Extended Data Fig. 6: Comparison of halo masses of dwarf galaxies derived from different methods.
From: Unexpected clustering pattern in dwarf galaxies challenges formation models
a–d, halo mass versus M* for dwarf samples with different Σ*. Symbols with error bars show the halo mass obtained by using the HI kinematics versus M* and their uncertainties. The error bars for halo mass represent 1-σ uncertainties, while the error bars for M*, taken from ref. 52, represent 16th and 84th percentiles of the likelihood distribution. Teal shadow region shows the SHMR14 and its 1σ uncertainty. Cyan symbols show the results for UDGs taken from ref. 44. These UDGs have spatially-resolved HI kinematics maps, therefore their halo mass measurements are more reliable than ours. As can be seen, these UDGs follow the same trend as our diffuse dwarfs.
