J/ApJS/208/27ivo://CDS.VizieR/J/ApJS/208/27doi:10.26093/cds/vizier.22080027CDSWood M.P.Lawler J.E.Sneden C.Cowan J.J.2013-12-23T21:42:32Z2013-12-02T10:18:47ZCDS support team

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

cds-question@unistra.fratomic-physicschemical-abundanceschemically-peculiar-starsthe-sunAtomic transition probability measurements for 364 lines of Ti II in the UV through near-IR are reported. Branching fractions from data recorded using a Fourier transform spectrometer (FTS) and a new echelle spectrometer are combined with published radiative lifetimes to determine these transition probabilities. The new results are in generally good agreement with previously reported FTS measurements. Use of the new echelle spectrometer, independent radiometric calibration methods, and independent data analysis routines enables a reduction of systematic errors and overall improvement in transition probability accuracy over previous measurements. The new Ti II data are applied to high-resolution visible and UV spectra of the Sun and metal-poor star HD 84937 to derive new, more accurate Ti abundances. Lines covering a range of wavelength and excitation potential are used to search for non-LTE effects. The Ti abundances derived using Ti II for these two stars match those derived using Ti I and support the relative Ti/Fe abundance ratio versus metallicity seen in previous studies.2013ApJS..208...27Whttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/208/27CatalogResearchIsServedByTAP VizieR generic servicerelated-toIII/193 : Chemical Abundances in Late-Type Stars (Thevenin, 1998)J/A+A/554/A96 : Metal-poor star spectra of the LiI 670.8nm line (Lind+, 2013)J/ApJS/199/8 : Interstellar column densities compilation (Gudennavar+, 2012)J/MNRAS/404/1321 : TiII in Milky way and Magellanic clouds (Welty+, 2010)J/MNRAS/396/1895 : MgI and sTiO index definitions (Cenarro+, 2009)J/MNRAS/367/1478 : Interstellar NaI, TiII + CaIIK obs. (Hunter+, 2006)J/A+A/404/187 : Equivalent widths for metal-poor stars (Gratton+, 2003)J/ApJ/562/528 : Teff and log(g) of low-metallicity stars (Snider+, 2001)J/A+AS/133/221 : Library of ELODIE spectra (F5-K7 stars) (Soubiran+ 1998)J/A+AS/109/193 : IRON project VIII. Ti-like ions (Berrington, 1995)J/AJ/90/2089 : Stars of very low metal abundance. I (Beers+, 1985)http://nsokp.nso.edu/ : Kitt Peak NSO home pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/208/27https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/208/27http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/208/27https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/208/27https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/208/27http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/208/27GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJS/208/27/table3Comparison of experimental branching fractions from FTS data for 364 lines of TiII from upper odd-parity levels organized by upper levelrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlamAir[2325/9748] Wavelength in air; Angstroms (G1)0.1nmem.wl;phys.atmol.transitiondoubleE1[29544/47626] Upper level (G2)cm**-1phys.energy;phys.atmol.leveldoubleJ1[0.5/5.5] Upper level J value (G2)phys.atmol.qnfloatE0[0/32333] Lower level (G2)cm**-1phys.energy;phys.atmol.leveldoubleJ0[0.5/5.5] Lower level J value (G2)phys.atmol.qnfloatBF-P01[0.0003/0.95]? Branching fraction; Pickering et al. 2001ApJS..132..403Pphys.atmol.branchingRatiodoublenullablee_BF-P01[1/43]? Uncertainty in BF-P01%stat.errorintnullableBF-B93[4.8e-05/0.8]? Branching fraction; Bizzarri et al. 1993A&A...273..707Bphys.atmol.branchingRatiodoublenullablee_BF-B93[1/57]? Uncertainty in BF-B93%stat.errorintnullableBF[6e-05/1] Branching fraction; this experimentphys.atmol.branchingRatiodoublee_BF[0/20] Uncertainty in BF%stat.errorintJ/ApJS/208/27/table4Experimental Atomic Transition Probabilities for 364 lines of TiII from upper odd-parity levels organized by increasing wavelength in airrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlamAir[2325/9748] Wavelength in air; Angstroms (G1)0.1nmem.wl;phys.atmol.transitiondoubleE1[29544/47626] Upper level (G2)cm**-1phys.energy;phys.atmol.leveldoubleJ1[0.5/5.5] Upper level J value (G2)phys.atmol.qnfloatE0[0/32333] Lower level (G2)cm**-1phys.energy;phys.atmol.leveldoubleJ0[0.5/5.5] Lower level J value (G2)phys.atmol.qnfloatA[0.015/198] Transition probability1e+06s**-1phys.atmol.transProbdoublee_A[0.002/10] Total uncertainty in A1e+06s**-1stat.errorfloatlog(gf)[-3.4/0.6] Log of degeneracy times oscillator strengthphys.atmol.oscStrengthfloatJ/ApJS/208/27/table5Solar Photospheric Titanium Abundances from Individual TiII LinesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlamAir[2474/9433] Wavelength in air0.1nmem.wl;phys.atmol.transitiondoubleE0[0/3.2] Lower level energyeVphys.energy;phys.atmol.levelfloatlog(gf)[-3.4/0.5] Log of degeneracy times oscillator strengthphys.atmol.oscStrengthfloatlog(eps)[2.8/5.1] Log of abundance (log{epsilon})phys.abundfloatJ/ApJS/208/27/table6Titanium Abundances from Individual TiII Lines in HD 84937recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlamAir[2474/9433] Wavelength in air0.1nmem.wl;phys.atmol.transitiondoubleE0[0/3.2] Lower level energyeVphys.energy;phys.atmol.levelfloatlog(gf)[-3.4/0.5] Log of degeneracy times oscillator strengthphys.atmol.oscStrengthfloatlog(eps)[2.8/5.1] Log of abundance (log{epsilon})phys.abundfloat