Classifying the satellite plane membership of Centaurus A's dwarf galaxies using orbital alignment constraints. Issue 4 (10th January 2023)

• Record Type: Journal Article
• Authors: Kanehisa, Kosuke Jamie; Pawlowski, Marcel S; Müller, Oliver; Sohn, Sangmo Tony
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 519:Issue 4(2023)
• Page Start: 6184
• Page End: 6198
• Publication Date: 2023-01-10
• Subjects: proper motions -- galaxies: dwarf -- galaxies: groups: individual: NGC5128 -- galaxies: kinematics and dynamics; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stad061
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The flattened, possibly co-rotating plane of satellite galaxies around Centaurus A, if more than a fortuitous alignment, adds to the pre-existing tension between the well-studied Milky Way and M31 planes and the Lambda cold dark matter model of structure formation. It was recently reported that the Centaurus A satellite plane (CASP) may be rotationally supported, but a further understanding of the system's kinematics is elusive in the absence of full 3D velocities. We constrain the transverse velocities of 27 satellites that would rotationally stabilize the Centaurus A plane, and classify the satellites by whether their possible orbits are consistent with the CASP. Five satellites are identified to be unlikely to participate in the plane, two of which are clearly non-members. Despite their previously reported line-of-sight velocity trend suggestive of a common co-rotating motion, 17 out of 22 potential CASP members are consistent with either orbital direction within both the full range of possible kinematics as well as when limiting orbits to those within the plane. On the other hand, disregarding the 5 off-plane satellites found to be inconsistent with CASP membership enhances the significance of the CASP's line-of-sight velocity trend fivefold. Our results are robust with different mass estimates of the Centaurus A halo, and the adoption of either spherical or triaxial NFW potentials.