J/AJ/164/243ivo://CDS.VizieR/J/AJ/164/243doi:10.26093/cds/vizier.51640243CDSRicher M.G.Arrieta A.Arias L.Castaneda-Carlos L.,Torres-Peimbert S.,Lopez J.A.,Galindo A.2023-03-29T13:18:02Z2023-02-10T07:24:46ZCDS support team

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

cds-question@unistra.frnebulaeinterstellar-mediumvisible-astronomyspectroscopyinfrared-astronomyultraviolet-astronomyWe study the kinematics of emission lines that arise from many physical processes in NGC6153 based upon deep, spatially resolved, high-resolution spectra acquired with the UVES spectrograph at the European Southern Observatory Very Large Telescope. Our most basic finding is that the plasma in NGC6153 is complex, especially its temperature structure. The kinematics of most emission lines defines a classic expansion law, with the outer part expanding fastest (normal nebular plasma). However, the permitted lines of OI, CII, NII, OII, and NeII present a constant expansion velocity that defines a second kinematic component (additional plasma component). The physical conditions imply two plasma components, with the additional plasma component having lower temperature and higher density. The [OII] density and the [NII] temperature are anomalous, but may be understood considering the contribution of recombination to these forbidden lines. The two plasma components have very different temperatures. The normal nebular plasma appears to have temperature fluctuations in part of its volume (main shell), but only small fluctuations elsewhere. The additional plasma component contains about half of the mass of the N2+ and O2+ ions, but only 3%-5% of the mass of H+ ions, so the two plasma components have very different chemical abundances. We estimate abundances of 12+log(O^2+^/H^+^)~9.2dex and He/H~0.13. Although they are all complications, multiple plasma components, temperature fluctuations, and the contributions of multiple physical processes to a given emission line are all part of the reality in NGC6153, and should generally be taken into account.2022AJ....164..243Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/164/243CatalogResearchIsServedByTAP VizieR generic servicerelated-toIII/211 : Keck/HIRES Sky Line Atlas (Osterbrock+ 1997)II/179 : Southern Spectrophotometric Standards. I + II (Hamuy+ 1992,94)VI/64 : Recombination line intensities for hydrogenic ions (Storey+ 1995)VI/141 : Nebular [OIII] collision strengths - SSB (Storey+, 2014)VI/150 : Recombination coefficients for O II lines - SSB2 (Storey+, 2017)J/A+AS/135/359 : HI and HeII fine structure components (Clegg+ 1999)J/MNRAS/368/1959 : Chemical abundances for Hf 2-2 (Liu+, 2006)J/MNRAS/395/855 : Spectroscopy (310-1040nm) of HH 202 (Mesa-Delgado+, 2009)J/A+A/500/1253 : Electron-impact excitation of ArIII (Munoz Burgos+, 2009)J/ApJ/723/658 : Abundances of the halo PN BoBn 1 (Otsuka+, 2010)J/ApJS/188/32 : Breit-Pauli transition probabilities for SII (Tayal+, 2010)J/A+A/530/A18 : Nebular NII lines effective recomb. coeff. (Fang+, 2013)J/AJ/153/140 : Kinematics of CII {lambda}6578 line in PNe (Richer+, 2017)J/MNRAS/480/4589 : Extreme abundance discrepancy factors in PNe (Wesson+, 2018)J/A+A/623/A155 : SII, ClII, ArIV nrj levels & transition data (Rynkun+, 2019)J/A+A/634/A47 : Planetary nebula NGC3132 MUSE images (Monreal-Ibero+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/164/243https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/164/243http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/164/243https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/164/243https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/164/243http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/164/243GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVOpticalInfrareddefaultJ/AJ/164/243/dcdCombined table from original tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintWaveWavelength in Angstrom0.1nmem.wldoubleIntervalWavelength interval namemeta.idcharFluxFlux valuephot.flux;em.opt.UdoubleJ/AJ/164/243/scdCombined table from original tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintWaveWavelength in Angstrom0.1nmem.wldoubleIntervalWavelength interval namemeta.idcharFluxFlux valuephot.flux;em.opt.Udouble