The star formation and chemical evolution history of the Fornax dwarf spheroidal galaxy

By T. D. Boer, E. Tolstoy, V. Hill, A. Saha, E. Olszewski, M. Mateo, E. Starkenburg, G. Battaglia, M. Walker. 2012

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We have combined deep photometry in the B, V and I bands from CTIO/MOSAIC of the Sculptor dwarf spheroidal galaxy, going down to the oldest main sequence turn-offs, with spectroscopic metallicity distributions of red giant branch stars. This allows us to obtain the most detailed and complete star formation history to date, as well as an accurate timescale for chemical enrichment. The star formation history shows that Sculptor is dominated by old (>10 Gyr), metal-poor stars, but that younger, more metal-rich populations are also present. Using star formation histories determined at different radii from the centre we show that Sculptor formed stars with an increasing central concentration with time. The old, metal-poor populations are present at all radii, while more metal-rich, younger stars are more centrally concentrated. We find that within an elliptical radius of 1 degree, or 1.5 kpc from the centre, a total mass in stars of 7.8 × 10^6 M

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/58bcb50942ed2d988f6cf0dd229d6c49f1f4decb

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Dark matter heats up in dwarf galaxies (2018, methodology): “Among the dSphs, by far the well studied are Fornax and Sculptor, which are relatively luminous and have the largest available stellarkinematic samples (for reviews, see Battaglia et al. 2013 and Walker 2013).”
THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I. HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS (2014, background): “…NGC 6822 Clementini et al. (2012) Leo T Monachesi et al. (2012) M32 Okamoto et al. (2012) CVn I, Bootes I, CVn II, and Leo IV Weisz et al. (2012) Leo T de Boer et al. (2012b) Sculptor de Boer et al. (2012a) Fornax Penny et al. (2012) Antlia Sand et al. (2012) Leo V, Pisces II, CVn II del Pino et…”
THE COUPLING BETWEEN THE CORE/CUSP AND MISSING SATELLITE PROBLEMS (2012, background): “Core size Recently, Walker & Peñarrubia (2011; WP11) have measured the slope of the halo mass profile (Γ) in the two brightest MW dSphs, Fornax and Sculptor (M⋆/M⊙ ≃ 3×107 and 8× 106 respectively; de Boer et al. 2012a,b).”