Suzaku Observations of Galaxy Groups (and related systems)

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Outline • Setting the stage: Groups, X-rays, and Suzaku • Early Suzaku results -- temperature structure, abundance gradients and patterns • Promise and Priorities
Matter in the Universe (the modern view) • Most of the matter in the universe is dark matter, collapsed into a hierarchy (10 7 -10 15 M ) of halos • Galaxies are embedded in halos (that may be embedded in larger halos…) • Larger halos have more galaxies that move faster σ M richness Becker et al. 2007
Page 1: Suzaku Observations of Galaxy Group
Page 5 and 6: Sub-types of interest X-ray: NASA/C
Page 7 and 8: Why Study Groups in X-rays? • The
Page 9 and 10: ROSAT and ASCA Highlights • Abund
Page 11 and 12: XMM-Newton and Chandra More heating
Page 13 and 14: XMM-Newton and Chandra • High res
Page 15 and 16: Cool (
Page 17 and 18: Temperature Structure XIS requires
Page 19 and 20: Abundances RGS: N(?), O, Ne, Mg, Fe
Page 21 and 22: Complementarity, , e.g. NGC 4472
Page 23 and 24: Abundance Profiles courtesy K. Mats
Page 25 and 26: Abundance Patterns Similar pattern
Page 27 and 28: Abundances in Groups with Suzaku: :
Page 29: Abundances in Groups with Suzaku: :

Suzaku Observations of Galaxy Groups (and related systems)

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