Abstract
Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling - a process known as active galactic nucleus feedback. Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 ± 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 ± 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure.
| Original language | English |
|---|---|
| Pages (from-to) | 117-121 |
| Number of pages | 5 |
| Journal | Nature |
| Volume | 535 |
| Issue number | 7610 |
| DOIs | |
| Publication status | Published - 2016 Jul 6 |
ASJC Scopus subject areas
- Medicine(all)
- General
Cite this
The quiescent intracluster medium in the core of the Perseus cluster. / Aharonian, Felix; Akamatsu, Hiroki; Akimoto, Fumie; Allen, Steven W.; Anabuki, Naohisa; Angelini, Lorella; Arnaud, Keith; Audard, Marc; Awaki, Hisamitsu; Axelsson, Magnus; Bamba, Aya; Bautz, Marshall; Blandford, Roger; Brenneman, Laura; Brown, Gregory V.; Bulbul, Esra; Cackett, Edward; Chernyakova, Maria; Chiao, Meng; Coppi, Paolo; Costantini, Elisa; De Plaa, Jelle; Den Herder, Jan Willem; Done, Chris; Dotani, Tadayasu; Ebisawa, Ken; Eckart, Megan; Enoto, Teruaki; Ezoe, Yuichiro; Fabian, Andrew C.; Ferrigno, Carlo; Foster, Adam; Fujimoto, Ryuichi; Fukazawa, Yasushi; Furuzawa, Akihiro; Galeazzi, Massimiliano; Gallo, Luigi; Gandhi, Poshak; Giustini, Margherita; Goldwurm, Andrea; Gu, Liyi; Guainazzi, Matteo; Haba, Yoshito; Hagino, Kouichi; Hamaguchi, Kenji; Harrus, Ilana; Hatsukade, Isamu; Hayashi, Katsuhiro; Hayashi, Takayuki; Hayashida, Kiyoshi; Hiraga, Junko; Hornschemeier, Ann; Hoshino, Akio; Hughes, John; Iizuka, Ryo; Inoue, Hajime; Inoue, Yoshiyuki; Ishibashi, Kazunori; Ishida, Manabu; Ishikawa, Kumi; Ishisaki, Yoshitaka; Itoh, Masayuki; Iyomoto, Naoko; Kaastra, Jelle; Kallman, Timothy; Kamae, Tuneyoshi; Kara, Erin; Kataoka, Jun; Katsuda, Satoru; Katsuta, Junichiro; Kawaharada, Madoka; Kawai, Nobuyuki; Kelley, Richard; Khangulyan, Dmitry; Kilbourne, Caroline; King, Ashley; Kitaguchi, Takao; Kitamoto, Shunji; Kitayama, Tetsu; Kohmura, Takayoshi; Kokubun, Motohide; Koyama, Shu; Koyama, Katsuji; Kretschmar, Peter; Krimm, Hans; Kubota, Aya; Kunieda, Hideyo; Laurent, Philippe; Lebrun, François; Lee, Shiu Hang; Leutenegger, Maurice; Limousin, Olivier; Loewenstein, Michael; Long, Knox S.; Lumb, David; Madejski, Grzegorz; Maeda, Yoshitomo; Maier, Daniel; Makishima, Kazuo; Markevitch, Maxim; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, Dan; McNamara, Brian; Mehdipour, Missagh; Miller, Eric; Miller, Jon; Mineshige, Shin; Mitsuda, Kazuhisa; Mitsuishi, Ikuyuki; Miyazawa, Takuya; Mizuno, Tsunefumi; Mori, Hideyuki; Mori, Koji; Moseley, Harvey; Mukai, Koji; Murakami, Hiroshi; Murakami, Toshio; Mushotzky, Richard; Nagino, Ryo; Nakagawa, Takao; Nakajima, Hiroshi; Nakamori, Takeshi; Nakano, Toshio; Nakashima, Shinya; Nakazawa, Kazuhiro; Nobukawa, Masayoshi; Noda, Hirofumi; Nomachi, Masaharu; ODell, Steve; Odaka, Hirokazu; Ohashi, Takaya; Ohno, Masanori; Okajima, Takashi; Ota, Naomi; Ozaki, Masanobu; Paerels, Frits; Paltani, Stephane; Parmar, Arvind; Petre, Robert; Pinto, Ciro; Pohl, Martin; Porter, F. Scott; Pottschmidt, Katja; Ramsey, Brian; Reynolds, Christopher; Russell, Helen; Safi-Harb, Samar; Saito, Shinya; Sakai, Kazuhiro; Sameshima, Hiroaki; Sato, Goro; Sato, Kosuke; Sato, Rie; Sawada, Makoto; Schartel, Norbert; Serlemitsos, Peter; Seta, Hiromi; Shidatsu, Megumi; Simionescu, Aurora; Smith, Randall; Soong, Yang; Stawarz, Lukasz; Sugawara, Yasuharu; Sugita, Satoshi; Szymkowiak, Andrew; Tajima, Hiroyasu; Takahashi, Hiromitsu; Takahashi, Tadayuki; Takeda, Shinichiro; Takei, Yoh; Tamagawa, Toru; Tamura, Keisuke; Tamura, Takayuki; Tanaka, Takaaki; Tanaka, Yasuo; Tanaka, Yasuyuki; Tashiro, Makoto; Tawara, Yuzuru; Terada, Yukikatsu; Terashima, Yuichi; Tombesi, Francesco; Tomida, Hiroshi; Tsuboi, Yohko; Tsujimoto, Masahiro; Tsunemi, Hiroshi; Tsuru, Takeshi; Uchida, Hiroyuki; Uchiyama, Hideki; Uchiyama, Yasunobu; Ueda, Shutaro; Ueda, Yoshihiro; Ueno, Shiro; Uno, Shinichiro; Urry, Meg; Ursino, Eugenio; De Vries, Cor; Watanabe, Shin; Werner, Norbert; Wik, Daniel; Wilkins, Dan; Williams, Brian; Yamada, Shinya; Yamaguchi, Hiroya; Yamaoka, Kazutaka; Yamasaki, Noriko Y.; Yamauchi, Makoto; Yamauchi, Shigeo; Yaqoob, Tahir; Yatsu, Yoichi; Yonetoku, Daisuke; Yoshida, Atsumasa; Yuasa, Takayuki; Zhuravleva, Irina; Zoghbi, Abderahmen.
In: Nature, Vol. 535, No. 7610, 06.07.2016, p. 117-121.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - The quiescent intracluster medium in the core of the Perseus cluster
AU - Aharonian, Felix
AU - Akamatsu, Hiroki
AU - Akimoto, Fumie
AU - Allen, Steven W.
AU - Anabuki, Naohisa
AU - Angelini, Lorella
AU - Arnaud, Keith
AU - Audard, Marc
AU - Awaki, Hisamitsu
AU - Axelsson, Magnus
AU - Bamba, Aya
AU - Bautz, Marshall
AU - Blandford, Roger
AU - Brenneman, Laura
AU - Brown, Gregory V.
AU - Bulbul, Esra
AU - Cackett, Edward
AU - Chernyakova, Maria
AU - Chiao, Meng
AU - Coppi, Paolo
AU - Costantini, Elisa
AU - De Plaa, Jelle
AU - Den Herder, Jan Willem
AU - Done, Chris
AU - Dotani, Tadayasu
AU - Ebisawa, Ken
AU - Eckart, Megan
AU - Enoto, Teruaki
AU - Ezoe, Yuichiro
AU - Fabian, Andrew C.
AU - Ferrigno, Carlo
AU - Foster, Adam
AU - Fujimoto, Ryuichi
AU - Fukazawa, Yasushi
AU - Furuzawa, Akihiro
AU - Galeazzi, Massimiliano
AU - Gallo, Luigi
AU - Gandhi, Poshak
AU - Giustini, Margherita
AU - Goldwurm, Andrea
AU - Gu, Liyi
AU - Guainazzi, Matteo
AU - Haba, Yoshito
AU - Hagino, Kouichi
AU - Hamaguchi, Kenji
AU - Harrus, Ilana
AU - Hatsukade, Isamu
AU - Hayashi, Katsuhiro
AU - Hayashi, Takayuki
AU - Hayashida, Kiyoshi
AU - Hiraga, Junko
AU - Hornschemeier, Ann
AU - Hoshino, Akio
AU - Hughes, John
AU - Iizuka, Ryo
AU - Inoue, Hajime
AU - Inoue, Yoshiyuki
AU - Ishibashi, Kazunori
AU - Ishida, Manabu
AU - Ishikawa, Kumi
AU - Ishisaki, Yoshitaka
AU - Itoh, Masayuki
AU - Iyomoto, Naoko
AU - Kaastra, Jelle
AU - Kallman, Timothy
AU - Kamae, Tuneyoshi
AU - Kara, Erin
AU - Kataoka, Jun
AU - Katsuda, Satoru
AU - Katsuta, Junichiro
AU - Kawaharada, Madoka
AU - Kawai, Nobuyuki
AU - Kelley, Richard
AU - Khangulyan, Dmitry
AU - Kilbourne, Caroline
AU - King, Ashley
AU - Kitaguchi, Takao
AU - Kitamoto, Shunji
AU - Kitayama, Tetsu
AU - Kohmura, Takayoshi
AU - Kokubun, Motohide
AU - Koyama, Shu
AU - Koyama, Katsuji
AU - Kretschmar, Peter
AU - Krimm, Hans
AU - Kubota, Aya
AU - Kunieda, Hideyo
AU - Laurent, Philippe
AU - Lebrun, François
AU - Lee, Shiu Hang
AU - Leutenegger, Maurice
AU - Limousin, Olivier
AU - Loewenstein, Michael
AU - Long, Knox S.
AU - Lumb, David
AU - Madejski, Grzegorz
AU - Maeda, Yoshitomo
AU - Maier, Daniel
AU - Makishima, Kazuo
AU - Markevitch, Maxim
AU - Matsumoto, Hironori
AU - Matsushita, Kyoko
AU - McCammon, Dan
AU - McNamara, Brian
AU - Mehdipour, Missagh
AU - Miller, Eric
AU - Miller, Jon
AU - Mineshige, Shin
AU - Mitsuda, Kazuhisa
AU - Mitsuishi, Ikuyuki
AU - Miyazawa, Takuya
AU - Mizuno, Tsunefumi
AU - Mori, Hideyuki
AU - Mori, Koji
AU - Moseley, Harvey
AU - Mukai, Koji
AU - Murakami, Hiroshi
AU - Murakami, Toshio
AU - Mushotzky, Richard
AU - Nagino, Ryo
AU - Nakagawa, Takao
AU - Nakajima, Hiroshi
AU - Nakamori, Takeshi
AU - Nakano, Toshio
AU - Nakashima, Shinya
AU - Nakazawa, Kazuhiro
AU - Nobukawa, Masayoshi
AU - Noda, Hirofumi
AU - Nomachi, Masaharu
AU - ODell, Steve
AU - Odaka, Hirokazu
AU - Ohashi, Takaya
AU - Ohno, Masanori
AU - Okajima, Takashi
AU - Ota, Naomi
AU - Ozaki, Masanobu
AU - Paerels, Frits
AU - Paltani, Stephane
AU - Parmar, Arvind
AU - Petre, Robert
AU - Pinto, Ciro
AU - Pohl, Martin
AU - Porter, F. Scott
AU - Pottschmidt, Katja
AU - Ramsey, Brian
AU - Reynolds, Christopher
AU - Russell, Helen
AU - Safi-Harb, Samar
AU - Saito, Shinya
AU - Sakai, Kazuhiro
AU - Sameshima, Hiroaki
AU - Sato, Goro
AU - Sato, Kosuke
AU - Sato, Rie
AU - Sawada, Makoto
AU - Schartel, Norbert
AU - Serlemitsos, Peter
AU - Seta, Hiromi
AU - Shidatsu, Megumi
AU - Simionescu, Aurora
AU - Smith, Randall
AU - Soong, Yang
AU - Stawarz, Lukasz
AU - Sugawara, Yasuharu
AU - Sugita, Satoshi
AU - Szymkowiak, Andrew
AU - Tajima, Hiroyasu
AU - Takahashi, Hiromitsu
AU - Takahashi, Tadayuki
AU - Takeda, Shinichiro
AU - Takei, Yoh
AU - Tamagawa, Toru
AU - Tamura, Keisuke
AU - Tamura, Takayuki
AU - Tanaka, Takaaki
AU - Tanaka, Yasuo
AU - Tanaka, Yasuyuki
AU - Tashiro, Makoto
AU - Tawara, Yuzuru
AU - Terada, Yukikatsu
AU - Terashima, Yuichi
AU - Tombesi, Francesco
AU - Tomida, Hiroshi
AU - Tsuboi, Yohko
AU - Tsujimoto, Masahiro
AU - Tsunemi, Hiroshi
AU - Tsuru, Takeshi
AU - Uchida, Hiroyuki
AU - Uchiyama, Hideki
AU - Uchiyama, Yasunobu
AU - Ueda, Shutaro
AU - Ueda, Yoshihiro
AU - Ueno, Shiro
AU - Uno, Shinichiro
AU - Urry, Meg
AU - Ursino, Eugenio
AU - De Vries, Cor
AU - Watanabe, Shin
AU - Werner, Norbert
AU - Wik, Daniel
AU - Wilkins, Dan
AU - Williams, Brian
AU - Yamada, Shinya
AU - Yamaguchi, Hiroya
AU - Yamaoka, Kazutaka
AU - Yamasaki, Noriko Y.
AU - Yamauchi, Makoto
AU - Yamauchi, Shigeo
AU - Yaqoob, Tahir
AU - Yatsu, Yoichi
AU - Yonetoku, Daisuke
AU - Yoshida, Atsumasa
AU - Yuasa, Takayuki
AU - Zhuravleva, Irina
AU - Zoghbi, Abderahmen
PY - 2016/7/6
Y1 - 2016/7/6
N2 - Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling - a process known as active galactic nucleus feedback. Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 ± 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 ± 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure.
AB - Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling - a process known as active galactic nucleus feedback. Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 ± 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 ± 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure.
UR - http://www.scopus.com/inward/record.url?scp=84978393058&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84978393058&partnerID=8YFLogxK
U2 - 10.1038/nature18627
DO - 10.1038/nature18627
M3 - Article
AN - SCOPUS:84978393058
VL - 535
SP - 117
EP - 121
JO - Nature
JF - Nature
SN - 0028-0836
IS - 7610
ER -