J/A+A/629/A10ivo://CDS.VizieR/J/A+A/629/A10doi:10.26093/cds/vizier.36290010CDSBosco F.Beuther H.Ahmadi A.Mottram J.C.Kuiper R.Linz H.,Maud L.T.Winters J.M.Henning T.Feng S.Peters T.Semenov D.,Klaassen P.D.Schilke P.Urquhart J.S.Beltran M.T.Lumsden S.L.,Leurini S.Moscadelli L.Cesaroni R.Sanchez-Monge A.Palau A.,Pudritz R.Wyrowski F.Longmore S.2019-08-23T08:36:15Z2019-08-23T07:44:03ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectsmillimeter-astronomysubmillimeter-astronomyThe formation process of high-mass stars (>8M_{sun}_) is poorly constrained, particularly, the effects of clump fragmentation creating multiple systems and the mechanism of mass accretion onto the cores. We study the fragmentation of dense gas clumps, and trace the circumstellar rotation and outflows by analyzing observations of the high-mass (~500M_{sun}_) star-forming region IRAS 23033+5951. Using the Northern Extended Millimeter Array (NOEMA) in three configurations and the IRAM 30-m single-dish telescope at 220GHz, we probe the gas and dust emission at an angular resolution of ~0.45", corresponding to 1900au. In the mm continuum emission, we identify a protostellar cluster with at least four mm-sources, where three of them show a significantly higher peak intensity well above a signal-to-noise ratio of 100. Hierarchical fragmentation from large to small spatial scales is discussed. Two fragments are embedded in rotating structures and drive molecular outflows, traced by ^13^CO (2-1) emission. The velocity profiles across two of the cores are similar to Keplerian but are missing the highest velocity components close to the center of rotation, which is a common phenomena from observations like these, and other rotation scenarios are not excluded entirely. Position-velocity diagrams suggest protostellar masses of ~6 and 19M_{sun}. Rotational temperatures from fitting CH_3_CN (12_K_-11_K_) spectra are used for estimating the gas temperature and by that the disk stability against gravitational fragmentation, utilizing Toomre's Q parameter. Assuming that the candidate disk is in Keplerian rotation about the central stellar object and considering different disk inclination angles, we identify only one candidate disk to be unstable against gravitational instability caused by axisymmetric perturbations. The dominant sources cover different evolutionary stages within the same maternal gas clump. The appearance of rotation and outflows of the cores are similar to those found in low-mass star-forming regions.2019A&A...629A..10Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/629/A10CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/629/A10https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/629/A10http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/629/A10https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/629/A10https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/629/A10http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/629/A10GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/629/A10/list (Description of FITS files)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/629/A10/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/629/A10/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/629/A10/list?GETtext/xml+votable180.050000true346.3542960.137760.0055555555555555566/14307https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/629/A10?format=asciiMillimeterdefaultJ/A+A/629/A10/listDescription of FITS filesrecnoRecord 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.mainScale[0.074] Scale of the imagearcsec/pixinstr.scalefloatNx[403/1024] Number of pixels along X-axismeta.numberintNy[403/1024] Number of pixels along Y-axismeta.numberintNz[31/1001]? Number of slices for datacubesmeta.numberintnullableRVmin[-2754/-64]? Lower value of radial velocity interval for data cubeskm/sphys.veloc;pos.heliocentricfloatnullableRVmax[-41/2647]? Upper value of radial velocity interval for data cubeskm/sphys.veloc;pos.heliocentricfloatnullabledRV[0.5/5.4]? Velocity resolutionkm/sspect.resolutionfloatnullableFreq[217/221]? Frequency of line observedGHzem.freq;spect.linefloatnullablesize[642/4100105] Size of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the filemeta.title;meta.file