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

Aharonian, F. A.; Akamatsu, H.; Akimoto, F.; Allen, S. W.; Angelini, L.; Arnaud, K. A.; Audard, M.; Awaki, H.; Axelsson, M.; Bamba, A.; Bautz, M. W.; Blandford, R. D.; Bulbul, E.; Brenneman, L. W.; Brown, G. V.; Cackett, E. M.; Chernyakova, M.; Chiao, M. P.; Coppi, P.; Costantini, E.; Plaa, J. de; Herder, J.-W. den; Done, C.; Dotani, T.; Ebisawa, K.; Eckart, M. E.; Enoto, T.; Ezoe, Y.; Fabian, A. C.; Ferrigno, C.; Foster, A. R.; Fujimoto, R.; Fukazawa, Y.; Furuzawa, A.; Galeazzi, M.; Gallo, L. C.; Gandhi, P.; Giustini, M.; Goldwurm, A.; Gu, L.; Guainazzi, M.; Haba, Y.; Hagino, K.; Hamaguchi, K.; Harrus, I.; Hatsukade, I.; Hayashi, K.; Hayashi, T.; Hayashida, K.; Hiraga, J.; Hornschemeier, A. E.; Hoshino, A.; Hughes, J. P.; Ichinohe, Y.; Iizuka, R.; Inoue, H.; Inoue, S.; Inoue, Y.; Ishibashi, K.; Ishida, M.; Ishikawa, K.; Ishisaki, Y.; Itoh, M.; Iwai, M.; Iyomoto, N.; Kaastra, J. S.; Kallman, T.; Kamae, T.; Kara, E.; Kataoka, J.; Katsuda, S.; Katsuta, J.; Kawaharada, M.; Kawai, N.; Kelley, R. L.; Khangulyan, D.; Kilbourne, C. A.; King, A. L.; Kitaguchi, T.; Kitamoto, S.; Kitayama, T.; Kohmura, T.; Kokubun, M.; Koyama, S.; Koyama, K.; Kretschmar, P.; Krimm, H. A.; Kubota, A.; Kunieda, H.; Laurent, P.; Lebrun, F.; Lee, S.-H.; Leutenegger, M. A.; Limousin, O.; Loewenstein, M.; Long, K. S.; Lumb, D. H.; Madejski, G. M.; Maeda, Y.; Maier, D.; Makishima, K.; Markevitch, M.; Matsumoto, H.; Matsushita, K.; McCammon, D.; McNamara, B. R.; Mehdipour, M.; Miller, E. D.; Miller, J. M.; Mineshige, S.; Mitsuda, K.; Mitsuishi, I.; Miyazawa, T.; Mizuno, T.; Mori, H.; Mori, K.; Moseley, H.; Mukai, K.; Murakami, H.; Murakami, T.; Mushotzky, R. F.; Nakagawa, T.; Nakajima, H.; Nakamori, T.; Nakano, T.; Nakashima, S.; Nakazawa, K.; Nobukawa, K.; Nobukawa, M.; Noda, H.; Nomachi, M.; Dell, S. L. O�; Odaka, H.; Ohashi, T.; Ohno, M.; Okajima, T.; Ota, N.; Ozaki, M.; Paerels, F.; Paltani, S.; Parmar, A.; Petre, R.; Pinto, C.; Pohl, M.; Porter, F. S.; Pottschmidt, K.; Ramsey, B. D.; Reynolds, C. S.; Russell, H. R.; Safi-Harb, S.; Saito, S.; Sakai, K.; Sameshima, H.; Sasaki, T.; Sato, G.; Sato, K.; Sato, R.; Sawada, M.; Schartel, N.; Serlemitsos, P. J.; Seta, H.; Shidatsu, M.; Simionescu, A.; Smith, R. K.; Soong, Y.; Stawarz, ?.; Sugawara, Y.; Sugita, S.; Szymkowiak, A. E.; Tajima, H.; Takahashi, H.; Takahashi, T.; Takeda, S.; Takei, Y.; Tamagawa, T.; Tamura, K.; Tamura, T.; Tanaka, T.; Tanaka, Yasuo; Tanaka, Yasuyuki; Tashiro, M.; Tawara, Y.; Terada, Y.; Terashima, Y.; Tombesi, F.; Tomida, H.; Tsuboi, Y.; Tsujimoto, M.; Tsunemi, H.; Tsuru, T.; Uchida, H.; Uchiyama, H.; Uchiyama, Y.; Ueda, S.; Ueda, Y.; Ueno, S.; Uno, S.; Urry, C. M.; Ursino, E.; Vries, C. P. de; Watanabe, S.; Werner, N.; Wik, D. R.; Wilkins, D. R.; Williams, B. J.; Yamada, S.; Yamaguchi, H.; Yamaoka, K.; Yamasaki, N. Y.; Yamauchi, M.; Yamauchi, S.; Yaqoob, T.; Yatsu, Y.; Yonetoku, D.; Yoshida, A.; Zhuravleva, I.; Zoghbi, A.; Hitomi Collaboration

doi:10.3847/2041-8213/aa61fa

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

Aharonian, F. A.; Akamatsu, H.; Akimoto, F.; Allen, S. W.; Angelini, L.; Arnaud, K. A.; Audard, M.; Awaki, H.; Axelsson, M.; Bamba, A.; Bautz, M. W.; Blandford, R. D.; Bulbul, E.; Brenneman, L. W.; Brown, G. V.; Cackett, E. M.; Chernyakova, M.; Chiao, M. P.; Coppi, P.; Costantini, E.; Plaa, J. de; Herder, J.-W. den; Done, C.; Dotani, T.; Ebisawa, K.; Eckart, M. E.; Enoto, T.; Ezoe, Y.; Fabian, A. C.; Ferrigno, C.; Foster, A. R.; Fujimoto, R.; Fukazawa, Y.; Furuzawa, A.; Galeazzi, M.; Gallo, L. C.; Gandhi, P.; Giustini, M.; Goldwurm, A.; Gu, L.; Guainazzi, M.; Haba, Y.; Hagino, K.; Hamaguchi, K.; Harrus, I.; Hatsukade, I.; Hayashi, K.; Hayashi, T.; Hayashida, K.; Hiraga, J.; Hornschemeier, A. E.; Hoshino, A.; Hughes, J. P.; Ichinohe, Y.; Iizuka, R.; Inoue, H.; Inoue, S.; Inoue, Y.; Ishibashi, K.; Ishida, M.; Ishikawa, K.; Ishisaki, Y.; Itoh, M.; Iwai, M.; Iyomoto, N.; Kaastra, J. S.; Kallman, T.; Kamae, T.; Kara, E.; Kataoka, J.; Katsuda, S.; Katsuta, J.; Kawaharada, M.; Kawai, N.; Kell...

Authors

F. A. Aharonian

H. Akamatsu

F. Akimoto

S. W. Allen

L. Angelini

K. A. Arnaud

M. Audard

H. Awaki

M. Axelsson

A. Bamba

M. W. Bautz

R. D. Blandford

E. Bulbul

L. W. Brenneman

G. V. Brown

E. M. Cackett

M. Chernyakova

M. P. Chiao

P. Coppi

E. Costantini

J. de Plaa

J.-W. den Herder

C. Done

T. Dotani

K. Ebisawa

M. E. Eckart

T. Enoto

Y. Ezoe

A. C. Fabian

C. Ferrigno

A. R. Foster

R. Fujimoto

Y. Fukazawa

A. Furuzawa

M. Galeazzi

L. C. 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

J. Hiraga

A. E. Hornschemeier

A. Hoshino

J. P. 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

J. S. Kaastra

T. Kallman

T. Kamae

E. Kara

J. Kataoka

S. Katsuda

J. Katsuta

M. Kawaharada

N. Kawai

R. L. Kelley

D. Khangulyan

C. A. Kilbourne

A. L. King

T. Kitaguchi

S. Kitamoto

T. Kitayama

T. Kohmura

M. Kokubun

S. Koyama

K. Koyama

P. Kretschmar

H. A. Krimm

A. Kubota

H. Kunieda

P. Laurent

F. Lebrun

S.-H. Lee

M. A. Leutenegger

O. Limousin

M. Loewenstein

K. S. Long

D. H. Lumb

G. M. Madejski

Y. Maeda

D. Maier

K. Makishima

M. Markevitch

H. Matsumoto

K. Matsushita

D. McCammon

B. R. McNamara

M. Mehdipour

E. D. Miller

J. M. Miller

S. Mineshige

K. Mitsuda

I. Mitsuishi

T. Miyazawa

T. Mizuno

H. Mori

K. Mori

H. Moseley

K. Mukai

H. Murakami

T. Murakami

R. F. Mushotzky

T. Nakagawa

H. Nakajima

T. Nakamori

T. Nakano

S. Nakashima

K. Nakazawa

K. Nobukawa

M. Nobukawa

H. Noda

M. Nomachi

S. L. O� Dell

H. Odaka

T. Ohashi

M. Ohno

T. Okajima

N. Ota

M. Ozaki

F. Paerels

S. Paltani

A. Parmar

R. Petre

C. Pinto

M. Pohl

F. S. Porter

K. Pottschmidt

B. D. Ramsey

C. S. Reynolds

Dr HELEN RUSSELL HELEN.RUSSELL@NOTTINGHAM.AC.UK
ANNE MCLAREN FELLOW

S. Safi-Harb

S. Saito

K. Sakai

H. Sameshima

T. Sasaki

G. Sato

K. Sato

R. Sato

M. Sawada

N. Schartel

P. J. Serlemitsos

H. Seta

M. Shidatsu

A. Simionescu

R. K. Smith

Y. Soong

?. Stawarz

Y. Sugawara

S. Sugita

A. E. Szymkowiak

H. Tajima

H. Takahashi

T. Takahashi

S. Takeda

Y. Takei

T. Tamagawa

K. Tamura

T. Tamura

T. Tanaka

Yasuo Tanaka

Yasuyuki Tanaka

M. Tashiro

Y. Tawara

Y. Terada

Y. Terashima

F. Tombesi

H. Tomida

Y. Tsuboi

M. Tsujimoto

H. Tsunemi

T. Tsuru

H. Uchida

H. Uchiyama

Y. Uchiyama

S. Ueda

Y. Ueda

S. Ueno

S. Uno

C. M. Urry

E. Ursino

C. P. de Vries

S. Watanabe

N. Werner

D. R. Wik

D. R. Wilkins

B. J. Williams

S. Yamada

H. Yamaguchi

K. Yamaoka

N. Y. Yamasaki

M. Yamauchi

S. Yamauchi

T. Yaqoob

Y. Yatsu

D. Yonetoku

A. Yoshida

I. Zhuravleva

A. Zoghbi

Hitomi Collaboration

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.

Citation

Aharonian, F. A., Akamatsu, H., Akimoto, F., Allen, S. W., Angelini, L., Arnaud, K. A., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M. W., Blandford, R. D., Bulbul, E., Brenneman, L. W., Brown, G. V., Cackett, E. M., Chernyakova, M., Chiao, M. P., Coppi, P., Costantini, E., …Hitomi Collaboration. (2017). Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster. Astrophysical Journal Letters, 837(1), L15. https://doi.org/10.3847/2041-8213/aa61fa

Journal Article Type	Article
Acceptance Date	Feb 19, 2017
Online Publication Date	Mar 3, 2017
Publication Date	Mar 1, 2017
Deposit Date	Sep 11, 2019
Publicly Available Date	Sep 24, 2019
Journal	Astrophysical Journal Letters
Print ISSN	2041-8205
Electronic ISSN	2041-8213
Publisher	American Astronomical Society
Peer Reviewed	Peer Reviewed
Volume	837
Issue	1
Article Number	L15
Pages	L15
DOI	https://doi.org/10.3847/2041-8213/aa61fa
Public URL	https://nottingham-repository.worktribe.com/output/2511789
Publisher URL	https://iopscience.iop.org/article/10.3847/2041-8213/aa61fa
Additional Information	Journal title: The Astrophysical Journal; Article type: paper; Article title: HitomiConstraints on the 3.5 keV Line in the Perseus Galaxy Cluster; Copyright information: © 2017. The American Astronomical Society. All rights reserved.; Date received: 2016-07-25; Date accepted: 2017-02-19; Online publication date: 2017-03-03
Contract Date	Sep 24, 2019