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Increasing evidence suggests that, similar to their low-mass counterparts,high-mass stars form through a disk-mediated accretion process. At the sametime, formation of high-mass stars still necessitates high accretion rates, andhence, high gas densities, which in turn can cause disks to become unstableagainst gravitational fragmentation. We study the kinematics and fragmentationof the disk around the high-mass star forming region AFGL 2591-VLA 3 which washypothesized to be fragmenting based on the observations that show multipleoutflow directions. We use a new set of high-resolution (0.19 arcsec)IRAM/NOEMA observations at 843 micron towards VLA 3 which allow us to resolveits disk, characterize the fragmentation, and study its kinematics. In additionto the 843 micron continuum emission, our spectral setup targets warm dense gasand outflow tracers such as HCN, HC$_3$N and SO$_2$, as well as vibrationallyexcited HCN lines. The high resolution continuum and line emission maps revealmultiple fragments with subsolar masses within the inner 1000 AU of VLA 3.Furthermore, the velocity field of the inner disk observed at 843 micron showsa similar behavior to that of the larger scale velocity field studied in theCORE project at 1.37 mm. We present the first observational evidence for diskfragmentation towards AFGL 2591-VLA 3, a source that was thought to be a singlehigh-mass core. While the fragments themselves are low-mass, the rotation ofthe disk is dominated by the protostar with a mass of 10.3$\pm 1.8~M_{\odot}$.These data also show that NOEMA Band 4 can obtain the highest currentlyachievable spatial resolution at (sub-)mm wavelengths in observations of strongnorthern sources.

Disk fragmentation in high-mass star formation. High-resolution observations towards AFGL 2591-VLA 3