J/MNRAS/495/3614ivo://CDS.VizieR/J/MNRAS/495/3614doi:10.26093/cds/vizier/bg-ff-3gyCDSContreras Pena C.Johnstone D.Baek G.Herczeg G.J.Mairs S.,Scholz A.Lee J.-E.2026-08-03T07:29:49Z2023-09-14T14:17:27ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectspre-main-sequence-starsvariable-starsastrometryinfrared-astronomymillimeter-astronomysubmillimeter-astronomyWe study the relationship between the mid-infrared (mid-IR) and sub-millimetre (sub-mm) variability of deeply embedded protostars using the multi-epoch data from the Wide-field Infrared Survey Explorer (WISE/NEOWISE) and the ongoing James Clerk Maxwell Telescope (JCMT) Transient Survey. Our search for signs of stochastic (random) and/or secular (roughly monotonic in time) variability in a sample of 59 young stellar objects (YSOs) revealed that 35 are variable in at least one of the two surveys. This variability is dominated by secular changes. Of those objects with secular variability, 14 objects (22 per cent of the sample) show correlated secular variability over mid-IR and sub-mm wavelengths. Variable accretion is the likely mechanism responsible for this type of variability. Fluxes of YSOs that vary in both wavelengths follow a relation of log_10_F_4.6_(t)={eta}log_10_F_850_(t) between the mid-IR and sub-mm, with {eta}=5.53+/-0.29. This relationship arises from the fact that sub-mm fluxes respond to the dust temperature in the larger envelope whereas the mid-IR emissivity is more directly proportional to the accretion luminosity. The exact scaling relation, however, depends on the structure of the envelope, the importance of viscous heating in the disc, and dust opacity laws.2020MNRAS.495.3614Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/495/3614CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/311 : WISE All-Sky Data Release (Cutri+ 2012)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/495/3614https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/495/3614http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/495/3614https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/495/3614https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/495/3614http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/495/3614GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/495/3614/table1 (The 59 sources where JCMT and WISE fluxes likely arise from the same source)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/495/3614/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/495/3614/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/495/3614/table1?GETtext/xml+votable180.050000true55.987532.0513610.0055555555555555566/859 862 1539 21439 22805 22855 22873 30341 30343 30366 429813.830199579824256e-20 4.8065244008477756e-20https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/495/3614?format=asciiInfraredMillimeterdefaultJ/MNRAS/495/3614/table1The 59 sources where JCMT and WISE fluxes likely arise from the same sourceSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRegionJCMT Transient Survey regionmeta.notecharIDSource numbermeta.idintRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainJCMTJCMT source designation (JCMTPP_JHHMMSS.s+DDMMSS)meta.id;meta.maincharNameOther namemeta.idcharYSOclassYSO class (1)src.classcharr_YSOclassReference for YSOclassmeta.ref;pos.framecharW2magAverage WISE W2 (4.6um) band magnitudemagphot.mag;em.IR.4-8umfloatE_W2magUpper error on W2mag (90th percentile)magstat.error;stat.maxfloate_W2magLower error on W2mag (10th percentile)magstat.error;phot.magfloatSD/SDfidWRatio of the standard deviation of the observed W2 flux to a fiducial model of the expected uncertainty (2)stat.stdevfloatS/dSWRatio of the slope of the linear fit to the W2 flux to the uncertainty in the slope measurement (2)stat.fit.paramfloatNW2Number of WISE points used in the analysis of variabilitymeta.numberintFluxJCMT/SCUBA-2 850um fluxJy/beamphot.flux.density;em.mm.200-400GHzfloatSD/SDfidJRatio of the standard deviation of the observed JCMT light curves to a fiducial model of the expected uncertainty (2)stat.stdevfloatS/dSJRatio of the slope of the linear fit to the JCMT flux to the uncertainty in the slope measurement (2)stat.fit.paramfloatNJCMTNumber of epochs used in the analysis of variabilitymeta.numberint