Eclipsing Binary Populations across the Northern Galactic Plane from the KISOGP survey

TL;DR

This paper catalogs over 7000 eclipsing binaries in the northern Galactic Plane from the KISOGP survey, deriving their parameters, distances, and the structure of the thin disk, and compares Gaia parallaxes with binary-based measurements.

Contribution

It provides a large, visually identified catalog of eclipsing binaries with detailed parameters, distances, and Galactic structure insights, including a calibration of Gaia parallaxes.

Findings

Identified 7055 eclipsing binaries across 330 square degrees.

Derived distances and extinction for EW-type binaries using period-luminosity relation.

Detected a Gaia parallax zero-point offset of -42.1 microarcseconds.

Abstract

We present a catalog of eclipsing binaries in the northern Galactic Plane from the Kiso Wide-Field Camera Intensive Survey of the Galactic Plane (KISOGP). We visually identified 7055 eclipsing binaries spread across $\sim$330 square degrees, including 4197 W Ursa Majoris/EW-, 1458 $\beta$ Lyrae/EB-, and 1400 Algol/EA-type eclipsing binaries. For all systems, $I$-band light curves were used to obtain accurate system parameters. We derived the distances and extinction values for the EW-type objects from their period--luminosity relation. We also obtained the structure of the thin disk from the distribution of our sample of eclipsing binary systems, combined with those of high-mass star-forming regions and Cepheid tracers. We found that the thin disk is inhomogeneous in number density as a function of Galactic longitude. Using this new set of distance tracers, we constrain the detailed structure of the thin disk. Finally, we report a global parallax zero-point offset of $ \Delta \pi=-42.1\pm1.9\mbox{(stat.)}\pm12.9\mbox{(syst.)}$ $\mu$as between our carefully calibrated EW-type eclipsing binary positions and those provided by Gaia Early Data Release 3. Implementation of the officially recommended parallax zero-point correction results in a significantly reduced offset. Additionally, we provide a photometric characterization of our EW-type eclipsing binaries that can be applied to further analyses.