J/MNRAS/438/426ivo://CDS.VizieR/J/MNRAS/438/426doi:10.26093/cds/vizier.74380426CDSHou L.G.Gao X.Y.2024-08-08T20:12:30Z2015-02-04T13:58:43ZCDS support team

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

cds-question@unistra.frh-ii-regionsinterstellar-mediumstellar-distanceThe expansion of interstellar bubbles is suggested to be an important mechanism of triggering material accumulation and star formation. In this work, we investigate the gaseous environment of a large sample of interstellar bubbles identified by the Spitzer space telescope, aiming to explore the possible evidence of triggered gas accumulation and star formation in a statistical sense. By cross-matching 6124 Spitzer interstellar bubbles from the Milky Way Project (MWP) and more than 2500 Galactic HII regions collected by us, we obtain the velocity information for 818 MWP bubbles. To study the gaseous environment of the interstellar bubbles and get rid of the projection effect as much as possible, we constrain the velocity difference between the bubbles and the ^13^CO(1-0) emission extracted from the Galactic Ring Survey (GRS). Three methods: the mean azimuthally averaged radial profile of ^13^CO emission, the surface number density of molecular clumps and the angular cross-correlation function of MWP bubbles and the GRS molecular clumps are adopted. Significant over density of molecular gas is found to be close to the bubble rims. 60 percent of the studied bubbles were found to have associated molecular clumps. By comparing the clump-associated and the clump-unassociated MWP interstellar bubbles, we reveal that the bubbles in associations tend to be larger and thicker in physical sizes. From the different properties shown by the bubble-associated and bubble-unassociated clumps, we speculate that some of the bubble-associated clumps result from the expansion of bubbles. The fraction of the molecular clumps associated with the MWP bubbles is estimated to be about 20 percent after considering the projection effect. For the bubble-clump complexes, we found that the bubbles in the complexes with associated massive young stellar object(s) (MYSO(s)) have larger physical sizes, hence the complexes tend to be older. We propose that an evolutionary sequence might exist between the relatively younger MYSO-unassociated bubble-clump complexes and the MYSO-associated complexes.2014MNRAS.438..426Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/438/426CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/293 : GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)J/MNRAS/424/2442 : Catalog of bubbles from Milky Way Project (Simpson+, 2012)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/438/426https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/438/426http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/438/426https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/438/426https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/438/426http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/438/426GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/438/426/tablea1 (Matched pairs of MWP bubbles (Milky Way Project, Simpson et al. 2012MNRAS.424.2442S) and Galactic HII regions)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/438/426/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/438/426/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/438/426/tablea1?GETtext/xml+votable180.050000true266.43375-28.802760.0055555555555555565/7207 7275 7377 7383 7578-7579 7605 7654 7673 7679 10543 6/12970-12971 12974-12975 14336 14340 14353-14355 14357 14359 14402-14403 14406 14409 28803 28808-28809 28811-28814 28824-28826 28852 28874-28875 28896-28897 28900-28901 28912-28913 28915-28916 28918-28919 29090-29091 29096-29097 29112 29114-29115 29118-29119 29460-29461 29463 29504-29505 29507 29522-29523 29528-29529 30218-30219 30222 30241 30244-30245 30247 30256-30258 30260 30262-30263 30268-30269 30271 30330 30405 30416-30417 30419 30594 30598 30600-30601 30604-30606 30622-30623 30641 30644-30645 30688 30690-30691 30701 30706-30707 30710 30712-30713 30715 32085 37906 41598-41599 41651 41655 41657-41661 41671 41676-41678 41681-41683 41689 41696-41697 41759 41765-41767 41769-41770 41772-41773 41776-41777 41780-41782 41798 41804-41805 41809 41811 41813-41815 41817 41820 41824 42159 42169-42171 42207 42210-42211 42214-42216 42218 42224-42225 42227-42230 42379 42382 42387 42391-42393 42396-42397 42435 42439-42441 42444-42445 42450-42451 42456-42458 42460-42462 42496-42498 42500 42512 43013 43017-43021 43024 43040https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/438/426?format=asciidefaultJ/MNRAS/438/426/tablea1Matched pairs of MWP bubbles (Milky Way Project, Simpson et al. 2012MNRAS.424.2442S) and Galactic HII regionsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMWPMWP name (1GLLLlll+BbbbbbA)meta.id;meta.maincharGLONBubble Galactic longitudedegpos.galactic.lonGLATBubble Galactic latitudedegpos.galactic.latReffEffective radiusarcminphys.angSizefloatGLON2Associated HII region Galactic longitudedegpos.galactic.lonGLAT2Associated HII region Galactic latitudedegpos.galactic.latfloatRefReference for associated HII region, in refs.dat filepos.framecharVHIILine-of-sight velocity for HII region (1)km/sspect.dopplerVeloc;obs.field;pos.heliocentricfloatD0? Trigonometric or photometric distancekpcpos.distance;pos.heliocentricfloatnullablee_D0? rms uncertainty on D0kpcstat.errorfloatnullabler_D0Reference for D0, in refs.dat filemeta.ref;pos.framecharDK? Kinematic distance (2)kpcpos.distance;pos.heliocentricfloatnullablee_DK? rms uncertainty on DKkpcstat.errorfloatnullableMarkSolution of the kinematical distance (3)meta.codecharr_MarkReference for Mark, in refs.dat filemeta.ref;pos.framecharSimbadSimbad column added by the CDSmeta.ref.urlchar_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data)degpos.eq.ranullableindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data)degpos.eq.decnullableindexedJ/MNRAS/438/426/refsReferencesRefReference codemeta.note;meta.maincharprimaryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBibCodeBicodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorcharComCommentsmeta.notechar