J/A+A/618/A110ivo://CDS.VizieR/J/A+A/618/A110doi:10.26093/cds/vizier.36180110CDSBodensteiner J.Baade D.Greiner J.Langer N.2018-11-05T10:52:51Z2018-10-19T08:55:51ZCDS support team

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

cds-question@unistra.frearly-type-starsemission-line-starsbe-starsmultiple-starsdiffuse-molecular-cloudsnebulaeRecent studies show that more than 70% of massive stars do not evolve as effectively single stars, but as members of interacting binary systems. The evolution of these stars is thus strongly altered compared to similar but isolated objects. We investigate the occurrence of parsec-scale mid-infrared nebulae around early-type stars. If they exist over a wide range of stellar properties, one possible overarching explanation is non-conservative mass transfer in binary interactions, or stellar mergers. For ~3850 stars (all OBA stars in the Bright Star Catalogue (BSC, Cat. V/50), Be stars, BeXRBs, and Be+sdO systems), we visually inspect WISE 22um images. Based on nebular shape and relative position, we distinguish five categories: offset bow shocks structurally aligned with the stellar space velocity, unaligned offset bow shocks, and centered, unresolved, and not classified nebulae. In the BSC, we find that 28%, 13%, and 0.4% of all O, B, and A stars, respectively, possess associated infrared (IR) nebulae. Additionally, 34/234 Be stars, 4/72 BeXRBs, and 3/17 Be+sdO systems are associated with IR nebulae. Aligned or unaligned bow shocks result from high relative velocities between star and interstellar medium (ISM) that are dominated by the star or the ISM, respectively. About 13% of the centered nebulae could be bow shocks seen head- or tail-on. For the rest, the data disfavor explanations as remains of parental disks, supernova remnants of a previous companion, and dust production in stellar winds. The existence of centered nebulae also at high Galactic latitudes strongly limits the global risk of coincidental alignments with condensations in the ISM. Mass loss during binary evolution seems a viable mechanism for the formation of at least some of these nebulae. In total, about 29% of the IR nebulae (2% of all OBA stars in the BSC) may find their explanation in the context of binary evolution.2018A&A...618A.110Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/618/A110CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toV/50 : Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)III/252 : Pulkovo radial velocities for 35493 HIP stars (Gontcharov, 2006)V/122 : SB9: 9th Catalogue of Spectroscopic Binary Orbits (Pourbaix+ 2005)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/618/A110https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/618/A110http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/618/A110https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/618/A110https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/618/A110http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/618/A110GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/618/A110/tableb2 (Overview over all the measured and calculated parameters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/618/A110/tableb2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/618/A110/tableb2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/618/A110/tableb2?GETtext/xml+votable180.050000true3.20937537.69366670.005555555555555556Cone search capability for table J/A+A/618/A110/tableb1 (Compilation of all parameter values from the literature)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/618/A110/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/618/A110/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/618/A110/tableb1?GETtext/xml+votable180.050000true3.20937537.69366670.0055555555555555566/257 418 463 472 474 496 867 903 1038 1164 1293 1549-1550 1554 1558 1577 1633 1708 1759 1766 1826 1929 1991 2017 2467 2872 2884 2903 2947 2949 2970 2976 3030 3044 3060 3132 3144 3183 3198 3242 3284 3430 3491 3595 6715 12651 12927 12943 13115 13276 13535 13554 13557 13559 13687 13703 13721 13729 13733 13748 13963 14008 14055 14167 14197 14209 14269 14307 14317 14431 14472 14545 14807 14922 15250 15392 15396 15453 15519 15568 15577 15583 15631 15673 15677 15702 15745 15760 15778 16016 19202 19245 19757 20447 20822 20847 20862 20900 20915 20952 21228 21432 21447 21479 21644 21647 21655 21879 22058 22216 22258 22615 22790 22805 22854 22859 22862 22911 23115 23255 23284 23298 23442 23451 23483 23673 23714 23717 23769 23779 24139 24142 24160 24186 24191 24266 24370 24449 28703 28943 29193 29208 29550 29621 29809 29876 30088 30325 30440 30482 30492 30630 30818 30851 31169 32095 32109 33190 34041 36651 36919 37105 37150 37214 37231 37452 37487 37662 37676 37682 37716 37750 37789 37802 37816 37869 37990 38248 38452 38457 38655 38996 39075 39168 39179 39189 39201 39217 39402 39539 39541 39685 39699 39704 39861 39869 39970 40421 40584 40599 41105 41606-41607 41709 41916 42116 42333 42343 42356 42800 42924 42932 42948 42959 42977 42984 43014 43035 43062 43067 43086 43137 43183 43211 43286 43338 43429 43538 43689 44305-44307 44312-44313 44360 44366 44378 44386 44502 44584 44903 45654 45729 46343 47824 478459.029279001593864e-21 9.029279001593864e-21https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/618/A110?format=asciidefaultJ/A+A/618/A110/tableb2Overview over all the measured and calculated parametersBe[x] known Be star ?meta.codecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameBSC Identifier of the starmeta.id;meta.maincharRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainMClassMorphological classification (1)src.morphcharn[x] has a nebulous spectrum ?meta.codecharbin[x] known binary ?meta.codechard? Distance determined from the parallaxpcpos.distance;pos.heliocentricfloatnullablee_d? rms uncertainty on Distancepcstat.errordoublenullableVspace? Space velocity calculated from the radial velocity, proper motion and distance (2)km/sphys.velocfloatnullablee_Vspace? Error in space velocitykm/sstat.errorfloatnullableSizeA? Angular size of the nebulaearcmin**2phys.angSizefloatnullableFlux? Total flux at 22umJyphot.flux.density;em.IR.15-30umfloatnullableSize? Physical size (3)pc**2phys.areafloatnullablee_Size? Error on linear sizepc**2stat.error;phys.angSizefloatnullablealpha? Misalignment angle between the proper motion of the star and the bow shock shape (4)degpos.pm;pos.angDistanceintnullableR0A? Angular distance R(0)_ang_ between the position of the star and the apex of the bow shockarcminpos.angDistancefloatnullableR0? Physical distance R(0) between the position of the star and the apex of the bow shockpcpos.angDistancefloatnullableJ/A+A/618/A110/tableb1Compilation of all parameter values from the literaturerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameBSC Identifier of the starmeta.id;meta.maincharRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainHDHD identification numbermeta.idintVmagApparent V-band magnitudemagphot.mag;em.opt.VfloatSpTypeSpectral classification listed in SIMBADsrc.spTypecharplx? Parallax (1) (2)maspos.parallax.trigfloatnullablee_plx? Parallax error (1) (2)masstat.error;pos.parallaxfloatnullablepmRAProper motion in RA (1)mas/yrpos.pm;pos.eq.rafloate_pmRA? Proper motion error in RA (1)mas/yrstat.error;pos.pm;pos.eq.rafloatnullablepmDEProper motion in DEC (1)mas/yrpos.pm;pos.eq.decfloate_pmDE? Proper motion error in DE (1)mas/yrstat.error;pos.pm;pos.eq.decfloatnullableRV? Radial velocitykm/sphys.veloc;pos.heliocentricfloatnullablee_RV? Radial velocity errorkm/sstat.errorfloatnullableSimbadSimbad column added by the CDSmeta.ref.urlchar