Theoretical isochrones in several photometric systems I. Johnson-Cousins-Glass, HST/WFPC2, HST/NICMOS, Washington, and ESO Imaging Survey filter sets

TL;DR

This paper presents a comprehensive set of theoretical isochrones across multiple photometric systems, enabling accurate stellar population analysis by providing bolometric corrections and magnitudes derived from an extensive spectral library.

Contribution

It introduces a unified formalism for converting synthetic spectra into bolometric corrections applicable to various photometric systems, along with updated stellar spectra and a database of isochrones.

Findings

Tables of bolometric corrections for multiple photometric systems are provided.

The spectral library covers a wide range of stellar parameters with improved accuracy.

The resulting isochrones are ready for use in diverse astrophysical applications.

Abstract

We provide tables of theoretical isochrones in several photometric systems. To this aim, the following steps are followed: (1) First, we re-write the formalism for converting synthetic stellar spectra into tables of bolometric corrections. The resulting formulas can be applied to any photometric system, provided that the zero-points are specified by means of either ABmag, STmag, VEGAmag, or a standard star system that includes well-known spectrophotometric standards. Interstellar absorption can be considered in a self-consistent way. (2) We assemble an extended and updated library of stellar intrinsic spectra. It is mostly based on non-overshooting ATLAS9 models, suitably extended to both low and high effective temperatures. This offers an excellent coverage of the parameter space of Teff, logg, and [M/H]. We briefly discuss the main uncertainties and points still deserving more improvement. (3) From the spectral library, we derive tables of bolometric corrections for Johnson-Cousins-Glass, HST/WFPC2, HST/NICMOS, Washington, and ESO Imaging Survey systems (this latter consisting on the WFI, EMMI, and SOFI filter sets). (4) These tables are used to convert several sets of Padova isochrones into the corresponding absolute magnitudes and colours, thus providing a useful database for several astrophysical applications. All data files are made available in electronic form.