Catalogue of Galactic globular-cluster surface-brightness profiles

Trager, S. C.; King, Ivan R.; Djorgovski, S. G.

doi:10.1086/117268

Cited by 453 publications

(721 citation statements)

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“…This feature has been attributed to a post-core collapse structure in some globular clusters (e.g. Trager et al 1995). Such a dynamical evolutionrelated feature 11 has also been detected in the RDP of some Gyr-old OCs, e.g.…”

Section: Cluster Structurementioning

confidence: 71%

The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters

Bonatto

Bica

2010

A&A

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Context. Close investigations of unstudied open-cluster candidates may improve the statistics of objects undergoing the dissolution phase. Aims. We plan to settle the nature and derive astrophysical (fundamental, structural, and stellar mass content) parameters for 34 unstudied open cluster candidates from the near-infrared Teutsch list. Methods. The analysis employs 2MASS photometry, field-star decontamination (to enhance the intrinsic colour-magnitude diagram morphology), and colour-magnitude filters (for high contrast in stellar radial density profiles). Results. We find 8 clusters younger than ∼30 Myr, 21 with ages within 100-900 Myr, 3 older than 1 Gyr, and possibly 1 as old as ∼7 Gyr. Part of the sample is affected by reddening as high as A V ∼ 9, and about half is located more than d ∼ 3 kpc away from the Sun, with a few reaching d = 6−9 kpc. The sample contains essentially low-luminosity clusters in the optical, with M V ≈ −3 ± 3. These properties are consistent with their near-infrared origin. Cluster size increases both with Galactocentric distance and height over the plane, which is consistent with the low level of tidal stress (and field contamination) associated with these regions. The average mass density falls off with cluster radius as ρ ∼ R −3 , which in clusters younger than ∼20 Myr and more massive than ∼10 3 M has been interpreted as diffusion-related cluster expansion. Conclusions. Besides the derivation of astrophysical parameters for a sample of unstudied open clusters, in this paper we identify a set of clusters older than several 10 2 Myr, with 4 of them having survived a few Gyr. Surveys of open cluster candidates should be further explored to fill in the gap between the detected and predicted number of clusters. An improved statistic, especially on the population of clusters in highly evolved phases, can be used to investigate cluster formation rates and constrain the dissolution-time scale in the Galaxy.

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Section: Cluster Structurementioning

confidence: 71%

The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters

Bonatto

Bica

2010

A&A

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“…The variations due to the 1σ confidence intervals lie within the thickness of the line. The dots with error bars show the collection of observed surface brightness measurements from Trager et al (1995) for NGC 288, which are clearly well represented by the best fit parameters and the MONDian dynamical model used. For comparison, the dashed line gives the best fit model for β = 0.3, which is appreciably less of a good fit, the slight offset and the many observed points available allow its rejection at a 1σ level.…”

Section: Mondian Isothermal Model For Ngc 288mentioning

confidence: 77%

MONDian dynamical modelling of NGC 288 with β ≠ 0

Hernández

Cortés

Scarpa

2016

Mon. Not. R. Astron. Soc.

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NGC 288 is a diffuse Galactic globular cluster, it is remarkable in that its low density results in internal accelerations being below the critical MOND a 0 acceleration throughout. This makes it an ideal testing ground for MONDian gravity, as the details of the largely unknown transition function between the Newtonian and modified regimes become unimportant. Further, exact analytical solutions exist for isothermal spherical equilibrium structures in MOND, allowing for arbitrary values of the anisotropy parameter, β. In this paper we use observations of the velocity dispersion profile of NGC 288, which is in fact isothermal, as dynamical constraints on MONDian models for this cluster, where the remaining free parameters are adjusted to fit the observed surface brightness profile. We find the optimal fit requires β = 0, an isotropic solution with a total mass of 3.5 ± 1.1 × 10 4 M ⊙ .

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“…1 For example, M 4, our target, shows no evidence for any central brightness cusp (Trager et al 1995), despite the fact that its age (∼ 1 Gyr, Bedin et al 2009) exceeds its present central relaxation time (∼ 0.08 Gyr, Harris 1996, as updated in 2010 by a factor ∼ 150. Can the lack of evidence of core collapse be traced to the presence of a large fraction of binaries?…”

Section: For Reviews)mentioning

confidence: 85%

The M 4 Core Project with HST: I. Overview and first epoch

et al. 2013

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We present an overview of the ongoing Hubble Space Telescope large program GO-12911. The program is focused on the core of M 4, the nearest Galactic globular cluster, and the observations are designed to constrain the number of binaries with massive companions (black holes, neutron stars, or white dwarfs) by measuring the "wobble" of the luminous (mainsequence) companion around the center of mass of the pair, with an astrometric precision of ∼ 50 μas. The high spatial resolution and stable medium-band PSFs of WFC3/UVIS will make these measurements possible. In this work we describe (i) the motivation behind this study, (ii) our observing strategy, (iii) the many other investigations enabled by this unique data set, and which of those our team is conducting, and (iv) a preliminary reduction of the first-epoch dataset collected on

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Catalogue of Galactic globular-cluster surface-brightness profiles

Cited by 453 publications

References 1 publication

The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters

The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters

MONDian dynamical modelling of NGC 288 with β ≠ 0

The M 4 Core Project with HST: I. Overview and first epoch

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