J/A+A/677/A107ivo://CDS.VizieR/J/A+A/677/A107doi:10.26093/cds/vizier.36770107CDSDuchene Q.Hottier C.Lallement R.Vergely J.L.Babusiaux C.,Marchal A.Arenou F.2024-11-06T20:05:40Z2023-09-13T08:07:44ZCDS support team

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

cds-question@unistra.frmolecular-cloudsstellar-distanceradial-velocityThree-dimensional (3D) kinetic maps of the Milky Way interstellar medium are an essential tool in studies of its structure and of star formation. We aim to assign radial velocities to Galactic interstellar clouds now spatially localized based on starlight extinction and star distances from Gaia and stellar surveys. We developed an automated search for coherent projections on the sky of clouds isolated in 3D extinction density maps on the one hand, and regions responsible for CO radio emissions at specific Doppler shifts on the other hand. The discrete dust structures were obtained by application of the Fellwalker algorithm to a recent 3D extinction density map. For each extinction cloud, a technique using a narrow sliding spectral window moved along the contour-bounded CO spectrum and geometrical criteria was used to select the most likely velocity interval. We applied the new contour-based technique to the 3D extinction density distribution within the volume encompassing the Taurus, Auriga, Perseus, and California molecular complexes. From the 45 clouds issued from the decomposition, 42 were assigned a velocity. The remaining structures correspond to very weak CO emission or extinction. We used the non-automated assignments of radial velocities to clouds of the same region presented in Paper I (Ivanova et al., 2021A&A...652A..22I) and based on KI absorption spectra as a validation test. The new fully automated determinations were found to be in good agreement with these previous measurements. Our results show that an automated search based on cloud-contour morphology can be efficient and that this novel technique may be extended to wider regions of the Milky Way and at larger distance. We discuss its limitations and potential improvements after combination with other techniques.2023A&A...677A.107Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A107CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/677/A107https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/677/A107http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/677/A107https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/677/A107https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/677/A107http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/677/A107GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/677/A107/table2 (3D position and assigned LSR velocity of each channel barycenter of the clumps)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/677/A107/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/677/A107/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/677/A107/table2?GETtext/xml+votable180.050000true348.7437957.203610.0055555555555555563/16 378-379 4/21 68 70-74 76-77 1469-1471 5/81 83 92-93 95 210-211 214-215 217 220-221 276 278 300-302 312-313 315-318 330 352 354 360 363 385-388 393 397 401-404 406 408-409 449 451 456 458 763 795-796 3551 3569 3571-3574 5873-5875 6030-6031 6042-6043 6114-6115 6120 6/277 320-321 323 329-331 352-353 357 365 376-377 379 469 471 477 479 501 503 839 850-851 854-855 864-865 867 877 888 1108-1110 1116 1118-1119 1212-1214 1256-1257 1259 1276-1277 1290 1312 1314-1315 1326 1412 1414 1422 1444 1448 1464 1466 1537-1539 1556 1559 1562 1565-1569 1571 1581 1583-1584 1586 1592 1594 1601-1603 1628 1630 1640-1641 1644 1648-1649 1663 1749 1801 1803 1828 1830 1836 1920 3002-3003 3006-3007 3050 3161-3164 3173-3175 3177 3179 3192 3194 3269 3280 3299 3304-3306 14191 14197-14199 14201-14203 14300 23422-23423 23453 23455 23477 23479 23485 23489-23491 24106-24107 24118-24119 24186-24187 24190-24191 24448 24450-24451 24454 24472 24474 24484-24485 24488https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/677/A107?format=asciidefaultJ/A+A/677/A107/table23D position and assigned LSR velocity of each channel barycenter of the clumps_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.raindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decindexedrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIndexIndex of the channel barycentermeta.idintGLONGalactic longitudedegpos.galactic.lonindexedGLATGalactix latitudedegpos.galactic.latindexedDistDistance from the Sunpcpos.distance;pos.heliocentricfloatvLSRLSR radial velocitykm/sspect.dopplerVeloc;pos.lsrfloat