Fig. 1.

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Left panel: Spatial distribution of the FLAMES spectroscopic sample. Newly discovered members are shown as red diamonds. Non-members from the FLAMES sample are shown as red crosses. Previously known members from the literature (K09 + B23) are represented as smaller blue circles. Misidentified literature members are shown as green crosses. The two half-light radii of Boo II as inferred by Muñoz et al. (2018, M18) are shown as a black ellipse. The small grey dots show all stars in the field with good quality SDSS photometry (i.e. broadband photometry uncertainties below 0.2 mag). Right panel: CMD of our spectroscopic sample superimposed with the favoured Boo II Dartmouth isochrone in yellow, chosen to match the system’s spectroscopically identified RGB stars. Three other isochrones of varying metallicity (one more metal-poor at [Fe/H] ∼ −2.5, two more metal-rich at ∼ − 1.5 and ∼ − 1.2) are also overplotted as dashed green lines. The g and i magnitudes are from SDSS.
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