Open AccessHubble Space Telescope observations of SV Cam – I. The importance of unresolved star‐spot distributions in light‐curve fitting
Author(s) -
Jeffers S. V.,
Barnes J. R.,
Cameron A. Collier,
Donati J.F.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09905.x
Subject(s) - physics , light curve , photometry (optics) , astrophysics , starspot , brightness , astronomy , advanced camera for surveys , space telescope imaging spectrograph , hubble space telescope , stars
ABSTRACT We have used maximum entropy eclipse‐mapping to recover images of the visual surface brightness distribution of the primary component of the RS CVn eclipsing binary SV Cam, using high‐precision photometry data obtained during three primary eclipses with Space Telescope Imaging Spectrograph aboard the Hubble Space Telescope ( HST ). These were augmented by contemporaneous ground‐based photometry secured around the rest of the orbit. The goal of these observations was to determine the filling factor and size distribution of star‐spots too small to be resolved by Doppler imaging. The information content of the final image and the fit to the data were optimized with respect to various system parameters using the χ 2 landscape method, using an eclipse‐mapping code that solves for large‐scale spot coverage. It is only with the unprecedented photometric precision of the HST data (0.000 15 mag) that it is possible to see strong discontinuities at the four contact points in the residuals of the fit to the light curve. These features can only be removed from the residual light curve by the reduction of the photospheric temperature, to synthesize high unresolvable spot coverage, and the inclusion of a polar spot. We show that this spottedness of the stellar surface can have a significant impact on the determination of the stellar binary parameters and the fit to the light curve by reducing the secondary radius from 0.794 ± 0.009 to 0.727 ± 0.009 R ⊙ . This new technique can also be applied to other binary systems with high‐precision spectrophotometric observations.