J/A+A/619/A41ivo://CDS.VizieR/J/A+A/619/A41doi:10.26093/cds/vizier.36190041CDSTeixeira G.D.C.Kumar M.S.N.Smith L.Lucas P.W.Morris C.,Borissova J.Monteiro M.J.P.F.G.Caratti o Garatti A.Contreras Pena C.,Froebrich D.Gameiro J.F.2018-11-05T08:58:26Z2018-11-05T08:31:55ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectspre-main-sequence-starsThe Vista Variables in the Via Lactea (VVV) survey has allowed for an unprecedented number of multi-epoch observations of the southern Galactic plane. In a recent paper, 13 massive young stellar objects (MYSOs) have already been identified within the highly variable ({Delta}Ks>1mag) YSO sample of another published work. This study aims to understand the general nature of variability in MYSOs. Here we present the first systematic study of variability in a large sample of candidate MYSOs. We examined the data for variability of the putative driving sources of all known Spitzer extended green objects (EGOs; 270) and bright 24um sources coinciding with the peak of 870um detected ATLASGAL clumps (448), a total of 718 targets. Of these, 190 point sources (139 EGOs and 51 non-EGOs) displayed variability (IQR>0.05, {Delta}Ks>0.15mag). 111 and 79 light-curves were classified as periodic and aperiodic respectively. Light-curves have been sub-classified into eruptive, dipper, fader, short-term-variable and long-period-variable-YSO categories. Lomb-Scargle periodogram analysis of periodic light-curves was carried out. 1-870um spectral energy distributions of all the variable sources were fitted with YSO models to obtain the representative properties of the variable sources. 41% of the variable sources are represented by >4M_{sun}_ objects, and only 6% were modelled as >8M_{sun}_ objects. The highest-mass objects are mostly non-EGOs, and deeply embedded, as indicated by nearly twice the extinction when compared with EGO sources. By placing them on the HR diagram we show that most of the lower mass, EGO type objects are concentrated on the putative birth-line position, while the luminous non-EGO type objects group around the zero-age-main-sequence track. Some of the most luminous far infrared (FIR) sources in the massive clumps and infrared quiet driving sources of EGOs have been missed out by this study owing to an uniform sample selection method. A high rate of detectable variability in EGO targets (139 out of 153 searched) implies that near-infrared variability in MYSOs is closely linked to the accretion phenomenon and outflow activity.2018A&A...619A..41Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/619/A41CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/337 : VISTA Variables in the Via Lactea Survey DR1 (Saito+, 2012)II/348 : VISTA Variable in the Via Lactea Survey DR2 (Minniti+, 2017)J/AJ/136/2391 : GLIMPSE Extended Green Objects catalog (Cyganowski+, 2008)J/ApJS/206/9 : New EGOs from Spitzer GLIMPSE II survey. I. (Chen+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/619/A41https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/619/A41http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/619/A41https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/619/A41https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/619/A41http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/619/A41GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/619/A41/table2 (Source coordinates, photometric data and variability)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/619/A41/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/619/A41/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/619/A41/table2?GETtext/xml+votable180.050000true182.9487-61.77250.0055555555555555565/7202 10453 10615 6/28806 28812 28814-28815 28817 28824-28825 28827-28828 28875 28879 28890 28896 28901 28912-28913 28919 29088 29096 41598 41653-41655 41661 41677 41681 41696 41767 41802 41807 41811 41817 41820 41825 42169-42174 42206-42207 42211 42213 42215 42217 42224-42225 42228-42230 42376 42379-42382 42387 42390-42393 42396 42434 42437-42439 42441 42450-42451 42454 42456-42457 42496-42497 42512 43014 43019 430412.283270615984385e-22 1.7003137259100215e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/619/A41?format=asciidefaultJ/A+A/619/A41/table2Source coordinates, photometric data and variabilitySimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintmoreindicates input data and/or results of the weighted averaging of the fit SEDs in tables A1/A2meta.ref.urlcharSourceSource namemeta.id;meta.maincharprimaryRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainKmagKmag (median)magphot.mag;em.IR.KfloatMADMedian Absolute Deviation of Light Curvemagstat.stdevfloatIQRInterquartile Range of Light Curvemagsrc.var.amplitudefloatDeltaKAmplitude of Light Curvemagphot.magfloatClassClassification (1)src.classcharPeriod? Best fit period (2)dtime.period;meta.modelledfloatnullableJ/A+A/619/A41/tablea1Input data to build the SEDsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceSource namemeta.id;meta.maincharFJ? J flux (2MASS)mJyphot.flux.density;em.IR.JfloatnullableFH? H flux (2MASS)mJyphot.flux.density;em.IR.HfloatnullableFK? K flux (2MASS)mJyphot.flux.density;em.IR.KfloatnullableF3.6? 3.6um flux (SPITZER)mJyphot.mag;em.IR.3-4umfloatnullableF4.5? 4.5um flux (SPITZER)mJyphot.mag;em.IR.4-8umfloatnullableF5.8? 5.8um flux (SPITZER)mJyphot.flux.density;em.IR.4-8umfloatnullableF8.0? 8.0um flux (SPITZER)mJyphot.flux.density;em.IR.8-15umfloatnullableF24? 24um flux (SPITZER)mJyphot.flux.density;em.IR.15-30umdoublenullableF70? PACS 70um flux (Herschel)mJyphot.flux.density;em.IR.30-60umdoublenullableF160? PACS 160um flux (Herschel)mJyphot.flux.density;em.mm.1500-3000GHzdoublenullableF250? SPIRE 250um flux (Herschel)mJyphot.flux.density;em.mm.750-1500GHzintnullableF350? SPIRE 350um flux (Herschel)mJyphot.flux.density;em.mm.750-1500GHzintnullableF500? SPIRE 500um flux (Herschel)mJyphot.flux.density;em.mm.400-750GHzintnullableF870? APEX 870um fluxmJyphot.flux.density;em.mm.200-400GHzintnullableJ/A+A/619/A41/tablea2Results of the weighted averaging of the fit SEDsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceSource namemeta.id;meta.maincharchi2Chi square fitstat.fit.chi2;stat.fit.param;meta.modelledfloats_chi2Chi square fit standard deviationstat.fit.chi2;stat.fit.param;meta.modelledfloatAvISM extinctionmagphys.absorptionfloats_AvISM extinction standard deviationmagstat.stdev;phys.absorptionfloatMMass of the EnvelopesolMassphys.massfloats_MMass of the Envelope standard deviationsolMassphys.massfloatlogdM/dtEnvelope accretion ratelog(solMass.yr**-1)arith.ratefloats_logdM/dt[] Envelope accretion rate standard deviationlog(solMass.yr**-1)arith.ratefloatlogMdDisk masslog(solMass)phys.massfloats_logMd[] Disk mass standard deviationlog(solMass)stat.stdev;phys.massfloatlogdMd/dtDisk accretion ratelog(solMass.yr**-1)arith.ratefloats_logdMd/dt[] Disk accretion rate standard deviationlog(solMass.yr**-1)arith.ratefloatlogLLuminositylog(solLum)phys.luminosityfloats_logL[] Luminosity standard deviationlog(solLum)stat.stdev;phys.luminosityfloatlogAgeAgelog(yr)time.agefloats_logAgeAge standard deviationlog(yr)stat.stdev;time.agefloat