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Article Dans Une Revue The Astrophysical Journal Année : 2009

The Chemical Composition of Cernis 52 (BD+31° 640)

Résumé

We present an abundance analysis of the star Cernis 52 in whose spectrum we recently reported the naphthalene cation in absorption at 6707.4 Å. This star is on a line of sight to the Perseus molecular complex. The analysis of high-resolution spectra using a chi2-minimization procedure and a grid of synthetic spectra provides the stellar parameters and the abundances of O, Mg, Si, S, Ca, and Fe. The stellar parameters of this star are found to be T eff = 8350 ± 200 K, log(g/cm s2)=4.2 ± 0.4 dex. We derived a metallicity of [Fe/H] = -0.01 ± 0.15. These stellar parameters are consistent with a star of ~2 M sun in a pre-main-sequence evolutionary stage. The stellar spectrum is significantly veiled in the spectral range lambdalambda5150-6730 Å up to almost 55% of the total flux at 5150 Å and decreasing toward longer wavelengths. Using Johnson-Cousins and Two Micron All Sky Survey photometric data, we determine a distance to Cernis 52 of 231+135 -85 pc considering the error bars of the stellar parameters. This determination places the star at a similar distance to the young cluster IC 348. This together with its radial velocity, vr = 13.7 ± 1 km s-1, its proper motion and probable young age support Cernis 52 as a likely member of IC 348. We determine a rotational velocity of vsin i = 65 ± 5 km s-1 for this star. We confirm that the stellar resonance line of Li I at 6707.8 Å is unable to fit the broad feature at 6707.4 Å. This feature should have a interstellar origin and could possibly form in the dark cloud L1470 surrounding all the cluster IC 348 at about the same distance.

Dates et versions

hal-03742654 , version 1 (02-08-2022)

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Citer

J. I. González Hernández, S. Iglesias-Groth, Rafael Rebolo Lopez, D. A. García-Hernández, A. Manchado, et al.. The Chemical Composition of Cernis 52 (BD+31° 640). The Astrophysical Journal, 2009, 706, pp.866-876. ⟨10.1088/0004-637X/706/1/866⟩. ⟨hal-03742654⟩
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