Notes. The columns are as follows – 1: MSX PSC name; 2: right ascension; 3: declination; 4: RMS classification; 5: number of detected flux data points, not including upper limits, included in the fit; 6: flags indicating which data were included in the SED. These are from left to right 2MASS (Y or N), TIMMI2 (Y or N), far-IR IGA (I) or MIPSGAL (M), submillimetre (Y or N) and millimetre (N, 1 = Beuther et al. 2002, 2 = Faúndez et al. 2004, 3 = Hill et al. 2005, 4 = Beltrán et al. 2006); 7: for the fit; 8: Δχ² at which at least 10 fits are found; 9: the number of fits; 10: the bolometric flux with uncertainty, calculated using Eqs. (1) and (2); 11: whether the kinematic distance has been solved (s) or the near/far ambiguity remains unsolved (nf). Sources with galactocentric radii  ≥ 8.5 kpc or at the tangent point are also indicated as solved (s); 12: the apportioning correction applied to large-beam fluxes, as discussed in Sect. 2.1, with a value of 1 meaning that no apportioning was performed; 13: type of apportioning used with “N” for none, “T” for TIMMI2 data, “G” for GLIMPSE data and “S” for a simple split of the remaining fraction between all multiple source components without TIMMI2 or GLIMPSE detections. A full version of this table is available online at the CDS.