First time-series optical photometry from Antarctica. sIRAIT monitoring of the RS CVn binary V841 Centauri and the δ-Scuti star V1034 Centauri

Details First time-series optical photometry from Antarctica. sIRAIT monitoring of the RS CVn binary V841 Centauri and the δ-Scuti star V1034 Centauri First time-series optical photometry from Antarctica. sIRAIT monitoring of the RS CVn binary V841 Centauri and the δ-Scuti star V1034 Centauri

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008a%26a...490..287s&link_type=abstract

Astronomy and Astrophysics, Volume 490, Issue 1, 2008, pp.287-295

Astronomy and Astrophysics

Astrophysics

14

Stars: Starspots, Stars: Variables: General, Stars: Activity, Stars: Oscillations, Stars: Individual: V841 Centauri, Stars: Individual: V1034 Centauri

Scientific paper

Context: Eradicating the problems associated with the Earth's day-night cycle is mandatory for long and continuous time-series photometry and had been achieved with either large ground-based networks of observatories at different geographic longitudes or when conducted from space. A third possibility is offered by a polar location with astronomically-qualified site characteristics. Aims: We present the first scientific stellar time-series optical photometry from Dome C in Antarctica and analyze approximately 13 000 CCD frames acquired in July 2007. Methods: The optical pilot telescope of the “International Robotic Antarctic Infrared Telescope”, named “small IRAIT” (sIRAIT), and its UBVRI CCD photometer were used in BVR for a continuous 243 h (10.15 days) with a duty cycle of 98% and a cadence of 155 s. The prime targets were the chromospherically active, spotted binary star V841 Cen and the non-radially pulsating δ-Scuti star V1034 Cen. Results: We confirmed the known 0.2-day fundamental period of V1034 Cen and detected a total of 23 further periods between 2.2 h and 3.5 days. In July 2007, V841 Cen's V amplitude due to spots appeared to be at a record high of 0.4 m in V. We completed a spot-model analysis with a light-curve inversion technique and discovered the star with a spot filling factor of 44% of the visible hemisphere, among the highest ever measured values for active stars, and a temperature-difference photosphere minus spot of 750 ± 100 K. Its odd-numbered (for a single site) rotation period was determined with a higher precision than before (5.8854 ± 0.0026 days), despite our comparably short data set. The rms scatter from a 2.4-h data subset was 3 mmag in V and 4.2 mmag in R. The differential data quality is 3-4 times higher than with the 25 cm Fairborn Automatic Photoelectric Telescope in southern Arizona and is probably due to the exceptionally low scintillation noise at Dome C. Conclusions: We conclude that high-precision CCD photometry with exceptional time coverage and cadence can be acquired at Dome C in Antarctica and be successfully used to complete time-series astrophysics.

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