The halo globular clusters of the giant elliptical galaxy Messier 87

Strom, S. E.; Forte, J. C.; Harris, W. E.; Strom, K. M.; Wells, D. C.; Smith, M.

doi:10.1086/158820

Cited by 80 publications

(84 citation statements)

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“…Most of the positions are taken from Strom et al (1981). We compare the velocities of common objects to determine the systematic offset between the data sets, and to estimate the measurement uncertainties (∆v z ∼ 100 km s −1 ).…”

Section: Globular Cluster Discrete Velocitiesmentioning

confidence: 99%

Dynamics of Stars and Globular Clusters in M87

Romanowsky

Kochanek

2001

ApJ

103

129

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We examine the dynamics of the stars and globular clusters in the nearby giant elliptical galaxy M87 and constrain the mass distribution, using all the available data over a large range of radii, including higher-order moments of the stellar line-of-sight velocity distributions and the discrete velocities of over two hundred globular clusters. We introduce an extension of spherical orbit modeling methods that makes full use of all the information in the data, and provides very robust constraints on the mass models. We conclusively rule out a constant mass-to-light ratio model, and infer that the radial density profile of the galaxy's dark halo falls off more slowly than r −2 , suggesting that the potential of the Virgo Cluster is already dominant at r ∼ 300 ′′ ∼ 20 kpc.

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Section: Globular Cluster Discrete Velocitiesmentioning

confidence: 99%

Dynamics of Stars and Globular Clusters in M87

Romanowsky

Kochanek

2001

ApJ

103

129

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“…In particular, radial density profiles of GCSs and their correlations with physical properties of their host galaxies have been discussed in terms of formation and evolution of elliptical galaxies (e.g., Harris 1986;Zepf & Ashman 1993;Ashman & Zepf 1998;Forbes et al 1996Forbes et al , 1997Bekki et al 2002. In particular, observational studies found that the GCSs in early-type galaxies were less centrally concentrated than the stellar light of the host galaxy (e.g., Harris & Racine 1979;Strom et al 1981;Grillmair et al 1994;Forbes et al 1996), and that the outer slope of the GCS density profile correlated with the host galaxy luminosity (e.g., Ashman & Zepf 1998;Harris 1986).…”

Section: Introductionmentioning

confidence: 99%

On the structure of globular cluster systems in elliptical galaxies

Bekki

Forbes

2005

A&A

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It has long been known that the radial density profiles of globular cluster systems (GCSs) in elliptical galaxies vary with the total luminosities of their host galaxies. In order to elucidate the origin of this structural non-homology in GCSs, we numerically investigate the structural properties of GCSs in elliptical galaxies formed from a sequence of major dissipationless galaxy merging. We find that the radial density profiles of GCSs in elliptical galaxies become progressively flatter as the galaxies experience more major merger events. The density profiles of GCSs in ellipticals are well described as power-laws with slopes (α gc ) ranging from −2.0 to −1.0. They are flatter than, and linearly proportional to, the slopes (α s ) of the stellar density profiles of their host galaxies. We also find that the GCS core radii (r c ) of the density profiles are larger in ellipticals that experienced more mergers. By applying a reasonable scaling relation between luminosities and sizes of galaxies to the simulation results, we show that α gc ≈ −0.36M V − 9.2, r c ≈ −1.85M V , and α gc ≈ 0.93α s , where M V is the total V-band absolute magnitude of a galaxy. We compare these predictions with observations and discuss their physical meaning. We suggest that the origin of structural non-homology of GCSs in ellipticals can be understood in terms of the growth of ellipticals via major dissipationless galaxy merging.

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“…14. The circular velocity was obtained by the mass modeling of Strom et al, (1981) and the r-band magnitude was found by integrating the surface brightness profile of Strom et al, (1981). The result of the method presented by Klypin et al, (2010) is that the Tully-Fisher relation is reproduced without the need for contraction or expansion.…”

Section: The Tully-fisher Zero-point Problemmentioning

confidence: 99%