Metal-Rich SX Phe Stars in the Kepler Field
1 Department of Physics & Astronomy, Camosun College, Victoria, B.C., V8P 5J2 Canada
2 International Statistics & Research Corporation, Brentwood Bay, B.C., V8M 1R3 Canada
3 University of Capetown, South African Astronomical Observatory, South Africa
4 Apache Point Observatory, Sunspot, NM, 88349 USA
5 Sydney Institute for Astronomy, School of Physics, University of Sydney, Australia
6 Korea Astronomy and Space Science Institute, Daejeon, 305-438, Korea
7 Jeremiah Horracks Institute, University of Central Lancashire, Preston, PR1 2HE UK
8 Astronomical Institute, Wroclaw University, Wroclaw, Poland
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Published online: 23 September 2015
High-resolution spectroscopic observations have been made for 32 of the 34 candidate SX Phe stars identified in the Kepler field by Balona & Nemec (2012). All available long-and short-cadence Q0-Q17 Kepler photometry has been analyzed for the 34 candidates. Radial velocities (RVs), space motions (U, V, W), projected rotation velocities (υ sin i), spectral types, and atmospheric characteristics (Teff, log g, [M/H], υmic, etc.) were derived from ~ 160 spectra taken with the ESPaDOnS spectrograph on the Canada-France-Hawaii 3.6-m telescope and with the ARCES spectrograph on the Apache Point Observatory 3.5-m telescope. Two thirds of the stars are fast rotators with υ sin i > 50 km/s, including four stars with υ sin i > 200 km/s. Three of the stars have (negative) RVs > 250 km/s and retrograde space motions, and seven stars have total space motions > 400 km/s. All the spectroscopically measured SX Phe candidates have positions in a Toomre diagram that are consistent with being bona fide halo and thick-disk stars. Although several stars show a marked metal weakness, the mean [Fe/H] of the sample is near 0.0 dex (σ ~ 0.25 dex), which is considerably more metal-rich than is normally expected for a sample of Pop. II stars. Observed pulsation frequency modulations and optical time delays suggest that at least eight of the SX Phe stars are in binary systems, some of which show significant RV variations. Six of the time-delay binaries have secondary masses ranging from 0.05 to 0.70 M☉ and orbital periods in the range 9 to 1570 days. Another star appears to be an ellipsoidal variable with a 2.3-day orbital period; and two other systems have orbital periods longer than the ~ 4-year sampling interval of the Kepler data.
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