J/A+A/581/A52ivo://CDS.VizieR/J/A+A/581/A52doi:10.26093/cds/vizier.35810052CDSTraven G.Zwitter T.Van Eck S.Klutsch A.Bonito R.Lanzafame A.C.,Alfaro E.J.Bayo A.Bragaglia A.Costado M.T.Damiani F.Flaccomio E.,Frasca A.Hourihane A.Jimenez-Esteban F.Lardo C.Morbidelli L.,Pancino E.Prisinzano L.Sacco G.G.Worley C.C.2017-07-04T07:07:58Z2015-09-01T07:06:59ZCDS support team

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

cds-question@unistra.fremission-line-starspeculiar-variable-starsspectroscopyWe discuss the properties of H{alpha} emission stars across the sample of 22035 spectra from the Gaia-ESO Survey internal data release, observed with the GIRAFFE instrument and largely belonging to stars in young open clusters. Automated fits using two independent Gaussian profiles and a third component accounting for the nebular emission allow us to discern distinct morphological types of H{alpha} line profiles with the introduction of a simplified classification scheme. Altogether we find 3765 stars with intrinsic emission and sort their spectra into eight distinct morphological categories: single component emission, emission blend, sharp emission peaks, double emission, P-Cygni, inverted P-Cygni, self absorption, and emission in absorption. We have more than one observation for 1430 stars in our sample, thus allowing a quantitative discussion of the degree of variability of H{alpha} emission profiles, which is expected for young, active objects. We present a catalogue of stars with properties of their H{alpha} emission line profiles, morphological classification, analysis of variability with time and the supplementary information from SIMBAD, VizieR and ADS databases. The records in SIMBAD indicate the presence of H{alpha} emission for roughly 25% of all stars in our catalogue while at least 305 of them have already been more thoroughly investigated according to the references in ADS. The most frequently identified morphological categories in our sample of spectra are emission blend (23%), emission in absorption (22%), and self absorption (16%). Objects with repeated observations demonstrate that our classification into discrete categories is generally stable through time while seemingly less stable are categories P-Cygni and Self absorption, which is the consequence of discrete classification rules as well as of the fundamental change in profile shape. Such records of emission stars can be valuable for automatic pipelines in large surveys, where it may prove very useful to pinpoint outliers during calculation of general stellar properties and elemental abundances. They can find use in studies of star formation processes, interacting binaries and other fields of stellar physics.2015A&A...581A..52Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/581/A52CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/581/A52https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/581/A52http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/581/A52https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/581/A52https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/581/A52http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/581/A52GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/581/A52/tabled2 (Cross-identifications to Simbad, Vizier and ADS)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/581/A52/tabled2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/581/A52/tabled2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/581/A52/tabled2?GETtext/xml+votable180.050000true97.27675-31.24594440.0055555555555555565/9239 9282 9398 6/20562 22078 23636-23637 23639 28890-28891 30215 30226 30301 30472 31787-31788 31790 31812 36953 36955 37122-37123 37586-37587 39181 39183 39192 39194 39205 39216-39218 41649 42959 42980-42981 42983 42992 43034 47125 47168https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/581/A52?format=asciiOpticaldefaultJ/A+A/581/A52/tabled1Master table with the main results for each analysed spectrumNeb[0/2] Nebular emission indication (1)meta.codeintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintObsDateDate and time of the observation (YYYY-MM-DDThh:mm:ss.sss) (DATEOBS)stime.epoch;obsnullableCnameSexagesimal, equatorial position-based source name (HHMMSSss+DDMMSSs) (CNAME)meta.id;meta.maincharlam11[6557/65667] Central wavelength {lambda}_1_ of first Gaussian fit, 1/5 (Halpha_lambda_1) (2)0.1nmem.wl.centralfloatlam12[6557/65667] Central wavelength {lambda}_1_ of first Gaussian fit, 2/5 (Halpha_lambda_1) (2)0.1nmem.wl.centralfloatlam13[6557/65667] Central wavelength {lambda}_1_ of first Gaussian fit, 3/5 (Halpha_lambda_1) (2)0.1nmem.wl.centralfloatlam14[6557/65667] Central wavelength {lambda}_1_ of first Gaussian fit, 3/5 (Halpha_lambda_1) (2)0.1nmem.wl.centralfloatlam15[6557/65667] Central wavelength {lambda}_1_ of first Gaussian fit, 4/5 (Halpha_lambda_1) (2)0.1nmem.wl.centralfloatsig11[0.15/2] Dispersion {sigma}_1_ of first Gaussian profile fit, 1/5 (Halpha_sigma_1) (2)0.1nmstat.fit.paramfloatsig12[0.15/2] Dispersion {sigma}_1_ of first Gaussian profile fit, 2/5 (Halpha_sigma_1) (2)0.1nmstat.fit.paramfloatsig13[0.15/2] Dispersion {sigma}_1_ of first Gaussian profile fit, 3/5 (Halpha_sigma_1) (2)0.1nmstat.fit.paramfloatsig14[0.15/2] Dispersion {sigma}_1_ of first Gaussian profile fit, 4/5 (Halpha_sigma_1) (2)0.1nmstat.fit.paramfloatsig15[0.15/2] Dispersion {sigma}_1_ of first Gaussian profile fit, 5/5 (Halpha_sigma_1) (2)0.1nmstat.fit.paramfloatA11Peak height A_1_ of the first Gaussian profile fit, 1/5 (Halpha_peak_1) (2)stat.fit.paramdoubleA12Peak height A_1_ of the first Gaussian profile fit, 2/5 (Halpha_peak_1) (2)stat.fit.paramdoubleA13Peak height A_1_ of the first Gaussian profile fit, 3/5 (Halpha_peak_1) (2)stat.fit.paramdoubleA14Peak height A_1_ of the first Gaussian profile fit, 4/5 (Halpha_peak_1) (2)stat.fit.paramdoubleA15Peak height A_1_ of the first Gaussian profile fit, 5/5 (Halpha_peak_1) (2)stat.fit.paramdoublelam21[6559/6569] Central wavelength {lambda}_2_ of second Gaussian fit, 1/5 (Halpha_lambda_2) (2)0.1nmem.wl.centralfloatlam22[6559/6569] Central wavelength {lambda}_2_ of second Gaussian fit, 2/5 (Halpha_lambda_2) (2)0.1nmem.wl.centralfloatlam23[6559/6569] Central wavelength {lambda}_2_ of second Gaussian fit, 3/5 (Halpha_lambda_2) (2)0.1nmem.wl.centralfloatlam24[6559/6569] Central wavelength {lambda}_2_ of second Gaussian fit, 4/5 (Halpha_lambda_2) (2)0.1nmem.wl.centralfloatlam25[6559/6569] Central wavelength {lambda}_2_ of second Gaussian fit, 5/5 (Halpha_lambda_2) (2)0.1nmem.wl.centralfloatsig21[0.15/2] Dispersion {sigma}_2_ of second Gaussian profile fit, 1/5 (Halpha_sigma_2) (2)0.1nmstat.fit.paramfloatsig22[0.15/2] Dispersion {sigma}_2_ of second Gaussian profile fit, 2/5 (Halpha_sigma_2) (2)0.1nmstat.fit.paramfloatsig23[0.15/2] Dispersion {sigma}_2_ of second Gaussian profile fit, 3/5 (Halpha_sigma_2) (2)0.1nmstat.fit.paramfloatsig24[0.15/2] Dispersion {sigma}_2_ of second Gaussian profile fit, 4/5 (Halpha_sigma_2) (2)0.1nmstat.fit.paramfloatsig25[0.15/2] Dispersion {sigma}_2_ of second Gaussian profile fit, 5/5 (Halpha_sigma_2) (2)0.1nmstat.fit.paramfloatA21Peak height A_2_ of the second Gaussian profile fit, 1/5 (Halpha_peak_2) (2)stat.fit.paramdoubleA22Peak height A_2_ of the second Gaussian profile fit, 2/5 (Halpha_peak_2) (2)stat.fit.paramdoubleA23Peak height A_2_ of the second Gaussian profile fit, 3/5 (Halpha_peak_2) (2)stat.fit.paramdoubleA24Peak height A_2_ of the second Gaussian profile fit, 4/5 (Halpha_peak_2) (2)stat.fit.paramdoubleA25Peak height A_2_ of the second Gaussian profile fit, 5/5 (Halpha_peak_2) (2)stat.fit.paramdoublelam31[6562/6564]?=0 Central wavelength {lambda}_3_ of third Gaussian fit, 1/5 (Halpha_lambda_neb) (2)0.1nmem.wl.centralfloatnullablelam32[6562/6564]?=0 Central wavelength {lambda}_3_ of third Gaussian fit, 2/5 (Halpha_lambda_neb) (2)0.1nmem.wl.centralfloatnullablelam33[6562/6564]?=0 Central wavelength {lambda}_3_ of third Gaussian fit, 3/5 (Halpha_lambda_neb) (2)0.1nmem.wl.centralfloatnullablelam34[6562/6564]?=0 Central wavelength {lambda}_3_ of third Gaussian fit, 4/5 (Halpha_lambda_neb) (2)0.1nmem.wl.centralfloatnullablelam35[6562/6564]?=0 Central wavelength {lambda}_3_ of third Gaussian fit, 5/5 (Halpha_lambda_neb) (2)0.1nmem.wl.centralfloatnullablesig31[0.26/0.45]?=0 Dispersion {sigma}_3_ of third Gaussian profile fit, 1/5 (Halpha_sigma_neb) (2)0.1nmstat.fit.paramfloatnullablesig32[0.26/0.45]?=0 Dispersion {sigma}_3_ of third Gaussian profile fit, 2/5 (Halpha_sigma_neb) (2)0.1nmstat.fit.paramfloatnullablesig33[0.26/0.45]?=0 Dispersion {sigma}_3_ of third Gaussian profile fit, 3/5 (Halpha_sigma_neb) (2)0.1nmstat.fit.paramfloatnullablesig34[0.26/0.45]?=0 Dispersion {sigma}_3_ of third Gaussian profile fit, 4/5 (Halpha_sigma_neb) (2)0.1nmstat.fit.paramfloatnullablesig35[0.26/0.45]?=0 Dispersion {sigma}_3_ of third Gaussian profile fit, 5/5 (Halpha_sigma_neb) (2)0.1nmstat.fit.paramfloatnullableA31?=0 Peak height A_3_ of the third Gaussian profile fit, 1/5 (Halpha_peak_neb) (2)stat.fit.paramdoublenullableA32?=0 Peak height A_3_ of the third Gaussian profile fit, 2/5 (Halpha_peak_neb) (2)stat.fit.paramdoublenullableA33?=0 Peak height A_3_ of the third Gaussian profile fit, 3/5 (Halpha_peak_neb) (2)stat.fit.paramdoublenullableA34?=0 Peak height A_3_ of the third Gaussian profile fit, 4/5 (Halpha_peak_neb) (2)stat.fit.paramdoublenullableA35?=0 Peak height A_3_ of the third Gaussian profile fit, 5/5 (Halpha_peak_neb) (2)stat.fit.paramdoublenullablechi2r1[0/800] Reduced {chi}^2^_r_ for the fit (1/5) (Halpha_red_chi)stat.fit.chi2floatchi2r2[0/820] Reduced {chi}^2^_r_ for the fit (2/5) (Halpha_red_chi)stat.fit.chi2floatchi2r3[0/830] Reduced {chi}^2^_r_ for the fit (3/5) (Halpha_red_chi)stat.fit.chi2floatchi2r4[0/831] Reduced {chi}^2^_r_ for the fit (4/5) (Halpha_red_chi)stat.fit.chi2floatchi2r5[0/831] Reduced {chi}^2^_r_ for the fit (5/5) (Halpha_red_chi)stat.fit.chi2floatchi2rf1[0/0.5] Reduced {chi}^2^_rf_ for flux normalized over whole fitting range(1/5) (Halpha_red_chi_f)stat.fit.chi2floatchi2rf2[0/0.5] Reduced {chi}^2^_rf_ for flux normalized over whole fitting range(2/5) (Halpha_red_chi_f)stat.fit.chi2floatchi2rf3[0/0.5] Reduced {chi}^2^_rf_ for flux normalized over whole fitting range(3/5) (Halpha_red_chi_f)stat.fit.chi2floatchi2rf4[0/0.5] Reduced {chi}^2^_rf_ for flux normalized over whole fitting range(4/5) (Halpha_red_chi_f)stat.fit.chi2floatchi2rf5[0/0.5] Reduced {chi}^2^_rf_ for flux normalized over whole fitting range(5/5) (Halpha_red_chi_f)stat.fit.chi2floatCatCategory in our classification scheme of Table 2 (Emission/Absorption/Nebular) (Halpha_category)src.classcharSt[0/1] 1 for intrinsic stellar emission (Halpha_intrinsic) (1)meta.codeintJ/A+A/581/A52/tabled2Cross-identifications to Simbad, Vizier and ADSrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintCnameSexagesimal, equatorial position-based source name (HHMMSSss+DDMMSSs) (CNAME)meta.id;meta.maincharprimaryNsNumber of spectra analyzed in table D1meta.ref.urlintnullableHa[0]? "0" for no temporal change in classification category of spectra from repeated observations (Halpha_profile_change)meta.codeintnullableSNameMain ID of the source in SIMBAD found for a given Cname (SIMBAD_main_id)meta.idcharOff[0/15]? Angular distance of the object to the SIMBAD source (SIMBAD_angular_distance)arcsecpos.angDistancefloatnullableoTypeSIMBAD object type for the source SIMBAD source (SIMBAD_otype)src.classcharSpTSIMBAD spectral type for the source SIMBAD source (SIMBAD_stype)src.spTypecharVR[0/11] Number of VizieR tables for Radio wavelength range in which object with Cname has a match (VizieR_n_Radio)meta.numberintVIR[0/60] Number of VizieR tables for IR wavelength range in which object with Cname has a match (VizieR_n_IR)meta.numberintVopt[0/61] Number of VizieR tables for optical wavelength range in which object with Cname has a match (VizieR_n_optical)meta.numberintVUV[0/2] Number of VizieR tables for UV wavelength range in which object with Cname has a match (VizieR_n_UV)meta.numberintVX[0/25] Number of VizieR tables for X-ray wavelength range in which object with Cname has a match (VizieR_n_Xray)meta.numberintVG[0/3] Number of VizieR tables for Gamma-ray wavelength range in which object with Cname has a match (VizieR_n_Gammaray)meta.numberintVGet results from All VizieR (within 3arcsec)meta.numberchar_RARight ascension (derived from Cname) for Eq=J2000degpos.eq.ra;meta.main_DEDeclination (derived from Cname) for Eq=J2000degpos.eq.dec;meta.mainADSA comma-separated list of indices (in tabled3) where we list the ADS references ordered by the number of occurrences for all analysed objects (ADS_literature)meta.ref;pos.frameJ/A+A/581/A52/tabled3Reference listBibCodeBibCodemeta.bib.bibcodecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRef[1/98] Reference numbermeta.id;meta.mainintN[1/157] Number of objects from the catalogue that have corresponding article in the search results from ADS (for N>=50)meta.numberintAutAuthor's namemeta.bib.authorcharComCommentsmeta.notecharTitleTitle of the papermeta.bibchar