Holly Thompson

  • Citations Per Year
Learn More
We present Ca II K and Ti II optical spectra of early-type stars taken mainly from the ultraviolet and visual echelle spectrograph (UVES) Paranal Observatory Project, plus H I 21-cm spectra, from the Vila-Elisa and Leiden-Dwingeloo Surveys, which are employed to obtain distances to intermediateand high-velocity clouds (IHVCs). H I emission at a velocity of(More)
We describe medium-resolution spectroscopic observations taken with the ESO Multi-Mode Instrument (emmi) in the Ca ii K line (λair=3933.661Å) towards 7 QSOs located in the line-of-sight to the Magellanic Bridge. At a spectral resolution R= λ/∆λ = 6,000, five of the sightlines have a signal-to-noise (S/N) ratio of∼ 20 or higher. Definite Ca absorption due to(More)
High-resolution HST ultra-violet spectra for five B-type stars in the Magellanic Bridge and in the Large and Small Magellanic Clouds have been analysed to estimate their iron abundances. Those for the Clouds are lower than estimates obtained from late-type stars or the optical lines in B-type stars by approximately 0.5 dex. This may be due to systematic(More)
An analysis of high-resolution Anglo-Australian Telescope (AAT)/ University College London Échelle Spectrograph (UCLÉS) optical spectra for the ultraviolet (UV)-bright star ROA5701 in the globular cluster ω Cen (NGC5139) is performed, using nonlocal thermodynamic equilibrium (non-LTE) model atmospheres to estimate stellar atmospheric parameters and chemical(More)
High resolution optical and ultraviolet spectra of two B-type post-Asymptotic Giant Branch (post-AGB) stars in globular clusters, Barnard29 in M13 and ROA5701 in ωCen, have been analysed using model atmosphere techniques. The optical spectra have been obtained with FEROS on the ESO 2.2-m telescope and the 2d-Coudé spectrograph on the 2.7-m McDonald(More)
The role of optical Fe iii absorption lines in B-type stars as iron abundance diagnostics is considered. To date, ultraviolet Fe lines have been widely used in B-type stars, although line blending can severely hinder their diagnostic power. Using optical spectra, covering a wavelength range ∼ 3560 – 9200 Å, a sample of Galactic B-type main-sequence and(More)
  • 1