J/ApJ/888/54ivo://CDS.VizieR/J/ApJ/888/54doi:10.26093/cds/vizier.18880054CDSMargon B.Manea C.Williams R.Bond H.E.Prochaska J.X.,Szymanski M.K.Morrell N.2021-10-25T10:12:43Z2021-07-13T14:50:54ZCDS support team

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

cds-question@unistra.frwolf-rayet-starsmagellanic-cloudsvisible-astronomyspectroscopyinfrared-astronomyradial-velocityline-intensitiesWe report the serendipitous discovery of an object, UVQSJ060819.93-715737.4, with a spectrum dominated by extremely intense, narrow CII emission lines. The spectrum is similar to those of the very rare, late-type [WC11] low-mass Wolf-Rayet stars. Despite the recognition of these stars as a distinct class decades ago, there remains barely a handful of Galactic members, all of which are also planetary-nebula central stars. Although no obvious surrounding nebulosity is present in J0608, [OII], [NII], and [SII] emission suggest the presence of an inconspicuous, low-excitation nebula. There is low-amplitude incoherent photometric variability on timescales of days to years, as well as numerous prominent P Cygni profiles, implying mass loss. There are indications of a binary companion. The star is located on the outskirts of the LMC, and the observed radial velocity (~+250km/s) and proper motion strongly suggest membership. If indeed an LMC member, this is the first extragalactic late [WC] star, and the first with an accurately determined luminosity, as the Galactic examples are too distant for precise parallax determinations. A high-quality, broad-coverage spectrum of the prototype of the late [WC] class, CPD -56 8032, is also presented. We discuss different excitation mechanisms capable of producing the great strength of the CII emission. Numerous autoionizing levels of C II are definitely populated by processes other than dielectronic recombination. Despite the spectacular emission spectra, observational selection makes objects such as these difficult to discover. Members of the [WC11] class may in fact be considerably more common than the handful of previously known late [WC] stars.2020ApJ...888...54Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/888/54CatalogResearchIsServedByTAP VizieR generic servicerelated-toIII/85 : Sixth Catalogue of Galactic Wolf-Rayet Stars (van der Hucht+ 1981)II/358 : SkyMapper Southern Sky Survey. DR1.1 (Wolf+, 2018)I/345 : Gaia DR2 (Gaia Collaboration, 2018)J/A+AS/121/407 : LMC planetary nebulae positions (Leisy+ 1997)J/A+AS/142/85 : Recombination coefficients for C II lines (Davey+, 2000)J/A+A/403/659 : Classification of WR planetary nebulae (Acker+, 2003)J/ApJS/149/157 : EMILI line-identification in IC 418 spectrum (Sharpee+, 2003)J/AcA/59/335 : VI light curves of LMC R CBr stars (Soszynski+, 2009)J/ApJ/724/748 : Galactic anticenter PNe and oxygen abundance (Henry+, 2010)J/A+A/526/A6 : Central stars of galactic planetary nebulae (Weidmann+, 2011)J/A+A/530/A90 : Optically bright post-AGB population of LMC (van Aarle+, 2011)J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)J/AJ/152/25 : The UV-bright Quasar Survey (UVQS) DR1 (Monroe+, 2016)J/ApJ/861/153 : Ultraviolet Extinction in the GALEX Bands. UVEXT (Sun+, 2018)J/A+A/616/A12 : Gaia DR2 sources in GC and dSph (Gaia Collaboration+, 2018)J/A+A/621/A38 : Gaia catalogue of hot subluminous stars (Geier+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/888/54https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/888/54http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/888/54https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/888/54https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/888/54http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/888/54GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/ApJ/888/54/table1Identification and measurements of UVQS J060819.93-715737.4 spectral linesTypeLine typephys.emissivitycharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIon1Line identifier (ion)phys.atmol.ionStagerlam1[3165.5/10830]? Ion1 rest wavelength in {AA}0.1nmem.wlfloatnullableIon2Added line identifier (ion) if anyphys.atmol.ionStagecharrlam2? Ion2 rest wavelength in {AA}0.1nmem.wlfloatnullableTrans1Transition for Ion1meta.id;phys.atmol.transitioncharTrans2Transition for Ion2meta.id;phys.atmol.transitioncharOWave1[3190/9257.5]? Observed wavelength on Dec. 30, 2017 in {AA}0.1nmem.wlfloatnullablel_RFlux1Limit flag on RFlux1meta.code.errorcharRFlux1[0.01/3.9]? Relative flux to the H{beta} line on Dec. 30, 2017 (1)pos.eq.dec;spect.linefloatnullableEW1[-1.2/-0.02]? Equivalent width on Dec. 30, 2017 in {AA}0.1nmspect.line.eqWidthfloatnullableRV1[159/299]? Heliocentric radial velocity on Dec. 30, 2017km/sspect.dopplerVeloc;pos.heliocentricintnullableOWave2[3168/10839]? Observed wavelength on May 3, 2019 in {AA}0.1nmem.wlfloatnullableRFlux2[0.03/3.5]? Relative flux to the H{beta} line on May 3, 2019 (2)phot.flux;spect.linefloatnullableEW2[-0.9/-0.03]? Equivalent width on May 3, 2019 in {AA}0.1nmspect.line.eqWidthfloatnullableRV2[146/284]? Heliocentric radial velocity on May 3, 2019km/sspect.dopplerVeloc;pos.heliocentricintnullable