{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2023,10,19]],"date-time":"2023-10-19T05:21:32Z","timestamp":1697692892484},"reference-count":25,"publisher":"Wiley","issue":"6","license":[{"start":{"date-parts":[[2008,7,22]],"date-time":"2008-07-22T00:00:00Z","timestamp":1216684800000},"content-version":"vor","delay-in-days":21,"URL":"http:\/\/onlinelibrary.wiley.com\/termsAndConditions#vor"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Astron Nachr"],"published-print":{"date-parts":[[2008,7]]},"abstract":"<jats:title>Abstract<\/jats:title><jats:p>The spectroscopic analysis of systems with transiting planets gives strong constraints on planetary masses and radii as well as the chemical composition of the systems. The properties of the system OGLE\u2010TR\u201010 are not well\u2010constrained, partly due to the discrepancy of previous measurements of the effective temperature of the host star.<\/jats:p><jats:p>This work, which is fully independent from previous works in terms of data reduction and analysis, uses the H<jats:italic>\u03b1<\/jats:italic> profile in order to get an additional constraint on the effective temperature. We take previously published <jats:italic>UVES<\/jats:italic> observations which have the highest available signal\u2010to\u2010noise ratio for OGLE\u2010TR\u201010. A proper normalization to the relative continuum is done using intermediate data products of the reduction pipeline of the UVES spectrograph. The effective temperature then is determined by fitting synthetic H<jats:italic>\u03b1<\/jats:italic> profiles to the observed spectrum.<\/jats:p><jats:p>With a result of <jats:italic>T<\/jats:italic><jats:sub>eff<\/jats:sub> = 6020 \u00b1 140 K, the H<jats:italic>\u03b1<\/jats:italic> profile clearly favours one of the previous measurements. The H<jats:italic>\u03b1<\/jats:italic> line is further consistent with dwarf\u2010like surface gravities as well as solar and super\u2010solar metallicities previously derived for OGLE\u2010TR\u201010.The H<jats:italic>\u03b1<\/jats:italic> line could not be used to its full potential, partly because of the varying shape of the UVES \u00e9chelle orders after flat field correction. We suggest to improve this feature when constructing future spectrographs. (\u00a9 2008 WILEY\u2010VCH Verlag GmbH &amp; Co. KGaA, Weinheim)<\/jats:p>","DOI":"10.1002\/asna.200710969","type":"journal-article","created":{"date-parts":[[2008,7,22]],"date-time":"2008-07-22T10:37:17Z","timestamp":1216723037000},"page":"573-578","source":"Crossref","is-referenced-by-count":2,"title":["New constraints from the H<i>\u03b1<\/i> line for the temperature of the transiting planet host star OGLE\u2010TR\u201010"],"prefix":"10.1002","volume":"329","author":[{"given":"M.","family":"Ammler\u2010von Eiff","sequence":"first","affiliation":[]},{"given":"N.C.","family":"Santos","sequence":"additional","affiliation":[]}],"member":"311","published-online":{"date-parts":[[2008,7,22]]},"reference":[{"key":"e_1_2_1_2_1","unstructured":"Ammler M.:2006a Characterisation of Young Nearby Stars \u2013 The Ursa Major group Der Verkannten Verlag Berlin"},{"key":"e_1_2_1_3_1","unstructured":"Ammler M.:2006b PhD Thesis"},{"key":"e_1_2_1_4_1","doi-asserted-by":"publisher","DOI":"10.1051\/0004-6361:20066686"},{"key":"e_1_2_1_5_1","doi-asserted-by":"publisher","DOI":"10.1051\/0004-6361:20041723"},{"key":"e_1_2_1_6_1","doi-asserted-by":"publisher","DOI":"10.1051\/0004-6361:20040170"},{"key":"e_1_2_1_7_1","doi-asserted-by":"publisher","DOI":"10.1086\/312457"},{"key":"e_1_2_1_8_1","unstructured":"Fuhrmann K.:1993 PhD Thesis"},{"key":"e_1_2_1_9_1","unstructured":"Fuhrmann K.:2000 http:\/\/www.usm.uni\u2010muenchen.de\/people\/gehren\/topics\/pap100.pdf"},{"key":"e_1_2_1_10_1","first-page":"3","volume":"325","author":"Fuhrmann K.","year":"2004","journal-title":"AN"},{"key":"e_1_2_1_11_1","first-page":"909","volume":"323","author":"Fuhrmann K.","year":"1997","journal-title":"A&A"},{"key":"e_1_2_1_12_1","doi-asserted-by":"publisher","DOI":"10.1051\/0004-6361:20077799"},{"key":"e_1_2_1_13_1","doi-asserted-by":"publisher","DOI":"10.1086\/510342"},{"key":"e_1_2_1_14_1","unstructured":"Holweger H.:1979 in: A. 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