the periods are consistent. For completeness, we note that using a period of 90 min rather than 82.9 min (Table 1) places J0305 at a distance of 31.9 kpc rather than 30.0 kpc assuming we have identified this period as the fundamental radial pulsation mode. We encourage additional photometry of all the sources shown in Table 1 to identify the mode of the pulsation seen in each star.

(14,19) (-0.4,-1.5)

(14,12) (-0.4,-9)

Spectral observations {#spectra}
=====================

We have spectroscopic observations of a small sample of our candidate blue pulsating stars (cf Table 1). We obtained spectra for two sources using the 4.2m William Herschel Telescope (WHT) and the Intermediate dispersion Spectrograph and Imaging System (ISIS) on La Palma, two using the SAAO 1.9m telescope and the Cassegrain spectrograph in Sutherland, South Africa and two using the 2.5m Nordic Optical Telescope and ALFOSC on La Palma. A spectrum of another source was obtained from the SDSS data archive[^2].

Both arms of ISIS were used giving spectral coverage from $\sim$3800–5200 Å and $\sim$5500–9000 Å in the blue (R158B grating) and red (R158R) arms respectively. Grating \#7 was used with the SAAO spectrograph giving a wavelength range of 3400–7500Å. The spectral resolution was 