J/AJ/121/362ivo://CDS.VizieR/J/AJ/121/362doi:10.26093/cds/vizier.51210362CDSRudy R.J.Lynch D.K.Mazuk S.Puetter R.C.Dearborn D.S.P.2026-03-18T11:39:11Z2015-08-07T14:36:28ZCDS support team

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

cds-question@unistra.frplanetary-nebulaeinfrared-astronomyspectroscopyInfrared spectroscopy from 0.8 to 2.5{mu}m is presented for the planetary nebula IC5117. The emission lines of IC5117 span a wide range of ionization that includes He II, [S III], [S II], [N I], and H2. The reddening measured from the hydrogen lines is E(B-V)=0.79, most of which is probably interstellar in origin. The He/H abundance ratio is 0.113+/-0.015, with approximately 10% of the helium being doubly ionized. Using our measurements of [S II] and [S III] lines and published observations of [S IV], we find a sulfur abundance, relative to hydrogen, of N(S)/N(H)=7.8 x 10^-6^, or approximately half the solar value. Fluxes and flux limits for several lines of molecular hydrogen are presented. Measurements of 1-0 transitions, together with the limits on 2-1 transitions, indicate Tvib~Trot=1900K, suggesting a purely collisional excitation mechanism. The ortho-to-para ratio is ~3, a value that is also indicative of collisional excitation. The presence of [C I] {lambda}9850 is consistent with previous studies of IC 5117 that indicated carbon is more abundant than oxygen. IC5117 follows the trend of planetary nebulae that display bipolar outflows and H2 emission to be carbon-rich. We confirm the results of Zhang & Kwok, who reported infrared continuum emission substantially in excess of that produced by the ionized gas. This emission is most likely due to hot dust (T~1300K) and accounts for roughly half of the continuum between 1.5 and 2{mu}m.2001AJ....121..362Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/121/362CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/121/362https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/121/362http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/121/362https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/121/362https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/121/362http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/121/362GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/AJ/121/362/table1Observed emission-line strengths of IC 5117recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLineLine identificationmeta.id;spect.linecharlambda[8046/24231] Wavelength {lambda} ({AA}) (1)0.1nmem.wlintOlambda? Wavelegth of nearby line with same line ID (1)0.1nmem.wlintnullableRatio[0.002/7.6]? Flux ratio relative to Pa{beta} (2)phot.flux;arith.ratiofloatnullablee_Ratio[0.0008/0.4]? Uncertainty in Ratiostat.error;arith.ratiofloatnullablef_Ratio"Atmosphere" Indicates an atmospheric linemeta.codechar