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SUMMARY:Exploring the kinematics of the Magellanic stellar periphery
DTSTART;VALUE=DATE-TIME:20230322T143000Z
DTEND;VALUE=DATE-TIME:20230322T145500Z
DTSTAMP;VALUE=DATE-TIME:20241114T092439Z
UID:indico-contribution-179@meetings.aip.de
DESCRIPTION:Speakers: Lara Cullinane (JHU)\nRecent panoramic maps of the M
 agellanic system have revealed a wealth of low-surface-brightness stellar 
 substructures surrounding both the Large and Small Magellanic Clouds (LMC/
 SMC)\; clear evidence of tidal interactions between the two Clouds\, as we
 ll as with the Milky Way. However\, the interaction history of the Magella
 nic system beyond the most recent LMC/SMC close passage remains poorly con
 strained. In order to shed light on this issue\, we have instigated a larg
 e-scale spectroscopic follow-up of stars in low-density features extending
  to distances beyond 20 degrees from the Clouds’ centres. We use a combi
 nation of Gaia astrometry and spectroscopically-derived radial velocities\
 , obtained with 2dF+AAOmega on the Anglo-Australian Telescope\, to determi
 ne 3D kinematics for thousands of stars in these features and the extended
  outer disks of the two Clouds. In this talk\, I will discuss new results 
 focussed on the southern outskirts of the LMC. Several substructures in th
 is region\, including claw-like features extending from the southern LMC d
 isk\, and a long arm-like substructure wrapping around the southern LMC ou
 tskirts toward the eastern SMC disk\, are found to be predominantly compos
 ed of perturbed LMC disk material. All substructures show significant pert
 urbations from equilibrium disk kinematics\, with one claw-like feature di
 splaying out-of-plane velocities exceeding 60 km/s and apparent counter-ro
 tation relative to the LMC’s disk. Such complex features plausibly requi
 re multiple previous interactions with the SMC to fully explain the observ
 ed dynamical properties. This demonstrates the efficacy of our data as a b
 enchmark for assessing dynamical models to disentangle the origins of Mage
 llanic substructures\, the masses of the two Clouds\, and the evolution of
  the Magellanic system. I will also briefly discuss new efforts to conduct
  analogous kinematic mapping of M33 and its outskirts\, which aim to simil
 arly understand the evolution of this massive dwarf galaxy.\n\nhttps://iau
 s379.aip.de/event/20/contributions/179/
LOCATION:Haus H\, Telegrafenberg
URL:https://iaus379.aip.de/event/20/contributions/179/
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