  Observed breakBRD ("break bulges in red disks") galaxies are a nearby sample
of face-on disk galaxies with particularly centrally-concentrated star
formation: they have red disks but recent star formation in their centers as
measured by the D$_n$4000 spectral index. In Kopenhafer et al. (2020), a
comparable population of breakBRD analogues was identified in the TNG
simulation, in which the central concentration of star formation was found to
reflect a central concentration of dense, starforming gas caused by a lack of
dense gas in the galaxy outskirts. In this paper we examine the circumgalactic
medium of the central breakBRD analogues to determine if the extended halo gas
also shows differences from that around comparison galaxies with comparable
stellar mass. We examine the circumgalactic medium gas mass, specific angular
momentum, and metallicity in these galaxy populations. We find less gas in the
circumgalactic medium of breakBRD galaxies, and that the breakBRD
circumgalactic medium is slightly more concentrated than that of comparable
stellar mass galaxies. In addition, we find that the angular momentum in the
circumgalactic medium of breakBRD galaxies tends to be low for their stellar
mass, and show more misalignment to the angular momentum vector of the stellar
disk. Finally, we find that the circumgalactic medium metallicity of breakBRD
galaxies tends to be high for their stellar mass. Together with their low SFR,
we argue that these CGM properties indicate a small amount of disk feeding
concentrated in the central regions, and a lack of low-metallicity gas
accretion from the intergalactic medium.
