Brown dwarfs and planetary-mass objects have photometric and spectroscopic properties similar to exoplanet orbiting stars but they are in isolation, making their characterisation easier. We present a solid spectral sequence of substellar late-M and L-type dwarf members with effective temperatures below 2000 Kelvins of five young regions and open clusters: sigma Orionis (3-8 Myr; 350 pc), Upper Scorpius (5-10 Myr; 145 pc), the Pleiades (125 Myr; 135 pc), Coma Berenices (500 Myr; 87 pc), and the Hyades (650 Myr; 47 pc). We compare their photometric and spectroscopic properties to members of young moving groups and older field L dwarfs.

Most of the diagrams and results presented in this poster have been published in refereed astronomical journals (or submitted): Sigma Orionis: Zapatero Osorio et al. (2017, ApJ, 842, 65) Upper Scorpius: Lodieu et al. (2018, MNRAS, 473, 2020) Pleiades: Zapatero Osorio et al. (2018, MNRAS, 475, 139) Hyades: Perez-Garrido et al. (2017, A&A, 599, 78); Martin et al. (2018, ApJ, 856, 40); Lodieu et al. (2018, A&A, 615, 12) Coma Berenices: Olivares et al. (2023, A&A, submitted)

{"references": ["Zapatero Osorio et al. (2017, ApJ, 842, 65)", "Lodieu et al. (2018, MNRAS, 473, 2020)", "Zapatero Osorio et al. (2018, MNRAS, 475, 139)", "P\u00e9rez-Garrido et al. (2017, A&A, 599, 78)", "Martin et al. (2018, ApJ, 856, 40)", "Lodieu et al. (2018, A&A, 615, 12)", "Olivares et al. (2023, A&A, submitted)"]}