The Kepler mission has provided a treasure trove of eclipsing binaries (EBs), observed at extremely high photometric precision, nearly continuously for several years. We are carrying out a survey of similar to 100 of these EBs to derive dynamical masses and radii with precisions of 3% or better. We use multiplexed near-infrared H-band spectroscopy from the Sloan Digital Sky Survey-III and -IV APOGEE instrument and optical spectroscopy from the Hobby-Eberly Telescope High-resolution Spectrograph to derive double-lined spectroscopic orbits and dynamical mass ratios (q) for the EB sample, two of which we showcase in this paper. This orbital information is combined with Kepler photometry to derive orbital inclination, dynamical masses of the system components, radii, and temperatures. These measurements are directly applicable for benchmarking stellar models that are integrating the next generation of improvements, such as the magnetic suppression of convection efficiency, updated opacity tables, and fine-tuned equations of state. We selected our EB sample to include systems with low-mass (M less than or similar to 0.8 M-circle dot) primary or secondary components, as well as many EBs expected to populate the relatively sparse parameter space below similar to 0.5 M-circle dot. In this paper, we describe our EB sample and the analytical techniques we are utilizing, and also present masses and radii for two systems that inhabit particularly underpopulated regions of mass-radius-period space: KIC 2445134 and KIC 3003991. Our joint spectroscopic and photometric analysis of KIC 2445134 (q = 0.411 +/- 0.001) yields masses and radii of M-A = 1.29 +/- 0.03 M-circle dot, M-B = 0.53 +/- 0.01 M-circle dot, R-A = 1.42 +/- 0.01 R-circle dot, R-B = 0.510 +/- 0.004 R-circle dot, and a temperature ratio of T-B/T-A = 0.635 +/- 0.001; our analysis of KIC 3003991 (q = 0.298 +/- 0.006) yields M-A = 0.74 +/- 0.04 M-circle dot, M-B = 0.222 +/- 0.007 M-circle dot, R-A = 0.84 +/- 0.01 R-circle dot, R-B = 0.250 +/- 0.004 R-circle dot, and a temperature ratio of T-B/T-A = 0.662 +/- 0.001.NASA ADAP grants [NNX13AF32G, 16-ADAP16-0201]; NSF grantNational Science Foundation (NSF) [AST 1517592]; Center for Exoplanets and Habitable Worlds; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; NSFNational Science Foundation (NSF) [AST 1006676, AST 1126413]; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA); National Science FoundationNational Science Foundation (NSF); Alfred P..Sloan FoundationAlfred P. Sloan Foundation; U.S. Department of Energy of ScienceUnited States Department of Energy (DOE); University of Arizona; Brazilian Participation Group; Brookhaven National LaboratoryUnited States Department of Energy (DOE); University of CambridgeUniversity of Cambridge; Carnegie Mellon University; University of FloridaUniversity of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins UniversityJohns Hopkins University; Lawrence Berkeley National LaboratoryUnited States Department of Energy (DOE); Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State UniversityOhio State University; University of Portsmouth; Princeton UniversityPrinceton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of WashingtonUniversity of Washington; Yale UniversityThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]
