J/AJ/158/73ivo://CDS.VizieR/J/AJ/158/73doi:10.26093/cds/vizier.51580073CDSKobulnicky H.A.Chick W.T.Povich M.S.2019-10-01T06:20:20Z2019-10-01T07:00:48ZCDS support team

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

cds-question@unistra.frearly-type-starsob-starsnebulaestellar-spectral-typesstellar-masseseffective-temperaturestellar-radiistellar-distanceradial-velocityspectroscopySecond only to initial mass, the rate of wind-driven mass loss determines the final mass of a massive star and the nature of its remnant. Motivated by the need to reconcile observational values and theory, we use a recently vetted technique to analyze the mass-loss rates in a sample of OB stars that generate bow shock nebulae. We measure peculiar velocities from new Gaia parallax and proper motion data and their spectral types from new optical and infrared spectroscopy. For our sample of 70 central stars in morphologically selected bow shock nebulae, 67 are OB stars. The median peculiar velocity is 11 km/s, significantly smaller than classical "runaway star" velocities. Mass-loss rates for these O and early B stars agree with recently lowered theoretical predictions, ranging from ~10^-7^ M_{sun}_/yr for mid-O dwarfs to 10^-9^ M_{sun}_/yr for late O dwarfs - a factor of about 2.7 lower than the often-used Vink et al. (2000A&A...362..295V, 2001A&A...369..574V) formulation. Our results provide the first observational mass-loss rates for B0-B3 dwarfs and giants - 10^-9^ to 10^-8^ M_{sun}_/yr. We find evidence for an increase in the mass-loss rates below a critical effective temperature, consistent with predictions of the bistability phenomenon in the range T_eff_=19000-27000 K. The sample exhibits a correlation between modified wind momentum and luminosity, consistent in slope but lower by 0.43 dex in magnitude compared to canonical wind-luminosity relations. We identify a small subset of objects deviating most significantly from theoretical expectations as probable radiation-driven bow wave nebulae by virtue of their low stellar-to-nebular luminosity ratios. For these, the inferred mass-loss rates must be regarded as upper limits.2019AJ....158...73Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/158/73CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/345 : Gaia DR2 (Gaia Collaboration, 2018)I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)J/ApJS/208/9 : Intrinsic colors and temperatures of PMS starsJ/ApJS/227/18 : Candidate stellar bowshock nebulae from MIRJ/AJ/154/201 : IR properties of stellar bowshock nebulaeJ/AJ/157/176 : X-ray emission from Galactic stellar bow shocksJ/MNRAS/488/1141 : Milky Way Project DR2 bubbles + bow shockshttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/158/73https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/158/73http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/158/73https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/158/73https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/158/73http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/158/73GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/158/73/catalog (Measured and adopted parameters (table 1) , kinematic data (table 2) and derived parameters (table 3) for stars and their bow shock nebulae)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/158/73/catalog?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/158/73/catalog?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/158/73/catalog?GETtext/xml+votable180.050000true267.0292083-29.13208330.0055555555555555566/3301 3307 3607 14270 14314 14337 14631 14640 14664 14670 14671 14688 14689 14693 14706 15640 15680 21644 21646 21647 28803 28814 28828 28831 28878 28903 28915 29094 29101 29102 29113 29463 29511 29534 30245 30312 30419 30818 37247 37333 37335 37340 37367 37743 37754 37839 37850 37930 38016 38018 39386 41675 41820 42171 42376 42378 42380 42381 42383 42387 42391 42397 42439 42461https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/158/73?format=asciidefaultJ/AJ/158/73/catalogMeasured and adopted parameters (table 1) , kinematic data (table 2) and derived parameters (table 3) for stars and their bow shock nebulaeSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[1/709] Identifier from Kobulnicky et al. (2016, J/ApJS/227/18)meta.idintn_ID[a] Note on ID (1)meta.notecharAliasCommon namemeta.id.crosscharNameGeneric identifier in Galactic coordinates (GLLL.llll+BB.bbbb)meta.id;meta.maincharSpTypeSpectral classificationsrc.spTypecharTeff[3800/41500] Adopted effective temperature (2)Kphys.temperature.effectiveintR*[4.3/50] Stellar radius based on spectral classification using the theoretical scale of Martins et al. (2005A&A...436.1049M)solRadphys.size.radiusfloatMass[1.1/58] Adopted stellar masssolMassphys.massfloatVinf[500/3000]? Adopted terminal wind velocity from Mokiem et al. (2007A&A...473..603M)km/sphys.veloc.expansionfloatnullableDist[112/5295] Adopted distance (3)pcpos.distanceintR01[1.9/299] Standoff distance in arcsecarcsecpos.angDistancefloatR02[0.015/1.905] Standoff distance in pc (4)pcpos.distancefloatPeak70[8/764] Peak 70 {mu}m surface brightness above adjacent background1e+07Jy.sr**-1phot.flux.density.sb;em.IR.60-100um;stat.maxintl[6/277] Angular diameter of the nebula defined by a chord intersecting the location of the peak surface brightnessarcsecphys.angSizeintObsSource(s) of spectroscopy (5)meta.codecharL*/LIR[0/22422] Ratio of stellar to infrared nebular luminosity L_*_/L_IR_phys.luminosity;arith.ratiointSourceGaia DR2 identifier (Cat. I/345)meta.idHRV[-108/71]? Heliocentric radial velocity measured or adopted, as described in the Appendixkm/sspect.dopplerVeloc;pos.heliocentricintnullablePlx[148/8910] Gaia DR2 parallaxmaspos.parallaxinte_Plx[26/785] Uncertainty in Plxmasstat.error;pos.parallaxintpmRA[-7909/15260] Gaia DR2 proper motion in RA (pmRA*cosDE)mas/yrpos.pm;pos.eq.rainte_pmRA[29/1377] Uncertainty in pmRAmas/yrstat.error;pos.pm;pos.eq.raintpmDE[-12128/24790] Gaia DR2 proper motion in DEmas/yrpos.pm;pos.eq.decinte_pmDE[39/1206] Uncertainty in pmDEmas/yrstat.error;pos.pm;pos.eq.decintLum[0.005/87] Stellar luminosity (computed from the effective temperature and radius in Table 1)10000solLumphys.luminosityfloatU[0/338] Dimensionless ratio of the radiant energy density (in erg/cm^3^) from the star to the mean interstellar radiant energy density estimated by Mathis et al. (1983A&A...128..212M)phys.density;arith.ratiointjv[0/302] Dust emission coefficient j_v_ (in 10^-13^ Jy/sr/cm^2^ per nucleon) following Draine & Li (2007ApJ...657..810D), after scaling by the factor f_j_1e-13Jy.sr**-1.cm**-2phys.emissMeasureintfj[1.6/4.48] Scale factor, f_j_, for dust emission coefficients on account of the harder radiation field near OB stars, as described in the textarith.factorfloatna[4/2111] Computed ambient interstellar number density, following Equation (5) of Kobulnicky et al. (2018ApJ...856...74K)cm**-3meta.number;phys.density;meta.modelledintVtot[5/78.1] Peculiar velocity in the star's local standard of rest (1)km/sphys.velocfloate_Vtot[0.1/14.3] Uncertainty in Vtotkm/sstat.errorfloatM[3/197923]? Computed mass-loss rate1e-10solMass.yr**-1phys.mass.lossintnullablee_M[1/72806]? Uncertainty in M (2)1e-10solMass.yr**-1stat.errorintnullableDlogM[-2.05/4.04]? The base 10 logarithm of our derived mass-loss rate minus the logarithm of the theoretical Vink et al. (2001A&A...369..574V) mass-loss rate, {Delta}log(M) (3)phys.mass.lossfloatnullable_RAPosition from Simbad name (right ascension part)degpos.eq.ra;meta.main_DEPosition from Simbad name (declination part)degpos.eq.dec;meta.main