The table contains the bolometric luminosities and radii in solar units for a subset of ultracool dwarfs from the Gaia DR3 catalogue, as well as some intermediate quantities used in the selection of sources and in the derivation of the luminosities and radii.
For more details please refer to Gaia Collaboration et al. (2023c).
A unique single numerical identifier of the source obtained from gaia_source (for a detailed description see gaia_source.source_id).
Multiplicative factor used to scale the total observed flux to obtain the total SED flux. It is derived using the CIFIST 2011-2015 BT Settl models of solar metallicity and and interpolating the ESP-UCD effective temperature in the BT Settl grid values.
Bolometric luminosity of the UCD in solar units obtained by scaling the observed flux using ftot_fobs and using the Gaia measured parallax.
Uncertainty in UCD bolometric luminosity calculated using a simple Taylor expansion and neglecting the correlations.
Radius of the UCD derived using the Stefan-Boltzmann law, the UCD bolometric luminosity and the ESP-UCD effective temperature.
Uncertainty in the UCD radius calculated using a simple Taylor expansion and neglecting the correlations.
Reduced of the Virtual Observatory SED Analyzer (VOSA) fit to the observed fluxes.