A NLTE analysis of the hot subdwarf O star Bd+28 4211. I. The UV spectrum

TL;DR

This study performs a detailed UV spectral analysis of the hot subdwarf star Bd+28 4211 using NLTE models, determining elemental abundances, effective temperature, and surface gravity, and discussing implications for its mass.

Contribution

It provides the first comprehensive NLTE UV spectral analysis of Bd+28 4211, deriving elemental abundances and stellar parameters with high precision.

Findings

Elemental abundances range from solar to 1/10 solar.

Effective temperature is constrained to 82,000 +/- 5,000 K.

Surface gravity estimated between log g = 6.1 and 6.5.

Abstract

We present a detailed analysis of the UV spectrum of the calibration star Bd+28 4211 using high-quality spectra obtained with the HST and FUSE satellites. To this aim, we compare quantitatively the observed data with model spectra obtained from state-of-the-art NLTE metal line-blanketed model atmospheres and synthetic spectra calculated with TLUSTY and SYNSPEC. We thus determine in a self-consistent way the abundances of eleven elements with well-defined lines in the UV, namely those of C, N, O, F, Mg, Si, P, S, Ar, Fe, and Ni. The derived abundances range from about solar to 1/10 solar. We find that the overall quality of the derived spectral fits is very satisfying. Our spectral analysis can be used to constrain rather tigthly the effective temperature of Bd+28 to a value of teff = 82,000 +/- 5000 K. We also estimate conservatively that its surface gravity falls in the range log g = 6.2 -0.1/+0.3. Assuming that the Hipparcos measurement for Bd+28 is fully reliable and that our model atmospheres are reasonably realistic, we can reconcile our spectroscopic constraints with the available parallax measurement only if the mass of Bd+28 is significantly less than the canonical value of 0.5 msun for a representative post-EHB star.