天文月報 2019-05 : 「ひとみ」によるダークマターX線の探査

http://www.asj.or.jp/geppou/contents/2019_05.html

http://www.asj.or.jp/geppou/archive_open/2019_112_05/112-5_285.pdf

An X-ray spectroscopic search for dark matter and unidentified line signatures in the Perseus cluster with Hitomi

https://academic.oup.com/pasj/advance-article/doi/10.1093/pasj/psz023/5420423?searchresult=1

Published:

 27 March 2019

https://arxiv.org/abs/1811.05767

https://ui.adsabs.harvard.edu/abs/2019PASJ..tmp...42T/abstract

An X-ray spectroscopic search for dark matter in the Perseus cluster with Suzaku

http://adsabs.harvard.edu/abs/2015PASJ...67...23T

https://academic.oup.com/pasj/article/67/2/23/2916026

Hitomi Limits on the 3.5 keV signal.

http://iopscience.iop.org/article/10.3847/2041-8213/aa61fa
http://adsabs.harvard.edu/abs/2017ApJ...837L..15A

Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster

ADS: papers cited the Hitomi 3.5 keV paper
https://goo.gl/NHDreE

Hitomi constraints on the 3.5 keV line in the Perseus galaxy cluster

http://arxiv.org/abs/1607.07420

XMM-Newton observations of the cluster of galaxies Abell 496

http://adsabs.harvard.edu/abs/2001A%26A...379..107T

The results from XMM-Newton observations of the relaxed cluster of galaxies Abell 496 are presented. The spatially-resolved X-ray spectra taken by the European Photon Imaging Cameras show a temperature drop and a Fe abundance increase in the intra-cluster medium (ICM) towards the cD galaxy at the cluster center. The abundances of Si and S also show a central enhancement. High resolution soft X-ray spectra obtained with the Reflection Grating Spectrometers provides a strong constraint on the temperature structure in the central cool plasma. Furthermore, the O abundance at the cluster core is accurately measured based on the O Viii Lyalpha line detected with the RGS. Contrary to the Si, S, and Fe abundances, the O abundance is radially constant over the cluster.

Tamura's paper list

- ADS list of papers including T.Tamura
https://goo.gl/8KFXP7

(2018-04-11)
Selected and retrieved 79 abstracts. Total citations: 5974


- http://scholar.google.com/citations?user=McTq83wAAAAJ&hl=en

Tamura's words

2015-04-17 taken from ADS lab.

http://goo.gl/XPmQ3d

Gas bulk motion in the Perseus cluster measured with SUZAKU

Tamura et al. 2013/2014

http://adsabs.harvard.edu/abs/2013arXiv1312.4526T

Suzaku Observations of the Cluster of Galaxies Abell 2052

Tamura et al. 2008

http://adsabs.harvard.edu/abs/2008PASJ...60..695T

Other pages on Me

http://www.isas.jaxa.jp/j/about/professor/t/tamura_takayuki.shtml

http://scholar.google.com/citations?user=McTq83wAAAAJ&hl=en

(Japanese)
http://researchmap.jp/takayuki.tamura/

http://kaken.nii.ac.jp/d/r/00370099.ja.html

http://jglobal.jst.go.jp/detail.php?JGLOBAL_ID=200901028844431929&q=田村隆幸&t=0

X-ray Spectroscopy of the Core of the Perseus Cluster with Suzaku: Elemental Abundances in the Intracluster Medium

http://www.isas.jaxa.jp/home/ttamura/PerseusCluster/

http://www.isas.jaxa.jp/home/ttamura/PerseusCluster/press2009/
(日本語での解説)

Tamura et al. 2009, ApJ Letter
http://adsabs.harvard.edu/abs/2009ApJ...705L..62T
http://iopscience.iop.org/1538-4357/705/1/L62/fulltext/apjl_705_1_62.html

X-Ray Measurements of the Gravitational Potential Profile in the Central Region of the Abell 1060 Cluster of Galaxies

2000, ApJ

https://iopscience.iop.org/article/10.1086/308882
https://ui.adsabs.harvard.edu/abs/2000ApJ...535..602T/abstract

This is based on my Ph.D thesis.

Abstract:

X-ray spectral and imaging data from ASCA and ROSAT were used to measure the total mass profile in the central region of Abell 1060, a nearby and relatively poor cluster of galaxies. The ASCA X-ray spectra, after being corrected for the spatial response of the X-ray telescope, show an isothermal distribution of the intracluster medium (ICM) within at least ~12' (or 160 h-170 kpc; H0=70 h70 km s-1 Mpc-1) in radius of the cluster center. The azimuthally averaged surface brightness profile from the ROSAT Position Sensitive Proportional Counter (PSPC) exhibits a central excess above an isothermal β model. The ring-sorted ASCA Gas Imaging Spectrometer spectra and the radial surface brightness distribution from the ROSAT PSPC were simultaneously utilized to constrain the gravitational potential profile. Some analytic models of the total mass density profile were examined. The ICM density profile was also specified by analytic forms. The ICM temperature distribution was constrained to satisfy the hydrostatic equilibrium and to be consistent with the data. Then, the total mass distribution was found to be described better by the universal dark halo profile recently proposed by Navarro, Frenk, & White than by a King-type model with a flat density core. A profile with a central cusp together with a logarithmic radial slope of ~1.5 was also consistent with the data. Discussions are presented concerning the estimated dark matter distribution around the cluster center.

Elemental abundances in the intracluster medium as observed with XMM-Newton

http://adsabs.harvard.edu/abs/2004A%26A...420..135T

XMM-Newton observations of 19 galaxy clusters are used to measure the elemental abundances and their spatial distributions in the intracluster medium. The sample mainly consists of X-ray bright and relaxed clusters with a cD galaxy. Along with detailed Si, S and Fe radial abundance distributions within 300-700 kpc in radius, the O abundances are accurately derived in the central region of the clusters. The Fe abundance maxima towards the cluster center, possibly due to the metals from the cD galaxy, are spatially resolved. The Si and S abundances also exhibit central increases in general, resulting in uniform Fe-Si-S ratios within the cluster. In contrast, the O abundances are in general uniform over the cluster. The mean O to Fe ratio within the cluster core is sub-solar, while that of the cluster scale is larger than the solar ratio. These measurements indicate that most of the Fe-Si-S and O in the intracluster medium have different origins, presumably in supernovae Ia and II, respectively. The obtained Fe and O mass are also used to discuss the past star formation history in clusters.

citations:
http://goo.gl/VbPdEq

X-ray spectroscopy of the cluster of galaxies Abell 1795 with XMM-Newton

Accepted on A&A in 2001.

Abstract
The initial results from XMM-Newton observations of the rich cluster of galaxies Abell 1795 are presented. The spatially-resolved X-ray spectra taken by the European Photon Imaging Cameras (EPIC) show a temperature drop at a radius of 200 kpc from the cluster center, indicating that the ICM is cooling. Both the EPIC and the Reflection Grating Spectrometers (RGS) spectra extracted from the cluster center can be described by an isothermal model with a temperature of 4 keV. The volume emission measure of any cool component (VIII Lyman line was detected with the RGS from the cluster core. The O abundance and its ratio to Fe at the cluster center is 0.2-0.5 and 0.5-1.5 times the solar value, respectively.

http://adsabs.harvard.edu/abs/2001A%26A...365L..87T

citation papers
http://goo.gl/4iwcJC