J/A+A/604/A6ivo://CDS.VizieR/J/A+A/604/A6doi:10.26093/cds/vizier.36040006CDSSanchez-Monge A.Schilke P.Schmiedeke A.Ginsburg A.,Cesaroni R.Lis D.C.Qin S.-L.Mueller H.S.P.Bergin E.,Comito C.Moeller T.2017-09-04T13:30:33Z2017-07-26T08:38:06ZCDS support team

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

cds-question@unistra.frinterstellar-mediummolecular-cloudsradio-continuum-emissionyoung-stellar-objectsThe two hot molecular cores SgrB2(M) and SgrB2(N), which are located at the center of the giant molecular cloud complex Sagittarius B2, have been the targets of numerous spectral line surveys, revealing a rich and complex chemistry. We seek to characterize the physical and chemical structure of the two high-mass star-forming sites SgrB2(M) and SgrB2(N) using high-angular resolution observations at millimeter wavelengths, reaching spatial scales of about 4000au. We used the Atacama Large Millimeter/submillimeter Array (ALMA) to perform an unbiased spectral line survey of both regions in the ALMA band 6 with a frequency coverage from 211GHz to 275GHz. The achieved angular resolution is 0.4-arcsec, which probes spatial scales of about 4000au, i.e., able to resolve different cores and fragments. In order to determine the continuum emission in these line-rich sources, we used a new statistical method, STATCONT, which has been applied successfully to this and other ALMA datasets and to synthetic observations. We detect 27 continuum sources in SgrB2(M) and 20 sources in SgrB2(N). We study the continuum emission variation across the ALMA band 6 (i.e., spectral index) and compare the ALMA 1.3mm continuum emission with previous SMA 345GHz and VLA 40GHz observations to study the nature of the sources detected. The brightest sources are dominated by (partially optically thick) dust emission, while there is an important degree of contamination from ionized gas free-free emission in weaker sources. While the total mass in SgrB2(M) is distributed in many fragments, most of the mass in SgrB2(N) arises from a single object, with filamentary-like structures converging toward the center. There seems to be a lack of low-mass dense cores in both regions. We determine H2 volume densities for the cores of about 10^7^-10^9^cm^-3^ (or 10^5^-10^7^M_{sun}_/pc^3^), i.e., one to two orders of magnitude higher than the stellar densities of super star clusters. We perform a statistical study of the chemical content of the identified sources. In general, SgrB2(N) is chemically richer than SgrB2(M). The chemically richest sources have about 100 lines per GHz and the fraction of luminosity contained in spectral lines at millimeter wavelengths with respect to the total luminosity is about 20%-40%. There seems to be a correlation between the chemical richness and the mass of the fragments, where more massive clumps are more chemically rich. Both SgrB2(N) and SgrB2(M) harbor a cluster of hot molecular cores. We compare the continuum images with predictions from a detailed 3D radiative transfer model that reproduces the structure of SgrB2 from 45pc down to 100au. This ALMA dataset, together with other ongoing observational projects in the range 5GHz to 200GHz, better constrain the 3D structure of SgrB2 and allow us to understand its physical and chemical structure.2017A&A...604A...6Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/604/A6CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJS/117/427 : Sgr B2 spectral survey (Nummelin+, 1998)J/ApJS/158/188 : Detection of glycolaldehyde toward Sgr B2 (Widicus+, 2005)J/A+A/482/179 : Interferometric study of SgrB2(N) (Belloche+, 2008)J/A+A/559/A47 : Sgr B2(N) and Sgr B2(M) IRAM 30m line survey (Belloche+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/604/A6https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/604/A6http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/604/A6https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/604/A6https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/604/A6http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/604/A6GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/604/A6/list (List of fits images)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/604/A6/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/604/A6/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/604/A6/list?GETtext/xml+votable180.050000true266.83398-28.38460.0055555555555555566/28830https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/604/A6?format=asciiRadiodefaultJ/A+A/604/A6/listList of fits imagesrecnoRecord 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.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintObs.DateObservation date *YYYY-MM-DDThh:mm:ss.ssssss)time.epoch;obscharsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar