VizieR Online Data Catalog: Eclipsing binaries RVs from APOGEE spectra (Cunningham+, 2019)

We use the following criteria and filters to arrive at a candidate sample of promising SEBs in the APOGEE/Kepler overlap. We begin with the Kepler EB catalog compiled by Kirk et al. (2016, J/AJ/151/68). From this catalog we select targets that have both their primary and secondary eclipses observed by Kepler; this limits our selection to binaries with inclinations close to 90°. We further require the light curve to be semi- or well-detached, with the morphology parameter significantly less than 1. Next, a luminosity limit of H<14 magnitudes was imposed, as fainter targets are unlikely to have H-band APOGEE spectra with a sufficiently high signal-to-noise ratio (S/N). We also require the targets to have multiple cross-correlation function (CCF) peaks from the APOGEE pipeline (Nidever et al. 2015AJ....150..173N) visible by eye in one epoch. Finally, the binaries must have been observed by APOGEE at least three times, and thus have at least three apVisit spectra, with no quality flags present. Taken together, these criteria result in 33 candidates, which are listed in Table 1, plus one additional candidate that has already been analyzed (Rawls et al. 2016ApJ...818..108R). The standard observing mode for APOGEE spectra has a total exposure time of roughly three hours, which is usually collected over a series of visits on different days. The visits are then combined into one spectrum per target (an apStar spectrum). We instead utilize individual visit spectra (apVisit), which are identified with their plate ID, date (MJD), and fiber ID. These may be retrieved from the SDSS Science Archive Server search tool with a simple search by APOGEE ID. We continuum normalize the visit spectra and then de-spike them to remove erroneous spectral features due to tellurics. De-spiking consists of identifying outliers above or below the continuum by 0.7 or 3 times the standard deviation of the normalized flux, respectively.

(2 data files).