# HIDES spectroscopy of bright detached eclipsing binaries from the $Kepler$ field - III. Spectral analysis, updated parameters, and new systems

## TL;DR

This paper refines the physical and orbital parameters of bright detached eclipsing binaries from the Kepler field using new high-resolution spectroscopy and photometry, improving model consistency and characterizing three new systems.

## Contribution

It provides updated parameters for DEBs with spectroscopic data, introduces spectral analysis with iSpec, and compares results with Gaia data for the first time.

## Key findings

- Most systems show good agreement with theoretical models.
- Distances derived are consistent with Gaia DR2.
- Spectral analysis yields effective temperatures and metallicities.

## Abstract

We present the latest results of our spectroscopic observations and refined modelling of a sample of detached eclipsing binaries (DEBs), selected from the $Kepler$} Eclipsing Binary Catalog, that are also double-lined spectroscopic binaries (SB2). New high resolution spectra obtained with the HIDES spectrograph, attached to the 1.88-m telescope of the Okayama Astrophysical Observatory supplemented the previous observations, allowing to improve physical parameters of some systems, and characterize three previously omitted. All the obtained radial velocities (RVs) were combined with $Kepler$ photometry, in order to derive a full set of orbital and physical parameters. Ten out of eleven SB2s have their component spectra tomographically disentangled, and spectral analysis was performed with iSpec, in order to derive effective temperatures of components and metallicities of the systems. By comparing our results with theoretical models, we assess the age and evolutionary status of the studied objects. We find a good match to all but one systems. We have derived distances from thus determined parameters, and compare them with those from the $Gaia$ Data Release 2. For systems previously studied by other authors, our new results lead to better consistency between observations and models.