J/MNRAS/442/2240ivo://CDS.VizieR/J/MNRAS/442/2240doi:10.26093/cds/vizier.74422240CDSWalsh A.J.Purcell C.R.Longmore S.N.Breen S.L.Green J.A.,Harvey-Smith L.Jordan C.H.2024-08-09T20:15:24Z2014-06-25T09:18:14ZCDS support team

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

cds-question@unistra.frastrophysical-masersradio-astronomyastrometryWe report on high spatial resolution water maser observations, using the Australia Telescope Compact Array, towards water maser sites previously identified in the H2O southern Galactic Plane Survey (HOPS) within the area covering Galactic coordinates from l=290 to l=30 and b=-0.5 to b=+0.5. Of the 540 maser sites identified in the single-dish observations of Walsh et al. (2011MNRAS.416.1764W, Cat. J/MNRAS/416/1764), we detect emission in all but 31 fields. These maser sites together comprise 2790 individual spectral features (maser spots), with brightnesses ranging from 0.06Jy to 576Jy and with velocities ranging from -238.5 to +300.5km/s. Based on a definition of maser site size of 4-arcsec (except for G000.667+0.028, also known as Sgr B2, which we treat as a special case), we identify 631 maser sites. We have compared the positions of these sites to the literature to associate the sites with astrophysical objects. We identify 433 (69%) with star formation, 121 (19%) with evolved stars and 77 (12%) as unknown. Comparing the properties of maser sites of different origins, we find that those associated with evolved stars tend to have more maser spots and have smaller angular sizes than those associated with star formation. We present evidence that maser sites associated with evolved stars show an increased likelihood of having a velocity range between 15 and 35 km/s compared to other maser sites. We suggest this is because many of these maser sites are associated with the circumstellar shells of the evolved stars, which are expanding at these velocities. Of the 31 non-detections, we conclude they were not detected due to intrinsic variability and confirm previous results showing that such variable masers tend to be weaker and have simpler spectra with fewer peaks. Of the small number of maser sites showing linear features, we find evidence for lines that are both perpendicular and parallel to known outflows, suggesting that in star formation, H_2_O maser origins may be as varied and as complex as those of class II methanol masers.2014MNRAS.442.2240Whttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/442/2240CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVIII/96 : 6-GHz methanol multibeam maser catalogue (Caswell+, 2010-12)J/MNRAS/416/1764 : H_2_O Southern Galactic Plane Survey (HOPS) (Walsh+, 2011)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/442/2240https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/442/2240http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/442/2240https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/442/2240https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/442/2240http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/442/2240GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/442/2240/table2 (Details of maser spots, based on ATCA observations)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/442/2240/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/442/2240/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/442/2240/table2?GETtext/xml+votable180.050000true266.64404167-28.999492780.0055555555555555565/7206 7228 10542 6/28808-28809 28812-28813 28828 28830-28831 28874-28875 28900-28901 28916 28918-28919 29090-29091 29096-29097 29100-29102 29114-29115 29118-29119 29460-29461 29504-29505 29507-29508 29510-29511 29522 29529 29532-29533 29535 30218-30219 30222 30244-30245 30247 30256 30258-30259 37895 37902-37903 37924 37926 41653-41655 41657-41658 41660 41662 41673 41675-41677 41681-41685 41688 41697 41759 41766-41767 41769-41770 41772 41776-41778 41780 41802 41804-41805 41807 41811 41813-41817 42155 42158-42159 42172-42173 42206-42207 42210-42211 42214-42217 42224-42226 42228-42229 42379 42381-42383 42390-42393 42396-42397 42434-42435 42438 42440-42441 42444-42445 42450-42451 42454-42457 42460-42461 42496-42498 42500-42501 43013-43015 43019 43040https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/442/2240?format=asciiRadiodefaultJ/MNRAS/442/2240/table2Details of maser spots, based on ATCA observationsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of maser site (GLLL.lll+B.bbb)meta.id;meta.maincharm_NameName of maser spot (AA)meta.code.multipcharn_Name[*] * indicates strongest spot in sitemeta.notecharRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainSpPeak flux density of H2O maserJyphot.flux.density;em.radio.12-30GHzfloatVpPeak velocity of H2O maserkm/sphys.veloc;stat.maxfloaterrMajRelative uncertainty in position major axisarcsecstat.errorfloaterrMinRelative uncertainty in position minor axisarcsecstat.errorfloaterrPA[-90/90] Relative uncertainty and beam position angledegstat.error;pos.posAng;instr.beamfloatBmajSynthesized beam major axisarcsecphys.angSizefloatBminSynthesized beam minor axisarcsecphys.angSize;srcfloatJ/MNRAS/442/2240/table3Associations with the water maser sitesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of maser site (GLLL.lll+B.bbb)meta.id;meta.maincharprimaryNsNumber of spots in this source (table2)meta.numberintnullableMeth[Y/N] Association with Methanol maser ?meta.codecharNH3[Y/N] Association with HOPS Ammonia ?meta.codecharRMSAssociation based on RMS catalogue (1)meta.codecharPapIAssociation based on HOPS Paper I, Walsh et al. 2011 (J/MNRAS/416/1764)meta.codecharGLIMPSEAssociation based on GLIMPSE images (2)meta.codecharASS-RESAssignment and Reason (3)meta.codechar