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http://hdl.handle.net/2445/161881
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DC Field | Value | Language |
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dc.contributor.author | Liu, C. | - |
dc.contributor.author | Bailer-Jones, C.A.L. | - |
dc.contributor.author | Sordo, R. | - |
dc.contributor.author | Vallenari, A. | - |
dc.contributor.author | Borrachero, Raúl | - |
dc.contributor.author | Luri Carrascoso, Xavier | - |
dc.contributor.author | Sartoretti, Paola | - |
dc.date.accessioned | 2020-05-21T08:27:45Z | - |
dc.date.available | 2020-05-21T08:27:45Z | - |
dc.date.issued | 2012-11-01 | - |
dc.identifier.issn | 0035-8711 | - |
dc.identifier.uri | http://hdl.handle.net/2445/161881 | - |
dc.description.abstract | Gaia will obtain astrometry and spectrophotometry for essentially all sources in the sky down to a broad band magnitude limit of G=20, an expected yield of 10^9 stars. Its main scientific objective is to reveal the formation and evolution of our Galaxy through chemo-dynamical analysis. In addition to inferring positions, parallaxes and proper motions from the astrometry, we must also infer the astrophysical parameters of the stars from the spectrophotometry, the BP/RP spectrum. Here we investigate the performance of three different algorithms (SVM, ILIUM, Aeneas) for estimating the effective temperature, line-of-sight interstellar extinction, metallicity and surface gravity of A-M stars over a wide range of these parameters and over the full magnitude range Gaia will observe (G=6-20mag). One of the algorithms, Aeneas, infers the posterior probability density function over all parameters, and can optionally take into account the parallax and the Hertzsprung-Russell diagram to improve the estimates. For all algorithms the accuracy of estimation depends on G and on the value of the parameters themselves, so a broad summary of performance is only approximate. For stars at G=15 with less than two magnitudes extinction, we expect to be able to estimate Teff to within 1%, logg to 0.1-0.2dex, and [Fe/H] (for FGKM stars) to 0.1-0.2dex, just using the BP/RP spectrum (mean absolute error statistics are quoted). Performance degrades at larger extinctions, but not always by a large amount. Extinction can be estimated to an accuracy of 0.05-0.2mag for stars across the full parameter range with a priori unknown extinction between 0 and 10mag. Performance degrades at fainter magnitudes, but even at G=19 we can estimate logg to better than 0.2dex for all spectral types, and [Fe/H] to within 0.35dex for FGKM stars, for extinctions below 1mag. | - |
dc.format.extent | 20 p. | - |
dc.format.mimetype | application/pdf | - |
dc.language.iso | eng | - |
dc.publisher | Royal Astronomical Society | - |
dc.relation.isformatof | Reproducció del document publicat a: https://doi.org/10.1111/j.1365-2966.2012.21797.x | - |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society, 2012, vol. 426, num. 3, p. 2463-2482 | - |
dc.relation.uri | https://doi.org/10.1111/j.1365-2966.2012.21797.x | - |
dc.rights | (c) Liu, C. et al., 2012 | - |
dc.source | Articles publicats en revistes (Física Quàntica i Astrofísica) | - |
dc.subject.classification | Estels | - |
dc.subject.classification | Espectrofotometria | - |
dc.subject.classification | Astrometria | - |
dc.subject.other | Stars | - |
dc.subject.other | Spectrophotometry | - |
dc.subject.other | Astrometry | - |
dc.title | The expected performance of stellar parametrization with Gaia spectrophotometry | - |
dc.type | info:eu-repo/semantics/article | - |
dc.type | info:eu-repo/semantics/publishedVersion | - |
dc.identifier.idgrec | 615694 | - |
dc.date.updated | 2020-05-21T08:27:45Z | - |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | - |
Appears in Collections: | Articles publicats en revistes (Física Quàntica i Astrofísica) |
Files in This Item:
File | Description | Size | Format | |
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615694.pdf | 3.38 MB | Adobe PDF | View/Open |
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