title: The XRISM/Resolve View of the Fe K Region of Cyg X-3
Creators: name: XRISM Collaboration
name: Audard, Marc
name: Awaki, Hisamitsu
name: Ballhausen, Ralf
name: Bamba, Aya
name: Behar, Ehud
name: Boissay-Malaquin, Rozenn
name: Brenneman, Laura
name: Brown, Gregory V.
name: Corrales, Lia
name: Costantini, Elisa
name: Cumbee, Renata
name: Trigo, Mar韆 D韆z
name: Done, Chris
name: Dotani, Tadayasu
name: Ebisawa, Ken
name: Eckart, Megan E.
name: Eckert, Dominique
name: Eguchi, Satoshi
name: Enoto, Teruaki
name: Ezoe, Yuichiro
name: Foster, Adam
name: Fujimoto, Ryuichi
name: Fujita, Yutaka
name: Fukazawa, Yasushi
name: Fukushima, Kotaro
name: Furuzawa, Akihiro
name: Gallo, Luigi
name: Garc韆, Javier A.
name: Gu, Liyi
name: Guainazzi, Matteo
name: Hagino, Kouichi
name: Hamaguchi, Kenji
name: Hatsukade, Isamu
name: Hayashi, Katsuhiro
name: Hayashi, Takayuki
name: Hell, Natalie
name: Hodges-Kluck, Edmund
name: Hornschemeier, Ann
name: Ichinohe, Yuto
name: Ishida, Manabu
name: Ishikawa, Kumi
name: Ishisaki, Yoshitaka
name: Kaastra, Jelle
name: Kallman, Timothy
name: Kara, Erin
name: Katsuda, Satoru
name: Kanemaru, Yoshiaki
name: Kelley, Richard
name: Kilbourne, Caroline
name: Kitamoto, Shunji
name: Kobayashi, Shogo
name: Kohmura, Takayoshi
name: Kubota, Aya
name: Leutenegger, Maurice
name: Loewenstein, Michael
name: Maeda, Yoshitomo
name: Markevitch, Maxim
name: Matsumoto, Hironori
name: Matsushita, Kyoko
name: McCammon, Dan
name: McNamara, Brian
name: Mernier, Fran鏾is
name: Miller, Eric D.
name: Miller, Jon M.
name: Mitsuishi, Ikuyuki
name: Mizumoto, Misaki
name: Mizuno, Tsunefumi
name: Mori, Koji
name: Mukai, Koji
name: Murakami, Hiroshi
name: Mushotzky, Richard
name: Nakajima, Hiroshi
name: Nakazawa, Kazuhiro
name: Ness, Jan-Uwe
name: Nobukawa, Kumiko
name: Nobukawa, Masayoshi
name: Noda, Hirofumi
name: Odaka, Hirokazu
name: Ogawa, Shoji
name: Ogorzalek, Anna
name: Okajima, Takashi
name: Ota, Naomi
name: Paltani, Stephane
name: Petre, Robert
name: Plucinsky, Paul
name: Porter, Frederick S.
name: Pottschmidt, Katja
name: Sato, Kosuke
name: Sato, Toshiki
name: Sawada, Makoto
name: Seta, Hiromi
name: Shidatsu, Megumi
name: Simionescu, Aurora
name: Smith, Randall
name: Suzuki, Hiromasa
name: Szymkowiak, Andrew
name: Takahashi, Hiromitsu
name: Takeo, Mai
name: Tamagawa, Toru
name: Tamura, Keisuke
name: Tanaka, Takaaki
name: Tanimoto, Atsushi
name: Tashiro, Makoto
name: Terada, Yukikatsu
name: Terashima, Yuichi
name: Tsuboi, Yohko
name: Tsujimoto, Masahiro
name: Tsunemi, Hiroshi
name: Tsuru, Takeshi
name: Uchida, Hiroyuki
name: Uchida, Nagomi
name: Uchida, Yuusuke
name: Uchiyama, Hideki
name: Ueda, Yoshihiro
name: Uno, Shinichiro
name: Vink, Jacco
name: Watanabe, Shin
name: Williams, Brian J.
name: Yamada, Satoshi
name: Yamada, Shinya
name: Yamaguchi, Hiroya
name: Yamaoka, Kazutaka
name: Yamasaki, Noriko
name: Yamauchi, Makoto
name: Yamauchi, Shigeo
name: Yaqoob, Tahir
name: Yoneyama, Tomokage
name: Yoshida, Tessei
name: Yukita, Mihoko
name: Zhuravleva, Irina
name: Tomaru, Ryota
name: Hayashi, Tasuku
name: Hakamata, Tomohiro
name: Miura, Daiki
name: Koljonen, Karri
name: McCollough, Mike
Publisher: name: IOP Science
Year: 2024

description: The X-ray binary system Cygnus X-3 (4U 2030+40, V1521 Cyg) is luminous but enigmatic owing to the high intervening absorption. High-resolution X-ray spectroscopy uniquely probes the dynamics of the photoionized gas in the system. In this Letter, we report on an observation of Cyg X-3 with the XRISM/Resolve spectrometer, which provides unprecedented spectral resolution and sensitivity in the 2� keV band. We detect multiple kinematic and ionization components in absorption and emission whose superposition leads to complex line profiles, including strong P Cygni profiles on resonance lines. The prominent Fe xxv He? and Fe xxvi Ly? emission complexes are clearly resolved into their characteristic fine-structure transitions. Self-consistent photoionization modeling allows us to disentangle the absorption and emission components and measure the Doppler velocity of these components as a function of binary orbital phase. We find a significantly higher velocity amplitude for the emission lines than for the absorption lines. The absorption lines generally appear blueshifted by ??500�0 km s?1. We show that the wind decomposes naturally into a relatively smooth and large-scale component, perhaps associated with the background wind itself, plus a turbulent, denser structure located close to the compact object in its orbit.