Reshaping the outskirts of planetary systems

Marcos, C. de la Fuente; Marcos, R. de la Fuente

doi:10.1051/0004-6361:20010421

Cited by 86 publications

(118 citation statements)

References 39 publications

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“…The situation is analogous to optical doubles and binary stars. New simulations (de la Fuente Marcos 1997 confirmed early numerical results characterizing OCRs as sparsely populated stellar aggregates, rich in binaries and higher multiplicity systems and poor in low-mass members. Another main conclusion of these simulations was the intrinsically specific stellar content of remnants coming from clusters with very different initial populations.…”

Section: Introductionsupporting

confidence: 71%

Not an open cluster after all: the NGC 6863 asterism in Aquila

Bidin

Marcos

et al. 2010

A&A

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Context. Shortly after birth, open clusters start dissolving; gradually losing stars into the surrounding star field. The time scale for complete disintegration depends both on their initial membership and location within the Galaxy. Open clusters undergoing the terminal phase of cluster disruption or open cluster remnants (OCRs) are notoriously difficult to identify. From an observational point, a combination of low number statistics and minimal contrast against the general stellar field conspire to turn them into very challenging objects. To make the situation even worst, random samples of field stars often display features that may induce to classify them erroneously as extremely evolved open clusters. Aims. In this paper, we provide a detailed study of the stellar content and kinematics of NGC 6863, a compact group of a few stars located in Aquila and described by the Palomar Observatory Sky Survey as a non existent cluster. Nonetheless, this object has been recently classified as OCR. The aim of the present work is to either confirm or disprove its OCR status by a detailed star-by-star analysis. Methods. The analysis is performed using wide-field photometry in the UBVI pass-band, proper motions from the UCAC3 catalogue, and high resolution spectroscopy as well as results from extensive N-body calculations.Results. The spectra of the four brightest stars in this field clearly indicate that they are part of different populations. Their radial velocities are statistically very different and their spectroscopic parallaxes are inconsistent with them being part of a single, bound stellar system. Out of the four stars, only two of them have similar metallicity. The color magnitude diagram for the field of NGC 6863 does not show any clear signature typical of actual open clusters. Consistently, spatial scan statistics confirms the absence of any statistically significant, kinematically supported over-density at the purported location of NGC 6863. Conclusions. Our results show that the four brightest stars commonly associated to NGC 6863 form an asterism, a group of nonphysically associated stars projected together, leading to the conclusion that NGC 6863 is not a real open cluster.

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Section: Introductionsupporting

confidence: 71%

Not an open cluster after all: the NGC 6863 asterism in Aquila

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Marcos

et al. 2010

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“…1 presents this star cluster aggregate (hereafter Perseus 1 cluster aggregate) formed by ECs with similar ages. Such groups were predicted or observed by Efremov (1995); Guillout et al (1998);Fellhauer & Kroupa (2005); de la Fuente Marcos & de la Fuente Marcos (2008, 2009a, 2010Feigelson et al (2011);Camargo et al (2011Camargo et al ( , 2012Camargo et al ( , 2013Camargo et al ( , 2015a. Several large dust emission bubbles in WISE images connect these clusters, suggesting second generation effects (Camargo et al 2015a).…”

Section: Discussionmentioning

confidence: 61%

Tracing the Galactic spiral structure with embedded clusters

Camargo

Bonatto

Bica

2015

Monthly Notices of the Royal Astronomical Society

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In the present work we investigate the properties of 18 embedded clusters (ECs). The sample includes 11 previously known clusters and we report the discovery of 7 ECs on WISE images, thus complementing our recent list of 437 new clusters. The main goal is to use such clusters to shed new light on the Galactic structure by tracing the spiral arms with cluster distances. Our results favour a four-armed spiral pattern tracing three arms, Sagitarius-Carina, Perseus, and the Outer arm. The SagitariusCarina spiral arm is probed in the borderline of the third and fourth quadrants at a distance from the Galactic centre of d 1 ∼ 6.4 kpc adopting R ⊙ = 7.2 kpc, or d 2 ∼ 7.2 kpc for R ⊙ = 8.0 kpc. Most ECs in our sample are located in the Perseus arm that is traced in the second and third quadrants and appear to be at Galactocentric distances in the range d 1 = 9 − 10.5 kpc or d 2 = 9.8 − 11.3 kpc. Dolidze 25, Bochum 2, and Camargo 445 are located in the Outer arm that extends along the second and third Galactic quadrants with a distance from the Galactic centre in the range of d 1 = 12.5 − 14.5 kpc or d 2 = 13.5 − 15.5 kpc. We find further evidence that in the Galaxy ECs are predominantly located within the thin disc and along spiral arms. They are excellent tools for tracing these Galactic features and therefore new searches for ECs can contribute to a better understanding of the Galactic structure. We also report an EC aggregate located in the Perseus arm.

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“…It is necessary to evaluate its evolutionary status through analysis of its density and other related parameters (see Aarseth 1996;de La Fuente Marcos 1997;Kroupa et al 2001) such as the slope of the mass spectrum. It is also routinely used as criteria for separating cluster-dominated from field-dominated regions in photometric diagrams (Baume et al 2004).…”

Section: Cluster Sizesmentioning

confidence: 99%

Open clusters in the Third Galactic Quadrant III. Alleged binary clusters

Vazquez

Moitinho

Carraro³

et al. 2010

A&A

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Aims. We aim to determine accurate distances and ages of eight open clusters in order to: (1) assess their possible binarity (2) provide probes to trace the structure of the Third Galactic Quadrant. Methods. Cluster reddenings, distances, ages and metallicities are derived from ZAMS and isochrone fits in UBVRI photometric diagrams. Field contamination is reduced by restricting analysis to stars within the cluster limits derived from star counts. Further membership control is done by requiring that stars have consistent positions in several diagrams and by using published spectral types. Results. The derived distances, ages and metallicities have shown that none of the analysed clusters compose binary/double systems. Of the four candidate pairs, only NGC 2383/NGC 2384 are close to each other, but have different metallicities and ages. Ruprecht 72 and Ruprecht 158 are not clusters but fluctuations of the field stellar density. Haffner 18 is found to be the superposition of two stellar groups at different distances: Haffner 18(1) at 4.5 kpc and Haffner 18(2) between 9.5 and 11.4 kpc from the Sun. The derived distances and ages have been used to situate the clusters in the Galactic context. In particular, young stellar groups trace spiral structure at large Galactocentric radii. At least two clusters formed during the last few 10 8 yr in an interstellar medium with less than solar abundances. Conclusions. In contrast with the LMC, double clusters are apparently rare, or even non existent, in the undisturbed environment of the Third Galactic Quadrant. This leaves open the question of whether binary clusters form more easily toward denser and more violent regions of the Milky Way such as the inner Galaxy.

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Reshaping the outskirts of planetary systems

Cited by 86 publications

References 39 publications

Not an open cluster after all: the NGC 6863 asterism in Aquila

Not an open cluster after all: the NGC 6863 asterism in Aquila

Tracing the Galactic spiral structure with embedded clusters

Open clusters in the Third Galactic Quadrant III. Alleged binary clusters

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