NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-05-20 T00:05:29 PDT
Help | Comment | NED Home

For refcode 1999MNRAS.304..225M:
Retrieve 49 NED objects in this reference.
Please click here for ADS abstract

NED Abstract

Copyright by Royal Astronomical Society. 1999MNRAS.304..225M The near-infrared Fundamental Plane of elliptical galaxies B. Mobasher, R. Guzman, A. Aragon-Salamanca and S. Zepf Accepted 1998 October 15. Received 1998 October 15; in original form 1996 November 22 ABSTRACT Near-infrared (2.2 mm) observations of a sample of 48 elliptical galaxies in the Coma cluster have been carried out and used to study the near- infrared Fundamental Plane (FP) of ellipticals in this cluster. An rms scatter of 0.072 dex is found for this relation, similar to that of its optical counterpart, using the same sample of galaxies. This corresponds to an uncertainty of 18 per cent in distances to individual galaxies derived from this relation. The sensitivity of the near-infrared FP to the star formation or changes in metallicity and stellar population among the ellipticals is explored and found to be small, although a likely source of scatter in this relation is contributions from the asymptotic giant branch (AGB) population to the near-infrared light. Allowing for observational uncertainties, we find an intrinsic scatter of 0.060 dex in the near- infrared FP. The cluster galaxies presented here provide the zero-point for the peculiar velocity studies, using the near-infrared FP. Changes in the slopes of the D-{sigma} and L-{sigma} relations of ellipticals between the optical and near-infrared wavelengths are investigated and found to be due to variations in metallicity or age (or a combination of them). However, it is not possible to disentangle the effects of age and metallicity in these relations. We find M/L is proportional to M^{alpha}^ with {alpha} = 0.18+/-0.01 in the near-infrared and {alpha} = 0.23+/-0.01 at optical wavelengths, using the same sample of galaxies. This relation is interpreted as being due to a mass-metallicity effect or changes in age or the initial mass function slope with mass. Using evolutionary population synthesis models, we find that the effects of age and metallicity decouple in the (M/L)_K_ versus Mg_2_ and (M/L)_K_ versus (V-K) diagrams. The models suggest that the observed trends in these relations may be due to an age sequence, while metallicity mainly contributes to the scatter. Key words:galaxies: clusters: individual: Coma - galaxies: elliptical and lenticular, cD - galaxies: fundamental parameters - galaxies: photometry - galaxies: stellar content - infrared: galaxies
Retrieve 49 NED objects in this reference.
Please click here for ADS abstract

Back to NED Home