K                    3.4 4.2         
  logg\_P          $\log_{10}$ of gravity according to the Parsec isochrones                        CGS                   3.8 4.8         
  recovery\_rate   fraction of recovered stars of same $G$ magnitude                                                    0.648 1.          
  age              best age                                                                         Gyr             $10^{-3}$ $10^{-1}$   
  mass             best mass                                                                   $\rm M_\odot$            0.026 5.3         
  Teff             best effective temperature                                                        K                   2632 $16.10^3$   
  LogL             best effective $\log_{10}$ of bolometric luminosity                               K                 $-2.8$ 3.0         
  AllWISE\_ID      ID in the AllWISE catalog                                                                                              
  logL\_SED        $\log_{10} $ bolometric luminosity according to the VOSA fit               $\rm Lbol_\odot$         $-3.6$ 2.4         
  Teff\_SED        effective temperature according to the VOSA fit                                   K                   1200 7000        
  disk\_type       Circumstellar disk classification                                                                                      
  SIMBAD\_Name     Primary SIMBAD name                                                                                                    
  Disk\_ref        Reference for circumstellar disk                                                                         1 18          
  ---------------- ------------------------------------------------------------------------- ------------------ ------------- ----------- --

\[memtable\]

Stellar masses and ages {#massage}
=======================

Individual mass and age determination {#massdet}
-------------------------------------

The high photometric quality of [[*Gaia*]{}]{} DR2 enables a straightforward fit between the observed absolute magnitudes $G$, $G_{\rm BP}$ and $G_{\rm RP}$ and the ones determined from stellar evolution theory. [[This method has some limitations: it is of course model dependent and the results will be as good as the assumptions made to derive the isochrones. The past accretion history max influence the results, although @Baraf12 suggests that this may not affect clusters aged 10Myr or older, except 