Disk fraction among free-floating planetary-mass objects in Upper Scorpius

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Table 1

Posterior estimates of the key regression and outlier model parameters from our Bayesian inference.

	Mass 5 Myr		Mass 10 Myr

Parameters	[25–105] M_Jup	[0–25] M_Jup	[25–105] M_Jup	[0–25] M_Jup
Intercept	${0.267}_{- 0.011}^{+ 0.009}$ $0.267_{ - 0.011}^{ + 0.009}$	${0.415}_{- 0.050}^{+ 0.045}$ $0.415_{ - 0.050}^{ + 0.045}$	${0.287}_{- 0.018}^{+ 0.017}$ $0.287_{ - 0.018}^{ + 0.017}$	${0.446}_{- 0.06}^{+ 0.061}$ $0.446_{ - 0.06}^{ + 0.061}$
Slope	$- {0.0005}_{- 0.0002}^{- 0.0002}$ $- 0.0005_{ - 0.0002}^{ - 0.0002}$	$- {0.0070}_{- 0.0025}^{+ 0.0027}$ $- 0.0070_{ - 0.0025}^{ + 0.0027}$	$- {0.0006}_{- 0.0002}^{+ 0.0002}$ $- 0.0006_{ - 0.0002}^{ + 0.0002}$	$- {0.0080}_{- 0.0035}^{+ 0.0032}$ $- 0.0080_{ - 0.0035}^{ + 0.0032}$
P_b	${0.290}_{- 0.055}^{+ 0.057}$ $0.290_{ - 0.055}^{ + 0.057}$	${0.363}_{- 0.101}^{+ 0.103}$ $0.363_{ - 0.101}^{ + 0.103}$	${0.252}_{- 0.063}^{+ 0.069}$ $0.252_{ - 0.063}^{ + 0.069}$	${0.329}_{- 0.117}^{+ 0.125}$ $0.329_{ - 0.117}^{ + 0.125}$
Y_b	${0.430}_{- 0.042}^{+ 0.041}$ $0.430_{ - 0.042}^{ + 0.041}$	${0.526}_{- 0.035}^{+ 0.034}$ $0.526_{ - 0.035}^{ + 0.034}$	${0.514}_{- 0.045}^{+ 0.041}$ $0.514_{ - 0.045}^{ + 0.041}$	${0.531}_{- 0.044}^{+ 0.039}$ $0.531_{ - 0.044}^{ + 0.039}$
σ_b	${0.179}_{- 0.025}^{+ 0.028}$ $0.179_{ - 0.025}^{ + 0.028}$	${0.073}_{- 0.023}^{+ 0.036}$ $0.073_{ - 0.023}^{ + 0.036}$	${0.106}_{- 0.028}^{+ 0.047}$ $0.106_{ - 0.028}^{ + 0.047}$	${0.056}_{- 0.027}^{+ 0.055}$ $0.056_{ - 0.027}^{ + 0.055}$

Notes. We separately show results for the high-mass (25–105 M_Jup) and low-mass (0–25 M_Jup) regimes and for the analysis with masses assuming ages of 5 and 10 Myr. The mass division between the low- and high-mass regimes is set at M = 25 M_Jup, following the observed break in the sequence (see Sect. 3.2). Reported values correspond to the posterior median, with uncertainties given as 3–97% HDIs in subscript and superscript. P_b is the global outlier fraction in the population. Y_b and σ_b are the center and scale of the outlier (excess) distribution in W1–W2 color space. The slope and intercept correspond to the best-fit linear regression for the photospheric sequence. Posteriors are well-converged with $\hat{R} ≃ 1.0$ $\hat R \simeq 1.0$ for all parameters.

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