Variable stars in Local Group galaxies - V. The fast and early evolution of the low-mass Eridanus II dSph galaxy

Martínez-Vázquez, C. E.; Monelli, M.; Cassisi, S.; Taibi, S.; Gallart, C.; Vivas, A. K.; Walker, A. R.; Martín-Ravelo, P.; Zenteno, A.; Battaglia, G.; Bono, G.; Calamida, A.; Carollo, D.; Cicuéndez, L.; Fiorentino, G.; Marconi, M.; Salvadori, S.; Balbinot, E.; Bernard, E. J.; Dall'Ora, M.; Stetson, P. B.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society

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We present a detailed study of the variable star population of Eridanus II (Eri II), an ultra-faint dwarf galaxy that lies close to the Milky Way virial radius. We analyse multi-epoch g, r, i ground-based data from Goodman and the Dark Energy Camera, plus F475W, F606W, F814W space data from the Advanced Camera for Surveys. We report the detection of 67 RR Lyrae (RRL) stars and 2 Anomalous Cepheids, most of them new discoveries. With the RRL stars, we measure the distance modulus of Eri II, μ0 = 22.84 ± 0.05 mag (D⊙ = 370 ± 9 kpc), and derive a metallicity spread of 0.3 dex (0.2 dex intrinsic). The colour distribution of the horizontal branch (HB) and the period distribution of the RRL stars can be nicely reproduced by a combination of two stellar models of [Fe/H] = (-2.62, -2.14). The overall low metallicity is consistent with the red giant branch bump location, 0.65 mag brighter than the HB. These results are in agreement with previous spectroscopic studies. The more metal-rich RRL and the RRab stars have greater central concentration than the more metal-poor RRL and the RRc stars that are mainly located outside ~1 rh. This is similar to what is found in larger dwarf galaxies such as Sculptor, and in agreement with an outside-in galaxy formation scenario. This is remarkable in such a faint dwarf galaxy with an apparently single and extremely short (<1 Gyr) star formation burst. Finally, we have derived new and independent structural parameters for Eri II and its star cluster using our new data that are in very good agreement with previous estimates.
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