000005941 001__ 5941
000005941 005__ 20221220155854.0
000005941 037__ $$aSCART-2022-0127
000005941 100__ $$ada Silva, R.
000005941 245__ $$aA new and homogeneous metallicity scale for Galactic classical Cepheids II. The abundance of iron and alpha elements
000005941 260__ $$c2022
000005941 520__ $$aContext. Classical Cepheids are the most popular distance indicators and tracers of young stellar populations. The key advantage is that they are bright and they can be easily identified in Local Group and Local Volume galaxies. Their evolutionary and pulsation properties depend on their chemical abundances. Aims. The main aim of this investigation is to perform a new and accurate abundance analysis of 20 calibrating Galactic Cepheids. We used high spectral resolution (R ∼ 40 000–115 000) and high S/N spectra (∼400), covering the entire pulsation cycle. Methods. We focused our attention on plausible systematics that would affect the estimate of atmospheric parameters and elemental abundances along the pulsation cycle. We cleaned the line list by using atomic transition parameters based on laboratory measurements and by removing lines that are either blended or that display abundance variations along the pulsation cycle. Results. The spectroscopic approach we developed brings forward small dispersions in the variation of the atmospheric parameters (σ(T eff ) ∼ 50 K, σ(log g) ∼ 0.2 dex, and σ(ξ) ∼ 0.2 km s−1 ) as well as in the abundance of both iron (.0.05 dex) and α elements (.0.10 dex) over the entire pulsation cycle. We also provide new and accurate effective temperature templates by splitting the calibrating Cepheids into four different period bins, ranging from short to long periods. For each period bin, we performed an analytical fit with Fourier series providing θ = 5040/T eff as a function of the pulsation phase. Conclusions. The current findings are a good viaticum for tracing the chemical enrichment of the Galactic thin disk by using classical Cepheids as a fundamental stepping stone for further investigations into the more metal-poor regime that is typical of Magellanic Cepheids.
000005941 594__ $$aNO
000005941 6531_ $$aGalaxy: disk
000005941 6531_ $$astars: abundances
000005941 6531_ $$astars: fundamental parameters
000005941 6531_ $$astars: variables: Cepheids
000005941 700__ $$aCrestani, J.
000005941 700__ $$aBono, G.
000005941 700__ $$aBraga, V.F.
000005941 700__ $$aD'Orazi, V.
000005941 700__ $$aLemasle, B.
000005941 700__ $$aBergemann, M.
000005941 700__ $$aDall'Ora, M.
000005941 700__ $$aFiorentino, G.
000005941 700__ $$aFrancois, P.
000005941 700__ $$aGroenewegen, M.A.T.
000005941 700__ $$aInno, L.
000005941 700__ $$aKovtyukh, V.
000005941 700__ $$aKudritzki, R.-P.
000005941 700__ $$aMatsunaga, N.
000005941 700__ $$aMonelli, M.
000005941 700__ $$aPietrinferni, A.
000005941 700__ $$aPorcelli, L.
000005941 700__ $$aStorm, J.
000005941 700__ $$aTantalo, M.
000005941 700__ $$aThevenin, F.
000005941 773__ $$nA104$$pA&A$$v661$$y2022
000005941 8560_ $$fmartin.groenewegen@observatoire.be
000005941 8564_ $$s20890398$$uhttps://publi2-as.oma.be/record/5941/files/daSilvaCrestaniBono_ea_22AA661_A104_MetallicityScale_GalacticCCs_IronAbundances.pdf
000005941 8564_ $$s3248$$uhttps://publi2-as.oma.be/record/5941/files/daSilvaCrestaniBono_ea_22AA661_A104_MetallicityScale_GalacticCCs_IronAbundances.gif?subformat=icon$$xicon
000005941 8564_ $$s7290$$uhttps://publi2-as.oma.be/record/5941/files/daSilvaCrestaniBono_ea_22AA661_A104_MetallicityScale_GalacticCCs_IronAbundances.jpg?subformat=icon-180$$xicon-180
000005941 905__ $$apublished in
000005941 980__ $$aREFERD