J/MNRAS/442/3604ivo://CDS.VizieR/J/MNRAS/442/3604doi:10.26093/cds/vizier.74423604CDSHubrig S.Castelli F.Gonzalez J.F.Carroll T.A.Ilyin I.Schoeller M.,Drake N.A.Korhonen H.Briquet M.2024-08-09T20:15:35Z2014-07-28T13:22:56ZCDS support team

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

cds-question@unistra.frpeculiar-variable-starsvariable-starschemical-abundancesmagnetic-fieldsThe aim of this study is to carry out an abundance determination, to search for spectral variability and for the presence of a weak magnetic field in the typical PGa star HD19400. High-resolution, high signal-to-noise HARPS spectropolarimetric observations of HD19400 were obtained at three different epochs in 2011 and 2013. For the first time, we present abundances of various elements determined using an ATLAS12 model, including the abundances of a number of elements not analysed by previous studies, such as NeI, GaII, and XeII. Several lines of As II are also present in the spectra of HD19400. To study the variability, we compared the behaviour of the line profiles of various elements. We report on the first detection of anomalous shapes of line profiles belonging to Mn, and Hg, and the variability of the line profiles belonging to the elements Hg, P, Mn, Fe, and Ga. We suggest that the variability of the line profiles of these elements is caused by their non-uniform surface distribution, similar to the presence of chemical spots detected in HgMn stars. The search for the presence of a magnetic field was carried out using the moment technique and the SVD method. Our measurements of the magnetic field with the moment technique using 22 MnII lines indicate the potential existence of a weak variable longitudinal magnetic field on the first epoch. The SVD method applied to the MnII lines indicates B_z_=-76+/-25G on the first epoch, and at the same epoch the SVD analysis of the observations using the Fe II lines shows B_z_=-91+/-35G. The calculated false alarm probability values, 0.008 and 0.003, respectively, are above the value 10^-3^, indicating no detection.2014MNRAS.442.3604Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/442/3604CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/442/3604https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/442/3604http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/442/3604https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/442/3604https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/442/3604http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/442/3604GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/MNRAS/442/3604/table3Line by line abundances of HD19400 from the ATLAS12 model with parameters T_eff_=13500K, logg=3.9recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[3856/6718] Wavelength of line {lambda}0.1nmem.wl;spect.linedoubleIonElement name and ionization stagephys.atmol.ionStagecharlog(gf)Oscillator strengthphys.atmol.oscStrengthfloatr_log(gf)Reference for oscillator strength, in refs.dat filemeta.ref;pos.framecharXlowLower state excitation potentialcm**-1phys.atmol.excitationdoubleEW? Equivalent width of line (m{AA})0.1pmspect.line.eqWidthfloatnullablen_log(N/Nt)[pn] "p" when the abundance is derived from the profile, "n" for non-observed linemeta.notecharl_log(N/Nt)[<= ] Limit flag on log(N/Nt) (the line was not observed)meta.code.errorcharlog(N/Nt)Derived abundance (log(N(Ion)/N_tot_))phys.abundfloatu_log(N/Nt)[: ] Uncertainty flag on log(N/Nt)meta.code.errorcharRemarksNotes on the fittingmeta.notecharJ/MNRAS/442/3604/refslog(gf) referencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference code for log(gf)meta.notecharBibCodeBibCodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorcharComCommentsmeta.notechar