Improved spectroscopic parameters for transiting planet hosts
We report homogeneous spectroscopic determinations of the effective temperature, metallicity, and projected rotational velocity for the host stars of 56 transiting planets. Our analysis is based primarily on the stellar parameter classification (SPC) technique. We investigate systematic errors by ex...
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| 格式: | Article |
| 語言: | en_US |
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IOP Publishing
2013
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| 在線閱讀: | http://hdl.handle.net/1721.1/76746 https://orcid.org/0000-0002-4265-047X |
| _version_ | 1826208791616552960 |
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| author | Winn, Joshua Nathan Torres, Guillermo Fischer, Debra A. Sozzetti, Alessandro Buchhave, Lars A. Holman, Matthew J. Carter, Joshua Adam |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Winn, Joshua Nathan Torres, Guillermo Fischer, Debra A. Sozzetti, Alessandro Buchhave, Lars A. Holman, Matthew J. Carter, Joshua Adam |
| author_sort | Winn, Joshua Nathan |
| collection | MIT |
| description | We report homogeneous spectroscopic determinations of the effective temperature, metallicity, and projected rotational velocity for the host stars of 56 transiting planets. Our analysis is based primarily on the stellar parameter classification (SPC) technique. We investigate systematic errors by examining subsets of the data with two other methods that have often been used in previous studies (Spectroscopy Made Easy (SME) and MOOG). The SPC and SME results, both based on comparisons between synthetic spectra and actual spectra, show strong correlations between T [subscript eff], [Fe/H], and log g when solving for all three quantities simultaneously. In contrast the MOOG results, based on a more traditional curve-of-growth approach, show no such correlations. To combat the correlations and improve the accuracy of the temperatures and metallicities, we repeat the SPC analysis with a constraint on log g based on the mean stellar density that can be derived from the analysis of the transit light curves. Previous studies that have not taken advantage of this constraint have been subject to systematic errors in the stellar masses and radii of up to 20% and 10%, respectively, which can be larger than other observational uncertainties, and which also cause systematic errors in the planetary mass and radius. |
| first_indexed | 2024-09-23T14:12:42Z |
| format | Article |
| id | mit-1721.1/76746 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T14:12:42Z |
| publishDate | 2013 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/767462022-10-01T19:46:09Z Improved spectroscopic parameters for transiting planet hosts Winn, Joshua Nathan Torres, Guillermo Fischer, Debra A. Sozzetti, Alessandro Buchhave, Lars A. Holman, Matthew J. Carter, Joshua Adam Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Winn, Joshua Nathan We report homogeneous spectroscopic determinations of the effective temperature, metallicity, and projected rotational velocity for the host stars of 56 transiting planets. Our analysis is based primarily on the stellar parameter classification (SPC) technique. We investigate systematic errors by examining subsets of the data with two other methods that have often been used in previous studies (Spectroscopy Made Easy (SME) and MOOG). The SPC and SME results, both based on comparisons between synthetic spectra and actual spectra, show strong correlations between T [subscript eff], [Fe/H], and log g when solving for all three quantities simultaneously. In contrast the MOOG results, based on a more traditional curve-of-growth approach, show no such correlations. To combat the correlations and improve the accuracy of the temperatures and metallicities, we repeat the SPC analysis with a constraint on log g based on the mean stellar density that can be derived from the analysis of the transit light curves. Previous studies that have not taken advantage of this constraint have been subject to systematic errors in the stellar masses and radii of up to 20% and 10%, respectively, which can be larger than other observational uncertainties, and which also cause systematic errors in the planetary mass and radius. 2013-02-06T16:16:37Z 2013-02-06T16:16:37Z 2012-09 2012-03 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/76746 Torres, Guillermo et al. “Improved Spectroscopic Parameters For Transiting Planet Hosts.” The Astrophysical Journal 757.2 (2012): 161. https://orcid.org/0000-0002-4265-047X en_US http://dx.doi.org/10.1088/0004-637X/757/2/161 Astrophysical Journal Creative Commons Attribution-Noncommercial-Share Alike 3.0 http://creativecommons.org/licenses/by-nc-sa/3.0/ application/pdf IOP Publishing arXiv |
| spellingShingle | Winn, Joshua Nathan Torres, Guillermo Fischer, Debra A. Sozzetti, Alessandro Buchhave, Lars A. Holman, Matthew J. Carter, Joshua Adam Improved spectroscopic parameters for transiting planet hosts |
| title | Improved spectroscopic parameters for transiting planet hosts |
| title_full | Improved spectroscopic parameters for transiting planet hosts |
| title_fullStr | Improved spectroscopic parameters for transiting planet hosts |
| title_full_unstemmed | Improved spectroscopic parameters for transiting planet hosts |
| title_short | Improved spectroscopic parameters for transiting planet hosts |
| title_sort | improved spectroscopic parameters for transiting planet hosts |
| url | http://hdl.handle.net/1721.1/76746 https://orcid.org/0000-0002-4265-047X |
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