Gavin Ramsay, Pasi Hakala, Steve B. Howell

Red giant pulsations from the suspected symbiotic star StHA 169 detected in Kepler data

Figure 4. The spectral energy distribution of StHa 169 from the near-UV to near IR. The absorbed flux unit is milli-Jy and we show the joint fit (solid line) from two blackbody models with temperature ∼2100K and ∼10200K and absorption EB−V =0.26. We have not used the WISE points (the three right most points) in the fit.


We present Kepler and Swift observations of StHa 169 which is currently classified as a symbiotic binary. The Kepler light curve shows quasi periodic behaviour with a mean period of 34 d and an amplitude of a few percent. Using Swift data we find a relatively strong UV source at the position of StHa 169 but no X-ray counterpart. Using a simple two component blackbody fit to model the combined Swift and 2MASS spectral energy distribution and an assessment of the previously published optical spectrum, we find that the source has a hot (∼10,000K) component and a cooler (∼3700K) component. The Kepler light is dominated by the cool component and we attribute the variability to pulsations in a red giant star. If we remove this approximate month long modulation from the light curve, we find no evidence for additional variability in the light curve. The hotter source is assigned to a late B or early A main sequence star. We briefly discuss the implications of these findings and conclude that StHA 169 is a red giant plus main sequence binary.

Full paper in PDF format

Last Revised: 2014 April 28th