Full metadata record
DC Field | Value | Language |
---|---|---|
dc.contributor.author | 안덕근 | * |
dc.date.accessioned | 2022-06-02T16:31:17Z | - |
dc.date.available | 2022-06-02T16:31:17Z | - |
dc.date.issued | 2022 | * |
dc.identifier.issn | 0067-0049 | * |
dc.identifier.other | OAK-31382 | * |
dc.identifier.uri | https://dspace.ewha.ac.kr/handle/2015.oak/261274 | - |
dc.description.abstract | The Sloan Extension for Galactic Understanding and Exploration 2 (SEGUE-2) obtained 128,288 low-resolution spectra (R ∼1800) of 118,958 unique stars in the first year of the Sloan Digital Sky Survey III (2008-2009). SEGUE-2 targeted prioritized distant halo tracers (blue horizontal-branch stars, K giants, and M giants) and metal-poor or kinematically hot populations. The main goal of SEGUE-2 was to target stars in the distant halo and measure their kinematics and chemical abundances to learn about the formation and evolution of the Milky Way. We present the SEGUE-2 field placement and target selection strategies. We discuss the success rate of the targeting based on the SEGUE-2 spectra and other spectroscopic and astrometric surveys. We describe the final SEGUE-2/SDSS-III improvements to the stellar parameter determinations based on the SEGUE Stellar Parameter Pipeline. We report a (g - i) color-effective temperature relation calibrated to the IRFM. We evaluate the accuracy and uncertainties associated with these stellar parameters by comparing with fundamental parameters, a sample of high-resolution spectra of SEGUE stars analyzed homogeneously, stars in well-studied clusters, and stars observed in common by the APOGEE survey. The final SEGUE spectra, calibration data, and derived parameters described here were released in SDSS-III Data Release 9 and continue to be included in all subsequent SDSS Data Releases. Because of its faint limiting magnitude and emphasis on the distant halo, the public SEGUE-2 data remain an important resource for the spectroscopy of stars in the Milky Way. © 2022. The American Astronomical Society. All rights reserved. | * |
dc.language | English | * |
dc.publisher | American Astronomical Society | * |
dc.title | SEGUE-2: Old Milky Way Stars Near and Far | * |
dc.type | Article | * |
dc.relation.issue | 2 | * |
dc.relation.volume | 259 | * |
dc.relation.index | SCIE | * |
dc.relation.index | SCOPUS | * |
dc.relation.journaltitle | Astrophysical Journal, Supplement Series | * |
dc.identifier.doi | 10.3847/1538-4365/ac5323 | * |
dc.identifier.wosid | WOS:000780053500001 | * |
dc.identifier.scopusid | 2-s2.0-85129071936 | * |
dc.author.google | Rockosi C.M. | * |
dc.author.google | Sun Lee Y. | * |
dc.author.google | Morrison H.L. | * |
dc.author.google | Yanny B. | * |
dc.author.google | Johnson J.A. | * |
dc.author.google | Lucatello S. | * |
dc.author.google | Sobeck J. | * |
dc.author.google | Beers T.C. | * |
dc.author.google | Allende Prieto C. | * |
dc.author.google | An D. | * |
dc.author.google | Bizyaev D. | * |
dc.author.google | Blanton M.R. | * |
dc.author.google | Casagrande L. | * |
dc.author.google | Eisenstein D.J. | * |
dc.author.google | Gould A. | * |
dc.author.google | Gunn J.E. | * |
dc.author.google | Harding P. | * |
dc.author.google | Ivans I.I. | * |
dc.author.google | Jacobson H.R. | * |
dc.author.google | Janesh W. | * |
dc.author.google | Knapp G.R. | * |
dc.author.google | Kollmeier J.A. | * |
dc.author.google | Lépine S. | * |
dc.author.google | López-Corredoira M. | * |
dc.author.google | Ma Z. | * |
dc.author.google | Newberg H.J. | * |
dc.author.google | Pan K. | * |
dc.author.google | Prchlik J. | * |
dc.author.google | Sayers C. | * |
dc.author.google | Schlesinger K.J. | * |
dc.author.google | Simmerer J. | * |
dc.author.google | Weinberg D.H. | * |
dc.contributor.scopusid | 안덕근(8661118800) | * |
dc.date.modifydate | 20240130115827 | * |