Schedule

including some tips - not exhaustive - which elements not forget to mention in your presentations

The aim of these presentations are to explain to the class what is each paper about. What are the assumptions and what are the results, what are the uncertainties.

I expect an electronic presentation from everyone - you can either give this to me afterwards as a ppt or keynote file or best of all as a pdf file. These will be linked to your names below and form part of your grade (40% per paper; 20% for class participation).

There is a computer in 161 you can use, or if you bring it on a memory stick we can use my laptop.

Tues 17 Feb:
chair: Caroline van Borm
Heger & Woosley (2002) ApJ, 567, 532 The Nucleosynthetic Signature of Population III (T) Sietske Bouma
important questions to answer: what kind of models are used; what are the predicted properties of the first stars, explain why they are different for different stellar masses; how can you test the predictions; how do the results on the subsequent generations of stars depend on the mass of the first stars

Cayrel et al. (2004) A&A, 416, 1117 First stars V - Abundance patterns from C to Zn and supernova yields in the early Galaxy (O) Helmer Koppelman
important questions to answer: what kind of survey is "First Stars"; how was the sample selected; with which instrument were they observed; what is the most important result of this work; how do the different element abundances vary in their properties and what does this mean.

Wed 18 Feb:
chair: Jaco Mentz
Recio-Blanco et al. (2014) The Gaia-ESO Survey: the Galactic thick to thin disc transition (O) Simon Steendam
important questions to answer: what is GAIA, what is the aim of the GAIA-ESO survey; what fraction of the data are considered here; how was the sample selected; what does the transition between the thin and thick disk mean; what is the most important result; why do people care about the different properties of the thin & the think disk.

Schoenrich & Binney (2009) MNRAS, 399, 1145 Origin and structure of the Galactic disc(s) (T) Johanna Hartke
important questions to answer: describe model used and assumptions involved; explain the different physical processes that occur in a galactic disk and how they will impact upon the observed abundance properties of the stars and how they are distributed over the disc with time (ie., creating or destroying gradients). This paper compares with data sets it is important to understand how well this works.

Tues 24 Feb:
chair: Aku Venhola
Karlsson et al. (2008) ApJ, 679, 6 Uncovering the Chemical Signature of the First Stars in the Universe (T) Anke Arentsen
important questions to answer: describe model used and assumptions involved; what is inhomogeneous mixing; what problem in our understanding of the first stars is this paper addressing; how does it suggest future surveys should be done differently

Caffau et al. (2012) A&A, 542, A51 A primordial star in the heart of the Lion (O) Tim Kefelaar
important questions to answer: how was this star found; why is it an important discovery; what is different from other similarly extremely metal poor stars; what do the abundance ratios suggest about its origins

Wed 25 Feb:
chair: Caroline van Borm
Kobayashi et al. (2006) ApJ, 653, 1145 Galactic Chemical Evolution: Carbon through Zinc (T) Helmer Koppelman
important questions to answer: describe model used and assumptions involved; how were the yields determined for the chemical evolution; what are the different types of supernovae models used; describe the comparison to the Milky Way; how reliable do you think the model results are.

Venn et al. (2004) AJ, 128, 1177 Stellar Chemical Signatures and Hierarchical Galaxy Formation (O) Sietske Bouma
important questions to answer: how are the different components of the Milky Way selected; how can a detailed comparison be made between the abundances of stars in dSph and the Milky Way; what implications to the results have for our understanding of galaxy formation & evolution; which element groups are considered particularly important and why.

Tues 3 March:
chair: Aku Venhola
Revaz & Jablonka (2012) A&A, 538, 82 The dynamical and chemical evolution of dwarf spheroidal galaxies with GEAR (T) Simon Steendam
important questions to answer: what is GEAR and why is it a good approach to model dwarf spheroidal galaxies; how accurately are the different physical processes included and which are the most important to determine the evolution of dwarf galaxies; which data, and which chemical elements are used to compare to the model results; how well do the models/simulations match real galaxies.

Norris et al. (2010) ApJ, 723, 1632 Chemical Enrichment in the Faintest Galaxies: The Carbon and Iron Abundance Spreads in the Boötes I Dwarf Spheroidal Galaxy and the Segue 1 System (O) Johanna Hartke
important questions to answer: what kind of data are used here; what are ultra-faint dwarfs and how do they differ from other (dwarf) galaxies, like dSph and dI; how do the proper ties of these two very faint galaxies compare with the halo of the Milky Way; why is Carbon abundance in metal poor stars particularly interesting; what does this suggest about the origins of these galaxies.

Wed 4 March:
chair: Eline Tolstoy
Becker et al. (2012) ApJ, 744, 91 Iron and α-element Production in the First One Billion Years after the Big Bang (O) Anke Arentsen
important questions to answer: which elements are most accurately measured in quasar absorption line systems; how well determined are these abundances, what are the major uncertainties; how does redshift compare to age; how do these abundances compare to those measured in stars in nearby galaxies

Salvadori et al. (2014) MNRAS, 437, 26L Metals and ionizing photons from dwarf galaxies (T)
important questions to answer: describe model used and assumptions involved; which physical processes are considered the most important to explain the link between dwarf galaxies and the gas around them; what is difference between circum-galactic medium and intergalactic medium; how is the metallicity floor in the absorption line systems linked to the star formation rate in ancient dwarf galaxies; what are the main uncertainties in this paper, how can they be improved upon.