Previous Schedule: 1998 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017


October 1–31

Paris for “Analytics, Inference, and Computation in Cosmology

  • 10/15-17: Give 90min x 3 lectures on the CMB at Laboratoire de l'Accélérateur Linéaire, Université Paris-Sud, Orsay, France

August 27–31

COSMO-18, Daejeon, Korea

July 22–28

International school on the “Large-scale Structure of the Universe” at Harnackhaus, Berlin-Dahlem

June 11–July 6

MIAPP workshop on “The extragalactic distance scale in the Gaia era”, Excellence Cluster, München

May 25

MPIfR, Bonn

  • 5/25: Colloquium on "Mapping Hot Gas in the Universe using the Sunyaev-Zeldovich effect” [11:00]
    • Abstract: Hot, thermal electrons in galaxy clusters up-scatter the cosmic microwave background photons, making clusters visible in the microwave sky. This effect, known as the Sunyaev-Zeldovich effect, has been detected routinely toward individual galaxy clusters. Since the SZ effect is proportional to a projected thermal pressure of gas, we can use this effect to map all hot gas pressure in the Universe in projection. We start this talk by presenting the first image of the SZ effect obtained by ALMA, which has the highest spatial (both angular and physical) resolution ever achieved for the SZ mapping observations. With such a high resolution map comparable to X-ray maps, this SZ map enables us to study astrophysics of galaxy clusters in a new way. The second part of the talk concerns a full-sky map of the SZ effect. Thanks to its multi-frequency coverage from space, ESA's Planck satellite has produced, for the first time, a full-sky map of the SZ effect. Statistics of this map, such as one-point PDF and the power spectrum, provides a powerful test of our theory for structure formation in the Universe. Unlike gravitational lensing of the CMB, which probes structure formation of the total matter, the statistics of the SZ effect tests our understanding of baryonic structure formation on large scales. We present state-of-the-art simulation of the SZ effect, and discuss what we learned from comparing the simulation with the Planck data. In the last part of the talk, we present a new analytical model for non-thermal gas pressure on galaxy clusters, which plays a crucial role in physical understanding of what we see in simulations and observations of the SZ effect.

May 17

Université catholique de Louvain, Belgium

May 2

Manchester, UK

March 19–23

HETDEX Collaboration Meeting, MPE, Garching

March 12–16

CERN for “Probing Fundamental Physics with Spectral Distortions” 

February 22,23

CPTS Sektionssitzung, Berlin-Dahlem

  • 2/21: KIX(11:00)-FRA(15:00); FRA(16:45)-TXL(17:55)
  • 2/23: TXL(14:30)-MUC(15:40)

February 13–20

Kyoto, Japan

February 8–12

Sendai, Japan

  • 2/8-9: MUC(15:35)-HND(10:55); then to Sendai by trains
  • 2/10,11: Workshop on “Cosmic Acceleration” at Tohoku University
  • 2/12: SDJ()-ITM(); stay at Takarazuka

January 31, February 1

“CMB in Germany” meeting at MPA, Garching

January 22,23

Université Paris-sud

  • 1/22: MUC()-CDG()
  • 1/23: CDG()-MUC()

January 17–19

Workshop on “AtLAST” at ESO, Garching

January 2–11

Fukushima. Will not be opening a laptop, or reading emails!!

  • 1/2: ITM(13:30)-SDJ(14:40)
  • 1/11: HND(12:45)-MUC(16:55)


December 27–January 1

Takarazuka. Will not be opening a laptop, or reading emails!!

  • 12/27-28: MUC(15:35)-HND-ITM(14:05)
komatsu_at_mpa-garching_dot_mpg_dot_de © EIICHIRO KOMATSU 2012