Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 858, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/2041-8213/aabf8e
Keywords
methods: data analysis; stars: distances; techniques: spectroscopic
Categories
Funding
- Institute for Advanced Study in Princeton
- Carnegie-Princeton Fellowship from Princeton University
- Carnegie-Princeton Fellowship from Carnegie Observatories
- Australian Research Council [DP160103747]
- Simons Foundation Society of Fellows
- Flatiron Institute Center for Computational Astrophysics in New York City
- European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC Grant [321035]
- DFG [SFB-881]
- National Development and Reform Commission
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Center for High-Performance Computing at the University of Utah
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Core helium-burning red clump (RC) stars are excellent standard candles in the Milky Way. These stars may have more precise distance estimates from spectrophotometry than from Gaia parallaxes beyond 3 kpc. However, RC stars have values of T-eff and log g that are very similar to some red giant branch (RGB) stars. Especially for low-resolution spectroscopic studies where T-eff, log g, and [Fe/H] can only be estimated with limited precision, separating RC stars from RGB through established methods can incur similar to 20% contamination. Recently, Hawkins et al. demonstrated that the additional information in single-epoch spectra, such as the C/N ratio, can be exploited to cleanly differentiate RC and RGB stars. In this second paper of the series, we establish a data-driven mapping from spectral flux space to independently determined asteroseismic parameters, the frequency and the period spacing. From this, we identify 210,371 RC stars from the publicly available LAMOST DR3 and APOGEE DR14 data, with similar to 9% of contamination. We provide an RC sample of 92249 stars with a contamination of only similar to 3%, by restricting the combined analysis to LAMOST stars with S/N-pix >= 75. This demonstrates that high-signal-to-noise ratio (S/N), low-resolution spectra covering a broad wavelength range can identify RC samples at least as pristine as their high-resolution counterparts. As coming and ongoing surveys such as TESS, DESI, and LAMOST will continue to improve the overlapping training spectroscopic-asteroseismic sample, the method presented in this study provides an efficient and straightforward way to derive a vast yet pristine sample of RC stars to reveal the three-dimensional (3D) structure of the Milky Way.
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