FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3034616775> ?p ?o ?g. }

• W3034616775 endingPage "162" @default.
• W3034616775 startingPage "161" @default.
• W3034616775 abstract "Long-slit spectra for the photometric axes of a sample of 14 elliptical galaxies, predominantly low-luminosity ellipticals, in the Virgo cluster and in nearby groups, are studied to investigate the galaxy kinematical structure and stellar evolutionary history. To determine the galaxy kinematical structure, the shape of the line-of-sight velocity distribution (hereafter LOSVD) is measured using the Fourier Correlation Quotient method of Bender (1990), adopting the parametrisation of the LOSVD due to van der Marel and Franx (1993). This parametrisation enables the asymmetrical and symmetrical deviations of the LOSVD from a Gaussian function to be measured by the amplitudes H(_3) and H(_4) of the Gauss-Hermite series respectively. Rotation, velocity dispersion (σ), H(_3) and H(_4) are determined as a function of radius for both the major and minor axes of our sample. To summarise, LOSVD asymmetries were measured for the major axes of 12 galaxies which in the majority of cases have been interpreted as evidence for central disk-like components; evidence of both radial and tangential anisotropy were found from the measurement of H(_4); central decreases in σ are measured for galaxies, which is interpreted as evidence that they have undergone some form of merger or interaction. On the basis of their measurements, galaxies are classified into classes: types and Type 1 galaxies show strong evidence for both disk and bulge components and have the greatest measured values of H(_3) for our sample. Galaxies of type 2 show strong evidence for embedded disk components and most (3 of 4) are measured to have central decreases in a. Type 3 galaxies have kinematically-decoupled cores. Other galaxies, not classified, are NGC 3379 and NGC 4468.Measurements of the line-strength indices Mg(_b), Mg(_2), Hβ, Fe5270, Fe5335 and are determined as a function of radius for all spectra and established to the Lick/IDS scale. The relations Mg’(_b)-Mg(_2), Mg’(_b), - log(σ), Mg(_b)- and Hβ-[Mg(_b) ] are then studied. The Mg’(_b),-Mg(_2) relation of Wegner et al. (1998) and the calibrations of Worthey (1994) are compared with measurements here: this is used as a check of our calibration of Mg’(b), and Mg(_2). Measurements in the Mg’(_b)-log(σ) plane are considered separately for each galaxy and compared with the central relation of Colless et al. (1998). Measurements for most galaxies are found to be in good agreement with this relation. Measurements of Mg(_b) and are similarly considered for each galaxy and compared with the predictions of the models of Worthey (1994). For the majority of galaxies, measurements are clearly offset from the Mg(_b)- model grid of Worthey (1994), representing an [(^Mg)-(_Fe)] overabundance. This is an important result which shows that the [(^Mg)-(_Fe)] overabundance detected previously for the giant ellipticals similarly exists for ellipticals of the low luminosities studied here. For most galaxies this overabundance is found to be a constant function of radius. For the type 2 galaxy NGC 3605, and NGC 4468, measurements are consistent with solar abundance ratios. Finally, measurements of Hβ and [Mg(_b) ] are compared with the models of Worthey (1994) to distinguish gradients in both age and metallicity. For all galaxies, gradients in metallicity are found with metallicity decreasing as a function of radius. For 5 galaxies (NGC 4564, NGC 3377, NGC 4478, NGC 4339 and NGC 3605) age gradients are also detected, with the galaxy centre shown to be younger than the surrounding galaxy. Interpreting these results together, different formation scenarios are proposed for the different galaxy types. For galaxies of type 1, formation by homogenous, dissipational collapse is proposed. Galaxies of type 2 show evidence for a less homogenous evolutionary history involving dissipationless collapse. No conclusive scenario is proposed for galaxies of type 3." @default.
• W3034616775 created "2020-06-19" @default.
• W3034616775 creator A5021267655 @default.
• W3034616775 date "2000-04-01" @default.
• W3034616775 modified "2023-10-18" @default.
• W3034616775 title "Low-luminosity elliptical galaxies" @default.
• W3034616775 hasPublicationYear "2000" @default.
• W3034616775 type Work @default.
• W3034616775 sameAs 3034616775 @default.
• W3034616775 citedByCount "0" @default.
• W3034616775 crossrefType "journal-article" @default.
• W3034616775 hasAuthorship W3034616775A5021267655 @default.
• W3034616775 hasConcept C10767094 @default.
• W3034616775 hasConcept C121332964 @default.
• W3034616775 hasConcept C12287442 @default.
• W3034616775 hasConcept C127529279 @default.
• W3034616775 hasConcept C1276947 @default.
• W3034616775 hasConcept C134122466 @default.
• W3034616775 hasConcept C165641701 @default.
• W3034616775 hasConcept C2779406902 @default.
• W3034616775 hasConcept C44870925 @default.
• W3034616775 hasConcept C77538465 @default.
• W3034616775 hasConcept C871022 @default.
• W3034616775 hasConcept C98444146 @default.
• W3034616775 hasConceptScore W3034616775C10767094 @default.
• W3034616775 hasConceptScore W3034616775C121332964 @default.
• W3034616775 hasConceptScore W3034616775C12287442 @default.
• W3034616775 hasConceptScore W3034616775C127529279 @default.
• W3034616775 hasConceptScore W3034616775C1276947 @default.
• W3034616775 hasConceptScore W3034616775C134122466 @default.
• W3034616775 hasConceptScore W3034616775C165641701 @default.
• W3034616775 hasConceptScore W3034616775C2779406902 @default.
• W3034616775 hasConceptScore W3034616775C44870925 @default.
• W3034616775 hasConceptScore W3034616775C77538465 @default.
• W3034616775 hasConceptScore W3034616775C871022 @default.
• W3034616775 hasConceptScore W3034616775C98444146 @default.
• W3034616775 hasLocation W30346167751 @default.
• W3034616775 hasOpenAccess W3034616775 @default.
• W3034616775 hasPrimaryLocation W30346167751 @default.
• W3034616775 hasRelatedWork W1617489088 @default.
• W3034616775 hasRelatedWork W1920975007 @default.
• W3034616775 hasRelatedWork W2028096488 @default.
• W3034616775 hasRelatedWork W2035225065 @default.
• W3034616775 hasRelatedWork W2065091826 @default.
• W3034616775 hasRelatedWork W2084530945 @default.
• W3034616775 hasRelatedWork W2108903848 @default.
• W3034616775 hasRelatedWork W2119489534 @default.
• W3034616775 hasRelatedWork W2120894112 @default.
• W3034616775 hasRelatedWork W2133713808 @default.
• W3034616775 hasRelatedWork W3013485212 @default.
• W3034616775 hasRelatedWork W3099192248 @default.
• W3034616775 hasRelatedWork W3099788495 @default.
• W3034616775 hasRelatedWork W3102016174 @default.
• W3034616775 hasRelatedWork W3102505617 @default.
• W3034616775 hasRelatedWork W3103168036 @default.
• W3034616775 hasRelatedWork W3103210465 @default.
• W3034616775 hasRelatedWork W3104510559 @default.
• W3034616775 hasRelatedWork W3124446639 @default.
• W3034616775 hasRelatedWork W3124697500 @default.
• W3034616775 hasVolume "120" @default.
• W3034616775 isParatext "false" @default.
• W3034616775 isRetracted "false" @default.
• W3034616775 magId "3034616775" @default.
• W3034616775 workType "article" @default.