Visible and Near Infrared Atlas of the Arcturus Spectrum 3727-9300 A

By K. Hinkle, L. Wallace, J. Valenti, D. Harmer. 2000

208 citations recorded by the source corpus.

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Citations in the corpus

• Spectral models for solar-scaled and α-enhanced stellar populations (2007, result): “Hinkle et al. 2000), we found that the synthetic indices were underestimated (as expected from the lack of N-LTE line profile calculation, see e.g. Cayrel et al. 1996), but the differences were typically 3 times smaller than the difference shown in Fig.”
• Multiwavelength Observations of Flares on AD Leonis (2003, methodology): “Spectra themselves were reduced in a standard way using software written in the IDL programing language and described by Hinkle et al. (2000).”
• New algorithms for reducing cross-dispersed echelle spectra (2002, methodology): “BERP evolved from procedures described in Valenti (1994), adding support for several spectrographs and implementing a form of optimal extraction inspired by Piskunov (1995).”
• A purely geometric distance to the binary star Atlas, a member of the Pleiades (2004, background): “Dottedline: spectrum observed in 1995 near quadrature, at phaseφ ∼ 0.1. trum of telluric lines provided by Hinkle et al. (2000) togeth r with their visible atlas of the Arcturus spectrum.”
• The GALAH Survey: Second Data Release (2018, background): “Figure 5) of the lines from Hinkle et al. (2000), indicated as blue regions, to measure element abundances.”
• Abundances in Stars from the Red Giant Branch Tip to Near the Main-Sequence Turnoff in M71. III. Abundance Ratios (2001, background): “However, the C i lines in stars with Teff d 4200 K may be blended with or completely dominated by lines from the red system of CN, as illustrated in the spectrum of Arcturus by Hinkle et al. (2000).”
• Transiting exoplanets from the CoRoT space mission . VI. CoRoT-Exo-3b: the first secure inhabitant of the brown-dwarf desert (2008, methodology): “We used 192 mostly non-blended lines and the abundances were calculated relative to the solar spectrum from Hinkle et al. (2000), following the approach by Bruntt et al. (2008).”
• Accurate fundamental parameters for 23 bright solar-type stars (2010, background): “Our reference spectrum was taken from the book by Hinkle et al. (2000) (published in original form by Kurucz et al. 1984).”
• A Two Micron All Sky Survey View of the Sagittarius Dwarf Galaxy. II. Swope Telescope Spectroscopy of M Giant Stars in the Dynamically Cold Sagittarius Tidal Stream (2004, methodology): “The choice of lines was guided by the stellar atmosphere studies of metal-poor stars (similar to that expected of the candidates) of Gratton & Sneden (1988), McWilliam et al. (1995), and Ramı́rez & Cohen (2003) and included those spectral lines that, when compared with the same lines in the…”
• THE INFRARED TELESCOPE FACILITY (IRTF) SPECTRAL LIBRARY: COOL STARS (2009, unknown): “5 III, Hinkle et al. 1995, 2000).”
• Chemical similarities between Galactic bulge and local thick disk red giants: O, Na, Mg, Al, Si, Ca, and Ti (2010, background): “Although both Fulbright et al. (2007) and Lecureur et al. (2007) used the giants Arcturus ([Fe/H] ∼ −0.5) andµ Leo ([Fe/H] ∼+0.3) as reference stars, their zero-points are ultimately based on the Sun8, which as shown in Table 3, may be inadequate for the study of giants.”