Figure 3 from Nearest Neighbor: The Low-mass Milky Way Satellite Tucana III

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Nearest Neighbor: The Low-mass Milky Way Satellite Tucana III

Authors: J. D. Simon, T. S. Li, A. Drlica-Wagner, K. Bechtol, J. L. Marshall, D. J. James, M. Y. Wang, L. Strigari, E. Balbinot, K. Kuehn, A. R. Walker, T. M. C. Abbott, S. Allam, J. Annis, A. Benoit-Lévy, D. Brooks, E. Buckley-Geer, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, C. E. Cunha, C. B. D'Andrea, L. N. da Costa, D. L. DePoy, S. Desai, P. Doel, E. Fernandez, B. Flaugher, J. Frieman, J. García-Bellido, E. Gaztanaga, D. A. Goldstein, D. Gruen, G. Gutierrez, N. Kuropatkin, M. A. G. Maia, P. Martini, F. Menanteau, C. J. Miller, R. Miquel, E. Neilsen, B. Nord, R. Ogando, A. A. Plazas, A. K. Romer, E. S. Rykoff, E. Sanchez, B. Santiago, V. Scarpine, M. Schubnell, I. Sevilla-Noarbe, R. C. Smith, F. Sobreira, E. Suchyta, M. E. C. Swanson, G. Tarle, L. Whiteway, and B. Yanny

2017 The Astrophysical Journal 838 11.

Provider: AAS Journals

Caption: Figure 3.

Posterior probability distribution from a maximum-likelihood fit for the systemic velocity and velocity dispersion (left set of panels) and the mean metallicity and metallicity dispersion (right set of panels) of Tuc III. In the upper left panels the 68% confidence intervals on the mean velocity and metallicity are indicated by the dashed gray lines. In the lower right panels the 95.5% upper limits on the velocity and metallicity dispersion are indicated by the dashed gray lines. We do not significantly resolve either the velocity dispersion or the metallicity dispersion of Tuc III.

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