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Feeling the Pull: A Study of Natural Galactic Accelerometers. II. Kinematics and Mass of the Delicate Stellar Stream of the Palomar 5 Globular Cluster

• Authors: Rodrigo A. Ibata, Geraint F. Lewis, Guillaume Thomas, Nicolas F. Martin, and Scott Chapman

2017 The Astrophysical Journal 842 120.

• Provider: AAS Journals

Caption: Figure 7.

As in Figure 5, but for the 22 stars of the Odenkirchen et al. (2009) sample. The membership probability criterion used here is ﹩{P}_{\mathrm{RGB}}\times {P}_{\mathrm{DDO}51}﹩, since we do not have access to the relevant spectral information to calculate ﹩{P}_{\mathrm{BS}12}﹩ or ﹩{P}_{[\mathrm{Fe}/{\rm{H}}]}﹩ for the entire sample. Panel (b) shows the 18 stars within the velocity selection box of Figure 5(a). The positions of two likely non-member stars (with ﹩{P}_{\mathrm{membership}}\lt 0.2)﹩ are shown with pentagonal “star” glyphs. One can see that the high-likelihood stars follow very closely the fit to the matched-filter map (red line).