Dissolving star cluster candidates

Bica, E.; Santiago, B.; Dutra, Carlos Maximiliano; Dottori, H.; Oliveira, M. R. de; Pavani, Daniela Borges

doi:10.1051/0004-6361:20000248

Cited by 50 publications

(99 citation statements)

References 23 publications

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“…De la Fuente Marcos (1998) has shown that our Galaxy should host several hundreds of thousands of open cluster remnants which have been disrupted by the Galaxy and by their own dynamical evolution (evaporation). Bica et al (2001) indeed observe several dissolving star cluster candidates.…”

Section: Introductionmentioning

confidence: 78%

Gravitational tidal effects on galactic open clusters

Bergond

Léon

Guibert

2001

A&A

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Abstract.We have investigated the 2-D stellar distribution in the outer parts of three nearby open clusters: NGC 2287 (≡M 41), NGC 2516, and NGC 2548 (≡M 48). Wide-field star counts have been performed in two colours on pairs of digitized ESO and SRC Schmidt plates, allowing us to select likely cluster members in the colour-magnitude diagrams. Cluster tidal extensions were emphasized using a wavelet transform. Taking into account observational biases, namely the galaxy clustering and differential extinction in the Galaxy, we have associated these stellar overdensities with real open cluster structures stretched by the galactic gravitational field. As predicted by theory and simulations, and despite observational limitations, we detected a general elongated (prolate) shape in a direction parallel to the galactic Plane, combined with tidal tails extended perpendicularly to it. This geometry is due both to the static galactic tidal field and the heating up of the stellar system when crossing the Disk. The time varying tidal field will deeply affect the cluster dynamical evolution, and we emphasize the importance of adiabatic heating during the Disk-shocking. In the case of NGC 2548, our dating of the last shocking with the Plane (based on a tidal clump) is consistent with its velocity. During the 10-20 Z-oscillations experienced by a cluster before its dissolution in the Galaxy, crossings through the galactic Disk contribute to at least 15% of the total mass loss. Using recent age estimations published for open clusters, we find a destruction time-scale of about 600 Myr for clusters in the solar neighbourhood.

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Section: Introductionmentioning

confidence: 78%

Gravitational tidal effects on galactic open clusters

Bergond

Léon

Guibert

2001

A&A

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“…An XDSS (second generation Digitized Sky Survey) blow-up of the concentration was shown in Fig. 4 of Bica et al (2001). We emphasize that the present set of stars related to the concentration is not BT's set of members.…”

Section: Introductionmentioning

confidence: 84%

“…Bassino et al (2000) find evidence of a possible remnant -M 73 (NGC 6994), but Carraro (2000) does not favour it. Bica et al (2001) presented 34 dissolving star cluster candidates which are located at relatively high galactic latitudes (|b| > 15 • ) and are underpopulated with respect to usual open clusters, but they possess a significant number density contrast as compared to the Galactic field. The distinction between an open cluster and a remnant is not obvious both observationally and theoretically.…”

Section: Introductionmentioning

confidence: 99%

“…NGC 1252 was discussed in Bica et al (2001), who refer to a stellar concentration at the southwest edge of Bouchet & Thé's (1983) definition of NGC 1252, which is a sparse collection of stars in a much larger field. NGC 1252 is described in the NGC as a star cluster containing 18 or 20 stars.…”

Section: Introductionmentioning

confidence: 99%

“…CCD photometry is obtained for NGC 1252 as in Bica et al (2001) at α = 3 h 10 m 49 s , δ = −57 • 46 00 (l = 274.…”

Section: Introductionmentioning

confidence: 99%

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Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Pavani

Bica

Dutra

et al. 2001

A&A

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Abstract. Photometry in the B and V bands is presented for the southern stellar groups NGC 1901 and NGC 1252. NGC 1901 is often described as an open cluster while NGC 1252 consists of a concentration of about 20 stars centered ≈20 north of the original New General Catalogue coordinates, and at the southwest edge of the large region previously assigned to this object in the literature. NGC 1901 has a clear main sequence and shares similarities with the Hyades. We derive a reddening value E(B −V ) = 0.04, a distance from the Sun d = 0.45 kpc (Z = −0.23 kpc) and an age 0.6 ± 0.1 Gyr. NGC 1901 is conclusively a physical system, dynamically comparable to or more evolved than the Hyades. The colour-magnitude diagram of NGC 1252 suggests a turnoff and main sequence, and a total of 12 probable members. We simulated the Galactic field colour-magnitude diagram in the same direction and found it to be a poor match to NGC 1252, suggesting that NGC 1252 is not a field fluctuation. Isochrone fitting to the probable members is consistent with E(B − V ) = 0.02, d = 0.64 kpc (Z = −0.46 kpc) and an age 3 ± 1 Gyr. NGC 1252 cannot be ruled out as a physical group with the available data. If so, evidence is found that it is not a classical open cluster, but rather an open cluster remnant.

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Characterization of Open Cluster Remnants

Pavani

Bica

2009

Globular Clusters - Guides to Galaxies

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Dissolving star cluster candidates

Cited by 50 publications

References 23 publications

Gravitational tidal effects on galactic open clusters

Gravitational tidal effects on galactic open clusters

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Characterization of Open Cluster Remnants

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