J/MNRAS/465/2432ivo://CDS.VizieR/J/MNRAS/465/2432doi:10.26093/cds/vizier.74652432CDSGrunhut J.H.Wade G.A.Neiner C.Oksala M.E.Petit V.Alecian E.,Bohlender D.A.Bouret J.-C.Henrichs H.F.Hussain G.A.J.Kochukhov O.2024-08-16T20:19:51Z2018-11-15T16:26:00ZCDS support team

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

cds-question@unistra.frearly-type-starso-starsmagnetic-fieldsWe present the analysis performed on spectropolarimetric data of 97 O-type targets included in the framework of the Magnetism in Massive Stars (MiMeS) Survey. Mean least-squares deconvolved Stokes I and V line profiles were extracted for each observation, from which we measured the radial velocity, rotational and non-rotational broadening velocities, and longitudinal magnetic field B_l_. The investigation of the Stokes I profiles led to the discovery of two new multiline spectroscopic systems (HD 46106, HD 204827) and confirmed the presence of a suspected companion in HD 37041. We present a modified strategy of the least-squares deconvolution technique aimed at optimizing the detection of magnetic signatures while minimizing the detection of spurious signatures in Stokes V. Using this analysis, we confirm the detection of a magnetic field in six targets previously reported as magnetic by the MiMeS collaboration (HD 108, HD 47129A2, HD 57682, HD 148937, CPD-28 2561, and NGC 1624-2), as well as report the presence of signal in Stokes V in three new magnetic candidates (HD 36486, HD 162978, and HD 199579). Overall, we find a magnetic incidence rate of 7+/-3 per cent, for 108 individual O stars (including all O-type components part of multiline systems), with a median uncertainty of the B_l_ measurements of about 50G. An inspection of the data reveals no obvious biases affecting the incidence rate or the preference for detecting magnetic signatures in the magnetic stars. Similar to A- and B-type stars, we find no link between the stars' physical properties (e.g. T_eff_, mass, and age) and the presence of a magnetic field. However, the Of?p stars represent a distinct class of magnetic O-type stars.2017MNRAS.465.2432Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/465/2432CatalogResearchIsServedByTAP 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/465/2432https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/465/2432http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/465/2432https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/465/2432https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/465/2432http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/465/2432GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/465/2432/stars (List of studied stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/465/2432/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/465/2432/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/465/2432/stars?GETtext/xml+votable180.050000true38.069791761.55416670.0055555555555555566/1196 1293 1299 1302 1332 1558 1790 1848 2409 2806 3066 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 21655-21656 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 39793 42203 42214 42236 42394 42416 42421 42458 42464 42470-42471 42483https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/465/2432?format=asciidefaultJ/MNRAS/465/2432/starsList of studied starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName adopted in the analysismeta.id;meta.maincharRAJ2000Simbad right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainTableName of the table with observations resultsmeta.id;meta.tablecharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/MNRAS/465/2432/tablec1Table of observations and magnetic results for spectroscopically single starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName adopted in the analysismeta.id;meta.maincharONameCommon namemeta.idSpTypeSpectral type and the luminosity classsrc.spTypecharMaskAdopted line maskmeta.id;instrcharObs.DateObservation datetime.epoch;obsnullableHJDHeliocentric Julian date at mid-exposure (HJD-2450000)dtime.epochdoubleTExpExposure time of the polarimetric sequencestime.duration;obs.exposurecharInst[NEH] Instrument used (G1)instr.setupcharS/N? Peak S/N in the co-added spectrum within the range of 500-600nmstat.snrintnullableWidth? Optimal velocity width determined for the binned LSD profilkm/sspect.line.widthfloatnullableDet[DD MD ND -] Detection flag (G2)meta.code.errorcharIntlim1? Integration range corresponding to the line profilekm/sinstr.bandwidthintnullableIntlim2? Integration range corresponding to the line profilekm/sinstr.bandwidthintnullableBl? Longitudinal magnetic field strengthGphys.magField;phys.atmol.collStrengthintnullableNl? Longitudinal field strength measured from the diagnostic null profileGphys.atmol.collStrength;obs.fieldintnullablee_Bl? Uncertainty of the longitudinal fieldGstat.errorintnullablevr? Radial velocity (G3)km/sphys.veloc;pos.heliocentricintnullablevsini? Projected rotational velocity (G3)km/sphys.veloc.rotatintnullablevmac? Additional non-rotational velocity considered macroturbulence (G3)km/sphys.velocintnullablevtot? Median total line broadening vtot, computed by summing vsini and vmac in quadrature (G3)km/sspect.line.broad;stat.medianintnullableJ/MNRAS/465/2432/tablec2Table of observations and magnetic results for spectroscopic binary systemsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName adopted in the analysismeta.id;meta.maincharONameCommon namemeta.idSpTypeSpectral type and the luminosity classsrc.spTypecharMaskAdopted line maskmeta.id;instrcharObs.DateObservation datetime.epoch;obsnullableHJDHeliocentric Julian date at mid-exposure (HJD-2450000)dtime.epochdoubleTExpExposure time of the polarimetric sequencestime.duration;obs.exposurecharInst[NEH] Instrument used (G1)instr.setupcharS/N? Peak S/N in the co-added spectrum within the range of 500-600nmstat.snrintnullableCompSpectroscopic componentmeta.code.multipcharWidth? Optimal velocity width determined for the binned LSD profilkm/sspect.line.widthfloatnullableDet[DD MD ND -] Detection flag (G2)meta.code.errorcharIntlim1? Integration range corresponding to the line profilekm/sinstr.bandwidthintnullableIntlim2? Integration range corresponding to the line profilekm/sinstr.bandwidthintnullableBl? Longitudinal magnetic field strengthGphys.magField;phys.atmol.collStrengthintnullableNl? Longitudinal field strength measured from the diagnostic null profileGphys.atmol.collStrength;obs.fieldintnullablee_Bl? Uncertainty of the longitudinal fieldGstat.errorintnullablevr? Radial velocity (G3)km/sphys.veloc;pos.heliocentricintnullablevsini? Projected rotational velocity (G3)km/sphys.veloc.rotatintnullablevmac? Additional non-rotational velocity considered macroturbulence (G3)km/sphys.velocintnullablevtot? Median total line broadening vtot, computed by summing vsini and vmac in quadrature (G3)km/sspect.line.broad;stat.medianintnullable