J/A+A/656/A101ivo://CDS.VizieR/J/A+A/656/A101doi:10.26093/cds/vizier.36560101CDSMazumdar P.Wyrowski F.Urquhart J.S.Colombo D.Menten K.M.,Neupane S.Thompson M.A.2022-03-21T07:03:46Z2021-12-07T08:33:25ZCDS support team

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

cds-question@unistra.frmolecular-cloudsmillimeter-astronomysubmillimeter-astronomyco-line-emissionG305 star-forming complex was observed in the 3-2 lines of 12 & 13CO to investigate the effect of feedback from the central OB stars on the complex. The region was decomposed into clumps using dendrogram analysis. A catalog of clump properties was created. The surface mass densities of the clumps were plotted as a function of the incident 8um flux. A mask of the region with 8um flux >100MJy/sr was created and clumps were categorized based on the extent of overlap with the mask into "mostly inside", "partly inside" & "outside". The surface mass density distribution of each of these populations were plotted. This was followed by comparing G305 clumps with the Galactic average taken from the ATLASGAL and CHIMPS clumps. Finally, the cumulative distribution functions (CDF) of the clump masses in G305 & their L/M ratios were compared to that of the Galactic sample. The surface mass densities of clumps showed a positive correlation with incident 8um flux. The data did not have sufficient velocity resolution to discern the effects of feedback on the linewidths of the clumps. The sub-sample of clumps named "mostly inside" had the highest surface mass densities followed by "partly -inside" and "outside" sub-samples. These differences between the three sub-samples were shown to be statistically significant using the KS test. The "mostly inside" sample also showed the highest level of fragmentation compared to the other two. These prove that clumps inside the G305 region are triggered. The G305 clump population is also statistically different from the Galactic average population rejecting redistribution as a likely consequence of feedback. The CDFs of clump masses and their L/M ratios are both flatter than the Galactic average, indicating that feedback in G305 has triggered star formation. The collect & collapse method is the dominant mechanism at play in G305.2021A&A...656A.101Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/656/A101CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/656/A101https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/656/A101http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/656/A101https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/656/A101https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/656/A101http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/656/A101GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/656/A101/list (List of fits datacubes)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/656/A101/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/656/A101/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/656/A101/list?GETtext/xml+votable180.050000true197.3872295-62.79741130.0055555555555555566/416552.483060040379131e-20 2.483060040379131e-20https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/656/A101?format=asciiMillimeterRadiodefaultJ/A+A/656/A101/table1Clump properties of 337 clumps extractedalphaVirial parameterphys.mass;arith.ratiofloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[0/336] Cluster ID sequential numbermeta.recordintStrTag[lb] Hierarchical Level: l=leaf, b=branchmeta.codecharXcGalactic x-coordinate in degreesdegpos.cartesian.x;pos.galacticfloatYcGalactic y-coordinate in degreesdegpos.cartesian.y;pos.galacticfloatRadRadius of the structurepcphys.angSize;srcfloatvrmsVelocity linewidth of the clumpkm/sspect.line.widthfloatLumLuminosity of the clumpK.km.pc**2.s**-1phys.luminosityfloatMassMass of clumpsolMassphys.massintnH2H_2_ number densitycm**-3meta.id;meta.mainintF8umAverage incident 8um flux on the clump (using GLIMPSE) (1)MJy/srphot.flux.density;em.IR.8-15umintJ/A+A/656/A101/listList of fits datacubesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGLONGalactic longitude of center (J2000)degpos.galactic.lonGLATGalactic latitude of center (J2000)degpos.galactic.latNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintNzNumber of pixels along Z-axismeta.numberintbVRADLower value of VRAD intervalm/sphys.veloc;pos.heliocentricintBVRADUpper value of VRAD intervalm/sphys.veloc;pos.heliocentricintdVRADVRAD resolutionm/sspect.resolutionintsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fits_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.ranullableindexed_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.decnullableindexed