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, Jun 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

    35 Citations (Scopus)

    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.

    Original languageEnglish
    Article numberL15
    JournalAstrophysical Journal Letters
    Volume837
    Issue number1
    DOIs
    Publication statusPublished - 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]. https://doi.org/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, Jun; 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. https://doi.org/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. https://doi.org/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, Jun ; 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{5b88e703ed0346428a7e722a9da4b498,
    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 Jun 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",

    }

    TY - JOUR

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

    AU - Aharonian, F. A.

    AU - Akamatsu, H.

    AU - Akimoto, F.

    AU - Allen, S. W.

    AU - Angelini, L.

    AU - Arnaud, K. A.

    AU - Audard, M.

    AU - Awaki, H.

    AU - Axelsson, M.

    AU - Bamba, A.

    AU - Bautz, M. W.

    AU - Blandford, R. D.

    AU - Bulbul, E.

    AU - Brenneman, L. W.

    AU - Brown, G. V.

    AU - Cackett, E. M.

    AU - Chernyakova, M.

    AU - Chiao, M. P.

    AU - Coppi, P.

    AU - Costantini, E.

    AU - Plaa, J. De

    AU - Herder, J. W.Den

    AU - Done, C.

    AU - Dotani, T.

    AU - Ebisawa, K.

    AU - Eckart, M. E.

    AU - Enoto, T.

    AU - Ezoe, Y.

    AU - Fabian, A. C.

    AU - Ferrigno, C.

    AU - Foster, A. R.

    AU - Fujimoto, R.

    AU - Fukazawa, Y.

    AU - Furuzawa, A.

    AU - Galeazzi, M.

    AU - Gallo, L. C.

    AU - Gandhi, P.

    AU - Giustini, M.

    AU - Goldwurm, A.

    AU - Gu, L.

    AU - Guainazzi, M.

    AU - Haba, Y.

    AU - Hagino, K.

    AU - Hamaguchi, K.

    AU - Harrus, I.

    AU - Hatsukade, I.

    AU - Hayashi, K.

    AU - Hayashi, T.

    AU - Hayashida, K.

    AU - Hiraga, J.

    AU - Hornschemeier, A. E.

    AU - Hoshino, A.

    AU - Hughes, J. P.

    AU - Ichinohe, Y.

    AU - Iizuka, R.

    AU - Inoue, H.

    AU - Inoue, S.

    AU - Inoue, Y.

    AU - Ishibashi, K.

    AU - Ishida, M.

    AU - Ishikawa, K.

    AU - Ishisaki, Y.

    AU - Itoh, M.

    AU - Iwai, M.

    AU - Iyomoto, N.

    AU - Kaastra, J. S.

    AU - Kallman, T.

    AU - Kamae, T.

    AU - Kara, E.

    AU - Kataoka, Jun

    AU - Katsuda, S.

    AU - Katsuta, J.

    AU - Kawaharada, M.

    AU - Kawai, N.

    AU - Kelley, R. L.

    AU - Khangulyan, D.

    AU - Kilbourne, C. A.

    AU - King, A. L.

    AU - Kitaguchi, T.

    AU - Kitamoto, S.

    AU - Kitayama, T.

    AU - Kohmura, T.

    AU - Kokubun, M.

    AU - Koyama, S.

    AU - Koyama, K.

    AU - Kretschmar, P.

    AU - Krimm, H. A.

    AU - Kubota, A.

    AU - Kunieda, H.

    AU - Laurent, P.

    AU - Lebrun, F.

    AU - Lee, S. H.

    AU - Leutenegger, M. A.

    AU - Limousin, O.

    AU - Loewenstein, M.

    AU - Long, K. S.

    AU - Lumb, D. H.

    AU - Madejski, G. M.

    AU - Maeda, Y.

    AU - Maier, D.

    AU - Makishima, K.

    AU - Markevitch, M.

    AU - Matsumoto, H.

    AU - Matsushita, K.

    AU - McCammon, D.

    AU - McNamara, B. R.

    AU - Mehdipour, M.

    AU - Miller, E. D.

    AU - Miller, J. M.

    AU - Mineshige, S.

    AU - Mitsuda, K.

    AU - Mitsuishi, I.

    AU - Miyazawa, T.

    AU - Mizuno, T.

    AU - Mori, H.

    AU - Mori, K.

    AU - Moseley, H.

    AU - Mukai, K.

    AU - Murakami, H.

    AU - Murakami, T.

    AU - Mushotzky, R. F.

    AU - Nakagawa, T.

    AU - Nakajima, H.

    AU - Nakamori, T.

    AU - Nakano, T.

    AU - Nakashima, S.

    AU - Nakazawa, K.

    AU - Nobukawa, K.

    AU - Nobukawa, M.

    AU - Noda, H.

    AU - Nomachi, M.

    AU - Dell, S. L.O.

    AU - Odaka, H.

    AU - Ohashi, T.

    AU - Ohno, M.

    AU - OKajima, T.

    AU - Ota, N.

    AU - Ozaki, M.

    AU - Paerels, F.

    AU - Paltani, S.

    AU - Parmar, A.

    AU - Petre, R.

    AU - Pinto, C.

    AU - Pohl, M.

    AU - Porter, F. S.

    AU - Pottschmidt, K.

    AU - Ramsey, B. D.

    AU - Reynolds, C. S.

    AU - Russell, H. R.

    AU - Safi-Harb, S.

    AU - Saito, S.

    AU - Sakai, K.

    AU - Sameshima, H.

    AU - Sasaki, T.

    AU - Sato, G.

    AU - Sato, K.

    AU - Sato, R.

    AU - Sawada, M.

    AU - Schartel, N.

    AU - Serlemitsos, P. J.

    AU - Seta, H.

    AU - Shidatsu, M.

    AU - Simionescu, A.

    AU - Smith, R. K.

    AU - Soong, Y.

    AU - Stawarz,

    AU - Sugawara, Y.

    AU - Sugita, S.

    AU - Szymkowiak, A. E.

    AU - Tajima, H.

    AU - Takahashi, H.

    AU - Takahashi, T.

    AU - Takeda, S.

    AU - Takei, Y.

    AU - Tamagawa, T.

    AU - Tamura, K.

    AU - Tamura, T.

    AU - Tanaka, T.

    AU - Tanaka, Yasuo

    AU - Tanaka, Yasuyuki

    AU - Tashiro, M.

    AU - Tawara, Y.

    AU - Terada, Y.

    AU - Terashima, Y.

    AU - Tombesi, F.

    AU - Tomida, H.

    AU - Tsuboi, Y.

    AU - Tsujimoto, M.

    AU - Tsunemi, H.

    AU - Tsuru, T.

    AU - Uchida, H.

    AU - Uchiyama, H.

    AU - Uchiyama, Y.

    AU - Ueda, S.

    AU - Ueda, Y.

    AU - Ueno, S.

    AU - Uno, S.

    AU - Urry, C. M.

    AU - Ursino, E.

    AU - Vries, C. P.De

    AU - Watanabe, S.

    AU - Werner, N.

    AU - Wik, D. R.

    AU - Wilkins, D. R.

    AU - Williams, B. J.

    AU - Yamada, S.

    AU - Yamaguchi, H.

    AU - Yamaoka, K.

    AU - Yamasaki, N. Y.

    AU - Yamauchi, M.

    AU - Yamauchi, S.

    AU - Yaqoob, T.

    AU - Yatsu, Y.

    AU - Yonetoku, D.

    AU - Yoshida, A.

    AU - Zhuravleva, I.

    AU - Zoghbi, A.

    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

    JF - Astrophysical Journal Letters

    SN - 2041-8205

    IS - 1

    M1 - L15

    ER -