Metallicities of Old Open Clusters

Friel, Eileen D.; Janes, K. A.; Tavarez, M.; Scott, J. S.; Katsanis, Rocio; Lotz, Jennifer M.; Hong, Linh; Miller, N. A.

doi:10.1086/344161

Cited by 356 publications

(707 citation statements)

References 88 publications

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“…However, not all the investigators have arrived at similar measures of the radial metallicity gradient which may be partly related to the different methods adopted (see for example, Magrini et al 2009;Heiter et al 2014). Our current understanding suggests a gradient of about −0.06 dex kpc −1 (Friel et al 2002;Pancino et al 2010) to −0.20 dex kpc −1 (Frinchaboy et al 2013) in the radial range 5 to 10 kpc with a nearly flat trend (−0.02 dex kpc −1 ) beyond 13 kpc (Carraro et al 2007;Sestito et al 2008;Pancino et al 2010;Yong et al 2012;Frinchaboy et al 2013;Cantat-Gaudin et al 2016).…”

Section: Introductionmentioning

confidence: 85%

“…Abundance gradients in the Milky Way can be measured using a wide variety of tracers including the young population of H ii regions, OB stars, and Cepheid variables, and planetary nebulae of different ages, cool unevolved stars and red giants in the field (see for example, Magrini et al 2010;Cheng et al 2012;Hayden et al 2014) and in open clusters (OCs; Friel et al 2002Friel et al , 2010Magrini et al 2010;Pancino et al 2010;Yong et al 2012;Frinchaboy et al 2013). The cooler main sequence stars or red giants which are members of OCs provide not only abundance estimates for elements sampling all the major processes of stellar nucleosynthesis -but a collection of stars whose age, distance, kinematics and metallicity can be measured with greater certainty than for field stars.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The evolution of the Milky Way: new insights from open clusters

Reddy¹,

Lambert²,

Giridhar³

2016

Mon. Not. R. Astron. Soc.

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We have collected high-dispersion echelle spectra of red giant members in the twelve open clusters (OCs) and derived stellar parameters and chemical abundances for 26 species by either line equivalent widths or synthetic spectrum analyses. We confirm the lack of an age−metallicity relation for OCs but argue that such a lack of trend for OCs arise from the limited coverage in metallicity compared to that of field stars which span a wide range in metallicity and age. We confirm that the radial metallicity gradient of OCs is steeper (flatter) for R gc < 12 kpc (>12 kpc). We demonstrate that the sample of clusters constituting a steep radial metallicity gradient of slope −0.052±0.011 dex kpc −1 at R gc < 12 kpc are younger than 1.5 Gyr and located close to the Galactic midplane (| z| < 0.5 kpc) with kinematics typical of the thin disc. Whereas the clusters describing a shallow slope of −0.015±0.007 dex kpc −1 at R gc > 12 kpc are relatively old, thick disc members with a striking spread in age and height above the midplane (0.5 < | z| < 2.5 kpc). Our investigation reveals that the OCs and field stars yield consistent radial metallicity gradients if the comparison is limited to samples drawn from the similar vertical heights. We argue via the computation of Galactic orbits that all the outer disc clusters were actually born inward of 12 kpc but the orbital eccentricity has taken them to present locations very far from their birthplaces.

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Section: Introductionmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 99%

The evolution of the Milky Way: new insights from open clusters

Reddy¹,

Lambert²,

Giridhar³

2016

Mon. Not. R. Astron. Soc.

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“…As shown in Fig. 10 of their paper, these authors investigated the abundance gradient as a function of time by combining the results derived from OC data by Friel et al (2002), and by Chen et al (2003). The theoretical tracks of Chappini et al (2001) and Hou et al (2000), are also shown, respectively.…”

Section: The Disk Abundance Gradient Based On Open Clustersmentioning

confidence: 98%

Open clusters: their kinematics and metallicities

et al. 2007

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Abstract. We review our work on Galactic open clusters in recent years, and introduce our proposed large program for the LOCS (LAMOST Open Cluster Survey). First, based on the most complete open clusters sample with metallicity, age and distance data as well as kinematic information, some preliminary statistical analysis regarding the spatial and metallicity distributions is presented. In particular, a radial abundance gradient of −0.058± 0.006 dex kpc −1 is derived. By dividing clusters into the age groups we show that the disk abundance gradient was steeper in the past. Secondly, proper motions, membership probabilities, and velocity dis- The open cluster system and the observational databaseOpen clusters (OCs) are considered excellent laboratories for studies of stellar evolution. Studies in the research area dealing with OCs show a rapid growth in 1990's and this area continues to develop vigorously. There may be several reasons for this recent growth of OC studies. New techniques are greatly beneficial to the OC observations, including, for example, the application of wide-field, high quality CCD cameras and, more recently, multi-object spectrographs. In addition, OC studies play a very important and unique role in determining the structure and evolution of the Galactic disk.OCs have long been used to trace the structure and evolution of the Galactic disk. From the observational point of view, there are some important advantages of using OCs as opposed to field stars. In OCs, we deal with groups of stars of nearly the same age, a similar composition and at a similar distance. We can observe OCs to large distances, and the photometric distances to most of the OC sample have already been derived. In particular, OCs have a relatively stable orbital motion, which can be used as a better tracer of the Galactic disk structure. OCs also have a wide range of ages, so that -combined with their spatial distribution and kinematic information -we can study the effects of dynamical evolution. Very young OCs are ideal objects for studies of the stellar initial mass function. Furthermore, when combined with abundance data, we can 433 at https://www.cambridge.org/core/terms. https://doi

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“…References for the data in Columns 7-12 are listed in the last column. Peniche et al (1990), (2) Carraro & Vallenari (2000), (3) Friel et al (2002), (4) Tadross (2003), (5) Park & Lee (1999), (6) Canterna et al (1986), (7) Geisler et al (1991Geisler et al ( , 1992, (8) Friel & Janes (1993), (9) Jacobson et al (2008), (10) Claria et al (1989), (11) Piatti et al (1995), (12) Twarog et al (1997), (13) Carraro et al (2007), (14) Ann et al (2002), (15) Cameron (1985), (16) Claria et al (1999), (17) Table 7. If we are to do a large survey with between 300 and 500 OCs, such comparisons are necessary and useful to evaluate the consistency and quality of the results in the literature, and to provide the offsets between all these different studies, ours and those in the literature.…”

Section: Correlations Of the Interstellar Reddeningsmentioning

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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Metallicities of Old Open Clusters

Cited by 356 publications

References 88 publications

The evolution of the Milky Way: new insights from open clusters

The evolution of the Milky Way: new insights from open clusters

Open clusters: their kinematics and metallicities

CCD UBV(RI)C photometry of twenty open clusters

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