J/A+A/623/A141ivo://CDS.VizieR/J/A+A/623/A141doi:10.26093/cds/vizier.36230141CDSFigueira M.Lopez-Calderon C.Bronfman L.Zavagno A.Hervias-Caimapo C.,Duronea N.Nyman L-A.2019-03-26T12:20:17Z2019-03-25T14:17:31ZCDS support team

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

cds-question@unistra.frh-ii-regionsmolecular-cloudsradio-astronomymillimeter-astronomysubmillimeter-astronomyThe star formation process requires the dust and gas present in the Milky Way to self-assemble into dense reservoirs of neutral material where the new generation of stars will emerge. Star-forming regions are usually studied in the context of Galactic surveys, but dedicated observations are sometimes needed when the study reaches beyond the survey area. A better understanding of the star formation process in the Galaxy can be obtained by studying several regions. This allows increasing the sample of objects (clumps, cores, and stars) for further statistical works and deeper follow-up studies. Here, we studied the G345.5+1.5 region, which is located slightly above the Galactic plane, to understand its star formation properties. We combined Large Apex BOlometer CAmera (LABOCA) and ^12^CO(4-3) transition line (NANTEN2) observations complemented with the Hi-GAL and Spitzer-GLIMPSE surveys to study the star formation toward this region. We used the Clumpfind algorithm to extract the clumps from the 870um and ^12^CO(4-3) data. Radio emission at 36cm was used to estimate the number of HII regions and to remove the contamination from the free-free emission at 870um. We employed color-color diagrams and spectral energy distribution (SED) slopes to distinguish between prestellar and protostellar clumps.We studied the boundedness of the clumps through the virial parameter. Finally, we estimated the star formation efficiency (SFE) and star formation rate (SFR) of the region and used the Schmidt-Kennicutt diagram to compare its ability to form stars with other regions of the Galactic plane. Of the 13 radio sources that we found using the MGPS-2 catalog, 7 are found to be associated with Hii regions corresponding to late-B or early-O stars. We found 45 870um clumps with diameters between 0.4 and 1.2pc and masses between 43M_{sun}_ and 3923M_{sun}_, and 107 ^12^CO clumps with diameters between 0.4 pc and 1.3pc and masses between 28M_{sun}_ and 9433M_{sun}_. More than 50% of the clumps are protostellar and bounded and are able to host (massive) star formation. High SFR and SFR density (S FR) values are associated with the region, with an SFE of a few percent. With submillimeter, CO transition, and short-wavelength infrared observations, our study reveals a population of massive stars, protostellar and bound starless clumps, toward G345.5+1.5. This region is therefore actively forming stars, and its location in the starburst quadrant of the Schmidt-Kennicutt diagram is comparable to other star-forming regions found within the Galactic plane.2019A&A...623A.141Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/623/A141CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/534/A131 : Clumps in the giant molecular cloud G345.5+1.0 (Lopez+, 2011)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/623/A141https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/623/A141http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/623/A141https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/623/A141https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/623/A141http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/623/A141GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/623/A141/tablea1 (Physical parameters of the 870um clumps)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/623/A141/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/623/A141/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/623/A141/tablea1?GETtext/xml+votable180.050000true254.92304-40.053810.005555555555555556Cone search capability for table J/A+A/623/A141/tablea2 (Physical parameters of the Hi-GAL clumps)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/623/A141/tablea2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/623/A141/tablea2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/623/A141/tablea2?GETtext/xml+votable180.050000true254.59571-40.731850.005555555555555556Cone search capability for table J/A+A/623/A141/tablea3 (Physical parameters of the ^12^CO clumps)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/623/A141/tablea3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/623/A141/tablea3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/623/A141/tablea3?GETtext/xml+votable180.050000true255.12429-40.57790.005555555555555556Cone search capability for table J/A+A/623/A141/list (List of fits images)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/623/A141/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/623/A141/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/623/A141/list?GETtext/xml+votable180.050000true255.3207801-39.93291640.0055555555555555566/42395 42398 424172.283270615984385e-22 2.283270615984385e-22https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/623/A141?format=asciiMillimeterRadiodefaultJ/A+A/623/A141/tablea1Physical parameters of the 870um clumpsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintId[1/45] Clump Indentification numbermeta.id;meta.mainintGLONGalactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latDiamDiameterpcpos.distancefloatFluxIntegrated flux at 870umJyphot.flux.density;em.mm.200-400GHzfloatFFContPercentage of contamination by free-free emission%instr.backgroundintMassMass of the clumpsolMassphys.massintColDensColumn Density of the clumpcm**-2phys.columnDensitydoubleVolDensVolume Density of the clumpcm**-3phys.densitydoubleIR[Y/N] Presence (Y) or absence (N) of IR counterparts for the clumpmeta.codechar_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.decnullableindexedJ/A+A/623/A141/tablea2Physical parameters of the Hi-GAL clumpsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintId[1/79] Clump Indentification numbermeta.id;meta.mainintGLONGalactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latTempTemperature of the clumpKphys.temperaturefloate_TempUncertainty on the temperatureKstat.errorfloatMassMass of the clumpsolMassphys.massinte_MassMass of the clumpsolMassstat.error;phys.massintLbolBolometric luminositysolLumphys.luminosityinte_LbolUncertainty of the bolometric luminositysolLumstat.errorintLRatioSubmillimetric to bolometric luminosity ratio%phys.luminosity;arith.ratiofloatIRNature of the source (Prestellar or Protostellar)meta.codechar_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.decnullableindexedJ/A+A/623/A141/tablea3Physical parameters of the ^12^CO clumpsDiamDiameterpcpos.distancefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintId[1/95] Clump Indentification numbermeta.id;meta.mainintGLONGalactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latMassMass of the clumpsolMassphys.massintLineWLine width of the clumpkm/sspect.line.widthfloat_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.decnullableindexedJ/A+A/623/A141/listList of fits imagesrecnoRecord 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.numberintNz? Number of slices, for the datacubemeta.numberintnullablebVRAD? Lower value of VRAD interval, for the datacubekm/sphys.veloc;pos.heliocentricfloatnullableBVRAD? Upper value of VRAD interval, for the datacubekm/sphys.veloc;pos.heliocentricfloatnullabledVRAD? VRAD resolution, for the datacubekm/spos.angResolutionfloatnullablesizeSize 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