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Article: The Durham/UKST Galaxy Redshift Survey - II. The field galaxy luminosity function

TitleThe Durham/UKST Galaxy Redshift Survey - II. The field galaxy luminosity function
Authors
KeywordsLarge-scale structure of Universe
Galaxies: distances and redshifts
Cosmology: observations
Galaxies: general
Galaxies: luminosity function, mass function
Surveys
Issue Date1998
Citation
Monthly Notices of the Royal Astronomical Society, 1998, v. 293, n. 2, p. 197-207 How to Cite?
AbstractWe present the results for the galaxy luminosity function as estimated from the Durham/UKST Galaxy Redshift Survey. This survey is magnitude-limited to bJ ∼ 17, contains ∼2500 galaxies sampled at a rate of one-in-three, and surveys a ∼4 × 106(h-1 Mpc)3 volume of space. The maximum-likelihood parameters for a standard Schechter luminosity function are estimated to be M*bj = -19.72±0.09, α= -1.14±0.08 and φ* = (1.2±0.2) × 10-2(h3 Mpc-3). Attempting to correct for the scatter in the observed magnitudes leads to a flatter faint-end slope, α= -1.04±0.08, which, combined with the different luminosity function shape, causes a higher normalization to be estimated, φ*=(1.7±0.3) × 10-2(h3 Mpc-3). Neither of these parametric functions provides a good formal fit to the non-parametric estimate of the luminosity function. A comparison with galaxy luminosity functions from other redshift surveys shows good agreement, and the shape of the luminosity function now appears to be well defined down to MbJ ≃ - 17. There are some discrepancies between the different surveys for galaxies fainter than this absolute magnitude. However, our estimate agrees well with that from the APM-Stromlo Galaxy Redshift Survey and we measure a fairly flat faint-end slope.
Persistent Identifierhttp://hdl.handle.net/10722/208837
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806

 

DC FieldValueLanguage
dc.contributor.authorRatcliffe, Andrew-
dc.contributor.authorShanks, Tom-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorFong, Richard-
dc.date.accessioned2015-03-23T02:01:52Z-
dc.date.available2015-03-23T02:01:52Z-
dc.date.issued1998-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 1998, v. 293, n. 2, p. 197-207-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/208837-
dc.description.abstractWe present the results for the galaxy luminosity function as estimated from the Durham/UKST Galaxy Redshift Survey. This survey is magnitude-limited to bJ ∼ 17, contains ∼2500 galaxies sampled at a rate of one-in-three, and surveys a ∼4 × 106(h-1 Mpc)3 volume of space. The maximum-likelihood parameters for a standard Schechter luminosity function are estimated to be M*bj = -19.72±0.09, α= -1.14±0.08 and φ* = (1.2±0.2) × 10-2(h3 Mpc-3). Attempting to correct for the scatter in the observed magnitudes leads to a flatter faint-end slope, α= -1.04±0.08, which, combined with the different luminosity function shape, causes a higher normalization to be estimated, φ*=(1.7±0.3) × 10-2(h3 Mpc-3). Neither of these parametric functions provides a good formal fit to the non-parametric estimate of the luminosity function. A comparison with galaxy luminosity functions from other redshift surveys shows good agreement, and the shape of the luminosity function now appears to be well defined down to MbJ ≃ - 17. There are some discrepancies between the different surveys for galaxies fainter than this absolute magnitude. However, our estimate agrees well with that from the APM-Stromlo Galaxy Redshift Survey and we measure a fairly flat faint-end slope.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectLarge-scale structure of Universe-
dc.subjectGalaxies: distances and redshifts-
dc.subjectCosmology: observations-
dc.subjectGalaxies: general-
dc.subjectGalaxies: luminosity function, mass function-
dc.subjectSurveys-
dc.titleThe Durham/UKST Galaxy Redshift Survey - II. The field galaxy luminosity function-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.scopuseid_2-s2.0-1842780966-
dc.identifier.volume293-
dc.identifier.issue2-
dc.identifier.spage197-
dc.identifier.epage207-

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