Figure B1 from On the Origin of a Rotating Metal-poor Stellar Population in the Milky Way Nuclear Cluster

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On the Origin of a Rotating Metal-poor Stellar Population in the Milky Way Nuclear Cluster

Authors: Manuel Arca Sedda, Alessia Gualandris, Tuan Do, Anja Feldmeier-Krause, Nadine Neumayer, and Denis Erkal

2020 The Astrophysical Journal Letters 901 L29.

Provider: AAS Journals

Caption: Figure B1.

Two-body relaxation (straight red line), SRR (dashed black line), and VRR (dotted blue line) timescales as a function of the cluster mass assuming a half-mass–radius of 3 pc and an SMBH mass of ﹩4.5\times {10}^{6}{M}_{\odot }﹩. Horizontal lines mark the relaxation time for the infalling SC and the whole NC.

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