J/A+A/667/A137ivo://CDS.VizieR/J/A+A/667/A137doi:10.26093/cds/vizier.36670137CDSBoegner R.Csengeri T.Montillaud J.Wienen M.Schneider N.,Wyrowsky F.Motte F.Toth L.V.2024-11-28T20:01:04Z2022-11-18T09:30:18ZCDS support team

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

cds-question@unistra.frinterstellar-mediummolecular-cloudsradio-astronomyThe Rosette molecular cloud complex is a well-known Galactic star forming region with a morphology pointing towards triggered star formation. The distribution of its young stellar population and the gas properties question whether star formation could be globally triggered in the region. We focus on the characterisation of the most massive pre- and protostellar cores distributed throughout the molecular cloud to help the understanding of the star formation processes in the region. We observed a sample of 33 dense cores, identified in Herschel continuum maps, with the Effelsberg 100-m telescope. Using NH_3_ (1,1) and (2,2) measurements we characterise the dense core population computing rotational and gas kinetic temperatures and NH3 column density with multiple methods. We also estimate the gas pressure ratio and virial parameters to examine the stability of the cores. Using results from Herschel data we examine possible correlations between gas and dust parameters. Ammonia emission is detected toward 31 out of the 33 selected targets. We estimate kinetic temperatures between 12 and 20K, and column densities within the 10^14^-2x10^15^cm^-2^ range in the selected targets. The virial analysis suggests that most sources are likely to be gravitationally bound, while the linewidths are dominated by non-thermal motions. Our results are compatible with large scale dust temperature maps suggesting that the temperature decreases and column density increases with distance from NGC 2244 except for the densest protoclusters. We also identify a small spatial shift between the ammonia and dust peaks in the regions most exposed to irradiation from the nearby NGC 2244 stellar cluster. However, we find no trends in terms of core evolution with spatial location, in the number of prestellar to protostellar core ratio or the virial parameter. Star formation is more likely based on the primordial structure of the cloud in spite of the impact of irradiation from the nearby cluster, NGC 2244. The physical parameters from the NH_3_ measurements suggest gas properties in between those of low- and high-mass star forming regions, suggesting that the Rosette molecular cloud could host on-going intermediate mass star formation, and is unlikely to form high-mass stars.2022A&A...667A.137Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/667/A137CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/667/A137https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/667/A137http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/667/A137https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/667/A137https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/667/A137http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/667/A137GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/667/A137/table1 (The parameters of the RMC dense cores from Motte et al. (2010A&A...518L..77M) and Hennemann et al. (2010A&A...518L..84H) selected for our sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/667/A137/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/667/A137/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/667/A137/table1?GETtext/xml+votable180.050000true98.65491674.21261110.0055555555555555566/22243 22249 22252https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/667/A137?format=asciiRadiodefaultJ/A+A/667/A137/table1The parameters of the RMC dense cores from Motte et al. (2010A&A...518L..77M) and Hennemann et al. (2010A&A...518L..84H) selected for our samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource numbermeta.id;meta.mainintRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainAreaLocation of the sourceobs.fieldcharTypeEvolutionary stagetime.agecharFWHMGeometric average of deconvolved major and minor FWHM of the source Gaussian ellipsepcphys.angSize;stat.meanfloatTdustDust temperatureKphys.temperatureintLbol? Bolometric luminositysolLumphys.luminosityintnullableM350MasssolMassphys.massfloatn_M350Note on Mass (1)meta.notecharSample[rce] Sample (2)src.samplecharsp1Show the NH3 (1,1) spectrummeta.ref.urlcharsp2Show the NH3 (2,2) spectrummeta.ref.urlcharJ/A+A/667/A137/table2Parameters calculated from the NH_3_ (1,1) and (2,2) lines with errors obtained from Monte Carlo (MC) calculationTkinOKinetic temperature calculated according to Ott et al. (2011ApJ...742...95O)Kphys.temperature;meta.modelledfloate_TkinOError in kinetic temperature calculated according to Ott et al. (2011ApJ...742...95O), from MC calculationsKstat.errorfloatTkinTKinetic temperature calculated according to Tafalla et al. (2004A&A...416..191T)Kphys.temperature;meta.modelledfloate_TkinTError in kinetic temperature calculated according to Tafalla et al. (2004A&A...416..191T) from MC calculationsKstat.errorfloatNtotFrNH_3_ column density calculated according to Friesen et al. (2009ApJ...697.1457F)1e+14cm**-2phys.columnDensity;meta.modelledfloate_NtotFrError in NH_3_ column density calculated according to Friesen et al. (2009ApJ...697.1457F) from MC calculations1e+14cm**-2stat.errorfloatNtotLNH_3_ column density calculated according to Lu et al. (2014ApJ...790...84L, Cat. J/ApJ/790/84) from MC calculations1e+14cm**-2phys.columnDensity;meta.modelledfloate_NtotLError in NH_3_ column density calculated according to Lu et al. (2014ApJ...790...84L, Cat. J/ApJ/790/84) from MC calculations1e+14cm**-2stat.errorfloatRpGas pressure ratiophys.pressurefloatMvirVirial masssolMassphys.massfloatalphavirVirial parameterphys.mass;arith.ratiofloate_TrotError in rotational temperatureKstat.errorfloatTexExcitation temperatureKphys.atmol.excitationfloatFlag[*] Flag (1)meta.code.errorcharnH2H2 volume density1000cm**-3phys.densityfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource numbermeta.id;meta.mainintSampleSamplesrc.samplecharTrotRotational temperatureKphys.temperaturefloatJ/A+A/667/A137/tableb1The parameters of the NH_3_ (1,1) and (2,2) lines obtained from CLASSrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource numbermeta.id;meta.mainintType[0/2] Evolutionary stage (1)time.ageintFWHM22? NH_3_ (2,2) FWHMkm/sspect.line.widthfloatnullableTantxtau? Antenna temperature times optical depthstat.fit.paramfloatnullablee_Tantxtau? Antenna temperature times optical depth errorstat.errorfloatnullablev11? NH_3_ (1,1) line velocitykm/sspect.dopplerVelocfloatnullablee_v11? NH_3_ (1,1) line velocity errorkm/sstat.errorfloatnullableT11? NH_3_ (1,1) main beam brightness temperatureKphys.temperature;meta.mainfloatnullablee_T11? NH_3_ (1,1) main beam brightness temperature errorKstat.errorfloatnullableSN11? signal to noise ratio of NH_3_ (1,1) linestat.snrfloatnullableArea22? NH_3_ (2,2) line areaK.km/sphys.area;spect.linefloatnullablee_Area22? NH_3_ (2,2) line area errorK.km/sstat.errorfloatnullablev22? NH_3_ (2,2) line velocitykm/sspect.dopplerVelocfloatnullableFWHM11? NH_3_ (1,1) FWHMkm/sspect.line.widthfloatnullablee_FWHM11? NH_3_ (1,1) FWHM errorkm/sstat.errorfloatnullabletau11? NH_3_ (1,1) main hyperfine component optical depthphys.absorption.opticalDepth;meta.mainfloatnullablee_tau11? NH_3_ (1,1) main hyperfine component optical depth errorstat.errorfloatnullablee_v22? NH_3_ (2,2) line velocity errorkm/sstat.errorfloatnullablee_FWHM22? NH_3_ (2,2) FWHM errorkm/sstat.errorfloatnullableT22? NH_3_ (2,2) main beam brightness temperatureKphys.temperature;meta.mainfloatnullablee_T22? NH_3_ (2,2) main beam brightness temperature errorKstat.errorfloatnullableSN22? signal to noise ratio of NH_3_ (2,2) linestat.snrfloatnullableSample[rce] Sample (2)src.samplechar