J/A+A/710/A390ivo://CDS.VizieR/J/A+A/710/A390CDSOlofsson H.Khouri T.Muller S.Unnikrishnan R.Groenewegen M.A.T.,Blommaert J.A.D.L.De Beck E.Kastner J.H.Maercker M.Patel N.,Ryde N.Sargent B.A.Srinivasan S.Vlemmings W.H.T.2026-07-01T07:46:51Z2026-07-01T08:46:14ZCDS support team

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

cds-question@unistra.frlate-type-starsstellar-mass-lossradio-astronomymillimeter-astronomyphotometrysubmillimeter-astronomyStars on the asymptotic giant branch (AGB) play important roles in a number of astronomical contexts. To quantify these roles, it is necessary to establish the mass-loss characteristics of stars as they evolve up and beyond the AGB. We used an equidistant sample of 77 AGB stars in the inner Galactic bulge, selected on the existence and strength of OH1612 MHz maser emission, to obtain information on the mass loss of O-rich AGB stars, and on its transformations in geometry and kinematics that occur at the tip of the AGB. Observations of circumstellar lines from several rotational transitions of 12CO, 13CO, and C18O were performed with the Atacama Large Millimeter/submillimeter Array (ALMA), and, for a sub-sample, with the Atacama Pathfinder EXperiment telescope (APEX). The ALMA observations also provide continuum data. Existing infrared photometry was used to estimate colours and produce stellar light curves. Based on mid-infrared colour, CO line, and near-infrared variability characteristics, the objects were divided into four categories of distinct stellar and/or circumstellar properties. Various circumstellar CO line characteristics are presented and compared between the categories, such as morphologies and extents of brightness distributions (BDs), line profiles (LPs), line intensity ratios, and kinematics. A majority of the objects form a homogenous group with sharply, centrally peaked BDs and LPs of the soft-parabola type, while the rest show extended and complex BDs and/or LPs with high-velocity wings. The C^18^O line and ALMA continuum detection rates vary significantly between the categories. CO line emission is also detected from interaction zones where the expanding circumstellar gas meets the interstellar medium. These data provide the foundation for more detailed studies, including radiative transfer analyses of the CO line and photometry data, on the evolution of stellar and circumstellar characteristics of O-rich stars on the upper AGB and beyond.2026A&A...710A.390Ohttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/710/A390CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/710/A390https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/710/A390http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/710/A390https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/710/A390https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/710/A390http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/710/A390GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/710/A390/tablec1a (ALMA CO line and continuum data, part 1)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/710/A390/tablec1a?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/710/A390/tablec1a?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/710/A390/tablec1a?GETtext/xml+votable180.050000true264.9896761-31.5991550.0055555555555555565/7206-7207 7213 7218 6/28807 28813 28815 28818-28820 28822-28823 28837 28839 28848-28850 28856-28857 28867 288967.089894440229571e-23 2.239611514764107e-22https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/710/A390?format=asciiMillimeterRadiodefaultJ/A+A/710/A390/tablec1aALMA CO line and continuum data, part 1recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceSource namemeta.id;meta.maincharvsysSystemic velocity (in LSR scale)km/sphys.velocintvinftyGas expansion velocitykm/sphys.veloc.expansionintvtot? Total velocity widthkm/sphys.velocintnullableSnu107? Continuum flux densities at 107GHzmJyphot.flux.density;em.mm.100-200GHzfloatnullableSnu233? Continuum flux densities at 233GHzmJyphot.flux.density;em.mm.200-400GHzfloatnullableSnu338? Continuum flux densities at 338GHzmJyphot.flux.density;em.mm.200-400GHzfloatnullableCommCommentsmeta.notecharSimbadSimbad column added by the CDSmeta.ref.urlchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/710/A390/tablec1bALMA CO line and continuum data, part 2recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceSource namemeta.id;meta.maincharLineLinemeta.id;spect.linecharSnu05? Line flux density within aperture 0.5"Jyphot.fluxfloatnullableint(Snu*dnu)05? Line velocity-integrated flux density within aperture 0.5"Jy.km/sphot.fluxfloatnullableSnu10? Line flux density within aperture 1.0"Jyphot.fluxfloatnullableint(Snu*dnu)10? Line velocity-integrated flux density within aperture 1.0"Jy.km/sphot.fluxfloatnullableSnu20? Line flux density within aperture 2.0"Jyphot.fluxfloatnullableint(Snu*dnu)20? Line velocity-integrated flux density within aperture 2.0"Jy.km/sphot.fluxfloatnullableSnu30? Line flux density within aperture 3.0"Jyphot.fluxfloatnullableint(Snu*dnu)30? Line velocity-integrated flux density within aperture 3.0"Jy.km/sphot.fluxfloatnullabletheta01? Angular extent at which the fit to the AARP reaches 10% of its peak valuearcsecphys.angSizefloatnullable