Full metadata record
DC Field | Value | Language |
---|---|---|
dc.contributor.author | 안덕근 | * |
dc.date.accessioned | 2016-08-28T12:08:14Z | - |
dc.date.available | 2016-08-28T12:08:14Z | - |
dc.date.issued | 2011 | * |
dc.identifier.issn | 0004-6256 | * |
dc.identifier.other | OAK-7318 | * |
dc.identifier.uri | https://dspace.ewha.ac.kr/handle/2015.oak/221396 | - |
dc.description.abstract | We present a method for the determination of [α/Fe] ratios from low-resolution (R = 2000) SDSS/SEGUE stellar spectra. By means of a star-by-star comparison with degraded spectra from the ELODIE spectral library and with a set of moderately high-resolution (R = 15, 000) and medium-resolution (R = 6000) spectra of SDSS/SEGUE stars, we demonstrate that we are able to measure [α/Fe] from SDSS/SEGUE spectra (with S/N>20/1) to a precision of better than 0.1 dex, for stars with atmospheric parameters in the range T eff = [4500, 7000] K, log g = [1.5, 5.0], and [Fe/H] = [-1.4, +0.3], over the range [α/Fe] = [-0.1, +0.6]. For stars with [Fe/H] <-1.4, our method requires spectra with slightly higher signal-to-noise to achieve this precision (S/N>25/1). Over the full temperature range considered, the lowest metallicity star for which a confident estimate of [α/Fe] can be obtained from our approach is [Fe/H] -2.5; preliminary tests indicate that a metallicity limit as low as [Fe/H] -3.0 may apply to cooler stars. As a further validation of this approach, weighted averages of [α/Fe] obtained for SEGUE spectra of likely member stars of Galactic globular clusters (M15, M13, and M71) and open clusters (NGC2420, M67, and NGC6791) exhibit good agreement with the values of [α/Fe] from previous studies. The results of the comparison with NGC6791 imply that the metallicity range for the method may extend to +0.5. © 2011. The American Astronomical Society. All rights reserved. | * |
dc.language | English | * |
dc.title | The SEGUE stellar parameter Pipeline. V. estimation of alpha-element abundance ratios from low-resolution SDSS/SEGUE stellar spectra | * |
dc.type | Article | * |
dc.relation.issue | 3 | * |
dc.relation.volume | 141 | * |
dc.relation.index | SCI | * |
dc.relation.index | SCIE | * |
dc.relation.index | SCOPUS | * |
dc.relation.journaltitle | Astronomical Journal | * |
dc.identifier.doi | 10.1088/0004-6256/141/3/90 | * |
dc.identifier.wosid | WOS:000287231000021 | * |
dc.identifier.scopusid | 2-s2.0-79953062348 | * |
dc.author.google | Lee Y.S. | * |
dc.author.google | Beers T.C. | * |
dc.author.google | Prieto C.A. | * |
dc.author.google | Lai D.K. | * |
dc.author.google | Rockosi C.M. | * |
dc.author.google | Morrison H.L. | * |
dc.author.google | Johnson J.A. | * |
dc.author.google | An D. | * |
dc.author.google | Sivarani T. | * |
dc.author.google | Yanny B. | * |
dc.contributor.scopusid | 안덕근(8661118800) | * |
dc.date.modifydate | 20240130115827 | * |