FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2024703746> ?p ?o ?g. }

• W2024703746 endingPage "18" @default.
• W2024703746 startingPage "1" @default.
• W2024703746 abstract "We present the results of an analysis of the rate of evolution of the Lyα absorption lines in the redshift interval 0.0 to ~1.5 based upon a sample of 987 Lyα absorption lines identified in the spectra of 63 QSOs obtained with the Faint Object Spectrograph (FOS) of the Hubble Space Telescope (HST). These spectra were obtained as part of the QSO Absorption Line Survey, an HST Key Project during the first four years of observations with the telescope. Fits to the evolution of the number of absorbers per unit redshift (dN/dz) of the form dN/dz = A × (1 + z)γ continue to yield values of γ in the range 0.1-0.3, decidedly flatter than results from ground-based data pertaining to the redshift range z > 1.7. These results are consistent with our previous results based on a much smaller sample of lines, but the uncertainties in the fit have been greatly reduced. The combination of the HST and ground-based data suggest a marked transition in the rate of evolution of the Lyα lines at a redshift of about 1.7. The 19 Lyα lines from an additional higher redshift QSO from our sample for which tentative line identifications are available (UM 18; zem = 1.89) support the suggestion of a rapid increase at around this redshift. We derive the cumulative distribution of the full sample of Lyα lines and show that the distribution in redshift can indeed be well represented by a power law of the form (1 + z)γ. For this same sample, the distribution of equivalent widths of the Lyα absorbers above a rest equivalent width of 0.1 Å is fit quite well by an exponential. Comparing samples of Lyα lines, one set of which has redshifts the same as, or very near to, the redshifts of ions from heavy elements and another set in which no ions from heavy elements have been identified, we find that the Lyα systems with heavy element detections have a much steeper slope than the high rest equivalent width portion of the Lyman-only sample. We argue that this result is not likely to be due to either line misidentification or incomplete spectral coverage. Considering the insensitivity of the equivalent width to large changes in the column density for saturated lines, we suggest that this result is probably attributable to rapid evolution of the very highest column density systems, rather than real differences in metallicity. We find evidence that the rate of evolution increases with increasing equivalent width. We compare our results for the variation of line density with redshift to recent numerical simulations of Lyα absorbers, in particular, to those of Riediger, Petitjean, & Mucket, which extend to zero redshift. We find fairly good agreement between these simulations and our results, though the rapid evolution we find in the Lyα systems containing heavy element ions is not predicted in their models. We speculate that these heavy element-containing Lyα systems involve those clouds closely associated with galaxies, whose column densities are too high and whose sizes are too small to be included in the Riediger et al. simulations. Our results for Lyα lines at the high end of our equivalent width distribution are compatible with the recent analysis of the absorber-galaxy correlation by Chen et al. For the weaker lines, however, our results suggest that whatever association exists between absorbers and galaxies is different from that for the stronger lines. We conclude with some suggestions for further observations." @default.
• W2024703746 created "2016-06-24" @default.
• W2024703746 creator A5007058019 @default.
• W2024703746 creator A5008915976 @default.
• W2024703746 creator A5016228290 @default.
• W2024703746 creator A5021977014 @default.
• W2024703746 creator A5030887415 @default.
• W2024703746 creator A5036596371 @default.
• W2024703746 creator A5037615659 @default.
• W2024703746 creator A5041369779 @default.
• W2024703746 creator A5047729711 @default.
• W2024703746 creator A5064171127 @default.
• W2024703746 creator A5064824868 @default.
• W2024703746 creator A5078742232 @default.
• W2024703746 creator A5080130360 @default.
• W2024703746 date "1998-10-10" @default.
• W2024703746 modified "2023-09-23" @default.
• W2024703746 title "The<i>Hubble Space Telescope</i>Quasar Absorption Line Key Project. XIV. The Evolution of Lyα Absorption Lines in the Redshift Interval<i>z</i>= 0–1.5" @default.
• W2024703746 cites W123661527 @default.
• W2024703746 cites W176246254 @default.
• W2024703746 cites W1966490527 @default.
• W2024703746 cites W1967825217 @default.
• W2024703746 cites W1971572444 @default.
• W2024703746 cites W1984479246 @default.
• W2024703746 cites W1994867525 @default.
• W2024703746 cites W1999911662 @default.
• W2024703746 cites W2000945613 @default.
• W2024703746 cites W2009109680 @default.
• W2024703746 cites W2011068285 @default.
• W2024703746 cites W2024657021 @default.
• W2024703746 cites W2025829476 @default.
• W2024703746 cites W2060037443 @default.
• W2024703746 cites W2092860954 @default.
• W2024703746 cites W2213776812 @default.
• W2024703746 cites W2325850497 @default.
• W2024703746 cites W2952882462 @default.
• W2024703746 cites W3101286524 @default.
• W2024703746 cites W3105025008 @default.
• W2024703746 cites W3106137129 @default.
• W2024703746 cites W3122992179 @default.
• W2024703746 cites W3124099744 @default.
• W2024703746 cites W6141495 @default.
• W2024703746 doi "https://doi.org/10.1086/306233" @default.
• W2024703746 hasPublicationYear "1998" @default.
• W2024703746 type Work @default.
• W2024703746 sameAs 2024703746 @default.
• W2024703746 citedByCount "126" @default.
• W2024703746 countsByYear W20247037462012 @default.
• W2024703746 countsByYear W20247037462013 @default.
• W2024703746 countsByYear W20247037462014 @default.
• W2024703746 countsByYear W20247037462015 @default.
• W2024703746 countsByYear W20247037462016 @default.
• W2024703746 countsByYear W20247037462017 @default.
• W2024703746 countsByYear W20247037462018 @default.
• W2024703746 countsByYear W20247037462019 @default.
• W2024703746 countsByYear W20247037462020 @default.
• W2024703746 countsByYear W20247037462022 @default.
• W2024703746 countsByYear W20247037462023 @default.
• W2024703746 crossrefType "journal-article" @default.
• W2024703746 hasAuthorship W2024703746A5007058019 @default.
• W2024703746 hasAuthorship W2024703746A5008915976 @default.
• W2024703746 hasAuthorship W2024703746A5016228290 @default.
• W2024703746 hasAuthorship W2024703746A5021977014 @default.
• W2024703746 hasAuthorship W2024703746A5030887415 @default.
• W2024703746 hasAuthorship W2024703746A5036596371 @default.
• W2024703746 hasAuthorship W2024703746A5037615659 @default.
• W2024703746 hasAuthorship W2024703746A5041369779 @default.
• W2024703746 hasAuthorship W2024703746A5047729711 @default.
• W2024703746 hasAuthorship W2024703746A5064171127 @default.
• W2024703746 hasAuthorship W2024703746A5064824868 @default.
• W2024703746 hasAuthorship W2024703746A5078742232 @default.
• W2024703746 hasAuthorship W2024703746A5080130360 @default.
• W2024703746 hasBestOaLocation W20247037461 @default.
• W2024703746 hasConcept C121332964 @default.
• W2024703746 hasConcept C1276947 @default.
• W2024703746 hasConcept C135041427 @default.
• W2024703746 hasConcept C169791425 @default.
• W2024703746 hasConcept C177272240 @default.
• W2024703746 hasConcept C198352243 @default.
• W2024703746 hasConcept C2524010 @default.
• W2024703746 hasConcept C2776968204 @default.
• W2024703746 hasConcept C33024259 @default.
• W2024703746 hasConcept C33923547 @default.
• W2024703746 hasConcept C44870925 @default.
• W2024703746 hasConcept C4839761 @default.
• W2024703746 hasConcept C96141758 @default.
• W2024703746 hasConcept C98444146 @default.
• W2024703746 hasConceptScore W2024703746C121332964 @default.
• W2024703746 hasConceptScore W2024703746C1276947 @default.
• W2024703746 hasConceptScore W2024703746C135041427 @default.
• W2024703746 hasConceptScore W2024703746C169791425 @default.
• W2024703746 hasConceptScore W2024703746C177272240 @default.
• W2024703746 hasConceptScore W2024703746C198352243 @default.
• W2024703746 hasConceptScore W2024703746C2524010 @default.
• W2024703746 hasConceptScore W2024703746C2776968204 @default.
• W2024703746 hasConceptScore W2024703746C33024259 @default.
• W2024703746 hasConceptScore W2024703746C33923547 @default.
• W2024703746 hasConceptScore W2024703746C44870925 @default.

• next