Elemental Abundance Ratios in Stars of the Outer Galactic Disk. I. Open Clusters

By David Yong, B. Carney, Maria Luísa Teixera de Almeida. 2005

185 citations recorded by the source corpus.

We summarize radial velocity studies of selected stars in the old, distant clusters Berkeley 20, Berkeley 21, NGC 2141, Berkeley 29, and Berkeley 31. Cluster members are identified using optical and infrared color-magnitude diagrams, as well as radial velocities derived from high-resolution echelle spectra. Three members of M67 were observed similarly, and those velocities compare extremely well with prior measures. Mean cluster radial velocities are determined. We also employ the highest quality spectra to analyze the chemical compositions of all six clusters for [Fe/H], as well as abundances of α-elements, iron-peak elements, and those synthesized in either the s-process or the r-process. In Be 21 our observed star is found to be rotating rapidly and overabundant in lithium, the second Li-rich star found in this sparse cluster. We confirm the lack of correlation between abundance and age. For the outer disk, the abundance gradient for [Fe/H] deviates from the trend defined near the solar neighborhood. Rather than declining with increasing galactocentric distance, [Fe/H] appears to reach a "basement" at [Fe/H] ≈ -0.5 beyond RGC ≈ 10–12 kpc. Our radial abundance distribution for [Fe/H] is not inconsistent with the radial abundance discontinuity exhibited by Cepheids. We find enhanced [O/Fe], [α/Fe], and [Eu/Fe] in the outer disk, revealing a rapid star formation history. The outer disk also exhibits enhancements for s-process elements. We compare the open cluster compositions with those of the thin disk, thick disk, halo, bulge, and dwarf spheroidal galaxies. None of these stellar populations perfectly matches the abundance ratios of the outer disk open clusters. Several key points arise from these comparisons: (1) [O/Fe] and [α/Fe] resemble those of the thick disk. (2) [Na/Fe] and [Al/Fe] are enhanced relative to those of the thin disk. (3) [Ni/Fe] and [Mn/Fe] are in accord with those of the thin disk, while [Co/Fe] may be slightly enhanced. (4) The neutron-capture elements indicate different ratios of s-process to r-process material, with no cluster showing a pure r-process distribution. (5) An unusual pattern exists among the α-elements, with [⟨Mg + Ti⟩/Fe] enhanced while [⟨Si + Ca⟩/Fe] is normal. Similar abundance ratios have been reported for Galactic bulge giants and indicate a common but not necessarily shared nucleosynthetic history between the bulge and the outer disk. Enhanced ratios of [Al/Fe] and [Co/Fe] offer another possible similarity between the bulge and the outer disk. An intriguing but tentative conclusion is that the outer disk open cluster abundance ratios are consistent with the outer disk being formed via a merger event or series of merger events. The basement in [Fe/H] and enhanced [α/Fe] suggest that the outer disk formed from a reservoir of gas with a star formation history distinct from the solar neighborhood. That the open clusters may be associated with an accreted dwarf galaxy or galaxies is appealing, since the clusters are young and have [α/Fe] ratios indicating a rapid star formation history. However, the high [α/Fe] ratios are unlike those seen in any current dwarf galaxies at the same [Fe/H]. Therefore, the open clusters may have formed as a result of star formation triggered by a merger event or series of mergers in the outer disk. The ages of the outer disk open clusters would then be a measure of when the merger(s) occurred. However, Be 29 is a candidate merger member, while Be 31 is not. One problem with the merger scenario is that open clusters with presumably very different origins have similar and unusual compositions.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Radial mixing and the transition between the thick and thin Galactic discs (2008, background): “Carney et al. (2005) and Yong et al. (2005) find that the metallicity of thin disc stars decreases towards the outer disc to reach a constant value of [Fe/H]≈-0.6 dex 2-4 kpc beyond the solar circle.”
A FIRST CONSTRAINT ON THE THICK DISK SCALE LENGTH: DIFFERENTIAL RADIAL ABUNDANCES IN K GIANTS AT GALACTOCENTRIC RADII 4, 8, AND 12 kpc (2011, background): “The outer disk is comparatively well studied, especially using red giants in open clusters (e.g., Yong et al. 2005; Jacobson et al. 2011, and references therein), and to very large RG indeed (> 20kpc, Carraro et al. 2007).”
THE SEGUE STELLAR PARAMETER PIPELINE. II. VALIDATION WITH GALACTIC GLOBULAR AND OPEN CLUSTERS (2007, methodology): “A value of [Fe/H] = +0.02 ± 0.03 was determined by Yong et al. (2005) from a high-resolution (R ∼ 28,000) spectroscopic analysis of three member stars.”
Three-dimensional hydrodynamical simulations of surface convection in red giant stars: impact on spectral line formation and abundance analysis (2007, methodology): “Red giants are also used to study Galactic metallicity gradients in the Galactic disk and open clusters (Yong et al. 2005; Carney et al. 2005) and star-to-star elemental abundance variations within globular clusters (for a review, see Gratton et al. 2004).”
A Gaia DR2 view of the open cluster population in the Milky Way (2018, background): “…in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/618/A93 Yong et al. 2005; Bragaglia & Tosi 2006; Carrera & Pancino 2011; Netopil et al. 2016; Casamiquela et al. 2017) and its evolution through time (e.g.…”
A Spectroscopic Study of the Ancient Milky Way: F- and G-Type Stars in the Third Data Release of the Sloan Digital Sky Survey (2005, background): “We note that the metallicity gradient of the thin disk may disappear beyond R 10 12 kpc (Twarog et al. 1997; Yong et al. 2005), and in that regime the observed abundance ratios show a more complicated behavior than what is observed in the solar neighborhood (Yong et al. 2005).”
The Distribution of the Elements in the Galactic Disk (2006, background): “These are the Yong et al. (2005) study of distant open clusters and, especially, the Yong et al. (2006) study of distant Cepheids.”
The evolution of the Galactic metallicity gradient from high-resolution spectroscopy of open clusters (2008, methodology): “…et al. (2007) NGC 2243 4.7 10.76 Friel et al. (2002) 100 30 000 2, gia EW −0.48 ± 0.15 Gratton & Contarini (1994) Be75 5.1 15.50 Carraro et al. (2007)∗ 25–40 40 000 1, gia EW −0.22 ± 0.20 Carraro et al. (2007) Be31 5.2 12.02 Friel et al. (2002) 100 28 000 5, gia EW −0.57 ± 0.23 Yong et al. (2005)…”
Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682) (2009, background): “…Hamdani et al. (2000) –0.18 Yong et al. (2005) +0.04 Smiljanic et al. (2008) –0.31 Sestito et al. (2008) NGC 2420 –0.57 Smith & Suntzeff (1987) Be 31 –0.40 Yong et al. (2005) NGC 2447 +0.03 Hamdani et al. (2000) Be 32 –0.29 Bragaglia et al. (2008) NGC 2477+0.07 Bragaglia et al. (2008) Be 66…”