Galaxy formation and evolution

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Molecular Gas and Star Formation in Local Early-Type Galaxies

(2011)

Authors:

M Bureau, TA Davis, K Alatalo, AF Crocker, L Blitz, LM Young, F Combes, M Bois, F Bournaud, M Cappellari, RL Davies, PT de Zeeuw, P-A Duc, E Emsellem, S Khochfar, D Krajnovic, H Kuntschner, P-Y Lablanche, RM McDermid, R Morganti, T Naab, T Oosterloo, M Sarzi, N Scott, P Serra, A Weijmans
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Investigating the merger origin of Early-Type Galaxies using ultra-deep optical images

(2011)

Authors:

P-A Duc, J-C Cuillandre, K Alatalo, L Blitz, M Bois, F Bournaud, M Bureau, M Cappellari, P Cote, RL Davies, TA Davis, PT de Zeeuw, E Emsellem, L Ferrarese, E Ferriere, S Gwyn, S Khochfar, D Krajnovic, H Kuntschner, P-Y Lablanche, L MacArthur, RM McDermid, L Michel-Dansac, R Morganti, T Naab, T Oosterloo, M Sarzi, N Scott, P Serra, A Weijmans, LM Young
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The SAURON project - XVIII. The integrated UV-linestrength relations of early-type galaxies

(2011)

Authors:

Martin Bureau, Hyunjin Jeong, Sukyoung K Yi, Kevin Schawinski, Ryan CW Houghton, Roger L Davies, Roland Bacon, Michele Cappellari, P Tim de Zeeuw, Eric Emsellem, Jesus Falcon-Barroso, Davor Krajnovic, Harald Kuntschner, Richard M McDermid, Reynier F Peletier, Marc Sarzi, Young-Jong Sohn, Daniel Thomas, Remco CE van den Bosch, Glenn van de Ven
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Most massive halos with Gumbel Statistics

(2011)

Authors:

Olaf Davis, Julien Devriendt, Stéphane Colombi, Joe Silk, Christophe Pichon
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Most massive halos with Gumbel Statistics

ArXiv 1101.2896 (2011)

Authors:

Olaf Davis, Julien Devriendt, Stéphane Colombi, Joe Silk, Christophe Pichon

Abstract:

We present an analytical calculation of the extreme value statistics for dark matter halos - that is, the probability distribution of the most massive halo within some region of the universe of specified shape and size. Our calculation makes use of the counts-in-cells formalism for the correlation functions, and the halo bias derived from the Sheth-Tormen mass function. We demonstrate the power of the method on spherical regions, comparing the results to measurements in a large cosmological dark matter simulation and achieving good agreement. Particularly good fits are obtained for the most likely value of the maximum mass and for the high-mass tail of the distribution, relevant in constraining cosmologies by observations of most massive clusters.
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