Browsing by Author "Smith, Verne V."

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    Chemical Abundances of Main-sequence, Turnoff, Subgiant, and Red Giant Stars from APOGEE Spectra. I. Signatures of Diffusion in the Open Cluster M67
    (2018) Souto, Diogo; Cunha, Katia; Smith, Verne V.; Allende Prieto, C.; Garcia-Hernandez, D. A.; Pinsonneault, Marc; Holzer, Parker; Frinchaboy, Peter; Holtzman, Jon; Johnson, J. A.; Jonsson, Henrik; Majewski, Steven R.; Shetrone, Matthew; Sobeck, J
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    Disk-like Chemistry of the Triangulum-Andromeda Overdensity as Seen by APOGEE
    (IOP PUBLISHING LTD, 2018) Hayes, Christian R.; Majewski, Steven R.; Hasselquist, Sten; Beaton, Rachael L.; Cunha, Katia; Smith, Verne V.; Price Whelan, Adrian M.; Anguiano, Borja; Beers, Timothy C.; Carrera, Ricardo; Fernandez Trincado, J. G.; Frinchaboy, Peter M.; Garcia Hernandez, D. A.; Lane, Richard R.; Nidever, David L.; Nitschelm, Christian; Roman Lopes, Alexandre; Zamora, Olga
    The nature of the Triangulum-Andromeda (TriAnd) system has been debated since the discovery of this distant, low-latitude Milky Way (MW) overdensity more than a decade ago. Explanations for its origin are either as a halo substructure from the disruption of a dwarf galaxy, or a distant extension of the Galactic disk. We test these hypotheses using the chemical abundances of a dozen TriAnd members from the Sloan Digital Sky Survey-IV's (SDSS-IV's) 14th Data Release (DR14) of Apache Point Observatory Galactic Evolution Experiment (APOGEE) data to compare to APOGEE abundances of stars with similar metallicity from both the Sagittarius (Sgr) dSph and the outer MW disk. We find that TriAnd stars are chemically distinct from Sgr across a variety of elements, (C+N), Mg, K, Ca, Mn, and Ni, with a separation in [X/Fe] of about 0.1 to 0.4 dex depending on the element. Instead, the TriAnd stars, with a median metallicity of about -0.8, exhibit chemical abundance ratios similar to those of the lowest metallicity ([Fe/H] similar to-0.7)stars in the outer Galactic disk, and are consistent with expectations of extrapolated chemical gradients in the outer disk of the MW. These results suggest that TriAnd is associated with the MW disk, and, therefore, that the disk extends to this overdensity-i.e., past a Galactocentric radius of 24 kpc -albeit vertically perturbed about 7 kpc below the nominal disk midplane in this region of the Galaxy.
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    Timing the Evolution of the Galactic Disk with NGC 6791: An Open Cluster with Peculiar High-alpha Chemistry as Seen by APOGEE
    (IOP PUBLISHING LTD, 2017) Linden, Sean T.; Pryal, Matthew; Hayes, Christian R.; Troup, Nicholas W.; Majewski, Steven R.; Andrews, Brett H.; Beers, Timothy C.; Carrera, Ricardo; Cunha, Katia; Fernandez Trincado, J. G.; Frinchaboy, Peter; Geisler, Doug; Lane, Richard R.; Nitschelm, Christian; Pan, Kaike; Allende Prieto, Carlos; Roman Lopes, Alexandre; Smith, Verne V.; Sobeck, Jennifer; Tang, Baitian; Villanova, Sandro; Zasowski, Gail
    We utilize elemental-abundance information for Galactic red giant stars in five open clusters (NGC 7789, NGC 6819, M67, NGC 188, and NGC 6791) from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) DR13 data set to age-date the chemical evolution of the high- and low-alpha element sequences of the Milky Way (MW). Key to this time-stamping is the cluster NGC 6791, whose stellar members have mean abundances that place it in the high-alpha, high-[Fe/H] region of the [alpha/Fe]-[Fe/H] plane. Based on the cluster's age (similar to 8 Gyr), Galactocentric radius, and height above the Galactic plane, as well as comparable chemistry reported for APOGEE stars in Baade's Window, we suggest that the two most likely origins for NGC 6791 are as an original part of the thick disk, or as a former member of the Galactic bulge. Moreover, because NGC 6791 lies at the high-metallicity end ([Fe/H] similar to 0.4) of the high-alpha sequence, the age of NGC 6791 places a limit on the youngest age of stars in the high-metallicity, high-alpha sequence for the cluster's parent population (i.e., either the bulge or the disk). In a similar way, we can also use the age and chemistry of NGC 188 to set a limit of similar to 7 Gyr on the oldest age of the low-alpha sequence of the MW. Therefore, NGC 6791 and NGC 188 are potentially a pair of star clusters that bracket both the timing and the duration of an important transition point in the chemical history of the MW.