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Revealing Elliptical Galaxy Halos

Revealing Elliptical Galaxy Halos. Duncan Forbes, Swinburne University. Collaborators. Robert Proctor (Sao Paulo) Alan Brito (Swinburne) George Hau (Swinburne) Lee Spitler (Swinburne) Caroline Foster (Swinburne) Christina Blom (Swinburne) Jean Brodie (UCSC) Aaron Romanowsky (UCSC)

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Revealing Elliptical Galaxy Halos

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  1. Revealing Elliptical Galaxy Halos Duncan Forbes, Swinburne University

  2. Collaborators • Robert Proctor (Sao Paulo) • Alan Brito (Swinburne) • George Hau (Swinburne) • Lee Spitler (Swinburne) • Caroline Foster (Swinburne) • Christina Blom (Swinburne) • Jean Brodie (UCSC) • Aaron Romanowsky (UCSC) • Jacob Arnold (UCSC) • Jay Strader (Harvard) • Soeren Larsen (Utrecht)

  3. Why study elliptical galaxy halos? Also some kinematic signatures of galaxy formation only apparent at large radii

  4. Halo stellar populations and kinematics using Deimos on Keckmultiplexing times 4 ! “Need outer halo kinematics” - Rix

  5. Deimos spectra and fits to the galaxy halo light in the 3 Calcium Triplet regions S/N

  6. NGC 2768: Deimos as an IFU

  7. Velocity map for NGC 2768 Reff = 64 arcsec Sauron maps

  8. NGC 821: a low DM galaxy? Radial Kinematics - NGC 821 Proctor,Forbes etal. 2009

  9. N2768 and N821

  10. Anisotropy (Binney) diagram NGC 2768 Fast -> Faster NGC 821 Fast -> Slow

  11. Metallicity gradients (<1Re) vs mass Log sigma MB Spolaor et al. 2009

  12. NGC 2768: Metallicity to ~3 Re

  13. New Halo vs Globular Cluster Mass (linear) Relation Galaxy Halo Mass Globular Cluster System Mass Spitler & Forbes 2008

  14. Globular Cluster Formation GC formation is directly proportional to the host halo mass with little environmental trend 0.007% of Halo Mass = (Globular Cluster System Mass)

  15. Science progresses best when observations force us to alter our preconceptions. Vera Rubin Teacher and Coauthor

  16. Conclusions New method for measuring 2D halo starlight kinematics and stellar populations to large Re Fast/slow rotators may change with radius. Outer gE halos may be very metal-poor, built by low mass progenitors? Mass modelling – see talk by Romanowsky. New method for obtaining halo masses (based on globular cluster system mass) – see poster by Spitler.

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