HST Spectroscopy of the Hottest White Dwarfs

TL;DR

This paper presents high-resolution UV spectroscopic analysis of the hottest white dwarfs using HST data, employing NLTE models with metal-line blanketing to determine their properties accurately.

Contribution

It introduces a comprehensive analysis of the hottest white dwarfs with advanced NLTE models including all metals from hydrogen to nickel, based on high-quality HST UV spectra.

Findings

Accurate temperature and ionization state determinations.

Enhanced understanding of metal line blanketing effects.

Refined models for hot white dwarf atmospheres.

Abstract

Spectral analysis needs the observation of lines of successive ionization stages in order to evaluate the ionization equilibrium (of a particular species) which is a sensitive indicator for the effective temperature. Since stars with effective temperatures as high as 100000 K have their flux maximum in the extreme ultraviolet (EUV) wavelength range and due to the high degree of ionization, most of the metal lines are found in the ultraviolet (UV) range. Thus, high-S/N and high-resolution UV spectra are a pre-requisite for a precise analysis. Consequently, we employed the Faint Object Spectrograph (FOS), the Goddard High Resolution Spectrograph (GHRS), and the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope (HST) in order to obtain suitable data. We present state-of-the-art analyses of the hottest (pre-) white dwarfs by means of NLTE model atmospheres which include the metal-line blanketing of all elements from hydrogen to nickel.