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Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster
Authors
FA Aharonian
H Akamatsu
+98 more
F Akimoto
SW Allen
L Angelini
KA Arnaud
M Audard
H Awaki
M Axelsson
A Bamba
MW Bautz
RD Blandford
LW Brenneman
GV Brown
E Bulbul
EM Cackett
M Chernyakova
MP Chiao
P Coppi
E Costantini
C Done
T Dotani
K Ebisawa
ME Eckart
T Enoto
Y Ezoe
AC Fabian
C Ferrigno
AR Foster
R Fujimoto
Y Fukazawa
A Furuzawa
M Galeazzi
LC Gallo
P Gandhi
M Giustini
A Goldwurm
L Gu
M Guainazzi
Y Haba
K Hagino
K Hamaguchi
I Harrus
I Hatsukade
K Hayashi
T Hayashi
K Hayashida
JWD Herder
J Hiraga
AE Hornschemeier
A Hoshino
JP Hughes
Y Ichinohe
R Iizuka
H Inoue
S Inoue
Y Inoue
K Ishibashi
M Ishida
K Ishikawa
Y Ishisaki
M Itoh
M Iwai
N Iyomoto
JS Kaastra
T Kallman
T Kamae
E Kara
J Kataoka
S Katsuda
J Katsuta
M Kawaharada
N Kawai
RL Kelley
D Khangulyan
CA Kilbourne
AL King
T Kitaguchi
S Kitamoto
T Kitayama
T Kohmura
M Kokubun
K Koyama
S Koyama
P Kretschmar
HA Krimm
A Kubota
H Kunieda
P Laurent
F Lebrun
SH Lee
MA Leutenegger
O Limousin
M Loewenstein
KS Long
DH Lumb
GM Madejski
Y Maeda
D Maier
JD Plaa
Publication date
1 March 2017
Publisher
Astrophysical Journal Letters
Doi
Cite
Abstract
© 2017. The American Astronomical Society. All rights reserved. High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E ≈ 3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of S xvi (E ≃ 3.44 keV rest-frame) - a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment
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Last time updated on 04/06/2018