<html><head><meta http-equiv="Content-Type" content="text/html charset=utf-8"></head><body style="word-wrap: break-word; -webkit-nbsp-mode: space; -webkit-line-break: after-white-space;" class=""><div class="">Dear all,</div><div class=""><br class=""></div><div class="">join us again on Astro Journal Club next Wednesday (Nov 22th) at 3 p.m. (sharp) in the seminar room F-201 of the Physics Department.</div><div class=""><br class=""></div><div class="">You can find informations about upcoming AJC seminars and links to previous AJC presentations @ <a href="https://lanaceraj.wixsite.com/ajc-main" class="">https://lanaceraj.wixsite.com/ajc-main</a> </div><div class=""><br class=""></div><div class=""><b class="">Presenter</b>: Marko Imbrišak</div><div class=""><br class=""></div><div class=""><b class="">Title of paper</b>: Ages and heavy element abundances from very metal-poor stars in the Sagittarius dwarf galaxy</div><div class=""><br class=""></div><div class=""><b class="">Authors</b>: Hansen et al. (2017)</div><div class=""><br class=""></div><div class=""><b class="">Abstract</b>: </div><div class="">Sagittarius (Sgr) is a massive disrupted dwarf spheroidal galaxy in the Milky Way halo that has undergone several stripping events. Previous chemical studies were restricted mainly to a few, metal- rich ([Fe/H]~ -1) stars that suggested a top-light initial mass function (IMF). Here we present the first high-resolution, very metal-poor ([Fe/H]=-1 to -3) sample of 13 giant stars in the main body of Sgr. We derive abundances of 13 elements namely C, Ca, Co, Fe, Sr, Ba, La, Ce, Nd, Eu, Dy, Pb, and Th which challenge the interpretation based on previous studies. Our abundances from Sgr mimic those of the metal-poor halo and our most metal-poor star ([Fe/H]~ -3) indicates a pure r-process pollution. Abundances of Sr, Pb, and Th are presented for the first time in Sgr, allowing for age determination using nuclear cosmochronology. We calculate ages of 9±2.5 Gyr. Most of the sample stars have been enriched by a range of asymptotic giant branch (AGB) stars with masses between 1.3 and 5 M⊙. Sgr J190651.47-320147.23 shows a large overabundance of Pb (2.05dex) and a peculiar abundance pattern best fit by a 3 M⊙ AGB star. Based on star-to-star scatter and observed abundance patterns a mixture of low- and high-mass AGB stars and supernovae (15-25 M⊙) are necessary to explain these patterns. The high level (0.29±0.05 dex) of Ca indicates that massive supernovae must have existed and polluted the early ISM of Sgr before it lost its gas. This result is in contrast with a top-light IMF with no massive stars polluting Sgr. </div><div class=""><br class=""></div><div class=""><b class="">Link to paper</b>: <a href="https://arxiv.org/abs/1711.02101" class="">https://arxiv.org/abs/1711.02101</a></div><div class=""><br class=""></div><div class="">If you’d like to present a paper from the field of astrophysics, please contact me via this email (<a href="mailto:lceraj@phy.hr" class="">lceraj@phy.hr</a>).</div><div class=""><br class=""></div><div class="">See you all on Wednesday.</div><div class=""><br class=""></div><div class="">Cheers,</div><div class="">Lana</div></body></html>