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

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 & 197 others 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, H. R. Russell, 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

Research output: Contribution to journalArticle

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Abstract

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.

LanguageEnglish
Article numberL15
JournalAstrophysical Journal Letters
Volume837
Issue number1
DOIs
StatePublished - 2017 Mar 1

Fingerprint

XMM-Newton telescope
galaxies
X-ray spectroscopy
energy
dark matter
K lines
prediction
nebulae
gas
charge exchange
newton
calorimeters
experiment
signatures
detection
high resolution
decay
predictions
gases
spectroscopy

Keywords

  • dark matter
  • galaxies: clusters: individual (A426)
  • galaxies: clusters: intracluster medium
  • X-rays: galaxies: clusters

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Aharonian, F. A., Akamatsu, H., Akimoto, F., Allen, S. W., Angelini, L., Arnaud, K. A., ... Zoghbi, A. (2017). Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster. Astrophysical Journal Letters, 837(1), [L15]. 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.; 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.

In: Astrophysical Journal Letters, Vol. 837, No. 1, L15, 01.03.2017.

Research output: Contribution to journalArticle

Aharonian, FA, Akamatsu, H, Akimoto, F, Allen, SW, Angelini, L, Arnaud, KA, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, MW, Blandford, RD, Bulbul, E, Brenneman, LW, Brown, GV, Cackett, EM, Chernyakova, M, Chiao, MP, Coppi, P, Costantini, E, Plaa, JD, Herder, JWD, Done, C, Dotani, T, Ebisawa, K, Eckart, ME, Enoto, T, Ezoe, Y, Fabian, AC, Ferrigno, C, Foster, AR, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, LC, 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, AE, Hoshino, A, Hughes, JP, 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, JS, Kallman, T, Kamae, T, Kara, E, Kataoka, J, Katsuda, S, Katsuta, J, Kawaharada, M, Kawai, N, Kelley, RL, Khangulyan, D, Kilbourne, CA, King, AL, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, S, Koyama, K, Kretschmar, P, Krimm, HA, Kubota, A, Kunieda, H, Laurent, P, Lebrun, F, Lee, SH, Leutenegger, MA, Limousin, O, Loewenstein, M, Long, KS, Lumb, DH, Madejski, GM, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, McCammon, D, McNamara, BR, Mehdipour, M, Miller, ED, Miller, JM, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Moseley, H, Mukai, K, Murakami, H, Murakami, T, Mushotzky, RF, Nakagawa, T, Nakajima, H, Nakamori, T, Nakano, T, Nakashima, S, Nakazawa, K, Nobukawa, K, Nobukawa, M, Noda, H, Nomachi, M, Dell, SLO, 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, FS, Pottschmidt, K, Ramsey, BD, Reynolds, CS, Russell, HR, Safi-Harb, S, Saito, S, Sakai, K, Sameshima, H, Sasaki, T, Sato, G, Sato, K, Sato, R, Sawada, M, Schartel, N, Serlemitsos, PJ, Seta, H, Shidatsu, M, Simionescu, A, Smith, RK, Soong, Y, Stawarz, Sugawara, Y, Sugita, S, Szymkowiak, AE, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, K, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Y, 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, CM, Ursino, E, Vries, CPD, Watanabe, S, Werner, N, Wik, DR, Wilkins, DR, Williams, BJ, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, NY, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Yoshida, A, Zhuravleva, I & Zoghbi, A 2017, 'Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster' Astrophysical Journal Letters, vol 837, no. 1, L15. DOI: 10.3847/2041-8213/aa61fa
Aharonian FA, Akamatsu H, Akimoto F, Allen SW, Angelini L, Arnaud KA et al. Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster. Astrophysical Journal Letters. 2017 Mar 1;837(1). L15. Available from, DOI: 10.3847/2041-8213/aa61fa
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 Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster. In: Astrophysical Journal Letters. 2017 ; Vol. 837, No. 1.
@article{a5cb87dd14524689b1cbad11d0e409e9,
title = "Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster",
abstract = "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.",
keywords = "dark matter, galaxies: clusters: individual (A426), galaxies: clusters: intracluster medium, X-rays: galaxies: clusters",
author = "Aharonian, {F. A.} and H. Akamatsu and F. Akimoto and Allen, {S. W.} and L. Angelini and Arnaud, {K. A.} and M. Audard and H. Awaki and M. Axelsson and A. Bamba and Bautz, {M. W.} and Blandford, {R. D.} and E. Bulbul and Brenneman, {L. W.} and Brown, {G. V.} and Cackett, {E. M.} and M. Chernyakova and Chiao, {M. P.} and P. Coppi and E. Costantini and Plaa, {J. De} and Herder, {J. W Den} and C. Done and T. Dotani and K. Ebisawa and Eckart, {M. E.} and T. Enoto and Y. Ezoe and Fabian, {A. C.} and C. Ferrigno and Foster, {A. R.} and R. Fujimoto and Y. Fukazawa and A. Furuzawa and M. Galeazzi and Gallo, {L. C.} and P. Gandhi and M. Giustini and A. Goldwurm and L. Gu and M. Guainazzi and Y. Haba and K. Hagino and K. Hamaguchi and I. Harrus and I. Hatsukade and K. Hayashi and T. Hayashi and K. Hayashida and J. Hiraga and Hornschemeier, {A. E.} and A. Hoshino and Hughes, {J. P.} and Y. Ichinohe and R. Iizuka and H. Inoue and S. Inoue and Y. Inoue and K. Ishibashi and M. Ishida and K. Ishikawa and Y. Ishisaki and M. Itoh and M. Iwai and N. Iyomoto and Kaastra, {J. S.} and T. Kallman and T. Kamae and E. Kara and J. Kataoka and S. Katsuda and J. Katsuta and M. Kawaharada and N. Kawai and Kelley, {R. L.} and D. Khangulyan and Kilbourne, {C. A.} and King, {A. L.} and T. Kitaguchi and S. Kitamoto and T. Kitayama and T. Kohmura and M. Kokubun and S. Koyama and K. Koyama and P. Kretschmar and Krimm, {H. A.} and A. Kubota and H. Kunieda and P. Laurent and F. Lebrun and Lee, {S. H.} and Leutenegger, {M. A.} and O. Limousin and M. Loewenstein and Long, {K. S.} and Lumb, {D. H.} and Madejski, {G. M.} and Y. Maeda and D. Maier and K. Makishima and M. Markevitch and H. Matsumoto and K. Matsushita and D. McCammon and McNamara, {B. R.} and M. Mehdipour and Miller, {E. D.} and Miller, {J. M.} and S. Mineshige and K. Mitsuda and I. Mitsuishi and T. Miyazawa and T. Mizuno and H. Mori and K. Mori and H. Moseley and K. Mukai and H. Murakami and T. Murakami and Mushotzky, {R. F.} and T. Nakagawa and H. Nakajima and T. Nakamori and T. Nakano and S. Nakashima and K. Nakazawa and K. Nobukawa and M. Nobukawa and H. Noda and M. Nomachi and Dell, {S. L O} and H. Odaka and T. Ohashi and M. Ohno and T. OKajima and N. Ota and M. Ozaki and F. Paerels and S. Paltani and A. Parmar and R. Petre and C. Pinto and M. Pohl and Porter, {F. S.} and K. Pottschmidt and Ramsey, {B. D.} and Reynolds, {C. S.} and Russell, {H. R.} and S. Safi-Harb and S. Saito and K. Sakai and H. Sameshima and T. Sasaki and G. Sato and K. Sato and R. Sato and M. Sawada and N. Schartel and Serlemitsos, {P. J.} and H. Seta and M. Shidatsu and A. Simionescu and Smith, {R. K.} and Y. Soong and Stawarz and Y. Sugawara and S. Sugita and Szymkowiak, {A. E.} and H. Tajima and H. Takahashi and T. Takahashi and S. Takeda and Y. Takei and T. Tamagawa and K. Tamura and T. Tamura and T. Tanaka and Yasuo Tanaka and Yasuyuki Tanaka and M. Tashiro and Y. Tawara and Y. Terada and Y. Terashima and F. Tombesi and H. Tomida and Y. Tsuboi and M. Tsujimoto and H. Tsunemi and T. Tsuru and H. Uchida and H. Uchiyama and Y. Uchiyama and S. Ueda and Y. Ueda and S. Ueno and S. Uno and Urry, {C. M.} and E. Ursino and Vries, {C. P De} and S. Watanabe and N. Werner and Wik, {D. R.} and Wilkins, {D. R.} and Williams, {B. J.} and S. Yamada and H. Yamaguchi and K. Yamaoka and Yamasaki, {N. Y.} and M. Yamauchi and S. Yamauchi and T. Yaqoob and Y. Yatsu and D. Yonetoku and A. Yoshida and I. Zhuravleva and A. Zoghbi",
year = "2017",
month = "3",
day = "1",
doi = "10.3847/2041-8213/aa61fa",
language = "English",
volume = "837",
journal = "Astrophysical Journal Letters",
issn = "2041-8205",
publisher = "IOP Publishing Ltd.",
number = "1",

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TY - JOUR

T1 - Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster

AU - Aharonian,F. A.

AU - Akamatsu,H.

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PY - 2017/3/1

Y1 - 2017/3/1

N2 - 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.

AB - 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.

KW - dark matter

KW - galaxies: clusters: individual (A426)

KW - galaxies: clusters: intracluster medium

KW - X-rays: galaxies: clusters

UR - http://www.scopus.com/inward/record.url?scp=85014948978&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85014948978&partnerID=8YFLogxK

U2 - 10.3847/2041-8213/aa61fa

DO - 10.3847/2041-8213/aa61fa

M3 - Article

VL - 837

JO - Astrophysical Journal Letters

T2 - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

SN - 2041-8205

IS - 1

M1 - L15

ER -