J/A+A/567/A116ivo://CDS.VizieR/J/A+A/567/A116doi:10.26093/cds/vizier.35670116CDSFrau P.Girart J.M.Zhang Q.Rao R.2015-01-15T17:32:00Z2014-07-24T11:57:21ZCDS support team

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

cds-question@unistra.frprotostarsmagnetic-fieldsinterferometryinterstellar-mediumNGC 7538 IRS 1-3 is a high-mass star-forming cluster with several detected dust cores, infrared sources, (ultra)compact HII regions, molecular outflows, and masers. In such a complex environment, interactions and feedback among the embedded objects are expected to play a major role in the evolution of the region. We study the dust, kinematic, and polarimetric properties of the NGC 7538 IRS 1-3 region to investigate the role of the different forces in the formation and evolution of high-mass star-forming clusters. Methods: We performed SMA high angular resolution observations at 880um with the compact configuration. We developed the RATPACKS code to generate synthetic velocity cubes from models of choice to be compared to the observational data. To quantify the stability against gravitational collapse we developed the "mass balance" analysis that accounts for all the energetics on core scales. We detect 14 dust cores from 3.5M_{sun}_ to 37M_{sun}_ arranged in two larger scale structures: a central bar and a filamentary spiral arm. The spiral arm presents large-scale velocity gradients in H^13^CO^+^ 4-3 and C^17^O 3-2, and magnetic field segments aligned well to the dust main axis. The velocity gradient is reproduced well by a spiral arm expanding at 9km/s with respect to the central core MM1, which is known to power a large precessing outflow. The energy of the outflow is comparable to the spiral-arm kinetic energy, which dominates gravitational and magnetic energies. In addition, the dynamical ages of the outflow and spiral arm are comparable. On core scales, those embedded in the central bar seem to be unstable against gravitational collapse and prone to forming high-mass stars, while those in the spiral arm have lower masses that seem to be supported by non-thermal motions and magnetic fields. The NGC 7538 IRS 1-3 cluster seems to be dominated by protostellar feedback. The dusty spiral arm appears to be formed in a snowplow fashion owing to the outflow from the MM1 core. We speculate that the external pressure from the redshifted lobe of the outflow could trigger star formation in the spiral arm cores. This scenario would form a small cluster with a few central high-mass stars, surrounded by a number of low-mass stars formed through protostellar feedback.2014A&A...567A.116Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/567/A116CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJ/696/471 : MIR spectroscopy of NGC 7538 IRS 1 (Knez+, 2009)J/A+A/543/A88 : NGC 7538 IRS 1 and NGC 7538 S 1.36mm maps (Beuther+, 2012)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/567/A116https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/567/A116http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/567/A116https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/567/A116https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/567/A116http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/567/A116GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/567/A116/table1 (Parameters of the 878{mu}m continuum sources)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/567/A116/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/567/A116/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/567/A116/table1?GETtext/xml+votable180.050000true348.4389541761.4695750.005555555555555556Cone search capability for table J/A+A/567/A116/list (List of FITS files)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/567/A116/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/567/A116/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/567/A116/list?GETtext/xml+votable180.050000true348.4390961.469510.0055555555555555566/143172.2621401108608354e-22 2.2621401108608354e-22https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/567/A116?format=asciidefaultJ/A+A/567/A116/table1Parameters of the 878{mu}m continuum sourcesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSrcSource designation (1 to 13)meta.id;meta.maincharRAJ2000Right Ascension J2000pos.eq.ra;meta.mainDEJ2000Declination J2000pos.eq.dec;meta.mainIpkPeak intensity I_peak_ at 341.4GHz (in Jy/beam)Jyphot.flux.density;em.mm.200-400GHzfloatSFlux at 341.4GHzJyphot.flux.density;em.mm.200-400GHzfloate_SMean error on 341.4GHz fluxJystat.errorfloatDiamSource diameter in 10^3^AU (1)(1000AU)phys.angSizefloatTdDust temperature (2)Kphys.temperatureintNH2H_2_ column density1e+23cm**-2phys.columnDensityfloatnH2H_2_ density1e+06cm**-3phys.densityfloatMassMass of source (3)solMassphys.massfloatJ/A+A/567/A116/listList of FITS filesfitsDownload the FITS filemeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainScaleScale of the imagearcsec/pixinstr.scalefloatNx[128] Number of pixels along X-axismeta.numberintNy[128] Number of pixels along Y-axismeta.numberintNz[6/12]? Number of slices for datacubesmeta.numberintnullablebVel[-68.0/-66.7]? Lower value of LSR velocity interval for data cubes (VELO-LSR)km/sphys.velocfloatnullableBVel[-60.8/-59.2]? Upper value of LSR velocity interval for data cubes (VELO-LSR)km/sphys.velocfloatnullabledVel[705/1400]? Velocity resolutionm/sspect.resolutionintnullableFreq[341.47]? LSR frequency, for maps (FREQ-LSR)GHzem.freqfloatnullablesize[96/799] Size of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the filemeta.note