adsabs/AstroCLIMB huggingface dataset:
Paper: Orbital Characterization of a Newly Discovered Small Satellite around Quaoar
Authors: Benjamin Proudfoot, Richard Nolthenius, Bryan J. Holler, Ana Carolina de Souza-Feliciano, Flavia L. Rommel, Cameron Collyer, Will M. Grundy, Estela Fernández-Valenzuela
Figure caption: PSF fitting residuals of JWST images of Quaoar. Black circles show a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩21 radius (7 NIRCam pixels), within which the newly discovered satellite should be. The expected surface brightness of the satellite in the NIRCam images (assuming V = 28 mag) is ∼1 MJy sr−1. No clear detection is apparent, with PSF subtraction residuals dominating the region in which we expect the satellite to be. Without improvements to the NIRCam PSF model, or high-quality empirical PSFs, recovery of the satellite will be nearly impossible.
Paper: Orbital Characterization of a Newly Discovered Small Satellite around Quaoar
Authors: Benjamin Proudfoot, Richard Nolthenius, Bryan J. Holler, Ana Carolina de Souza-Feliciano, Flavia L. Rommel, Cameron Collyer, Will M. Grundy, Estela Fernández-Valenzuela
Figure caption: Probability of recovering the new satellite as a function of number of observing stations spaced at minimum a satellite diameter (D) apart. Solid lines show the probability when stations are placed in regions of highest probability first (in descending order), while dotted lines show the probability with random site selection (although with at least D km apart). For D = 30 km—the lower limit on the satellite’s size—a campaign must have at least 98 observing stations to have a > 80% chance of recovery, assuming ideal station placement and perfect recovery if in the shadow path.
Paper: Orbital Characterization of a Newly Discovered Small Satellite around Quaoar
Authors: Benjamin Proudfoot, Richard Nolthenius, Bryan J. Holler, Ana Carolina de Souza-Feliciano, Flavia L. Rommel, Cameron Collyer, Will M. Grundy, Estela Fernández-Valenzuela
Figure caption: Similar to Figure 2, but for an orbit fit where eccentricity was allowed to be a free parameter. Aside from a slight expansion of the probability distribution away from the initial detection, the main effect is to eliminate the pinch at the top left of the probability distribution.
Paper: Comparing XRISM Cluster Velocity Dispersions with Predictions from Cosmological Simulations: Are Feedback Models Too Ejective?
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, 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, 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, Weiguang Cui, Stefano Ettori, Skylar Grayson, Annie Heinrich, Hannah McCall, Dylan Nelson, Nobuhiro Okabe, Yuki Omiya, Arnab Sarkar, Evan Scannapieco, Ming Sun, Keita Tanaka, Nhut Truong, Daniel R. Wik, Congyao Zhang, John ZuHone
Figure caption: Comparison between XRISM observations and simulation predictions of the kinetic pressure ratio. The descriptions are similar to those in Figure 2.
Paper: Comparing XRISM Cluster Velocity Dispersions with Predictions from Cosmological Simulations: Are Feedback Models Too Ejective?
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, 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, 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, Weiguang Cui, Stefano Ettori, Skylar Grayson, Annie Heinrich, Hannah McCall, Dylan Nelson, Nobuhiro Okabe, Yuki Omiya, Arnab Sarkar, Evan Scannapieco, Ming Sun, Keita Tanaka, Nhut Truong, Daniel R. Wik, Congyao Zhang, John ZuHone
Figure caption: Comparison between XRISM observations and simulation predictions of the gas temperature. The descriptions are similar to those in Figure 2.
Paper: Comparing XRISM Cluster Velocity Dispersions with Predictions from Cosmological Simulations: Are Feedback Models Too Ejective?
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, 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, 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, Weiguang Cui, Stefano Ettori, Skylar Grayson, Annie Heinrich, Hannah McCall, Dylan Nelson, Nobuhiro Okabe, Yuki Omiya, Arnab Sarkar, Evan Scannapieco, Ming Sun, Keita Tanaka, Nhut Truong, Daniel R. Wik, Congyao Zhang, John ZuHone
Figure caption: The number of simulated analogs of the observed clusters contained in the three simulation suites, TNG-Cluster and the 300 GADGET-X and GIZMO-SIMBA, as a function of the halo mass (M200c). The analogs are selected based on the observed halo mass and core properties (see Section 2.3).
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Top panel: evolution of the spectral photon index β with time (where Fν ∝ ν−β), showing clear evidence for spectral hardening until the time of the flare peak at ≳50 days, followed by softening of the emission. Aside from the flare peak, the plotted β values apply to the broadband soft+hard X-ray spectral range; at the time of the flare peak, when there is evidence for a BPL spectrum, the plotted value represents the index below the spectral break. The gray shaded area marks the region of the parameter space associated with a rising Fν spectrum. Bottom panel: 0.3–10 keV unabsorbed luminosity light curve (red filled circles, orange squares, and orange diamonds for XRT, CXO, and XMM observations, respectively) and 0.3–30 keV light curve (blue crosses) derived from a self-consistent time-dependent flux calibration. Vertical gray dotted lines mark the time of broadband X-ray spectrum acquisition. Dashed gold line: best-fitting power-law luminosity decay in the time period 10–50 days.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Selection of X-ray transmission spectra from a central source with intrinsic spectrum Fν ∝ ν−0.5 (black dashed line) from the simulations presented in R. Margutti et al. (2019) for a range of Thomson optical depth values τT showing the increasing dominance of the Compton hump flux in the 0.3–10 keV band as τT decreases. These simulations do not account for time-dependent ionization effects in the transmission layer. See main text and R. Margutti et al. (2019) for more details on these simulations.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Evolution of the SPL (orange) and hump (lime green) component luminosities (left) and their ratio (middle) with time in the fixed observer-frame energy band 0.3–10 keV as constrained by our analysis of Section 4.2. The Compton hump contribution increases with time as the optical depth of the reprocessing layer decreases, causing the peak of the hump of emission (initially at >10 keV) to cascade to lower energies and enter the spectral window of interest (Figure 5). The hump dominates the 0.3–10 keV emission at δt ≈ 50 days. Right: cartoon of the SPL+hump model showing how the progressive “emergence” of the hump of emission in the 0.3–10 keV band at δt ≤ 50 days leads to hardening with time.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Effective optical depth to X-rays derived following the reprocessing model of B. D. Metzger (2022) and the observed X-ray and UVOIR emission for AT 2024wpp  (filled circles) and AT 2018cow (stars). AT 2024wpp  maintains higher τX for a significantly longer time, a behavior that is consistent with the delayed appearance of the Compton hump (Section 4.2). The gray dashed line shows τX ∝ t−2 scaling expected for radiation shining through a medium expanding with constant velocity. We assume an arbitrary slow-moving ejecta covering fraction ϕ0 = 0.5.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Probability density distributions of the spectral photon indices (left panel) and spectral break energy (middle panel), for the BPL model that best fits the broadband X-ray SED at the time of the flare peak (right panel, unfolded spectrum). The CXO data (red) indicate a rising spectrum with extreme properties: Fν ∝ ν1.25. The lack of bright hard X-ray emission at the same time, as constrained by NuSTAR, demands the presence of a spectral break and significantly softer emission above Ebreak, with the spectrum bending to Fν ∝ ν−1.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Probability density distributions of the spectral photon indices derived from the broadband X-ray spectral fitting of Section 4 with a BPL model. At the time of the flare peak at ≈50 days, we find evidence for a BPL spectrum with a rising spectrum Fν ∝ ν1.25 at hν ≲ 8 keV. There is a hint for a harder spectral index at softer energies at earlier times (i.e., β2 < β1), which suggests the presence of multiple spectral components, with the relative strength of the harder component increasing with time until the time of the flare peak (see Section 4.2).
Paper: Comparing XRISM Cluster Velocity Dispersions with Predictions from Cosmological Simulations: Are Feedback Models Too Ejective?
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, 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, 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, Weiguang Cui, Stefano Ettori, Skylar Grayson, Annie Heinrich, Hannah McCall, Dylan Nelson, Nobuhiro Okabe, Yuki Omiya, Arnab Sarkar, Evan Scannapieco, Ming Sun, Keita Tanaka, Nhut Truong, Daniel R. Wik, Congyao Zhang, John ZuHone
Figure caption: Comparison between emission-weighted vs. spectral fitting quantities. Top: X-ray surface brightness map of a Perseus-like cluster in TNG-Cluster (left) and its mock X-ray C0 spectrum (right). Bottom: comparisons for two individual systems: Perseus (CC) and A2319 (NCC). The two derivation methods are in close agreement. The XRISM data points are shown for illustration only—the simulated clusters are not expected to match the observed ones precisely.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Density profile of the medium around LFBOTs AT 2024wpp (this work), AT 2018cow (A. Y. Q. Ho et al. 2019; R. Margutti et al. 2019), CSS 161010 (D. L. Coppejans et al. 2020), AT2020xnd (J. S. Bright et al. 2022; A. Y. Q. Ho et al. 2022), AT 2020mrf (Y. Yao et al. 2022), AT 2022tsd (A. Y. Q. Ho et al. 2023b), and AT 2023fhn (A. A. Chrimes et al. 2024a). Dashed black lines denote number density profiles corresponding to constant mass-loss rates for an arbitrary wind velocity of vw ≈ 1000 km s−1. The vertical blue and green lines denote the position of the optical photosphere at optical peak (δt ≈ 4 days) and at δt ≈ 17.5 days, respectively (Paper I). The solid red line denotes the CSM density profile ρCSM(r) ∝ r−1.3 inferred from interpreting the NIR excess as related to effects of free–free emission (see Section 6.2 in Paper I). The inferred CSM density profiles of different events at >1016 cm are remarkably similar, which suggests a simple physical mechanism or a self-regulating process (Section 8.1).