Old open clusters as key tracers of Galactic chemical evolution

Bragaglia, A.; Sestito, P.; Villanova, S.; Carretta, E.; Randich, S.; Tosi, M.

doi:10.1051/0004-6361:20077904

Cited by 89 publications

(114 citation statements)

References 53 publications

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“…The turn-off masses of these clusters are about 2 M (Sestito et al 2006;Bragaglia et al 2008). This mass range has previously not been well covered, therefore these clusters are suitable targets in which to study the dispersion of abundances that might be caused by rotation-induced mixing in stars of similar mass and evolutionary status.…”

Section: Introductionmentioning

confidence: 99%

“…The lowresolution spectroscopy performed by Friel et al (2002) gave [Fe/H] = −0.13±0.10. The high-resolution spectroscopic metallicity value is [Fe/H] = 0.07 ± 0.03 (Bragaglia et al 2008).…”

Section: Introductionmentioning

confidence: 99%

“…More recently, Piatti et al (2004) used V Ic and Washington photometry to derive an age of about 440 Myr, a distance of 3.8 kpc, reddening 0.25, and metallicity of about −0.30 dex. The analysis of low-resolution spectra reported by Friel et al (2002) provided [Fe/H]=−0.15 ± 0.16, while the analysis of high-resolution spectra, which we use here, has been performed by Bragaglia et al (2008) and produced [Fe/H]=−0.17 ± 0.05.…”

Section: Introductionmentioning

confidence: 99%

“…This mass range has previously not been well covered, therefore these clusters are suitable targets in which to study the dispersion of abundances that might be caused by rotation-induced mixing in stars of similar mass and evolutionary status. We analyse part of the same spectra as used by Sestito et al (2006) and Bragaglia et al (2008) in their studies. Investigations of NGC 2324 have begun with Cuffey (1941), who built a colour-magnitude diagram and estimated a distance of about 3320 parsecs.…”

Section: Introductionmentioning

confidence: 99%

“…The photometric metallicity deter- minations range from [Fe/H] = −0.68 (determined by Geisler et al 1992 using Washington photometry) to −0.06 dex by Piatti et al 1998, who used DDO photometry. Based on low-resolution spectra, Friel & Janes (1993) (2006) for NGC 3960 (also adopted by Bragaglia et al 2008). v sin i values were derived in this work.…”

Section: Introductionmentioning

confidence: 99%

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CNO abundances and carbon isotope ratios in evolved stars of the open clusters NGC 2324, NGC 2477, and NGC 3960

Tautvaišienė

Drazdauskas

Bragaglia

et al. 2016

A&A

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Aims. Our main aim is to determine carbon-to-nitrogen and carbon isotope ratios for evolved giants in the open clusters NGC 2324, NGC 2477, and NGC 3960, which have turn-off masses of about 2 M , and to compare them with predictions of theoretical models. Methods. High-resolution spectra were analysed using a differential synthetic spectrum method. Abundances of carbon were derived using the C 2 Swan (0,1) band heads at 5135 and 5635.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

CNO abundances and carbon isotope ratios in evolved stars of the open clusters NGC 2324, NGC 2477, and NGC 3960

Tautvaišienė

Drazdauskas

Bragaglia

et al. 2016

A&A

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A dynamical evolution study of 40 2MASS open clusters

2017

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We investigate the dynamical evolution of 40 open clusters (OCs) by means of their astrophysical parameters derived from field-decontaminated 2MASS photometry. We find a bifurcation in the planes' core radius versus age and cluster radius versus age, in which part of the clusters appear to expand with time probably due to the presence of stellar black holes while others seem to shrink due to dynamical relaxation. Mass functions (MFs) are built for three-fourth of the sample (31 OCs), which are used to search for indications of mass segregation and external dynamical processes by means of relations between astrophysical, structural, and evolutionary parameters. We detect a flattening of MF slopes occurring at the evolutionary parameters core ≤ 32 and overall ≤ 30, respectively. Within the uncertainties involved, the overall MF slopes of 14 out of 31 OCs with m overall > 500 M ⊙ are consistent with Kroupa's initial mass function, implying little, or no dynamical evolution for these clusters. The remaining 17 OCs with MF slopes departing from that of Kroupa show mild/large-scale mass segregation due to dynamical evolution. KEYWORDS CCD 2 MASS photometry -open clusters and associations -stars1

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Outer Regions of the Milky Way

Figueras¹

2017

Astrophysics and Space Science Library

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With the start of the Gaia era, the time has come to address the major challenge of deriving the star formation history and evolution of the disk of our Milky Way. Here we review our present knowledge of the outer regions of the Milky Way disk population. Its stellar content, its structure and its dynamical and chemical evolution are summarized, focussing on our lack of understanding both from an observational and a theoretical viewpoint. We describe the unprecedented data that Gaia and the upcoming ground-based spectroscopic surveys will provide in the next decade. More in detail, we quantify the expect accuracy in position, velocity and astrophysical parameters of some of the key tracers of the stellar populations in the outer Galactic disk. Some insights on the future capability of these surveys to answer crucial and fundamental issues are discussed, such as the mechanisms driving the spiral arms and the warp formation. Our Galaxy, the Milky Way, is our cosmological laboratory for understanding the process of formation and evolution of disk galaxies. What we learn in the next decades will be naturally transferred to the extragalactic domain.

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Old open clusters as key tracers of Galactic chemical evolution

Cited by 89 publications

References 53 publications

CNO abundances and carbon isotope ratios in evolved stars of the open clusters NGC 2324, NGC 2477, and NGC 3960

CNO abundances and carbon isotope ratios in evolved stars of the open clusters NGC 2324, NGC 2477, and NGC 3960

A dynamical evolution study of 40 2MASS open clusters

Outer Regions of the Milky Way

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