Figure 12
![[Ba/Eu] versus [Fe/H] observed in Ursa Minor dSph galaxy compared to the predictions of the chemical evolution model for Ursa Minor. The solid line represents the best model (ν= 0.2 Gyr−1, wi = 10) and the dotted lines the lower (ν= 0.05 Gyr−1) and upper (ν= 0.5 Gyr−1) limits for the SF efficiency. The thin line represents the best model without Ba production in massive stars.](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/mnras/365/2/10.1111/j.1365-2966.2005.09700.x/2/365-2-477-fig012.jpeg?Expires=1749852634&Signature=UUSFr7~ca9C0Nlpnoidrm2obDUiadsjc5aa9KdexnA2R1fVa4Dr83GOwwS4dU31LL5tSpAdkRp5V~Wmnd0LYxTd9BXlILvpZ~mq3VGMZRY6YEIvo-C5WNiv4VhXBVNTORExnRug5uz-mRYtlHxqWhocPx7PZuW1E7AhFxNqFjWihgdWE01S8XR5g2dA7Hw1NgJJe6zwWTv9-19PpGQyaKYEeDi2F6EZmcGlB5XaT4qyZzUBO7LHxEVpTLwrr2Y0HDvGM5vkrfESRUd9HKMYX~HYZLY8znKUbN7J8gJnl6DIo~qAKAadFs5uR9UrkvO4w7NTnUcJ-kCRr62IBH58ugg__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
[Ba/Eu] versus [Fe/H] observed in Ursa Minor dSph galaxy compared to the predictions of the chemical evolution model for Ursa Minor. The solid line represents the best model (ν= 0.2 Gyr−1, wi = 10) and the dotted lines the lower (ν= 0.05 Gyr−1) and upper (ν= 0.5 Gyr−1) limits for the SF efficiency. The thin line represents the best model without Ba production in massive stars.
