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dc.creatorStorm, Jesperen_US
dc.creatorGieren, Wolfgangen_US
dc.creatorFouque, Pascalen_US
dc.creatorBarnes, Thomas G.en_US
dc.creatorPietrzynski, G.en_US
dc.creatorNardetto, Nicolasen_US
dc.creatorWeber, M.en_US
dc.creatorGranzer, T.en_US
dc.creatorStrassmeier, K. G.en_US
dc.date.accessioned2016-04-22T19:47:43Z
dc.date.available2016-04-22T19:47:43Z
dc.date.issued2011-10en
dc.identifierdoi:10.15781/T28N50
dc.identifier.citationStorm, Jesper, Nicolas Nardetto, Wolfgang Gieren, Pascal Fouqué, and Thomas G. Barnes. >Calibrating the Cepheid Period-Luminosity relation from the near-infrared surface brightness technique.> Astrophysics and Space Science, Vol. 341, No. 1 (Oct., 2012): pp. 115-121.en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/2152/34507
dc.description.abstractAims. We determine period-luminosity relations for Milky Way Cepheids in the optical and near-IR bands. These relations can be used directly as reference for extra-galactic distance determination to Cepheid populations with solar metallicity, and they form the basis for a direct comparison with relations obtained in exactly the same manner for stars in the Magellanic Clouds, presented in an accompanying paper. In that paper we show that the metallicity effect is very small and consistent with a null effect, particularly in the near-IR bands, and we combine here all 111 Cepheids from the Milky Way, the LMC and SMC to form a best relation. Methods. We employ the near-IR surface brightness (IRSB) method to determine direct distances to the individual Cepheids after we have recalibrated the projection factor using the recent parallax measurements to ten Galactic Cepheids and the constraint that Cepheid distances to the LMC should be independent of pulsation period. Results. We confirm our earlier finding that the projection factor for converting radial velocity to pulsational velocity depends quite steeply on pulsation period, p = 1.550-0.186 log(P) in disagrement with recent theoretical predictions. We find PL relations based on 70 MilkyWay fundamental mode Cepheids of M(K) = -3.33(+/- 0.09)(log(P)-1.0)-5.66(+/- 0.03), W(VI) = -3.26(+/- 0.11)(log(P)-1.0)-5.96(+/- 0.04). Combining the 70 Cepheids presented here with the results for 41 Magellanic Cloud Cepheids which are presented in an accompanying paper, we find M(K) = -3.30(+/- 0.06)(log(P) - 1.0) - 5.65(+/- 0.02), W(VI) = -3.32(+/- 0.08)(log(P) - 1.0) - 5.92(+/- 0.03). Conclusions. We delineate the Cepheid PL relation using 111 Cepheids with direct distances from the IRSB analysis. The relations are by construction in agreement with the recent HST parallax distances to Cepheids and slopes are in excellent agreement with the slopes of apparent magnitudes versus period observed in the LMC.en_US
dc.description.sponsorshipAIP through the State of Brandenburgen_US
dc.description.sponsorshipFederal Ministry for Education and Science in Germanyen_US
dc.description.sponsorshipChilean Center for Astrophysics FONDAP 15010003en_US
dc.description.sponsorshipBASAL Centro de Astrofisica y Tecnologias Afines (CATA) PFB-06/2007en_US
dc.language.isoEnglishen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectstars: variables: cepheidsen_US
dc.subjectstars: fundamental parametersen_US
dc.subjectstars:en_US
dc.subjectdistancesen_US
dc.subjectdistance scaleen_US
dc.subjectlarge-magellanic-clouden_US
dc.subjecthigh-resolution spectroscopyen_US
dc.subjectbase-lineen_US
dc.subjectinterferometryen_US
dc.subjecthubble-space-telescopeen_US
dc.subjectradial-velocity dataen_US
dc.subjectrr-lyraeen_US
dc.subjectvariablesen_US
dc.subjectclassical cepheidsen_US
dc.subjectsouthern cepheidsen_US
dc.subjectgalactic cepheidsen_US
dc.subjectdistance determinationen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleCalibrating The Cepheid Period-Luminosity Relation From The Infrared Surface Brightness Technique I. The P-Factor, The Milky Way Relations, And A Universal K-Band Relationen_US
dc.typeArticleen_US
dc.description.departmentMcDonald Observatoryen_US
dc.identifier.doi10.1051/0004-6361/201117155en_US
dc.contributor.utaustinauthorBarnes, Thomas G.en_US
dc.contributor.utaustinauthorNicolas Nardettoen_US
dc.relation.ispartofserialAstronomy & Astrophysicsen_US


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