By L. Casagrande and D. A. VandenBerg (2014, 2018)
What it does
A survey measures the light of a star inside one filter, while the bolometric magnitude counts all of its light. The bolometric correction bridges the two. It depends on the star's spectrum, and so on its temperature, surface gravity, metallicity and reddening.
L. Casagrande and D. A. VandenBerg computed synthetic photometry from MARCS model spectra through the passbands of many systems, among them Johnson-Cousins, SDSS, 2MASS, HST, Tycho, Hipparcos, Pan-STARRS1, SkyMapper, JWST and Gaia DR2 and DR3. Their codes interpolate the resulting tables to the temperature, gravity, metallicity and reddening of a star.
How I used it
In my MSc thesis I used BCCode to compute bolometric corrections and luminosities, including Monte Carlo sensitivity tests (Sect. 4.2.1, Figs 4.4 to 4.7).
The animation
The spectrum is an observed one, of the star HD 42256 from the X-shooter Spectral Library. It stands in for the model spectra the tables are computed from. The Gaia DR3 passbands are the real ones, and the correction tables are the real tables of Casagrande and VandenBerg at solar metallicity for four values of reddening.
Where the star lands, the layout, the colours, the camera and the vertical scale of the surfaces are drawn.