DDO Metal Abundances of High-Luminosity Late-Type Stars in Galactic Open Clusters

Clariá, J. J.; Piatti, Andrés E.; Osborn, W.

doi:10.1086/133784

Cited by 21 publications

(24 citation statements)

References 20 publications

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“…(g) Averages of measurements obtained from the Hipparcos parallaxes by van den Heuvel (1969);Maeder (1971); Mathieu & Mazeh (1988); Mazzei & Pigatto (1988); Boesgaard (1989);Tsvetkov (1993); Piatti et al (1995); Claria et al (1996); Hernandez et al (1998); Loktin & Beshenov (2001); Salaris et al (2004); Kraus & Hillenbrand (2007); and Gáspár et al (2009). assumed that log g = 4.437, T eff, = 5770 K and M bol, = 4.75, in conformity with the IAU recommendations (Andersen 1999). As above, we averaged all our estimates to obtain log g (phot) , listed in Col. 5 of Table 4.…”

Section: Referencesmentioning

confidence: 95%

“…(b) Averages of measurements by Johnson (1953);Roman (1955);Johnson (1961); Rohlfs & Vanysek (1962); Arp (1962); Eggen (1963); Crawford & Barnes (1970); Patenaude (1978); Hardy (1979);Nicolet (1981); Twarog (1983); Barry et al (1987);Nissen (1988); Mazzei & Pigatto (1988); Eggen (1989); Francic (1989);Boesgaard (1991); Dzervitis & Paupers (1993);Carraro et al (1993); Meynet et al (1993);Daniel et al (1994); Piatti et al (1995); Dinescu et al (1995); Milone et al (1995); Claria et al (1996); Dutra & Bica (2000); Loktin & Beshenov (2001); Blake (2002); Blake & Rucinski (2004); Salaris et al (2004); Bartašiūtė et al (2007);Taylor (2007); and Giardino et al (2008).…”

Section: Referencesmentioning

confidence: 99%

“…Its metal content was derived with different methods (e.g., Friel & Boesgaard 1992;Komarov & Basak 1993;Claria et al 1996;Hui-Bon-Hoa & Alecian 1998;Burkhart & Coupry 1998, 2000Dias et al 2002;Pace et al 2008). In general, all the quoted studies obtained a metallicity either barely or definitely supersolar.…”

Section: Praesepe (Ngc 2632)mentioning

confidence: 99%

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Chemical abundance analysis of the open clusters Berkeley 32, NGC 752, Hyades, and Praesepe

Carrera

Pancino

2011

A&A

128

139

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Context. Open clusters are ideal test particles for studying the chemical evolution of the Galactic disc. However, the number and accuracy of existing high-resolution abundance determinations, not only of [Fe/H], but also of other key elements, remains largely insufficient. Aims. We attempt to increase the number of Galactic open clusters that have high quality abundance determinations, and to gather all the literature determinations published so far. Methods. Using high-resolution (R ∼ 30 000), high-quality (S /N ≥ 60 per pixel), we obtained spectra for twelve stars in four open clusters with the fibre spectrograph FOCES, at the 2.2 Calar Alto Telescope in Spain. We employ a classical equivalent-width analysis to obtain accurate abundances of sixteen elements: Al, Ba, Ca, Co, Cr, Fe, La, Mg, Na, Nd, Ni, Sc, Si, Ti, V, and Y. We derived oxygen abundances by means of spectral synthesis of the 6300 Å forbidden line. Results. We provide the first determination of abundance ratios other than Fe for NGC 752 giants, and ratios in agreement with the literature for the Hyades, Praesepe, and Be 32. We use a compilation of literature data to study Galactic trends of [Fe/H] and [α/Fe] with Galactocentric radius, age, and height above the Galactic plane. We find no significant trends, but some indication for a flattening of [Fe/H] at large R gc , and for younger ages in the inner disc. We also detect a possible decrease in [Fe/H] with |z| in the outer disc, and a weak increase in [α/Fe] with R gc .

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Section: Referencesmentioning

confidence: 95%

Section: Referencesmentioning

confidence: 99%

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Chemical abundance analysis of the open clusters Berkeley 32, NGC 752, Hyades, and Praesepe

Carrera

Pancino

2011

A&A

128

139

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“…We recalculated the metallicity based on the remaining two stars with the reddening and calibration used by Twarog et al (1997). We also noticed a typo in the star list for Stock 2 by Claria et al (1996), HD 13209 is actually HD 13207 and a radial velocity member of the cluster.…”

Section: Photometric Metallicitiesmentioning

confidence: 98%

On the metallicity of open clusters

Netopil

Paunzen

Heiter

et al. 2016

A&A

205

243

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Context. Open clusters are known as excellent tools for various topics in Galactic research. For example, they allow accurately tracing the chemical structure of the Galactic disc. However, the metallicity is known only for a rather low percentage of the open cluster population, and these values are based on a variety of methods and data. Therefore, a large and homogeneous sample is highly desirable. Aims. In the third part of our series we compile a large sample of homogenised open cluster metallicities using a wide variety of different sources. These data and a sample of Cepheids are used to investigate the radial metallicity gradient, age effects, and to test current models. Methods. We used photometric and spectroscopic data to derive cluster metallicities. The different sources were checked and tested for possible offsets and correlations. Results. In total, metallicities for 172 open cluster were derived. We used the spectroscopic data of 100 objects for a study of the radial metallicity distribution and the age-metallicity relation. We found a possible increase of metallicity with age, which, if confirmed, would provide observational evidence for radial migration. Although a statistical significance is given, more studies are certainly needed to exclude selection effects, for example. The comparison of open clusters and Cepheids with recent Galactic models agrees well in general. However, the models do not reproduce the flat gradient of the open clusters in the outer disc. Thus, the effect of radial migration is either underestimated in the models, or an additional mechanism is at work. Conclusions. Apart from the Cepheids, open clusters are the best tracers for metallicity over large Galactocentric distances in the Milky Way. For a sound statistical analysis, a sufficiently large and homogeneous sample of cluster metallicities is needed. Our compilation is currently by far the largest and provides the basis for several basic studies such as the statistical treatment of the Galactic cluster population, or evolutionary studies of individual star groups in open clusters.

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“…; (4) Gustafsson et al (1974); (5) Claria et al (1996); (6) Boesgaard (1987); (7) Friel & Boesgaard (1992); (8) Cayrel et al (1988); (9) Gebran et al (2008). For the sake of discussion, we searched for simple correction terms to the expressions of Ramirez & Melendez (2005) and McWilliams (1990) that would remove the differences between them and with χ 2 temperatures.…”

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confidence: 99%

A spectroscopic survey of faint, high-Galactic-latitude red clump stars

Valentini

Munari

2010

A&A

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Context. Their high intrinsic brightness and small dispersion in absolute magnitude make red clump (RC) stars a prime tracer of Galactic structure and kinematics. Aims. We aim to derive accurate, multi-epoch radial velocities and atmospheric parameters (T eff , log g, [M/H], V rot sin i) of a large sample of carefully selected RC stars, fainter than those present in other spectroscopic surveys and located over a great circle at high Galactic latitudes. Methods. We acquired data of the program stars of high signal-to-noise ratio (S/N) and high resolution with the Asiago Echelle spectrograph. Radial velocities were obtained by applying cross-correlation and atmospheric parameters via χ 2 fit to a synthetic spectral library. Extensive tests were carried out by re-observing with the same instrument a large number of standard stars taken from a variety of sources in the literature. During these tests, we found that the absolute Tycho V T magnitude of local red clump stars is not dependent on metallicity Results. A total of 277 red clump stars (101 of them with a second epoch observation) of the extended solar neighborhood and 55 calibration stars were observed and included in an output catalog that contains (in addition to relevant support astrometric and photometric data taken from literature) the main output of our survey: accurate multi-epoch radial velocities (σ(RV) ≤ 0.4 km s −1 ), accurate atmospheric parameters (σ(T eff ) = 68 K, σ(log g) = 0.11 dex, σ([M/H]) = 0.10 dex, σ(V rot sin i) = 1.1 km s −1 ), distances, and space velocities (U, V, W).

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DDO Metal Abundances of High-Luminosity Late-Type Stars in Galactic Open Clusters

Cited by 21 publications

References 20 publications

Chemical abundance analysis of the open clusters Berkeley 32, NGC 752, Hyades, and Praesepe

Chemical abundance analysis of the open clusters Berkeley 32, NGC 752, Hyades, and Praesepe

On the metallicity of open clusters

A spectroscopic survey of faint, high-Galactic-latitude red clump stars

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