VizieR Online Data Catalog: Differential photometry & RVs of HATS-59 (Sarkis+, 2018)

The HATS-59 system was identified by the HATSouth instruments as potentially hosting a transiting planet. The star was observed between UT 2010 January 19 and UT 2010 August 10 using the HS-1, HS-3, and HS-5 units at the Las Campanas Observatory (LCO) in Chile, the H.E.S.S. site in Namibia, and the Siding Springs Observatory (SSO) in Australia, respectively. A total of 3113, 4690 and 658 of useful images were obtained with the HS-1, HS-3, and HS-5 telescopes, respectively, using the Sloan r filter with an exposure time of 240 s. An ingress was observed with the 0.3 m Perth Exoplanet Telescope (PEST) on 2013 March 3, using the R_C filter. The photometric precision of the light curve was 5.0 mmag with a cadence of 130 s. Another ingress was observed on 2013 April 10 using the Faulkes Telescope South (FTS), which is a fully automated telescope operated as part of the Las Cumbres Observatory Global Telescope (LCOGT; Brown et al. 2013PASP..125.1031B). The transit was observed in the i-band filter achieving a photometric precision of 1.6 mmag with a cadence of 113 s. An egress was obtained on 2013 December 21 with the multiband imager GROND (Greiner et al. 2008PASP..120..405G), mounted on the 2.2 m telescope in La Silla Observatory, using four different filters (g, r, i, z). The light curve had a precision of 1.7 mmag in the g band, 1.0 mmag in r, 1.1 mmag in i, and 1.1 mmag in z, with a cadence of 168 s. HATS-59 was spectroscopically observed between 2011 April and 2016 March. We obtained nine spectra with the CORALIE spectrograph (Queloz et al. 2001Msngr.105....1Q) at the Euler 1.2 m telescope at La Silla. We also obtained five spectra with the Planet Finder Spectrograph (PFS; Crane et al. 2010SPIE.7735E..53C) on the Magellan Clay 6.5 m telescope and seven spectra with CYCLOPS on the 3.9 m Anglo-Australian Telescope. Most of the spectra used in this analysis, most importantly for the discovery of the second outer companion, were obtained with FEROS on the MPG 2.2 m (Kaufer & Pasquini 1998SPIE.3355..844K) in La Silla Observatory. Twenty-four spectra were acquired with FEROS, which is a high-resolution echelle spectrograph (Kaufer & Pasquini 1998SPIE.3355..844K).

(2 data files).