quasar luminosity be quite tightly correlated with the parent halo properties. Another application is to the diffuse X-ray background. If this is generated by discrete sources associated with dark haloes then the upper limits on the X-ray angular correlation function constrain the halo masses to be |$lt 10^{12} enspace h^{-1} enspace M_odot$|. We have considered two simple models for galaxy formation. In the first, which has some attractions for disc galaxies, we identify galaxies with dark haloes forming at the present epoch. We find that haloes with abundance like that of |$L_ast$| galaxies have large-scale clustering which is nearly unbiased, and the smaller haloes are antibiased — quite a negative feature. In the second, the galaxies we see today are assumed to be a fossil remnant of haloes which formed earlier. The stellar and dark particle velocity dispersions are assumed to be equal, and the luminosity for each halo is adjusted to give a tight and universal L–V relation like that observed. We identify an epoch when the comoving number density of haloes with a given luminosity is maximized, and we calculate how this number density is biased by long wavelength modes. The results here are more encouraging: All of the ‘galaxies’ in this model are positively biased. The enhancement of the light-to-mass ratios for rich clusters is substantial, though dependent on the normalization. For a low normalization the bias is strong enough to reconcile virial estimates of M/L for clusters with Ω = 1." @default.
- W2085387831 created "2016-06-24" @default.
- W2085387831 creator A5045427366 @default.
- W2085387831 creator A5060836964 @default.
- W2085387831 date "1989-04-01" @default.
- W2085387831 modified "2023-09-29" @default.
- W2085387831 title "Biased clustering in the cold dark matter cosmogony" @default.
- W2085387831 doi "https://doi.org/10.1093/mnras/237.4.1127" @default.
- W2085387831 hasPublicationYear "1989" @default.
- W2085387831 type Work @default.
- W2085387831 sameAs 2085387831 @default.
- W2085387831 citedByCount "347" @default.
- W2085387831 countsByYear W20853878312012 @default.
- W2085387831 countsByYear W20853878312013 @default.
- W2085387831 countsByYear W20853878312014 @default.
- W2085387831 countsByYear W20853878312015 @default.
- W2085387831 countsByYear W20853878312016 @default.
- W2085387831 countsByYear W20853878312017 @default.
- W2085387831 countsByYear W20853878312018 @default.
- W2085387831 countsByYear W20853878312019 @default.
- W2085387831 countsByYear W20853878312020 @default.
- W2085387831 countsByYear W20853878312021 @default.
- W2085387831 countsByYear W20853878312022 @default.
- W2085387831 countsByYear W20853878312023 @default.
- W2085387831 crossrefType "journal-article" @default.
- W2085387831 hasAuthorship W2085387831A5045427366 @default.
- W2085387831 hasAuthorship W2085387831A5060836964 @default.
- W2085387831 hasBestOaLocation W20853878311 @default.
- W2085387831 hasConcept C121332964 @default.
- W2085387831 hasConcept C12287442 @default.
- W2085387831 hasConcept C126320844 @default.
- W2085387831 hasConcept C1276947 @default.
- W2085387831 hasConcept C135041427 @default.
- W2085387831 hasConcept C151532515 @default.
- W2085387831 hasConcept C159249277 @default.
- W2085387831 hasConcept C174802034 @default.
- W2085387831 hasConcept C184665706 @default.
- W2085387831 hasConcept C26405456 @default.
- W2085387831 hasConcept C44870925 @default.
- W2085387831 hasConcept C88148261 @default.
- W2085387831 hasConcept C98444146 @default.
- W2085387831 hasConceptScore W2085387831C121332964 @default.
- W2085387831 hasConceptScore W2085387831C12287442 @default.
- W2085387831 hasConceptScore W2085387831C126320844 @default.
- W2085387831 hasConceptScore W2085387831C1276947 @default.
- W2085387831 hasConceptScore W2085387831C135041427 @default.
- W2085387831 hasConceptScore W2085387831C151532515 @default.
- W2085387831 hasConceptScore W2085387831C159249277 @default.
- W2085387831 hasConceptScore W2085387831C174802034 @default.
- W2085387831 hasConceptScore W2085387831C184665706 @default.
- W2085387831 hasConceptScore W2085387831C26405456 @default.
- W2085387831 hasConceptScore W2085387831C44870925 @default.
- W2085387831 hasConceptScore W2085387831C88148261 @default.
- W2085387831 hasConceptScore W2085387831C98444146 @default.
- W2085387831 hasIssue "4" @default.
- W2085387831 hasLocation W20853878311 @default.
- W2085387831 hasOpenAccess W2085387831 @default.
- W2085387831 hasPrimaryLocation W20853878311 @default.
- W2085387831 hasRelatedWork W2027119365 @default.
- W2085387831 hasRelatedWork W2053647613 @default.
- W2085387831 hasRelatedWork W2064918579 @default.
- W2085387831 hasRelatedWork W2084847985 @default.
- W2085387831 hasRelatedWork W2134753723 @default.
- W2085387831 hasRelatedWork W3098997918 @default.
- W2085387831 hasRelatedWork W3103395327 @default.
- W2085387831 hasRelatedWork W3105569209 @default.
- W2085387831 hasRelatedWork W3122666341 @default.
- W2085387831 hasRelatedWork W3211732184 @default.
- W2085387831 hasVolume "237" @default.
- W2085387831 isParatext "false" @default.
- W2085387831 isRetracted "false" @default.
- W2085387831 magId "2085387831" @default.
- W2085387831 workType "article" @default.