For the list of typos in Komatsu et al. (2009) [WMAP 5-year paper], please click here. [Last updated: March 8, 2012]
For the list of typos in Komatsu et al. (2011) [WMAP 7-year paper], please click here. [Last updated: May 2, 2012]Click here to download a note on the WMAP 5-year distance prior including BAO. [Last updated: October 12, 2009]
First Pitch! Prize! More Recent Prize! My Academic Tree
こんな活動も大好きです こんなのも 最近はこんな感じです より最近はこんな感じ
Max-Planck-Institut fuer Astrophysik
85741 Garching, Germany
[Research Activities (12/31)]
[News Papers/Magazines/Books (8/19)] [Yoshinoya] [Same Class] [Tips (12/21)] [Links]
[Cosmology Routine Library (CRL) in Fortran (4/25)]
PhD party for Masa Shoji at my place, November 21, 2011
"My PhD students, as of November 2011. Back: Hyunbae Park (2nd year), Chi-Ting Chiang (3rd year), Jonathan Ganc (5th year), and Inh Jee (1st year). Front: Myself and Masatoshi Shoji (with the graduation T-shirt on). Photo courtesy of Hyo Jeong Kim."
[Past group photos: 2008, 2009 and 2010]
Abstract: Can we use the Fermi satellite like WMAP? In 2006, S. Ando and I proposed to use anisotropies in the gamma-ray background (not CMB!) as a smoking-gun signature of annihilation of dark matter particles in the universe. The idea is simple: since dark matter traces the large-scale structure of the universe, the emission from dark matter must be anisotropic, and its spatial pattern is predictable. The use of anisotropy (especially the power spectrum) was new to the gamma-ray community, so I teamed up with the Fermi-LAT team to look for this signature. Here, we report on the first detection of anisotropy in the diffuse gamma-ray background measured by Fermi-LAT. We find that the detected signal is very likely due to unresolved blazers. Subtracting this signal, we can place a fairly stringent upper limit on the residual anisotropy signal, which would then put constraints on dark matter properties.
Abstract: Hobby-Eberly Dark Energy Experiment (HETDEX) will yield about 800,000 blindly-detected spectra of distant (z=1.9-3.5) galaxies, providing an unprecedented opportunity to measure the large-scale structure of the universe in a high-redshift universe. This unique dataset is expected to improve our understanding of the physics of inflation, the nature of dark matter and dark energy, and the properties of neutrinos. In this talk, I will describe the experiment and discuss cosmological constraints expected from the HETDEX 3-year survey.
Abstract: How did inflation actually happen? Precision measurements of statistical properties of primordial fluctuations generated during inflation offer a direct probe of the physics of inflation. When we calculate statistical properties of primordial fluctuations generated during inflation, we usually assume that the initial state of quantum fluctuations is in a preferred vacuum state called Bunch-Davies vacuum. While there is some motivation for choosing such a state, this is an assumption, and thus needs to be tested by observations. In this talk I will present new probes of initial state of quantum fluctuations during inflation: the 3-point function of the cosmic microwave background anisotropy, the 2-point function of galaxies, and a spectral distortion of the thermal spectrum of the cosmic microwave background.
Abstract: 宇宙はどのように始まり、どのように進化してきたのだろう？宇宙は何からできているのだろう？宇宙に終わりがあるとすれば、どのように終わるのだろう？現代科学の急速な発展により、このような、私たちの起源に関わる基本的な問いに対し、科学的な答えが得られようとしています。この講義では、最新の観測データと 天文学・物理学を駆使して我々が到達した最新の科学的宇宙モデルを解説し、現代宇宙論が明らかにした驚くべき宇宙の姿を紹介します。
Abstract: We reconsider the pixel-based, "template" polarized foreground removal method within the context of a next-generation, low-noise, low-resolution (0.5 degree FWHM) space-borne experiment measuring the cosmological B-mode polarization signal in the cosmic microwave background (CMB). This method was put forward by the Wilkinson Microwave Anisotropy Probe (WMAP) team and further studied by Efstathiou et al. We need at least 3 frequency channels: one is used for extracting the CMB signal, whereas the other two are used to estimate the spatial distribution of the polarized dust and synchrotron emission. No external template maps are used. We extract the tensor-to-scalar ratio (r) from simulated sky maps consisting of CMB, noise (2 micro K arcmin), and a foreground model, and find that, even for the simplest 3-frequency configuration with 60, 100, and 240 GHz, the residual bias in r is as small as Delta r~0.002. This bias is dominated by the residual synchrotron emission due to spatial variations of the synchrotron spectral index. With an extended mask with fsky=0.5, the bias is reduced further down to <0.001.
What's New!! 2011
Since August 3, 2012
e-mail: komatsu [at] mpa-garching [dot] mpg [dot] de
phone: +49-89-30000-2208 [089-30000-2208]
office: 231 (in the MPA building)