J/A+A/689/A140ivo://CDS.VizieR/J/A+A/689/A140doi:10.26093/cds/vizier.36890140CDSShen H.Esimbek J.Henkel C.Xu Y.Zhou J.Li D.He Y.Tang X.,Wu G.Komesh T.Tursun K.Zhou D.Imanaly E.Berdikhan D.2024-11-29T20:05:26Z2024-09-10T08:30:01ZCDS support team

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

cds-question@unistra.frmolecular-cloudsco-line-emissionradio-astronomygalaxy-classification-systemsgalaxy-kinematicsThe feedback effect of massive stars can either accelerate or inhibit star formation activity within molecular clouds. Studying the morphology of molecular clouds near W5 offers an excellent opportunity to examine this feedback effect. We conducted a comprehensive survey of the W5 complex using the Purple Mountain Observatory 13.7m millimeter telescope. This survey includes ^12^CO, ^13^CO, and C^18^O (J=1-0), with a sky coverage of 6.6deg^2^ (136.0{deg}<l<138.75{deg}, 0{deg}<b<2.4{deg}). Furthermore, we performed simultaneous observations of the NH_3_ (1,1) and NH_3_ (2,2) lines in the four densest star-forming regions of W5, using the 26m radio telescope of the Xinjiang Astronomy Observatory (XAO). Our analysis of the morphological distribution of the molecular clouds, distribution of high-mass young stellar objects (HMYSOs), ^13^CO/C^18^O abundance ratio, and the stacked average spectral line distribution at different 8um thresholds provide compelling evidence of triggering. Within the mapped region, we identified a total of 212 molecular clumps in the ^13^CO cube data using the astrodendro algorithm. Remarkably, approximately 26.4% (56) of these clumps demonstrate the potential to form massive stars and 42.9% (91) of them are gravitationally bound. Within clumps that are capable of forming high-mass stars, there is a distribution of class I YSOs, all located in dense regions near the boundaries of the Hii regions. The detection of NH_3_ near the most prominent cores reveals moderate kinetic temperatures and densities (as CO). Comparing the Tkin and Tex values reveals a reversal in trends for AFGL 4029 (higher Tex and lower Tkin) and W5-w1, indicating the inadequacy of optically thick CO for dense region parameter calculations. Moreover, a comparison of the intensity distributions between NH_3_ (1,1) and C^18^O (1-0) in the four densest region reveals a notable depletion effect in AFGL 4029, characterised by a low Tkin (9K) value and a relatively high NH_3_ column density, 2.5x10^14^cm^-2^. By classifying the ^13^CO clumps as: "feedback", "non-feedback", "outflow", or "non-outflow" clumps, we observe that the parameters of the "feedback" and "outflow" clumps exhibit variations based on the intensity of the internal 8um flux and the outflow energy, respectively. These changes demonstrate a clear linear correlation, which distinctly separate them from the parameter distributions of the "non-feedback" and "non-outflow" clumps, thus providing robust evidence to support a triggering scenario.2024A&A...689A.140Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/689/A140CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/689/A140https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/689/A140http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/689/A140https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/689/A140https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/689/A140http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/689/A140GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/689/A140/table1 (^13^CO clump properies derived from ^13^CO dendrogram leaves of W5)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/689/A140/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/689/A140/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/689/A140/table1?GETtext/xml+votable180.050000true42.790561.57380.0055555555555555560/https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/689/A140?format=asciiOpticalRadiodefaultJ/A+A/689/A140/table1^13^CO clump properies derived from ^13^CO dendrogram leaves of W5recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[0/328] Leaf numbermeta.id;meta.mainintGLONGalactic Longitudedegpos.galactic.lonGLATGalactic Latitudedegpos.galactic.latVmeanMean velocity of the structurekm/sphys.veloc;stat.meanfloatFWHMFWHM line widthkm/sspect.line.widthfloatRadiusLeaf radiuspcphys.angSize;srcfloatLumLuminositysolLumphys.luminosityfloatN(H2)H_2_ column density1e+22cm**-2phys.columnDensityfloatM(LTE)LTE masssolMassphys.massfloatMvirVirial masssolMassphys.massfloatalphavirVirial parameterstat.fit.paramfloatn(H2)Volume density10000cm**-3phys.densityfloatSigmaSurface mass densitysolMass.pc**-2phot.flux.density.sbfloatL/MThe ratio of luminosity to LTE mass0.001solLum.solMass**-1phys.luminosityfloatTexCO excitation temperatureKphys.atmol.excitation;spect.linefloatVthermThermal velocity dispersionkm/sphys.veloc.dispersionfloatVnthermNon-thermal velocity dispersionkm/sphys.veloc.dispersionfloatVntherm/VthermThe ratio of Vnthermal/vthermalphys.velocfloat_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.raindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decindexed