J/ApJ/760/147ivo://CDS.VizieR/J/ApJ/760/147doi:10.26093/cds/vizier.17600147CDSQian L.Li D.Goldsmith P.F.2014-03-31T11:43:49Z2014-03-31T11:40:03ZCDS support team

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

cds-question@unistra.frmolecular-cloudsinterstellar-mediumco-line-emissionYoung stars form in molecular cores, which are dense condensations within molecular clouds. We have searched for molecular cores traced by ^13^CO J=1-->0 emission in the Taurus molecular cloud and studied their properties. Our data set has a spatial dynamic range (the ratio of linear map size to the pixel size) of about 1000 and spectrally resolved velocity information, which together allow a systematic examination of the distribution and dynamic state of ^13^CO cores in a large contiguous region. We use empirical fit to the CO and CO_2_ ice to correct for depletion of gas-phase CO. The ^13^CO core mass function (^13^CO CMF) can be fitted better with a log-normal function than with a power-law function. We also extract cores and calculate the ^13^CO CMF based on the integrated intensity of ^13^CO and the CMF from Two Micron All Sky Survey. We demonstrate that core blending exists, i.e., combined structures that are incoherent in velocity but continuous in column density. The core velocity dispersion (CVD), which is the variance of the core velocity difference {delta}v, exhibits a power-law behavior as a function of the apparent separation L: CVD(km/s){prop.to}L(pc)^0.7^. This is similar to Larson's law for the velocity dispersion of the gas. The peak velocities of ^13^CO cores do not deviate from the centroid velocities of the ambient ^12^CO gas by more than half of the line width. The low velocity dispersion among cores, the close similarity between CVD and Larson's law, and the small separation between core centroid velocities and the ambient gas all suggest that molecular cores condense out of the diffuse gas without additional energy from star formation or significant impact from converging flows.2012ApJ...760..147Qhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/760/147CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/760/147https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/760/147http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/760/147https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/760/147https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/760/147http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/760/147GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/760/147/table4 (Properties of the cores found in the 3D ^13^CO data cube (from erratum, 2013, ApJ, 765, 161))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/760/147/table4?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/760/147/table4?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/760/147/table4?GETtext/xml+votable180.050000true68.91041724.1139170.0055555555555555565/93 259 262 263 265 266 268 269 270 6/380 381 383 1030 1031 1042 1045 1046 1047 1057 1058 1059 1068 1070 1071 1084 1090 1099 1103 1124 1153 1157 1159 1164 1165 1167 1168 24250https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/760/147?format=asciiRadiodefaultJ/ApJ/760/147/table4Properties of the cores found in the 3D ^13^CO data cube (from erratum, 2013, ApJ, 765, 161)IDIndex identifierspect.indexintMMasssolMassphys.massfloatTPeakPeak temperatureKphys.temperaturefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Hour of Right Ascension (J2000)pos.eq.ra;meta.mainDEJ2000Degree of Declination (J2000)pos.eq.dec;meta.mainRmajSemi-major axisarcminphys.angSize.smajAxisfloatRminSemi-minor axisarcminphys.angSize.sminAxisfloatPAPosition angle; angle from north to Rmajdegpos.posAngfloatMVirVirial masssolMassphys.massfloatFWHMLine Full-Width of Half-Maximumkm/sspect.line.widthfloatNH2Estimated mean N_H2_ densitycm**-3phys.columnDensityint