Spectroscopic Binaries, Velocity Jitter, and Rotation in Field Metal-poor Red Giant and Red Horizontal-Branch Stars

By B. Carney, D. Latham, R. Stefanik, J. B. Laird, J. Morse. 2003

139 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d93aa1dba99cb3d985cbd72a692511ab978b6122

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In Astronomy and Astrophysics

1. Timothy C. Beers
2. C. Sneden
3. D. Schneider
4. A. Frebel
5. Martin Asplund
6. J. Norris
7. J. Brinkmann
8. J. Cowan

In Instrumentation

1. Timothy C. Beers
2. C. Sneden
3. A. Frebel
4. D. Schneider
5. J. Norris
6. E. Carretta
7. J. Cowan
8. R. Gratton

Citations in the corpus

• ROTATIONAL AND RADIAL VELOCITIES FOR A SAMPLE OF 761 HIPPARCOS GIANTS AND THE ROLE OF BINARITY (2007, methodology): “Second, we note that we do not see as much excess line broadening for the most luminous stars in our sample in contrast to the result found by Carney et al. (2003) for a metal-poor sample of red giants.”
• Binarity in carbon-enhanced metal-poor stars (2014, methodology): “This would be in agreement with claims that binarity is generallyhigher in lower metallicity populations (e.g. Carney et al. 2003).”
• Multiple populations in globular clusters (2012, methodology): “The benchmark sample is presently the Carretta et al. (2009b) one, with homogeneous abundances of O, Na, Mg, Al, and Si for more than 200 RGB stars in 19 globular clusters, based on high-resolution UVES spectra.”
• The Rise of the s-Process in the Galaxy (2004, background): “G 095-57A , G 095-57B (Tomkin & Lambert 1999) and HD 135148 (Shetrone et al. 1999; Carney et al. 2003).”
• The Binary Frequency Among Carbon-enhanced, s-Process-rich, Metal-poor Stars (2004, background): “This value is somewhat larger than the spectroscopic binary frequency measured by Carney et al. (2003), ∼17% for metal-poor field stars.”
• Abundances In Very Metal-Poor Dwarf Stars (2004, background): “Latham et al. (2002) and Carney et al. (2003) find no difference in the binary frequency they establish for moderately metal poor halo populations compared to that of nearby more metal-rich populations; the formal frequency of spectroscopic binaries and multiple systems per target is 17.0±1.0%.”
• THE MOST METAL-POOR STARS. IV. THE TWO POPULATIONS WITH [Fe/H] ≲ −3.0 (2012, background): “Of the other stars in our Table 1, we are aware of detailed observations of only BD+44◦493, which was extensively monitored for variations by Carney et al. (2003).”
• Stellar SEDs from 0.3 to 2.5 μm: Tracing the Stellar Locus and Searching for Color Outliers in the SDSS and 2MASS (2007, result): “Corrected for the sparse sampling of the study (most objects were only observed twice), Pourbaix et al. (2005) derive a total spectroscopic binary fraction of 18%, consistent with the findings of a similar study of halo stars by Carney et al. (2003).”
• A Multicolor and Fourier Study of RR Lyrae Variables in the Globular Cluster NGC 5272 (M3) (2004, background): “In this respect we note that Carney et al. (2003) detected line broadening, that was interpreted as a sign of rotation, among luminous RGB and red HB stars in the field, and a similar behavior was found among luminous red giants in M3 by Carney et al. (2004).”
• A SEARCH FOR STARS OF VERY LOW METAL ABUNDANCE. VI. DETAILED ABUNDANCES OF 313 METAL-POOR STARS (2014, methodology): “For these stars, we list the systemic velocity as determined by Preston & Sneden (2000, 2001), Latham et al. (2002), Carney et al. (2003), Sneden et al. (2003), Pourbaix et al. (2004), or Roederer et al. (2014).”
• The Close Binary Fraction of Solar-type Stars Is Strongly Anticorrelated with Metallicity (2018, methodology): “Of all the metal-poor giants with companions across P=35–104 days, we calculate that 55% would have been detected as SBs by Carney et al. (2003) at the >5σ significance level.”