GRB Hosts

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Large L/M dyn of a Cluster (F) in M82 M82 Salpeter (Kroupa) IMF L/M dyn ~ 7‐12 L sun /M sun (for 60Myr age) Observed 42±10 L sun /M sun Bastian et al. 2007
Change of M dyn /L along the time: Cluster Ellipticals l Fundamental lPlane at z=0.1‐0.8 0108 Fundamental Plane Evolution Changes in M/L Is more consistent it t with flat (x=0.3) IMF Van Dokkum 2008 Δ(U V) ~ A Δ(U‐V) ~ Age, Not depending as much on IMF slope as on age
Page 2 and 3: Probing High‐z Universe with GRB
Page 4 and 5: GRB Hosts: SFR/Stellar Mass GRB hos
Page 6 and 7: GRB Hosts: Morphology Morphology of
Page 8 and 9: GRB Hosts (long burst, w/OA) ● SF
Page 10 and 11: GRB as a tracer of high‐z star‐
Page 12 and 13: Some Evidence of Flat/Top‐Heavy I
Page 16 and 17: Cosmic SF History and IMF Inconsist
Page 18 and 19: Cosmic SF Rate Density and Stellar
Page 20 and 21: Large Equivalent Width of Lyα Emit
Page 22 and 23: Large Equivalent Width of Lyα Emit
Page 24 and 25: Very eyBlue UV Slop Sopof z=7 Galax
Page 26 and 27: Massive Star Formation at High Reds
Page 28 and 29: WISH Wide-field Imaging Surveyor fo
Page 30 and 31: Cosmic Microwave Background (CMB) U
Page 32 and 33: WISH Specifications Quick Summary P
Page 34 and 35: WISH 5 Years Survey Plan Surveys Ar

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