J/ApJ/875/129ivo://CDS.VizieR/J/ApJ/875/129doi:10.26093/cds/vizier.18750129CDSKondo S.Fukue K.Matsunaga N.Ikeda Y.Taniguchi D.Kobayashi N.,Sameshima H.Hamano S.Arai A.Kawakita H.Yasui C.Izumi N.,Mizumoto M.Otsubo S.Takenaka K.Watase A.Asano A.Yoshikawa T.,Tsujimoto T.2021-01-04T08:41:12Z2020-10-12T09:14:36ZCDS support team

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

cds-question@unistra.frinfrared-astronomyspectroscopygiant-starschemical-abundancesFor a detailed analysis of stellar chemical abundances, high-resolution spectra in the optical have mainly been used, while the development of near-infrared (NIR) spectrograph has opened new wavelength windows. Red giants have a large number of resolved absorption lines in both the optical and NIR wavelengths, but the characteristics of the lines in different wave passbands are not necessarily the same. We present a selection of FeI lines in the z', Y, and J bands (0.91-1.33{mu}m). On the basis of two different lists of lines in this range, the Vienna Atomic Line Database (VALD) and the catalog published by Melendez & Barbuy in 1999 (MB99; Cat. J/ApJS/124/527), we selected sufficiently strong lines that are not severely blended and compiled lists with 107 FeI lines in total (97 and 75 lines from VALD and MB99, respectively). Combining our lists with high-resolution ({lambda}/{Delta}{lambda}=28000) and high signal-to-noise (>500) spectra taken with an NIR spectrograph, WINERED, we present measurements of the iron abundances of two prototype red giants: Arcturus and {mu} Leo. A bootstrap method for determining the microturbulence and abundance together with their errors is demonstrated. The standard deviations of log{epsilon}_Fe_ values from individual FeI lines are significantly smaller when we use the lines from MB99 instead of those from VALD. With the MB99 list, we obtained {xi}=1.20+/-0.11km/s and log{epsilon}_Fe_=7.01+/-0.05dex for Arcturus, and {xi}=1.54+/-0.17km/s and log{epsilon}_Fe_=7.73+/-0.07dex for {mu} Leo. These final values show better agreements with previous values in the literature than the corresponding values we obtained with VALD.2019ApJ...875..129Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/875/129CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/324/435 : Chemical composition of 6 K supergiants in the SMC (Hill 1997)J/ApJS/124/527 : Oscillator strengths for lines in J&H bands (Melendez+, 1999)J/AJ/129/1063 : Abundances of stars within 15pc of the Sun (Luck+, 2005)J/ApJ/636/821 : Abundances of Baade's Window K giants (Fulbright+, 2006)J/A+A/475/1003 : Stellar parameters of G and K giant stars (Hekker+, 2007)J/A+A/465/799 : Abundances of Galactic Bulge red giants (Lecureur+, 2007)J/A+A/465/271 : Oxygen abundances in nearby stars (Ramirez+, 2007)J/A+A/528/A121 : Normalized spectra of 20 red giants (Bruntt,+, 2011)J/A+A/543/A160 : Normalized spectra of 82 Kepler red giants (Thygesen+, 2012)J/ApJ/764/78 : Oxygen abundances in nearby FGK stars (Ramirez+, 2013)J/A+A/564/A133 : Gaia FGK benchmark stars: metallicity (Jofre+, 2014)J/ApJ/808/16 : Cannon: a new approach to determine abundances (Ness+, 2015)J/ApJS/221/24 : SDSS-III APOGEE H-band spectral line lists (Shetrone+, 2015)J/A+A/587/A2 : SP_Ace derived data from stellar spectra (Boeche+, 2016)J/AJ/151/144 : ASPCAP weights for APOGEE chemical elements (Garcia+, 2016)http://vald.astro.uu.se/ : VALD3 home pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/875/129https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/875/129http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/875/129https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/875/129https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/875/129http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/875/129GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/ApJ/875/129/linesList of FeI lines selected from VALD3 (Table 2) and MB99 (Table 3) and abundancesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceVALD3 = Vienna Atomic Line Database (Ryabchikova+ 2015PhyS...90e4005R); or MB99 = Melendez & Barbuy, 1999, J/ApJS/124/527meta.bibcharlambda[9117.1/13291.8] Wavelength in Angstroms0.1nmem.wldoubleEP[2.17/6.21] Excitation potentialeVphys.atmol.excitationfloatloggf[-5.1/0.15] log, statistical weight*oscillator strengthstat.weight;phys.atmol.oscStrengthfloatlogAFe1[5.88/7.68]? log of iron abundance from line, Arcturusphys.abund.Fefloatnullablef_logAFe1Flag on logAFe1 (1)meta.codecharlogAFe2[6.74/8.65]? log of iron abundance from line, {mu} Leophys.abund.Fefloatnullablef_logAFe2Flag on logAFe2 (1)meta.codechar