no code implementations • 12 Feb 2021 • Angelo Caravano, Eiichiro Komatsu, Kaloian D. Lozanov, Jochen Weller
In this paper we use a lattice simulation to reproduce the well-known results of some simple models of single-field inflation, particularly for the scalar field perturbation.
Cosmology and Nongalactic Astrophysics General Relativity and Quantum Cosmology High Energy Physics - Phenomenology
1 code implementation • 3 Jul 2020 • Yi-Kuan Chiang, Ryu Makiya, Eiichiro Komatsu, Brice Ménard
As cosmic structures form, matter density fluctuations collapse gravitationally and baryonic matter is shock-heated and thermalized.
Cosmology and Nongalactic Astrophysics
1 code implementation • 18 Jul 2019 • Ryu Makiya, Chiaki Hikage, Eiichiro Komatsu
This value of $B$ is lower than that needed to reconcile the tSZ data with the primordial CMB and CMB lensing data, i. e., $B = 1. 64 \pm 0. 19$, but is consistent with the mass bias expected from hydrodynamical simulations, $B = 1. 28 \pm 0. 20$.
Cosmology and Nongalactic Astrophysics
1 code implementation • 13 Apr 2018 • Ryu Makiya, Shin'ichiro Ando, Eiichiro Komatsu
We present a first joint analysis of the power spectra of the thermal Sunyaev-Zeldovich (tSZ) effect measured by the Planck and the number density fluctuations of galaxies in the 2MASS redshift survey (2MRS) catalog, including their cross-correlation.
Cosmology and Nongalactic Astrophysics
1 code implementation • 3 Dec 2017 • Boris Bolliet, Barbara Comis, Eiichiro Komatsu, Juan Francisco Macías-Pérez
Finally, by combining the tSZ power spectrum and the CMB data we find, in the $\Lambda$ Cold Dark Matter (CDM) model, the mass bias of $B=1. 71\pm 0. 17$, i. e., $1-b=0. 58\pm 0. 06$ (68% CL).
Cosmology and Nongalactic Astrophysics Astrophysics of Galaxies
no code implementations • 22 Sep 2014 • Christian Wagner, Fabian Schmidt, Chi-Ting Chiang, Eiichiro Komatsu
The large-scale statistics of observables such as the galaxy density are chiefly determined by their dependence on the local coarse-grained matter density.
Cosmology and Nongalactic Astrophysics
1 code implementation • 27 May 2002 • Eiichiro Komatsu, Uros Seljak
It receives a dominant contribution from cluster region between 20-40% of the virial radius and is thus insensitive to the poorly known gas physics in the cluster centre, such as cooling or (pre)heating.
astro-ph