adsabs/AstroCLIMB huggingface dataset:
Paper: On the Orbital Effects of Stellar Collisions in Galactic Nuclei: Tidal Disruption Events and Ejected Stars
Authors: Sanaea C. Rose, Brenna Mockler
Figure caption: We show a simulation that uses the Rauch99 prescription that includes relaxation. There are 4000 sample stars in this simulation. About 0.7% became unbound, and one became a TDE immediately postcollision. Some other collision-affected stars also became TDEs; collisions would have affected their orbital evolution, but it was the relaxation prescription that pushed them into the tidal radius. The symbols are consistent with those in our other figures, with the addition of the dark green stars to represent TDEs from our relaxation prescription. Indicated by the gray shaded region, we place a caveat on the dark green stars (relaxation TDEs) with a final semimajor axis within 0.001 pc, which are also the TDEs with the shortest orbital period. The applicability of our relaxation prescription within this region is uncertain.
Paper: On the Orbital Effects of Stellar Collisions in Galactic Nuclei: Tidal Disruption Events and Ejected Stars
Authors: Sanaea C. Rose, Brenna Mockler
Figure caption: This figure has the same form as Figure 5. The symbols are the same as in previous figures, except with the addition of crosses, which represent stars placed on such radial orbits that they were deposited within the Schwarzschild radius of the SMBH. In the first row, we show another example of a Rauch99 simulation similar to the one in the first row of Figure 2. In the second row, we show a Rauch99 with dissipation during high-speed collisions: we scaled the postcollision speed by 50% in the center-of-mass frame following high-speed, destructive collision cases. The last row shows a Lai+93 simulation for a sample of stars out to 1 pc.
Paper: Model-independent H0 within FLRW: Joint Constraints from GWTC-3 Standard Sirens and Strong Lensing Time Delays
Authors: Ji-Yu Song, Jing-Zhao Qi, Jing-Fei Zhang, Xin Zhang
Figure caption: Posterior distributions of H0 using 47 GW events and RXJ1131-1231 in the polynomial model. The red solid line and the blue dashed line represent the cases of using the H0LiCOW method and the TDCOSMO method to break MST, respectively. The pink and green shaded areas show the 68% confidence interval from the Planck 2018 CMB inference in the ΛCDM model and the SH0ES distance ladder measurement in the local Universe, respectively.
Paper: Model-independent H0 within FLRW: Joint Constraints from GWTC-3 Standard Sirens and Strong Lensing Time Delays
Authors: Ji-Yu Song, Jing-Zhao Qi, Jing-Fei Zhang, Xin Zhang
Figure caption: Redshift distributions for GW190814, GW200105, and GW190412 obtained using different methods, with cosmological and population model parameters fixed.
Paper: The Giant Eruption in Solar Cycle 25 Caused by Collisional Shearing
Authors: Tao Ding, Jun Zhang, Yijun Hou
Figure caption: Temporal evolution of flux ropes (sheared arcades) revealed by NLFFF extrapolation. Panels (a)–(f) and (g1) show the top view of the flux ropes (sheared arcades), and panels (g2) and (g3) display the side view of the flux ropes. The blue-red maps in panels (g2) and (g3) are the distributions of the magnetic twist in the vertical planes based on the red and yellow cuts denoted in panel (g1), respectively.
Paper: The Giant Eruption in Solar Cycle 25 Caused by Collisional Shearing
Authors: Tao Ding, Jun Zhang, Yijun Hou
Figure caption: Overview of the eruption on 2024 October 3. Panel (a): an SDO/HMI LOS magnetogram. The red square outlines the fields of view (FOVs) in panels (b)–(d) and Figure 2(a1). The green curve inset displays the GOES soft X-ray flux variation of the X9.0 flare. Panel (b): the SDO/AIA EUV data in 131 Å wavelength. The SDO/HMI LOS magnetogram at +500 G and −500 G are shown by red and blue solid contours, respectively. Panels (c) and (d): the SDO/AIA 94 Å and 211 Å observations. The cyan and yellow dashed lines in panel (d) outline two sets of postflare loops. Panel (e): a SOHO/LASCO C2 image.
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: (a) Apoareon and periareon altitudes above the Martian surface for the Tianwen-1 orbiter from 2021 June to 2024 October. The blue line and right Y-axis denote the apoareon altitudes, and the red line and left Y-axis denote the periareon altitudes. (b) The observation duration of each arc; the average tracking time is 2.635 hr.
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: (a) Ratios of atmospheric density (orange) and drag acceleration (blue) relative to periapsis altitude at different altitudes. These ratios do not depend on the physical parameters of the spacecraft. The a priori density is from the Mars Climate Database. (b) Atmospheric drag acceleration (blue) and solar radiation pressure (orange) acceleration as a function of orbital altitude.
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: (a) The postfit residual rms with respect to the SEP angle. (b) The statistical information of the residual rms; the red line denotes the 90% percentile. (c) Earth–Mars distance and SEP angle time series. The red curve and the left Y-axis denote the Earth–Mars distance, and the blue curve and the right Y-axis denote the SEP angle.
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: Rms of range-rate data postfit residual for 1 day arcs of the Tianwen-1 orbiter data using two gravity field models. The blue “diamond” line denotes the MRO120D model, and the orange “x” line denotes the TW80 model.
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: Rms of orbit overlap differences in the radial (a), along-track (b), and cross-track (c) directions and in total position (d) for 12 hr orbit predictions from 1 day data arcs using two gravity field models.
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: (a) The ground track distribution with altitude variation. (b) The data density distribution of tracking data. Maps are plotted in Hammer projection; colors closer to yellow indicate lower orbital altitude (a) and higher data density (b).
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree of the solved gravity field model with a Kaula power-law constraint. The gravity field coefficients are denoted by a blue solid line, the Kaula power law is denoted by a green solid line, and the formal uncertainties of the gravity field coefficients are denoted by an orange dashed line.
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: The global (a) correlation and (b) admittance between topography and the MRO120D (red) and TW80 (blue) gravity field models. The correlation and admittance were generated using the shtools software (M. A. Wieczorek & M. Meschede 2018).
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: The TW80 free-air gravity anomalies truncated to degree 74 (Hammer projection). This shows the magnitude of the gravity acceleration on the Mars areoid minus the gravity from a reference ellipsoid (ae = 3397 km, 1/f = 196.9).
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: Gravity anomaly errors at the reference surface computed from the full covariance matrix (Hammer projection). The minimum, maximum, and rms of the anomaly errors are 6.5, 72.8, and 35.8 mGal, respectively.
Paper: Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: The south pole region localized (a) correlations and (b) admittances between topography and the MRO120D (red) and TW80 (blue) gravity field models.
Paper: Galactic Accelerations from the GD-1 Stream Suggest a Tilted Dark Matter Halo
Authors: Jacob Nibauer, Ana Bonaca
Figure caption: Black points indicate the data (with 1σ errors), while the red band represents the 99% credible interval of our stream track for a spline with five knots. Knot locations are shown as lines in the top panel for the case of four (navy), five (green), and six (orange) knots. The (ϕ1, ϕ2) data are from Gaia (N. Starkman et al. 2025); solar-reflex correct radial velocities vGSR are from DESI (M. Valluri et al. 2025), SDSS 9 (C. P. Ahn et al. 2012), and LAMOST DR8.2 The distance track is from the subgiant branch (M. Valluri et al. 2025).
Paper: Galactic Accelerations from the GD-1 Stream Suggest a Tilted Dark Matter Halo
Authors: Jacob Nibauer, Ana Bonaca
Figure caption: The inferred 3D accelerations from GD-1 in cylindrical Galacocentric components. Error bands represent regions of 68% (dark) and 95% (light) confidence. Constraints are marginalized over four to six spline knots. We overplot three common potential models, including MWPotential2014 from Galpy (black; J. Bovy 2015), MilkyWayPotential2022 from Gala (red; A. M. Price-Whelan 2017), and the potential from P. J. McMillan (2017; green). The three models are axisymmetric (aϕ = 0). Our data-driven accelerations are of a similar magnitude to all three model though the best match is with J. Bovy (2015). We find a 2σ discrepancy from axisymmetry at ϕ1 ≈ −20° where constraints are the tightest.
Paper: Galactic Accelerations from the GD-1 Stream Suggest a Tilted Dark Matter Halo
Authors: Jacob Nibauer, Ana Bonaca
Figure caption: We fit an ellipsoidal density model with rotation to the inferred accelerations and find two posterior modes that are compatible with our measurement (Mode 1 in top row, Mode 2 in the bottom). The total matter density (heat map and black contours) of both modes are plotted in Galactocentric slices at the median location of GD-1 (white text labels). White arrows indicate the inferred median accelerations of GD-1, and black arrows correspond to the fitted triaxial model. Mode 1 has density axis ratios of 1:0.75:0.7 and a halo tilt of ≈18° out of the disk’s plane in the direction of the Sun, remarkably similar to stellar halo constraints (dashed cyan contours, J. J. Han et al. 2022). Mode 2 has axis ratios 1:0.95:0.65 and a tilt angle of ≈56°. Acceleration measurements at different locations are needed to distinguish the two modes.
Paper: Galactic Accelerations from the GD-1 Stream Suggest a Tilted Dark Matter Halo
Authors: Jacob Nibauer, Ana Bonaca
Figure caption: Mass-enclosed profile of the Milky Way, with data compiled from J. A. S. Hunt & E. Vasiliev (2025). Our measurement is shown in red, below the labeled arrow, and agrees well with other inner halo measurements. The tracer type is indicated by the symbol, and the dashed gray line is MilkyWay Potentia l2022 from Gala (A. M. Price-Whelan 2017), while the dotted–dashed black line is MWPotential2014 from Galpy (J. Bovy 2015). Residuals are relative to MilkyWayPotential2022. See the Appendix for references.
Paper: Galactic Accelerations from the GD-1 Stream Suggest a Tilted Dark Matter Halo
Authors: Jacob Nibauer, Ana Bonaca
Figure caption: The shape of the inner halo when assuming an axisymmetric global mass model. Our constraint is shown by the purple error band. Constraints on the z-axis flattening in the density are shown for Pal 5 (above the dashed line) and GD-1 (below). Symbols indicate the potential model, while the y-axis labels indicate the method used to model the stream (streakline, generative action angle, action-angle clustering, orbit fitting, and particle spray).
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: UV attenuation laws normalized at 3000 Å for various dust models and observations. MW attenuation laws span the range shaded in gray, and the SMC law, often taken as standard for very high-redshift galaxies, is shown with the dotted line. The thick gray line shows the inferred attenuation law from V. Markov et al. (2024), who fit to JWST spectra of galaxies with 6.3 < z < 11.5. In solid black, we show the empirical attenuation law measured by W. Gao et al. (2020), which we adopt as our fiducial attenuation law. This empirical attenuation law is comparable to the theoretical extinction models of SN dust from H. Hirashita et al. (2005) and S. Bianchi & R. Schneider (2007), although the models have steeper UV slopes. The W. Gao et al. (2020) attenuation law has a comparable UV slope to the attenuation laws found for simulated z > 8 galaxies from D. Narayanan et al. (2025; red hatched), which are almost completely flat throughout the UV and optical.
Paper: XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stéphane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Andrew Fabian, Dylan Nelson, Nobuhiro Okabe, Annalisa Pillepich, Cicely Potter, Manon Regamey, Kosei Sakai, Mona Shishido, Nhut Truong, Daniel R. Wik, John ZuHone
Figure caption: XRISM Resolve measurements of (a) the LOS velocities relative to the mean velocity of cluster member galaxies and (b) LOS velocity dispersion, overlaid on the XMM-Newton image. Uncertainties are statistical 1σ. The values to the left of the fields represent the entire ﹩{3}^{{\prime} }\times {3}^{{\prime} }﹩ field, while the values inside the FOV pertain to the 1﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5 quadrants, for which the relatively small PSF smearing effect is not included. The two brightest galaxies are marked along with their relative LOS velocities. Green labels mark the quadrants discussed in Sections 3.2–3.3.
Paper: XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stéphane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Andrew Fabian, Dylan Nelson, Nobuhiro Okabe, Annalisa Pillepich, Cicely Potter, Manon Regamey, Kosei Sakai, Mona Shishido, Nhut Truong, Daniel R. Wik, John ZuHone
Figure caption: The spectrum for the NW quadrant of the Center field (the one with the highest velocity dispersion; see Figure 3(b)). Only the Fe Heα line complex is displayed, binned by 4 eV. Two velocity components are needed to model the line profile. The main component (blue) is blueshifted from the cluster mean by 470 km s−1, while the additional component (magenta) is at the cluster optical mean velocity and contributes 22% ± 7% of the emission measure.
Paper: XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stéphane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Andrew Fabian, Dylan Nelson, Nobuhiro Okabe, Annalisa Pillepich, Cicely Potter, Manon Regamey, Kosei Sakai, Mona Shishido, Nhut Truong, Daniel R. Wik, John ZuHone
Figure caption: The XRISM value of pkin/ptot for Coma, derived from the central line width, is compared with predictions from several cosmological simulations. Open symbols represent all clusters, while filled symbols select only the disturbed Coma-like clusters. For TNG-Cluster, there is an additional selection based on cluster mass and weighting by X-ray emission measure (see Appendix B). The horizontal intervals show the 16th–84th percentiles of the simulated cluster populations. The measured value is at the low end of the predictions.