J/AJ/153/99ivo://CDS.VizieR/J/AJ/153/99doi:10.26093/cds/vizier.51530099CDSCarraro G.Sales Silva J.V.Moni Bidin C.Vazquez R.A.2018-05-16T07:09:03Z2018-04-24T06:28:18ZCDS support team

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

cds-question@unistra.frmilky-way-galaxyopen-star-clustersinfrared-photometryvisible-astronomyphotometrychemical-abundanceseffective-temperatureradial-velocityinterstellar-reddeningstellar-distanceline-intensitiesWe employ optical photometry and high-resolution spectroscopy to study a field toward the open cluster Tombaugh 1, where we identify a complex population mixture that we describe in terms of young and old Galactic thin disks. Of particular interest is the spatial distribution of the young population, which consists of dwarfs with spectral types as early as B6 and is distributed in a blue plume feature in the color-magnitude diagram. For the first time, we confirm spectroscopically that most of these stars are early-type stars and not blue stragglers or halo/thick-disk subdwarfs. Moreover, they are not evenly distributed along the line of sight but crowd at heliocentric distances between 6.6 and 8.2 kpc. We compare these results with present-day understanding of the spiral structure of the Galaxy and suggest that they trace the outer arm. This range of distances challenges current Galactic models adopting a disk cutoff at 14 kpc from the Galactic center. The young dwarfs overlap in space with an older component, which is identified as an old Galactic thin disk. Both young and old populations are confined in space since the disk is warped at the latitude and longitude of Tombaugh 1. The main effects of the warp are that the line of sight intersects the disk and entirely crosses it at the outer arm distance and that there are no traces of the closer Perseus arm, which would then be either unimportant in this sector or located much closer to the formal Galactic plane. Finally, we analyze a group of giant stars, which turn out to be located at very different distances and to possess very different chemical properties, with no obvious relation to the other populations.2017AJ....153...99Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/153/99CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/275/101 : Chemical evolution of the galactic disk I. (Edvardsson+ 1993)J/A+A/350/955 : Atmospheric parameters in metal-poor stars. IIJ/MNRAS/340/304 : [X/Fe] of Galactic disc F and G dwarfs (Reddy+, 2003)J/A+A/421/991 : CT1 photometry in Tombaugh 1 (Piatti+, 2004)J/AJ/144/95 : Abundance in stars of the outer galactic disk. IV.J/AJ/151/6 : Spectroscopic and photometric properties of Tombaugh 1https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/153/99https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/153/99http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/153/99https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/153/99https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/153/99http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/153/99GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/153/99/table2 (Fundamental Information for the Spectroscopically Observed Stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/153/99/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/153/99/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/153/99/table2?GETtext/xml+votable180.050000true105.0619584-20.59597120.0055555555555555566/20833 208363.322582951404819e-19 3.852589004194616e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/153/99?format=asciiInfraredOpticaldefaultJ/AJ/153/99/table4Abundance Ratios ([X/Fe]) for the Elements, from Na to Cr, for the Stars from Box Bo_[Si/Fe][1/3]? Number of Si lines employedmeta.numberintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[11029/32782] Star identification numbermeta.id;meta.mainint[Na/Fe][0.19/0.42]? Abundance ratio [Na/Fe] (1)phys.abund;arith.ratiofloatnullablee_[Na/Fe][0.01]? Uncertainty in [Na/Fe]stat.error;phys.abundfloatnullableo_[Na/Fe][1/2]? Number of Na lines employedmeta.numberintnullable[Mg/Fe][-0.21/0.67]? Abundance ratio [Mg/Fe]phys.abund;arith.ratiofloatnullablee_[Mg/Fe][0.06/0.13]? Uncertainty in [Mg/Fe]stat.error;phys.abundfloatnullableo_[Mg/Fe][1/2]? Number of Mg lines employedmeta.numberintnullable[Al/Fe][0.1/0.59]? Abundance ratio [Al/Fe]phys.abund;arith.ratiofloatnullablee_[Al/Fe][0.01/0.11]? Uncertainty in [Al/Fe]stat.error;phys.abundfloatnullableo_[Al/Fe][1/4]? Number of Al lines employedmeta.numberintnullable[Si/Fe][0.07/0.54]? Abundance ratio [Si/Fe]phys.abund;arith.ratiofloatnullablee_[Si/Fe][0.05/0.17]? Uncertainty in [Si/Fe]stat.error;phys.abundfloatnullable[Ca/Fe][-0.3/0.47]? Abundance ratio [Ca/Fe]phys.abund;arith.ratiofloatnullablee_[Ca/Fe][0.03/0.17]? Uncertainty in [Ca/Fe]stat.error;phys.abundfloatnullableo_[Ca/Fe][2/4]? Number of Ca lines employedmeta.numberintnullable[Ti/Fe][0.21/0.54] Abundance ratio [Ti/Fe]phys.abund;arith.ratiofloate_[Ti/Fe][0.03/0.15] Uncertainty in [Ti/Fe]stat.error;phys.abundfloato_[Ti/Fe][2/6] Number of Ti lines employedmeta.numberint[Cr/Fe][-0.21/0.35] Abundance ratio [Cr/Fe]phys.abund;arith.ratiofloate_[Cr/Fe][0.02/0.13]? Uncertainty in [Cr/Fe]stat.error;phys.abundfloatnullableo_[Cr/Fe][1/3] Number of Cr lines employedmeta.numberint[Ni/Fe][-0.22/0.24] Abundance ratio [Ni/Fe]phys.abund;arith.ratiofloate_[Ni/Fe][0.07/0.16]? Uncertainty in [Ni/Fe]stat.error;phys.abundfloatnullableo_[Ni/Fe][1/11] Number of Ni lines employedmeta.numberintJ/AJ/153/99/LinesObserved Fe I and Fe II lines (table 6) and other lines studied (table 7)ElElementphys.atmol.elementcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4730.04/8773.91] Wavelength {lambda} ({AA})0.1nmem.wlfloatchi[0.02/6.18] Excitation potential {chi}eVphys.atmol.excitationfloatloggf[-5.95/0.42] Oscillator strength (1)phys.atmol.oscStrengthfloatRefReference of the atomic parameters (only in table 7) (2)meta.refcharEW-11029[20/160]? Equivalent width for star 11029 (m{AA})0.1pmspect.line.eqWidthintnullableEW-13540[23/156]? Equivalent width for star 13540 (m{AA})0.1pmspect.line.eqWidthintnullableEW-13964[40/154]? Equivalent width for star 13964 (m{AA})0.1pmspect.line.eqWidthintnullableEW-26606[36/147]? Equivalent width for star 26606 (m{AA})0.1pmspect.line.eqWidthintnullableEW-27955[17/149]? Equivalent width for star 27955 (m{AA})0.1pmspect.line.eqWidthintnullableEW-28064[10/153]? Equivalent width for star 28064 (m{AA})0.1pmspect.line.eqWidthintnullableEW-31364[22/151]? Equivalent width for star 31364 (m{AA})0.1pmspect.line.eqWidthintnullableEW-32782[40/155]? Equivalent width for star 32782 (m{AA})0.1pmspect.line.eqWidthintnullableJ/AJ/153/99/table2Fundamental Information for the Spectroscopically Observed StarsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBox[BCD] Box designationobs.fieldcharID[6507/36132] Star identification numbermeta.id;meta.mainintprimaryRAJ2000Right Ascension in decimal degrees (J2000)degpos.eq.ra;meta.mainDEJ2000Declination in decimal degrees (J2000)degpos.eq.dec;meta.mainVmag[15.57/19.38] V band magnitudemagphot.mag;em.opt.VfloatV-I[0.458/1.512] V-I color indexmagphot.color;em.opt.V;em.opt.IfloatS/N[10/75] Spectral signal-to-noise ratio at 6000{AA}stat.snrintmoreindicates data in table Parameters and/or table 4 for this starmeta.ref.urlcharEWEquivalent widths from table Lines (except for stars 29403 and 35658)meta.ref.urlcharJ/AJ/153/99/ParametersAtmospheric parameters from spectroscopy of stars of Box B (table 3) , Box C (table 9) and Box D (table 10)n_ID[abc] Note on ID (1)meta.notecharBoxBox designationobs.fieldcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[6507/36132] Star identification numbermeta.id;meta.mainintTeff[4600/14500]? Effective temperatureKphys.temperature.effectiveintnullablee_Teff[20/4200]? Uncertainty in TeffKstat.error;phys.temperature.effectiveintnullablelogg[2/5.5]? Surface gravity (not in table 10) (dex)log(cm.s**-2)phys.gravityfloatnullablee_logg[0/3.2]? Uncertainty in logg (not in table 10)log(cm.s**-2)stat.errorfloatnullableksi[1.5/3]? Microturbulent velocity {ksi} (only in table 3)km/sphys.velocfloatnullablee_ksi[0.3/1]? Uncertainty in ksi (only in table 3)km/sstat.errorfloatnullablevsini[0/310]? Rotational velocity (only in table 9)km/sphys.veloc.rotatintnullablen_vsini[c] Note on visini (only in table 9) (1)meta.notechar[FeI/H][-0.68/0.03]? Abundance ratio [FeI/H] (only in table 3)phys.abund;arith.ratiofloatnullablee_[FeI/H][0.13/0.34]? Uncertainty in [FeI/H] (only in table 3)stat.error;phys.abundfloatnullableo_[FeI/H][16/43]? Number of FeI lines employed (only in table 3)meta.numberintnullable[FeII/H][-0.7/0.05]? Abundance ratio [FeII/H] (only in table 3)phys.abund;arith.ratiofloatnullablee_[FeII/H][0.07/0.26]? Uncertainty in [FeII/H] (only in table 3)stat.error;phys.abundfloatnullableo_[FeII/H][1/8]? Number of FeII lines employed (only in table 3)meta.numberintnullableRVmean[0.9/139] Mean radial velocitykm/sspect.dopplerVeloc;stat.meanfloate_RVmean[0.3/45] Uncertainty in RVmeankm/sstat.errorfloatE(V-I)[0.3/0.82]? Reddeningphot.color.excessfloatnullablee_E(V-I)[0.02/0.28]? Uncertainty in E(V-I)stat.errorfloatnullable(m-MV)0[10.46/16.81]? Reddening-corrected distance modulus (m-M_V_)_0_magphot.mag.distModfloatnullablee_(m-MV)0[0.05/1.74]? Uncertainty in (V-Mnu)0magstat.errorfloatnullableDist[1200/23000]? Distancepcpos.distance;pos.heliocentricintnullablee_Dist[100/11600]? Uncertainty in Distpcstat.errorintnullable