J/MNRAS/489/5669ivo://CDS.VizieR/J/MNRAS/489/5669doi:10.26093/cds/vizier.74895669CDSPetit V.Wade G.A.Schneider F.R.N.Fossati L.Kamp K.Neiner C.,David-Uraz A.Alecian E.(the MiMeS Collaboration)2024-08-20T20:13:17Z2023-02-14T14:42:04ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frearly-type-starso-starsmagnetic-fieldsstellar-agesstellar-spectral-typesvisible-astronomyIn this paper, we describe an analysis of the MiMeS (Magnetism in Massive Stars) survey of O-type stars to explore the range of dipolar field strengths permitted by the polarization spectra that do not yield a magnetic detection. We directly model the Stokes V profiles with a dipolar topology model using Bayesian inference. The noise statistics of the Stokes V profiles are in excellent agreement with those of the null profiles. Using a Monte Carlo approach, we conclude that a model in which all the stars in our sample were to host 100G, dipolar magnetic field can be ruled out by the MiMeS data. Furthermore, if all the stars with no detection were to host a magnetic field just below their detection limit, the inferred distribution in strength of these undetected fields would be distinct from the known distribution in strength of the known magnetic O-type stars. This indicates that the 'initial magnetic field function' (IBF) is likely bimodal - young O-type stars are expected to have either weak/absent magnetic fields or strong magnetic fields. We also find that better upper limits, by at least a factor of 10, would have been necessary to rule out a detection bias as an explanation for the apparent lack of evolved main-sequence magnetic O-type stars reported in the literature, and we conclude that the MiMeS survey cannot confirm or refute a magnetic flux decay in O-type stars.2019MNRAS.489.5669Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/489/5669CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/456/2 : MiMeS survey of magnetism in massive stars (Wade+, 2016)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/489/5669https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/489/5669http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/489/5669https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/489/5669https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/489/5669http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/489/5669GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/489/5669/table2 (Results from our Bayesian analysis)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/489/5669/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/489/5669/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/489/5669/table2?GETtext/xml+votable180.050000true4.429430651.43308780.0055555555555555566/1196 1293 1299 1302 1332 1558 1790 2409 2806 3245 3301 3307 3430 12943 13255 13557 14008 14179 14240 14283 14456 14630-14631 14643 14646 14653-14654 14745 14824 15369 15476 15478 15486 15625 15631 15656 15672 15745 20613 21432 21438-21439 21647 21656 22216 22243 22249 22253 22258 22854 22884 23637 23717 23982 24179 24496 28890-28891 28900 28913 29089 29095 29463 30818 37333 38016 39327 39374 39775 42203 42236 42394 42416 42421 42458 42464 42470-42471 42483https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/489/5669?format=asciiOpticaldefaultJ/MNRAS/489/5669/table2Results from our Bayesian analysisSimbadNameSimbad column added by the CDSmeta.idcharnullableNameStar namemeta.id;meta.mainchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[1/102] Internal object identifiermeta.idintf_IDFlag on ID (G1)meta.codecharSpTypeSpectral type reproduced from Grunhut et al. (2017MNRAS.465.2432G, Cat. J/MNRAS/465/2432) (Paper I)src.spTypecharNobsNumber of nightly averaged observationsmeta.numberintvsiniRotational broadening adopted in our modelskm/sphys.veloc.rotatintOddsVOdds ratio obtained from the Stokes V profile (1)statfloatOddsNOdds ratio obtained from the null profile (1)statfloat68VUpper limit to the 68.3 per cent credible region obtained from Stokes V0.0001Tphys.magFieldint95VUpper limit to the 95.4 per cent credible region obtained from Stokes V0.0001Tphys.magFieldint68NUpper limit to the 68.3 per cent credible region obtained from the null profile0.0001Tphys.magFieldint95NUpper limit to the 95.4 per cent credible region obtained from the null profile0.0001Tphys.magFieldintModeVMode of the probability density function marginalized for B_pole_ obtained from Stokes V0.0001Tphys.magFieldintModeNMode of the probability density function marginalized for B_pole_ obtained from the null profile0.0001Tphys.magFieldintJ/MNRAS/489/5669/table3Results from the BONNSAI analysisf_IDFlag on ID (G1)meta.codecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[1/102] Internal object identifiermeta.idintNameStar namemeta.id;meta.maincharSpTypeSpectral type reproduced from Grunhut et al. (2017MNRAS.465.2432G, Cat. J/MNRAS/465/2432) (Paper I)src.spTypecharAge? Star ageMyrtime.agefloatnullableM*? Star masssolMassphys.massfloatnullableR*? Star radiussolRadphys.size.radiusfloatnullablefracAge? Fractional main-sequence agetime.agefloatnullable