We present an abundance analysis of the star Cernis 52 in whose spectrum we recently reported the napthalene 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 \chi 2 -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 _ { \mathrm { eff } } = 8350 \pm 200 K , \log ( g / { cm~ { } s } ^ { 2 } ) = 4.2 \pm 0.4 dex .
We derived a metallicity of \mathrm { [ Fe / H ] } = -0.01 \pm 0.15 .
These stellar parameters are consistent with a star of \sim 2 M _ { \odot } in a pre-main-sequence evolutionary stage .
The stellar spectrum is significantly veiled in the spectral range \lambda \lambda 5150 - 6730 Å up to almost 55 per cent of the total flux at 5150 Å and decreasing towards longer wavelengths .
Using Johnson-Cousins and 2MASS 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 , v _ { r } = 13.7 \pm 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 v \sin i = 65 \pm 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 .