Metallicities of Old Open Clusters

By E. Friel, K. Janes, M. Tavarez, Jennifer E. Scott, Rocio M. Katsanis, J. Lotz, L. N. Hong, Nathan D Miller. 2002

292 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

THE SEGUE STELLAR PARAMETER PIPELINE. V. ESTIMATION OF ALPHA-ELEMENT ABUNDANCE RATIOS FROM LOW-RESOLUTION SDSS/SEGUE STELLAR SPECTRA (2010, unknown): “…the overall metallicity of NGC 2420 derived by Pancino et al. (2010) in Table 3 is relatively higher (by about 0.3 to 0.4 dex) than other studies (e.g., Friel & Janes 1993; Friel et al. 2002; Anthony-Twarog et al. 2006), which are based on medium-resolution spectra or intermediate-band photometry.”
THE SEGUE STELLAR PARAMETER PIPELINE. II. VALIDATION WITH GALACTIC GLOBULAR AND OPEN CLUSTERS (2007, background): “Friel et al. (2002) determined [Fe/H] = −0.38 ± 0.07, based on medium-resolution spectra of 20 member stars.”
A Gaia DR2 view of the open cluster population in the Milky Way (2018, background): “…et al. 2005; Bragaglia & Tosi 2006; Carrera & Pancino 2011; Netopil et al. 2016; Casamiquela et al. 2017) and its evolution through time (e.g. Friel et al. 2002; Magrini et al. 2009; Yong et al. 2012; Frinchaboy et al. 2013; Jacobson et al. 2016), providing insight on the formation of the…”
The Gaia-ESO Survey : radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk (2014, background): “Open clusters and planetary nebulae also provide information about older populations (Friel et al. 2002; Stanghellini & Haywood 2010; Yong et al. 2012; Heiter et al. 2014): open clusters up to 8−9 Gyr and planetary nebulae up to 6 Gyr (Maciel et al. 2010).”
The Victoria-Regina Stellar Models: Evolutionary Tracks and Isochrones for a Wide Range in Mass and Metallicity that Allow for Empirically Constrained Amounts of Convective Core Overshooting (2005, background): “Based on their extensive moderate-resolution spectra (for many open clusters), Friel et al. (2002) concluded that NGC 6819 is about 0.04 dex more metal rich than M67, implying an ½Fe/H 0:0.”
Homogeneous Photometry. III. A Star Catalog for the Open Cluster NGC 6791 (2003, unknown): “Still more recently, Friel et al. (2002) have derived a metallicity of [Fe/H] p based upon spectroscopy of 39 cluster0.”
Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682) (2009, methodology): “We corrected Friel et al. (2002) data by this amount before plotting them.”
Astrophysical supplements to the ASCC‐2.5: Ia. Radial velocities of ∼55000 stars and mean radial velocities of 516 Galactic open clusters and associations (2007, background): “An other big project carried out by Friel (1989), Friel & Janes (1993), Friel et al. (2002), Friel, Liu & Janes (1989), Thorgersen, Friel & Fallon (1993) provided physical parameters, includingRVs, of 28 old open clusters.”
On the metallicity of open clusters. III. Homogenised sample (2015, methodology): “We note that the tabulated [Fe/H] values by Warren & Cole (2009) are on a different scale than those by the other two references because they used the results by Friel et al. (2002) for the metal-rich regime to calibrate W ′.”
The evolution of the Galactic metallicity gradient from high-resolution spectroscopy of open clusters (2008, methodology): “…a slope for the cumulative sample of −0.067 dex kpc−1, and for only the old bin of −0.079 dex kpc−1, in closer agreement with their results: −0.075 dex kpc−1 for the sample of Chen et al. (2003) with ages >0.8 Gyr and −0.075 dex kpc−1 for the sample of Friel et al. (2002) with ages >4 Gyr.”
OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, background): “Present-day elemental abundance gradients with Galactocentric distance for both oxygen and iron have been observed (e.g., Deharveng et al. 2000; Friel et al. 2002; Jacobson et al. 2007; Henry et al. 2010), implying that radial migration provides a way to explain the range of elemental abundances…”
The local surface density of disc matter mapped by Hipparcos (2004, background): “…the validity of a clear age-metallicity relation has now been put into question by most modern investigations (Feltzing, Holmberg, & Hurley 2001; Friel et al. 2002; Nordström et al. 2004), as well as already noted by FF; the evidence for the high metallicity cut as a means of excluding the…”
Isochrone ages for field dwarfs: method and application to the age–metallicity relation (2004, background): “The indication from older open clusters is more ambiguous (Twarog 1980; Piatti, Claria & Abadi 1995; Carraro et al. 1998; Friel et al. 2002), showing a large scatter that can be mostly attributed to a radial metallicity gradient.”
Galactic Metallicity Gradients Derived from a Sample of OB Stars (2004, methodology): “Observational indication that the gradients flatten with time was presented in Friel et al. (2002) and also in Chen, Hou, & Wang (2003), based on analyses of open cluster metallicities.”
Analysis and calibration of CaII triplet spectroscopy of red giant branch stars from VLT/FLAMES observations (2007, methodology): “These previous studies all calibrated the CaT W ′ on the CG97 scale, and Friel et al. (2002) for the open clusters, meaning that the relation between [Fe/H] and W ′ has been derived assuming that the calibration clusters have the metallicities derived by CG97.”
Riding the Spiral Waves: Implications of Stellar Migration for the Properties of Galactic Disks (2008, background): “However, evidence suggests that a large amount of scatter is present in the AMR of field stars (Edvardsson et al. 1993; Nordström et al. 2004) and open clusters (Friel et al. 2002), meaning that stars of the same age are observed to have a wide range of metallicities.”
The age of the oldest Open Clusters (2003, methodology): “This is the opposite as found by Friel et al. (2002) who determined a steeper gradient for clusters older than 3 Gyr, with respect to younger objects.”
Stellar population gradients in galaxy discs from the CALIFA survey - The influence of bars (2014, background): “Flatter abundance gradients in the younger population are also found in the Milky Way (Friel et al. 2002; Chen et al. 2003; Maciel et al. 2003; Daflon & Cunha 2004), although recent results by Maciel & Costa (2013) do not detect variations in the slope of the metallicity gradient measured in planeta”