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Abstract <p>Nowadays Gaia DR3 is one of the most widely used data products in astronomy. The difference in pipelines for <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(G\)</EquationSource> <!--BPhysMGU2570174Chulkov-m1--> </InlineEquation>, <InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(BP\)</EquationSource> <!--BPhysMGU2570174Chulkov-m2--> </InlineEquation>, and <InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(RP\)</EquationSource> <!--BPhysMGU2570174Chulkov-m3--> </InlineEquation> photometry induces artifacts specific to double stars with <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(0.1\lesssim\rho\lesssim 2\)</EquationSource> <!--BPhysMGU2570174Chulkov-m4--> </InlineEquation> arcsec angular separation, which can be easily misinterpreted and are addressed in this manuscript.</p>

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Partially Resolved Binary Stars in Gaia

  • 期刊论文

  • 发表日期：

    2025年12月1日

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  • D. A. Chulkov

摘要

Abstract

Nowadays Gaia DR3 is one of the most widely used data products in astronomy. The difference in pipelines for \(G\) , \(BP\) , and \(RP\) photometry induces artifacts specific to double stars with \(0.1\lesssim\rho\lesssim 2\) arcsec angular separation, which can be easily misinterpreted and are addressed in this manuscript.