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Abridged. Eclipsing spectroscopic double-lined binaries are the prime sourceof precise and accurate measurements of masses and radii of stars. Thesemeasurements provide a stringent test of models of stellar evolution that arepersistently reported to contain major shortcomings. The mass discrepancyobserved for the eclipsing spectroscopic double-lined binaries is one of themanifestations of shortcomings in stellar evolution models. Our ultimate goalis to provide an observational mapping of the mass discrepancy and propose arecipe for its solution. We initiate a spectroscopic monitoring campaign of 573candidate eclipsing binaries of which 83 are analysed in this work with themethods of least-squares deconvolution and spectral disentangling. TESS lightcurves are used to provide photometric classification of the systems accordingto the type of their intrinsic variability. We confirm 69 systems as eitherspectroscopic binaries or higher-order multiple systems. Twelve stars areclassified as single and two more objects are found at the interface of theirline profile variability being interpreted as due to binarity and intrinsicvariability of the star. Moreover, 20 eclipsing binaries are found to containat least one component that exhibits stellar oscillations. The sample presentedin this work contains both detached and semi-detached systems and covers arange in the effective temperature and mass of the star of Teff = [7000,30000]K and M = [1.5,15] M_Sun, respectively. We conclude an appreciable capabilityof the spectral disentangling method to deliver precise and accuratespectroscopic orbital elements from as few as 6-8 orbital phase-resolvedspectroscopic observations. Orbital solutions obtained this way are accurateenough to deliver age estimates with accuracy of 10% or better, an importantresource for calibration of stellar evolution models.

Observational mapping of the mass discrepancy in eclipsing binaries: Selection of the sample and its photometric and spectroscopic properties