XRISM Observations of Accretion Disk Corona in Cyg X-2
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arXiv
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2025
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| author | Mizumoto, Misaki Takahashi, Hiromitsu Behar, Ehud Boissay-Malaquin, Rozenn Corrales, Lia Costantini, Elisa Diaz-Trigo, Maria Miller, Eric D. Miller, Jon M. |
| author_facet | Mizumoto, Misaki Takahashi, Hiromitsu Behar, Ehud Boissay-Malaquin, Rozenn Corrales, Lia Costantini, Elisa Diaz-Trigo, Maria Miller, Eric D. Miller, Jon M. |
| contents | We present the high-resolution X-ray spectrum of the Z-source Cygnus X-2, obtained with X-Ray Imaging and Spectroscopy Mission (XRISM). The observations have enabled a precise characterization of the Fe-K emission lines from the accretion disk corona (ADC) and a possible detection of an ultra-fast outflow (UFO). The ADC component has at least two distinct regions. The Fe-K emission lines are remarkably broad, with a velocity dispersion of $σ_v=2300^{+900}_{-700}$~km~s$^{-1}$. This can be larger than what was observed in previous Chandra observations ($1120\pm870$~km~s$^{-1}$) and recent XRISM observations of the similar Z-source GX 340+0 (360--800~km~s$^{-1}$). Furthermore, we marginally detect a blueshifted absorption feature, which we identify as either \ion{Fe}{26} or \ion{Fe}{25}, with outflow velocities of $-0.29c$ or $-0.26c$, respectively. The mass loss rate is $\dot{M}\sim10^{-8}M_\odot\,\mathrm{yr}^{-1}$. Our findings suggest that the ADC in Cyg X-2 has a kinematically active environment with a high degree of turbulence and kinetic energy. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2512_00589 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | XRISM Observations of Accretion Disk Corona in Cyg X-2 Mizumoto, Misaki Takahashi, Hiromitsu Behar, Ehud Boissay-Malaquin, Rozenn Corrales, Lia Costantini, Elisa Diaz-Trigo, Maria Miller, Eric D. Miller, Jon M. High Energy Astrophysical Phenomena We present the high-resolution X-ray spectrum of the Z-source Cygnus X-2, obtained with X-Ray Imaging and Spectroscopy Mission (XRISM). The observations have enabled a precise characterization of the Fe-K emission lines from the accretion disk corona (ADC) and a possible detection of an ultra-fast outflow (UFO). The ADC component has at least two distinct regions. The Fe-K emission lines are remarkably broad, with a velocity dispersion of $σ_v=2300^{+900}_{-700}$~km~s$^{-1}$. This can be larger than what was observed in previous Chandra observations ($1120\pm870$~km~s$^{-1}$) and recent XRISM observations of the similar Z-source GX 340+0 (360--800~km~s$^{-1}$). Furthermore, we marginally detect a blueshifted absorption feature, which we identify as either \ion{Fe}{26} or \ion{Fe}{25}, with outflow velocities of $-0.29c$ or $-0.26c$, respectively. The mass loss rate is $\dot{M}\sim10^{-8}M_\odot\,\mathrm{yr}^{-1}$. Our findings suggest that the ADC in Cyg X-2 has a kinematically active environment with a high degree of turbulence and kinetic energy. |
| title | XRISM Observations of Accretion Disk Corona in Cyg X-2 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2512.00589 |