Theoretical isochrones in several photometric systems

I. Johnson-Cousins-Glass, HST/WFPC2, HST/NICMOS, Washington, and ESO Imaging Survey filter sets

¹ Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, 35122 Padova, Italy
² Osservatorio Astronomico di Trieste, via Tiepolo 11, 34131 Trieste, Italy
³ Istituto di Astrofisica Spaziale, CNR, via del Fosso del Cavaliere, 00133 Roma, Italy
⁴ Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy
⁵ PACS ICC-team, Instituut voor Sterrenkunde, Celestijnenlaan 200B, 3001 Heverlee, Belgium
⁶ European Southern Observatory, Karl-Schwarzschild-Str.  2, 85740 Garching bei München, Germany
⁷ Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str.  1, 85740 Garching bei München, Germany

Corresponding author: L. Girardi, Lgirardi@ts.astro.it

Received: 5 November 2001
Accepted: 19 April 2002

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 , , and . 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.