The angular sizes of dwarf stars and subgiants - Non-linear surface brightness relations in BVRcIc from interferometry

TL;DR

This paper calibrates non-linear surface brightness relations using BVRcIc photometry and interferometry to accurately predict the angular sizes of dwarf and subgiant stars, aiding various astronomical observations.

Contribution

It introduces polynomial SBC relations based on visible colours for dwarf and subgiant stars, improving angular diameter predictions with 5% accuracy.

Findings

SBC relations are non-linear due to spectral features.

Polynomial fits enable 5% accurate diameter predictions.

Relations are applicable to nearby stars, with reddening considerations for distant ones.

Abstract

Context: The prediction of stellar angular diameters from broadband photometry plays an important role for different applications. In particular, long-baseline interferometry, gravitational microlensing, extrasolar planet transits, and many other observing techniques require accurate predictions of the angular size of stars. These predictions are based on the surface brightness-colour (SBC) relations. Aims: Our goal is to calibrate general-purpose SBC relations using visible colours, the most commonly available data for most stars. Methods: We compiled the existing long-baseline interferometric observations of nearby dwarf and subgiant stars and the corresponding broadband photometry in the Johnson B V and Cousins Rc Ic bands. We then adjusted polynomial SBC models to these data. Results: Due to the presence of spectral features that depend on the effective temperature, the SBC relations are usually not linear for visible colours. We present polynomial fits that can be employed with BVRcIc based colours to predict the limb-darkened angular diameters (i.e. photospheric) of dwarf and subgiant stars with a typical accuracy of 5%. Conclusions: The derived polynomial relations provide a satisfactory approximation to the observed surface brightness of nearby dwarfs and subgiants. For distant stars, the interstellar reddening should be taken into account, and will usually introduce an additional uncertainty to the predicted angular diameters.