adsabs/AstroCLIMB huggingface dataset:
Paper: Robust Detection of Hot Intragroup Medium in Optically Selected, Poor Galaxy Groups by eROSITA
Authors: Dawei Li, Taotao Fang, Chong Ge, Teng Liu, Lin He, Zhiyuan Li, Fabrizio Nicastro, Xiaohu Yang, Xiaoxia Zhang, Yun-Liang Zheng
Figure caption: The distance distribution of member galaxies to the group centers in the actual group samples and control samples. The group centers were defined based on DESI LS data as the luminosity-weighted centers of the member galaxies, for both real and mock groups. Both samples were normalized.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: Images of NGC 2981, the host galaxy of SN 2020acct. Left: stacked HST images (F555W and F814W bands). The 3″ × 3″ inset image zooms in on the local environment with red crosshairs marking the location of SN 2020acct. Right: PS1 r-band images of SN 2020acct during the first (top) and second (bottom) peaks used for astrometric measurements.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: Two low-mass helium star models for the first peak of SN 2020acct. Left: a model that experienced a silicon flash 101 days before exploding with a very low energy, 2.3 × 1049 erg. The light curve is produced by the explosion impacting the shell ejected by the flash. The initial helium star mass was 2.6 M⊙ and the pre-SN mass, 2.14 M⊙, of which the flash ejected 0.47 M⊙ with energy 6 × 1047 erg. The first peak is fit well by this model, but the required explosion is low for neutrino-powered SNe in this mass range, and there is no obvious mechanism for making the second peak. Right: a similar model without a silicon flash that interacted with a steady wind of 0.1 M⊙ yr−1 with velocity 1000 km s−1. The initial helium core mass here was 2.7 M⊙, the pre-SN mass was 2.21 M⊙, and the explosion kinetic energy was 9 × 1049 erg. The initial peak is fit well, but the model declines too slowly after the peak. This could indicate decreasing optical efficiency for the shock, which lies above the photosphere (dashed line), or a nonsteady wind with density declining faster than r−2.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: Bolometric light curve of SN 2020acct (points) compared to two standard PPISN models and modified models. Left: impact of increasing neutrino losses. The dashed line here shows the standard model of a 71 M⊙ helium star (mass at the onset of PPI of 52 M⊙) that undergoes four pulses prior to collapse. The solid line shows the modified model in which neutrino losses have been increased by 30%. Increasing neutrino losses reduces the central temperature of the core, shortening the time delay between peaks. Right: impact of increased carbon abundance. With the solid line, we show a 72 M⊙ helium star (mass at the point of PPI of 52.92 M⊙) with a slightly enhanced carbon abundance but no neutrino losses. Despite having four pulses, the model generates only a single peak. Including both enhanced carbon and neutrino losses (dashed line), a weak fifth pulse makes the second peak of the light curve. See Section 5 for more details.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: Prospector SED fitting of the global (top panel) and local (bottom panel) host photometry within 1″ of the explosion site of SN 2020acct. Fitting the global SED, we find a stellar mass of ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })=11.2{9}_{-0.06}^{+0.04}﹩ and a current SFR of ﹩(\mathrm{SFR}/{M}_{\odot }{\mathrm{yr}}^{-1})=1{7}_{-11}^{+15}﹩. For the stellar population, we find an SFR of ﹩\mathrm{log}(\mathrm{SFR}/{M}_{\odot }{\mathrm{yr}}^{-1})=-1.{1}_{-0.7}^{+0.9}﹩ and an average stellar age of tage = 9.13﹩{}_{-3.3}^{+4.5}﹩ Myr.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: Evolution of the best-fitting PPISN model to the light curve of SN 2020acct. The red dashed line gives the effective temperature evolution of the model, while the corresponding bolometric light curve is shown in green. The radial evolution of the model follows the luminosity as ﹩R=L/{(4\,\pi \,\sigma \,{T}^{4})}^{0.5}﹩.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: PPI modeling of SN 2020acct, compared to its bolometric light curve. From a 72 M⊙ He core (corresponding to a mass at the onset of PPI of 52.9 M⊙), the first peak is the result of colliding shells produced by three quick successive pulsations, while the second peak is produced by a weak final pulse that induces final collapse of the core to a 47.5 M⊙ black hole. The weak model peak before the first observed peak comes from the collision of closely spaced pulses 2 and 3, and its actual presence is uncertain.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: Modeling the emission profiles around λ4650 as He II and N III. To recreate the profile, an additional He II absorption component was included. The profiles of both emission lines are narrow (900 km s−1 for N III and 450 km s−1 for He II) and are offset by >300 km s−1 from the rest frame. As narrow lines typically indicate the presence of low-density/optically thin material, the only way to produce this blueshift would be through attenuation of the red wing of the line through dust condensation.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: MOSFiT parameter distributions to CSM interaction modeling of the first peak of SN 2020acct with fixed s = 0. We note the minimal change to fit quality when setting s = 2 or leaving it as a free parameter. Our resulting parameters are given in Table 4.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: Luminosity, temperature, and radial evolution of the blackbody fits to the two peaks of SN 2020acct. Phases are given with respect to the second peak.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: MOSFiT modeling of SN 2020acct, fitting the first peak with CSM interaction from E. Chatzopoulos et al. (2012; here showing the output for shell-like CSM, S = 0) and the second peak with W. D. Arnett (1982) 56Ni decay. Faded triangles are photometric upper limits.
Paper: PDS 70b Shows Stellar-like Carbon-to-oxygen Ratio
Authors: Chih-Chun Hsu, Jason J. Wang, 劲飞 王, Geoffrey A. Blake, Jerry W. Xuan, Yapeng Zhang, Jean-Baptiste Ruffio, Katelyn Horstman, Julianne Cronin, Ben Sappey, Yinzi Xin, Luke Finnerty, Daniel Echeverri, Dimitri Mawet, Nemanja Jovanovic, Clarissa R. Do Ó, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Gregory W. Doppmann, Michael P. Fitzgerald, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: KPIC spectrum of PDS 70b and its best-fit forward model using the BT-Settl model grids. The spectra were taken on 2024 May 23 (UT). Orders 31–33 on fiber 4 are shown in black lines. The full forward model, with the stellar speckle and planet fluxes, is in cyan lines. The stellar model, directly from the observed on-axis KPIC spectrum of PDS 70 A, is shown in blue lines. The planet model, including the best-fit BT-Settl model with the observed telluric profile, is illustrated in red lines. The residual (data—full forward model) is depicted in gray dots, and data noise is shown in the orange shaded region.
Paper: PDS 70b Shows Stellar-like Carbon-to-oxygen Ratio
Authors: Chih-Chun Hsu, Jason J. Wang, 劲飞 王, Geoffrey A. Blake, Jerry W. Xuan, Yapeng Zhang, Jean-Baptiste Ruffio, Katelyn Horstman, Julianne Cronin, Ben Sappey, Yinzi Xin, Luke Finnerty, Daniel Echeverri, Dimitri Mawet, Nemanja Jovanovic, Clarissa R. Do Ó, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Gregory W. Doppmann, Michael P. Fitzgerald, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Top: posteriors of the derived physical parameters of PDS 70b using the BT-Settl models, including effective temperature, surface gravity, and projected rotational and radial velocities. See Section 4.2 for details. Bottom: the posteriors of RV, C/O ratio, and metallicity [C/H] derived from KPIC spectra of PDS 70b using the petitRADTRANS retrieval framework. See Section 5 for details.
Paper: Robust Detection of Hot Intragroup Medium in Optically Selected, Poor Galaxy Groups by eROSITA
Authors: Dawei Li, Taotao Fang, Chong Ge, Teng Liu, Lin He, Zhiyuan Li, Fabrizio Nicastro, Xiaohu Yang, Xiaoxia Zhang, Yun-Liang Zheng
Figure caption: Comparison of luminosities and baryon masses within r500 between this work (red symbols) and previous studies, including poor galaxy groups (green) and rich galaxy groups and clusters (blue). In the left panel, the solid line represents the LX–M500 relation for galaxy groups from L. Lovisari et al. (2015), while the dashed line represents the LX–M500 relation for galaxy clusters from G. Schellenberger & T. H. Reiprich (2017). The solid line of the right panel displays the predicted Mb at corresponding M500 based on the ΛCDM model.
Paper: PDS 70b Shows Stellar-like Carbon-to-oxygen Ratio
Authors: Chih-Chun Hsu, Jason J. Wang, 劲飞 王, Geoffrey A. Blake, Jerry W. Xuan, Yapeng Zhang, Jean-Baptiste Ruffio, Katelyn Horstman, Julianne Cronin, Ben Sappey, Yinzi Xin, Luke Finnerty, Daniel Echeverri, Dimitri Mawet, Nemanja Jovanovic, Clarissa R. Do Ó, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Gregory W. Doppmann, Michael P. Fitzgerald, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Cross-correlation functions (CCFs) of our PDS 70b KPIC spectra against the molecular templates derived from the Sonora Bobcat models. Left: CCF (red solid line) of our KPIC spectra for the CO molecular templates. The stellar barycentric–included RV is depicted by the gray vertical dashed line. The auto-correlation function (ACF) of the CO molecular templates, normalized to the peak of CCF, is plotted as a dashed red line. The ACF serves as a guide to detections of given molecular templates. Middle: same as the left panel for the H2O molecular templates in blue. Right: same as the upper panel for the CO + H2O molecular templates in magenta.
Paper: Robust Detection of Hot Intragroup Medium in Optically Selected, Poor Galaxy Groups by eROSITA
Authors: Dawei Li, Taotao Fang, Chong Ge, Teng Liu, Lin He, Zhiyuan Li, Fabrizio Nicastro, Xiaohu Yang, Xiaoxia Zhang, Yun-Liang Zheng
Figure caption: The surface brightness profiles of subsamples. Blue crosses show the background-subtracted profile. The blue solid lines represent the best-fit β model for each subsample, except for the four undetected subsamples. The data error bars correspond to the quadratic sum of photon Poisson errors and the stacking uncertainty. The orange dashed lines represent the PSF profile of eROSITA. The unit of halo mass (Mhalo) is h−1 M⊙.
Paper: Robust Detection of Hot Intragroup Medium in Optically Selected, Poor Galaxy Groups by eROSITA
Authors: Dawei Li, Taotao Fang, Chong Ge, Teng Liu, Lin He, Zhiyuan Li, Fabrizio Nicastro, Xiaohu Yang, Xiaoxia Zhang, Yun-Liang Zheng
Figure caption: From top to bottom, the three rows represent the results for luminosity, gas mass, and gas fraction within r180, respectively. The first column uses halo mass as the X-axis, while the second column uses redshift as the X-axis. The error bars correspond to the 1σ errors of the best-fit parameters. The unit of halo mass (Mhalo) is h−1 M⊙.
Paper: Robust Detection of Hot Intragroup Medium in Optically Selected, Poor Galaxy Groups by eROSITA
Authors: Dawei Li, Taotao Fang, Chong Ge, Teng Liu, Lin He, Zhiyuan Li, Fabrizio Nicastro, Xiaohu Yang, Xiaoxia Zhang, Yun-Liang Zheng
Figure caption: Background-subtracted surface brightness images of all subsamples in the 0.2–2.3 keV band. The annulus shows the region used to compute the background. Emission is seen in most subsamples but is more extended and brighter in the high-mass groups subsamples. The scale bar corresponds to 200 kpc in each panel. The unit of halo mass (Mhalo) is h−1 M⊙.
Paper: Double “acct”: A Distinct Double-peaked Supernova Matching Pulsational Pair Instability Models
Authors: C. R. Angus, S. E. Woosley, R. J. Foley, M. Nicholl, V. A. Villar, K. Taggart, M. Pursiainen, P. Ramsden, S. Srivastav, H. F. Stevance, T. Moore, K. Auchettl, W. B. Hoogendam, N. Khetan, S. K. Yadavalli, G. Dimitriadis, A. Gagliano, M. R. Siebert, A. Aamer, T. de Boer, K. C. Chambers, A. Clocchiatti, D. A. Coulter, M. R. Drout, D. Farias, M. D. Fulton, C. Gall, H. Gao, L. Izzo, D. O. Jones, C.-C. Lin, E. A. Magnier, G. Narayan, E. Ramirez-Ruiz, C. L. Ransome, A. Rest, S. J. Smartt, K. W. Smith
Figure caption: MOSFiT parameter distributions to the 56Ni-powered light-curve model to the second peak of SN 2020acct.
Paper: The XRISM/Resolve View of the Fe K Region of Cyg X-3
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, María Díaz 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, 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 Ogorzalek, Takashi Okajima, Naomi Ota, Stephane 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, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, 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, Ryota Tomaru, Tasuku Hayashi, Tomohiro Hakamata, Daiki Miura, Karri Koljonen, Mike McCollough
Figure caption: Top: velocity shift of the photoionized emission components of the spectrum as a function of orbital phase. Middle: velocity shift of the photoionized absorption components of the spectrum as a function of orbital phase. Red curves show fits of the radial velocity profile (see text for details). Bottom: 2–10 keV XRISM/Resolve light curve folded on the orbital period of 17,252 s. Two orbital cycles are shown for clarity.
Paper: The XRISM/Resolve View of the Fe K Region of Cyg X-3
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, María Díaz 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, 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 Ogorzalek, Takashi Okajima, Naomi Ota, Stephane 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, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, 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, Ryota Tomaru, Tasuku Hayashi, Tomohiro Hakamata, Daiki Miura, Karri Koljonen, Mike McCollough
Figure caption: The XRISM/Resolve spectrum in the Fe K region showing the observed data and our best-fit model using multiple photoionized absorption and emission components as described in the text. The top panel shows the observed count data (black) together with the best-fit model. The second and third panels show the contributions to χ2 vs. energy and the ratio of the best-fit model to the observed counts. The final two panels show the models for line emission and absorption, respectively. Note the energy offset between the emission and absorption.