New D — σ Results for Coma Ellipticals

Lucey, J. R.; Guzmán, R.; Carter, D.; Terlevich, Elena

doi:10.1007/978-94-011-3510-8_18

Cited by 7 publications

(20 citation statements)

References 9 publications

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“…The bootstrap error is roughly proportional to ( S N ) −1 , but there is evidence of curvature relative to this model. We conclude that spectra of S N =25–30 are needed to suppress random errors in σ to the 5 per cent level (in agreement with Lucey & Carter 1988 and Jørgensen et al 1995b). The bootstrap uncertainty on the recession velocity measurements is well described by ɛ cz ɛ /1.2, in accord with the results of Tonry & Davis (1981).…”

Section: Data Reductionsupporting

confidence: 89%

“…The SMAC cluster sample was defined initially as the subset of Abell clusters studied by LP with cz ⊙ <12 000 km s −1 , yielding 65 clusters. At the outset of the survey (1993), published FP data already existed for a total of 10 clusters in this sample from Lucey & Carter (1988), Faber et al (1989) and Lucey et al (1991). A further seven clusters in the sample were observed as part of concurrent projects by Jørgensen, Franz & Kjærgaard (1995a,b), Smith et al (1997) and Lucey et al (1997 and in preparation).…”

Section: Selection Of Target Clusters and Galaxiesmentioning

confidence: 96%

“…Extensive overlap was also secured with external data sets, to facilitate construction of the final merged catalogue (see SMAC‐III). In particular, galaxies in certain specific data sets were targeted, such as the extensive LICK system of Davies et al (1987), the high signal‐to‐noise data of González (1993), and the southern FOCAP data of Lucey & Carter (1988) and Lucey et al (in preparation). We obtained ∼200 observations for ∼80 galaxies in the EFAR data base (Wegner et al 1996), in order to improve the overlap between these two large FP surveys.…”

Section: Observational Techniquesmentioning

confidence: 99%

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Streaming motions of galaxy clusters within 12 000 km s-1 -- I. New spectroscopic data

Smith¹,

Lucey²,

Hudson³

et al. 2000

Monthly Notices of the Royal Astronomical Society

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165

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We present new spectroscopic data for 532 early‐type galaxies, predominantly Abell cluster members with cz<12 000 km s−1. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, σ, and magnesium line‐strength indices, Mg2 and Mgb. The median estimated error, per measurement, in σ is 5 per cent. The Mg2 line‐strength data have median errors of 0.009 mag. The observed scatter between repeat measurements is largely accounted for by photon‐counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.

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Section: Data Reductionsupporting

confidence: 89%

Section: Selection Of Target Clusters and Galaxiesmentioning

confidence: 96%

Section: Observational Techniquesmentioning

confidence: 99%

See 1 more Smart Citation

Streaming motions of galaxy clusters within 12 000 km s-1 -- I. New spectroscopic data

Smith¹,

Lucey²,

Hudson³

et al. 2000

Monthly Notices of the Royal Astronomical Society

Self Cite

165

View full text Add to dashboard Cite

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“…Davies, Sadler & Peletier 1993). The C93 spectra are not of sufficient resolution and signal‐to‐noise ratio to measure accurate central velocity dispersions for our galaxies, so instead we construct a ‘Faber–Jackson’ relation (Faber & Jackson 1976) between our V ‐band 8.8‐arcsec diameter aperture magnitudes m V (see Section 2.3), and the velocity dispersions ( σ ) of Lucey et al (1997). A biweight fit (cf.…”

Section: The Datamentioning

confidence: 99%

“…(with 1 σ bootstrap errors). We used this relation to find values of σ for those galaxies in the C93 sample which were not present in the Lucey et al (1997) data.…”

Section: The Datamentioning

confidence: 99%

Colour-magnitude relations and spectral line strengths in the Coma cluster

Terlevich

Küntschner

Bower

et al. 1999

Monthly Notices of the Royal Astronomical Society

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We use the C24668, Fe4383, HγA and HδA spectral absorption line indices, together with U‐ and V‐band photometry of 101 galaxies in the Coma cluster, to investigate how mean age and metal abundance correlate with galaxy luminosity. In particular, we use the line index measurements to address the origin of the colour–magnitude relation (CMR). We find that the CMR in Coma is driven primarily by a luminosity–metallicity correlation. We additionally show evidence for a relation between age and luminosity, in the direction predicted by the semi‐analytic hierarchical clustering models of Kauffmann & Charlot, but this is only present in the C24668 index models, and could be an effect of the lack of non‐solar abundance ratios in the Worthey models used. By comparing deviations from the CMR with deviations in absorption index from analogous ‘index–magnitude’ relations, we find that colour deviations bluewards of the mean relation are strongly correlated with the hydrogen Balmer line series absorption. We show that the properties of these blue galaxies are consistent with the presence of a young stellar population in the galaxies, rather than with a reduced metallicity.

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The IRAS PSCz dipole

Rowan‐Robinson¹,

Sharpe²,

Oliver³

et al. 2000

Monthly Notices of the Royal Astronomical Society

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A B S T R A C TWe use the PSCz IRAS galaxy redshift survey to analyse the cosmological galaxy dipole out to a distance of 300 h 21 Mpc. The masked area is filled in three different ways, first by sampling the whole sky at random, secondly by using neighbouring areas to fill a masked region, and thirdly using a spherical harmonic analysis. The method of treatment of the mask is found to have a significant effect on the final calculated dipole.The conversion from redshift space to real space is accomplished by using an analytical model of the cluster and void distribution, based on 88 nearby groups, 854 clusters and 163 voids, with some of the clusters and all of the voids found from the PSCz data base.The dipole for the whole PSCz sample appears to have converged within a distance of 200 h 21 Mpc and yields a value for b V 0X6 ab 0X75 0X11 20X08 , consistent with earlier determinations from IRAS samples by a variety of methods. For b 1Y the 2s range for V 0 is 0.43±1.02.The direction of the dipole is within 138 of the cosmic microwave background (CMB) dipole, the main uncertainty in direction being associated with the masked area behind the Galactic plane. The improbability of further major contributions to the dipole amplitude coming from volumes larger than those surveyed here means that the question of the origin of the CMB dipole is essentially resolved.

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New D — σ Results for Coma Ellipticals

Cited by 7 publications

References 9 publications

Streaming motions of galaxy clusters within 12 000 km s-1 -- I. New spectroscopic data

Streaming motions of galaxy clusters within 12 000 km s-1 -- I. New spectroscopic data

Colour-magnitude relations and spectral line strengths in the Coma cluster

The IRAS PSCz dipole

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