Star cluster disruption by giant molecular clouds

Gieles, M.; Zwart, Simon F. Portegies; Baumgardt, Holger; Athanassoula, E.; Lamers, H. J. G. L. M.; Sipior, M.; Leenaarts, J.

doi:10.1111/j.1365-2966.2006.10711.x

Cited by 261 publications

(329 citation statements)

References 35 publications

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“…To first order this is probably due to our small sample plus our selection procedure, and the interstellar extinction, which is very strong mainly in these directions. But also, this is partly due to the high frequency of encounters with Giant Molecular Clouds (GMCs) inside the Solar circle, as discussed by Gieles et al (2006) and Camargo et al (2009), which tends to reduce the relative number of OCs. A |z| versus R GC plot is displayed in Fig.…”

Section: Spatial Distribution Of 20 Ocsmentioning

confidence: 99%

CCD UBV(RI)C photometry of twenty open clusters

Oralhan¹,

Karataş²,

Schuster³

et al. 2015

New Astronomy

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Fundamental astrophysical parameters have been derived for 20 open clusters (OCs) using CCD UBV(RI) C photometric data observed with the 84 cm telescope at the San Pedro Mártir National Astronomical Observatory, México.The interstellar reddenings, metallicities, distances, and ages have been compared to the literature values. Significant differences are usually due to the usage of diverse empirical calibrations and differing assumptions, such as concerning cluster metallicity, as well as distinct isochrones which correspond to differing element-abundance ratios, internal stellar physics, and photometric systems. Different interstellar reddenings, as well as varying reduction and cluster-membership techniques, are also responsible for these kinds of systematic differences and errors.The morphological ages, which are derived from the morphological indices (δV and δ1) in the CM diagrams, are in good agreement with the isochrone ages of 12 OCs, those with good red clump (RC) and red giant (RG) star candidates. No metal abundance gradient is detected for the range 6.82 ≤ R GC ≤ 15.37 kpc, nor any correlation between the cluster ages and metal abundances for these 20 OCs.Young, metal-poor OCs, observed here in the third Galactic quadrant, may be associated with stellar over-densities, such as that in Canis Major (Martin et al.) and the Monoceros Ring (Newberg et al.), or signatures of past accretion events, as discussed by Yong et al. and Carraro et al.

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Section: Spatial Distribution Of 20 Ocsmentioning

confidence: 99%

CCD UBV(RI)C photometry of twenty open clusters

Oralhan¹,

Karataş²,

Schuster³

et al. 2015

New Astronomy

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show abstract

“…Theoretically, disruption should depend on the cluster's initial mass and its environment, with clusters in weaker tidal fields or higher masses surviving longer (e.g. Baumgardt & Makino 2003;Gieles et al 2006c). However, empirical studies have resulted in two separate theories for the disruption process.…”

Section: Cluster Disruptionmentioning

confidence: 99%

Properties of the cluster population of NGC 1566 and their implications

Hollyhead

Adamo

Bastian

et al. 2016

Mon. Not. R. Astron. Soc.

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We present results of a photometric study into the cluster population of NGC 1566, a nearby grand design spiral galaxy, sampled out to a Galactocentric radius of ≈ 5.5 kpc. The shape of the mass-limited age distribution shows negligible variation with radial distance from the centre of the galaxy, and demonstrates three separate sections, with a steep beginning, flat middle and steep end. The luminosity function can be approximated by a power law at lower luminosities with evidence of a truncation at higher luminosity. The power law section of the luminosity function of the galaxy is best fitted by an index ≈ −2, in agreement with other studies, and is found to agree with a model luminosity function, which uses an underlying Schechter mass function. The recovered power law slope of the mass distribution shows a slight steepening as a function of galactocentric distance, but this is within error estimates. It also displays a possible truncation at the high mass end. Additionally, the cluster formation efficiency (Γ) and the specific U-band luminosity of clusters (T L (U )) are calculated for NGC 1566 and are consistent with values for similar galaxies. A difference in NGC 1566, however, is that the fairly high star formation rate is in contrast with a low Σ SF R and Γ, indicating that Γ can only be said to depend strongly on Σ SF R , not the star formation rate.

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“…The disruption scenarios and the survival rates of Galactic OCs have been studied since the sixties (Spitzer & Harm 1958;. Recently, Nbody simulations (e.g., Gieles et al 2006;Gieles & Baumgardt 2008) have also shown the impact of giant molecular clouds and of the initial structure of OCs on their dissolution. The OC orbits have generally small eccentricities and they tend to be located at a small height (Z) on the Galactic plane, as a consequence they are expected to pass many times trough the Galactic disk.…”

Section: Introductionmentioning

confidence: 99%

Evidence of tidal distortions and mass-loss from the old open cluster NGC 6791

Dalessandro

Miocchi

Carraro³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present the first evidence of clear signatures of tidal distortions in the density distribution of the fascinating open cluster NGC 6791. We used deep and wide-field data obtained with the Canada-France-Hawaii-Telescope covering a 2 • ×2 • area around the cluster. The two-dimensional density map obtained with the optimal matched filter technique shows a clear elongation and an irregular distribution starting from ∼ 300 ′′ from the cluster center. At larger distances, two tails extending in opposite directions beyond the tidal radius are also visible. These features are aligned to both the absolute proper motion and to the Galactic center directions. Moreover, other overdensities appear to be stretched in a direction perpendicular to the Galactic plane.Accordingly to the behaviour observed in the density map, we find that both the surface brightness and the star count density profiles reveal a departure from a King model starting from ∼ 600 ′′ from the center.These observational evidence suggest that NGC 6791 is currently experiencing mass loss likely due to gravitational shocking and interactions with the tidal field. We use this evidence to argue that NGC 6791 should have lost a significant fraction of its original mass. A larger initial mass would in fact explain why the cluster survived so long. Using available recipes based on analytic studies and N -body simulations, we derived the expected mass loss due to stellar evolution and tidal interactions and estimated the initial cluster mass to be M ini = (1.5-4) × 10 5 M ⊙ .

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Star cluster disruption by giant molecular clouds

Cited by 261 publications

References 35 publications

CCD UBV(RI)C photometry of twenty open clusters

CCD UBV(RI)C photometry of twenty open clusters

Properties of the cluster population of NGC 1566 and their implications

Evidence of tidal distortions and mass-loss from the old open cluster NGC 6791

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