A High-Resolution Spectrum of the Extremely Metal-rich Bulge G Dwarf OGLE-2006-BLG-265

@article{Johnson2007AHS,
  title={A High-Resolution Spectrum of the Extremely Metal-rich Bulge G Dwarf OGLE-2006-BLG-265},
  author={Jennifer A. Johnson and Avishay Gal-yam and Douglas C. Leonard and Joshua D. Simon and Andrzej Udalski and A. Gould},
  journal={The Astrophysical Journal Letters},
  year={2007},
  volume={655},
  pages={L33 - L36}
}
We present an R = 45,000 Keck spectrum of the microlensed Galactic bulge G dwarf OGLE-2006-BLG-265, which has high (~60) signal-to-noise ratio despite its short (15 minute) exposure time, because the source was magnified by A ~ 135. While it is very metal-rich ([Fe/H] = 0.56), the higher temperature of this star compared with the luminous red giants usually measured in the bulge gives its spectrum many unblended atomic lines. We measure the abundances of 17 elements, including the first… 
A High-Resolution Spectrum of the Highly Magnified Bulge G Dwarf MOA-2006-BLG-099S
We analyze a high-resolution spectrum of a microlensed G dwarf in the Galactic bulge, acquired when the star was magnified by a factor of 110. We measure a spectroscopic temperature, derived from the
Clues to the Metallicity Distribution in the Galactic Bulge: Abundances in OGLE-2007-BLG-349S
We present an abundance analysis based on high-dispersion and high signal-to-noise ratio Keck spectra of a very highly microlensed Galactic bulge dwarf, OGLE-2007-BLG-349S, with Teff ∼ 5400 K. The
CHEMICAL COMPOSITION OF FAINT (I ∼ 21 mag) MICROLENSED BULGE DWARF OGLE-2007-BLG-514S
We present a high-resolution spectrum of a microlensed G dwarf in the Galactic bulge with spectroscopic temperature Teff = 5600 ± 180 K. This I ∼ 21 mag star was magnified by a factor ranging from
OGLE-2009-BLG-076S: THE MOST METAL-POOR DWARF STAR IN THE GALACTIC BULGE
Measurements based on a large number of red giant stars suggest a broad metallicity distribution function (MDF) for the Galactic bulge, centered on [Fe/H] ≈ −0.1. However, recently, a new opportunity
The metallicity distribution of bulge clump giants in Baade’s window
Aims. We seek to constrain the formation of the Galactic bulge by analysing the detailed chemical composition of a large sample of red clump stars in Baade’s window. These stars were selected to
LIGHT, ALPHA, AND Fe-PEAK ELEMENT ABUNDANCES IN THE GALACTIC BULGE
We present radial velocities and chemical abundances of O, Na, Mg, Al, Si, Ca, Cr, Fe, Co, Ni, and Cu for a sample of 156 red giant branch stars in two Galactic bulge fields centered near (l, b) =
The age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way
Abstract The four main findings about the age and abundance structure of the Milky Way bulge based on microlensed dwarf and subgiant stars are: (1) a wide metallicity distribution with distinct peaks
Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars
Lithium abundances are presented for 91 dwarf and subgiant stars in the Galactic bulge. The analysis is based on line synthesis of the 7Li line at 6707 Å in high-resolution spectra obtained during
Abundances in Galactic Bulge Dwarfs and the Origin of the Elements in the Bulge
c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. The Galactic Bulge has a very different chemical evolution history than the
...
...

References

SHOWING 1-10 OF 33 REFERENCES
Abundances of Baade’s Window Giants from Keck HIRES Spectra. I. Stellar Parameters and [Fe/H] Values
We present the first results of a new abundance survey of the Milky Way bulge based on Keck HIRES spectra of 27 K giants in the Baade's Window (l = 1°, b = -4°) field. The spectral data used in this
Detailed Analysis of Nearby Bulgelike Dwarf Stars. III. α-Element and Heavy-Element Abundances
The present sample of nearby bulgelike dwarf stars has kinematics and metallicities characteristic of a probable inner disk or bulge origin. Ages derived by using isochrones give 10-11 Gyr for these
Detailed Analysis of Nearby Bulgelike Dwarf Stars. I. Stellar Parameters, Kinematics, and Oxygen Abundances
High-resolution échelle spectra were obtained with the Fiber-fed Extended Range Optical Spectrograph at the 1.5 m ESO telescope for 35 nearby bulgelike stars with metallicities in the range -0.8 ≤
Detection of Lithium in a Main-Sequence Bulge Star Using Keck I as a 15 Meter Diameter Telescope
The bulge contains the most chemically evolved old stellar population in the Milky Way. Thanks to microlensing, it is now possible to obtain high-resolution echelle spectra of bulge stars near the
Chemical Abundances of Old Metal-rich Stars in the Solar Neighborhood
We report on chemical abundances for 15 old metal-rich stars in the solar neighborhood based on high-resolution, high signal-to-noise ratio observations. It is found that [O/Fe], [S/Fe], and probably
Primordial Lithium: Keck Observations in M92 Turnoff Stars
We present new Keck I/HIRES observations at R = 45,000 (=3 pixels) of seven stars near the turnoff of the old, metal-poor globular cluster M92. In three of these stars, we have signal-to-noise ratios
Elemental abundance survey of the Galactic thick disc
We have performed an abundance analysis for F- and G- dwarfs of the Galactic thick-disc component. A sample of 176 nearby (d≤ 150 pc) thick-disc candidate stars was chosen from the Hipparcos
A Jovian-Mass Planet in Microlensing Event OGLE-2005-BLG-071
We report the discovery of a several-Jupiter-mass planetary companion to the primary lens star in microlensing event OGLE-2005-BLG-071. Precise (≲1%) photometry at the peak of the event yields an
OGLE-2003-BLG-262: Finite-Source Effects from a Point-Mass Lens
We analyze OGLE-2003-BLG-262, a relatively short (tE = 12.5 ± 0.1 day) microlensing event generated by a point-mass lens transiting the face of a K giant source in the Galactic bulge. We use the
Oxygen trends in the Galactic thin and thick disks
We present oxygen abundances for 72 F and G dwarf stars in the solar neighbourhood. Using the kinematics of the stars we divide them into two sub-samples with space velocities that are typical for
...
...