adsabs/AstroCLIMB huggingface dataset:
Paper: Retention of Surface Water on Tidally Locked Rocky Planets in the Venus Zone around M Dwarfs
Authors: Yueyun Ouyang, Feng Ding, 峰 丁, Jun Yang, 军 杨
Figure caption: Mass of surface water in the collapsed state as a function of the stellar flux S* and the background surface pressure pdry (A), and a function of S* and the CO2 concentration ﹩{f}_{{\rm{C}}{{\rm{O}}}_{2}}﹩ (B). In panel (A), ﹩{f}_{{\rm{C}}{{\rm{O}}}_{2}}=376﹩ ppmv; in panel (B), pdry = 1 bar. Gray dashed curves in both panels mark the boundaries of the runaway greenhouse state where no surface water can exist, and red stars correspond to the example shown in Figure 2.
Paper: Gravitational-wave Parameter Estimation in Non-Gaussian Noise Using Score-based Likelihood Characterization
Authors: Ronan Legin, Maximiliano Isi, Kaze W. K. Wong, Yashar Hezaveh, Laurence Perreault-Levasseur
Figure caption: Example similar to Figure 1 of a posterior distribution sampled using SLIC (blue) compared to a Gaussian likelihood (orange), utilizing real noise from the Livingston detector with no visible signs of non-Gaussianity. The contours indicate the 68% and 99% credible intervals. The ground truth parameters for the waveform are ﹩{ \mathcal M }=39.1{M}_{\odot }﹩, η = 0.167, χ1 = −0.534, χ2 = −0.033, dL = 463 Mpc, and ϕc = 0.540. The true trigger time, tc, is 0.603 s in relative time, corresponding to an absolute GPS time of 1,131,113,090.603 s. The segment of LIGO noise used for this mock observation begins at GPS time 1,131,113,090 s and lasts for 4 s. The signal-to-noise ratio of the true waveform is 15.3.
Paper: Retention of Surface Water on Tidally Locked Rocky Planets in the Venus Zone around M Dwarfs
Authors: Yueyun Ouyang, Feng Ding, 峰 丁, Jun Yang, 军 杨
Figure caption: Schematic diagram illustrating a possible climate evolution of tidally locked planets in the Venus zone. Stage 1: primordial steam-dominated atmosphere is gradually lost by intense stellar radiation and atmospheric heat transport is weakened. Stage 2: water begins to condense from the atmosphere to the surface. Stage 3: the planet is trapped in the collapsed state. Red and blue curves in panel (A) represent the evolution of surface temperature on the dayside and nightside, respectively. Orange and purple curves in panel (B) represent the evolution of atmospheric and surface water mass, respectively.
Paper: Gravitational-wave Parameter Estimation in Non-Gaussian Noise Using Score-based Likelihood Characterization
Authors: Ronan Legin, Maximiliano Isi, Kaze W. K. Wong, Yashar Hezaveh, Laurence Perreault-Levasseur
Figure caption: Coverage probability test for our sampled posteriors from 200 mock observations with real noise from the Livingston detector and 200 from the Hanford detector. The orange (Livingston) and blue (Hanford) shaded regions represent the 1σ error estimated by bootstrapping over the set of sampled posteriors. The shaded gray regions show the 1σ and 3σ errors of the null hypothesis, in which the sampled posteriors are accurate.
Paper: Retention of Surface Water on Tidally Locked Rocky Planets in the Venus Zone around M Dwarfs
Authors: Yueyun Ouyang, Feng Ding, 峰 丁, Jun Yang, 军 杨
Figure caption: Critical global mean value of water vapor (mv) that triggers surface water condensation on the close-in synchronously rotating planet Gl 581c, when the surface partial pressure of N2 is varied from 100 to 1000 hPa. Black solid curve with filled circles is estimated by GCM simulations in J. Leconte et al. (2013b), and blue dashed curve with squares is estimated by our MRCS model.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Comparative analysis of multimessenger observational parameters for BNS mergers across 10 GW detector network configurations. The figure shows the SNR histogram (top left), 90% credible sky localization area (top right), and uncertainties in the relative distance (bottom left) and the inclination angle (bottom right). All uncertainties are presented at the 68% credibility level. All panels, except for the SNR, include events with SNR ≥ 10, ensuring that localization and parameter estimation comparisons are made for confidently detected signals. Across all metrics, CE4020ET performs best, followed closely by CE40I♯ET. CE40LI+ and CE40LI♯ show nearly indistinguishable detection performance. The luminosity distance and inclination angle uncertainties for CE40I♯ET, CE40I+ET, CE40LET, CE4020I+, and CE4020I♯ are similar. Insets reveal network curves that are otherwise obscured due to overlapping traces.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Detection rate as a function of redshift for 10 GW detector networks. Solid circles and squares represent detection rates evaluated with SNR thresholds of 10 and 100, respectively. The solid black line is the cosmic BNS merger rate, and the gray-shaded region is the variation in the merger rate due to current uncertainties in local merger rate density. For both SNR thresholds, CE4020ET exhibits the highest detection rate, while HLI♯ shows the lowest. For SNR ≥ 10, nearly all networks (except HLI♯) have similar rates and thus overlap in the main plot. For SNR ≥ 100, CE40LI+ and CE40LI♯ are indistinguishable, and the rate curves for CE4020L, CE4020I+, CE4020I♯, CE40LET, and CE40I+ET are hidden behind that of CE40I♯ET. Two zoomed-in insets highlight these regions of overlap.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Comparative analysis of multimessenger observational parameters for BNS mergers—representing ∼ 7.5% of the annual BNS merger population—for optimal GW networks: CE4020ET and CE40I♯ET. The figure presents BNS detection capabilities as a function of SNR, sky localization area, relative distance measurement uncertainty, and inclination angle measurement uncertainty. The black and dark gray lines represent the BILBY analysis results for CE4020ET and CE40I♯ET, respectively, while the blue and pink lines correspond to the  analysis for the same networks. The two networks exhibit comparable performance across all metrics, and the two analysis methods show close agreement, reinforcing confidence in the robustness of parameter recovery.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: The figure displays (from left to right) the number of events that can be localized to within sky areas of 1, 10, and 100 deg2, respectively, as a function of redshift. In the 1 and 10 deg2 panels, CE40LI+ and HLI♯ show nearly coincident curves, whereas at 100 deg2, CE40LI+ significantly outperforms HLI♯. Similarly, CE40I+ET and CE40LET localize a comparable number of events to within 10 deg2, and CE4020ET, CE40I♯ET, CE40I+ET, and CE40LET show similar performance at 100 deg2. Overall, CE4020ET precisely localizes the highest number of events, followed by CE40I♯ET. The variation in localization accuracy across networks—with some maintaining high precision at higher redshifts, while others show a rapid decline—underscores the role of network design in counterpart identification (see Section 6.1. for details).
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: The number of events as a function of SNR (left panels) and sky localization area (right panels) for which early warning alerts can be issued at 1 minute (upper panels) and 10 minutes (bottom panels) before the BNS merger. Longer lead times with sufficient localization precision allow telescope prepositioning, improving the chances of detecting prompt GRB emission and early KN phases, while shorter windows require greater localization precision to enable these searches. Due to similar detection and localization capabilities, CE40I♯ET, CE40I+ET, and CE40LET are nearly indistinguishable. Similarly, CE4020I+, CE4020I♯, and CE4020L overlap in the SNR panels, and they overlap with the aforementioned three in the top SNR panel. CE40LI+ and CE40LI♯ also show nearly identical detection performance.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Parameter estimation corner plots and sky maps for two representative BNS merger events in the CE4020ET (left) and CE40I♯ET (right) configurations. The corner plots show the posterior distributions for key source parameters, including mass ratio (q), chirp mass (﹩{ \mathcal M }﹩), luminosity distance (dL), and inclination angle (θJN). The 1D marginalized distributions for each parameter are shown along the diagonal, while the off-diagonal plots show the 2D correlation between parameter pairs. The corresponding sky maps above each corner plot display the 50% and 90% credible regions for source localization in the sky.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Amplitude spectral density (ASD) of detector noise for LIGO at A+ and A♯ sensitivities, 20 km and 40 km CE, and ET.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: The detection efficiency as a function of redshift for 10 GW detector networks. The solid circles represent values evaluated with a threshold SNR of 10, and the solid squares represent the values with a threshold SNR of 100. The solid lines are sigmoid fits for efficiency.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Probability density function (PDF) distributions for key observational parameters of BNS mergers, representing ∼7.5% of the annual BNS merger population, as detected by CE4020ET and CE40I♯ET networks. The panels present BNS detection capabilities as a function of SNR, sky localization area, relative distance measurement uncertainty, and inclination angle measurement uncertainty, respectively. Results are shown for two methods: GWBENCH (blue for CE4020ET and pink for CE40I♯ET) and BILBY (black and dark gray for the respective networks).
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Number of events that can be localized within sky areas of 1 (left), 10 (middle), and 100 deg2 (right), respectively, as a function of redshift for four networks incorporating a Southern Hemisphere detector in Australia. The CE4020ET network is shown for reference.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Cumulative distribution functions of SNR, 90% credible localization area, and parameter uncertainties for networks incorporating a Southern Hemisphere detector in Australia (S20 and S♯ variants), with CE4020ET shown for reference.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: Comparative analysis of multimessenger observational parameters for BNS mergers across 10 GW detector network configurations. The figure presents multiple panels, each illustrating the probability density function (PDF) distributions of BNS detection capabilities as a function of SNR, sky localization area, relative distance measurement uncertainty, and inclination angle measurement uncertainty, respectively.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: This figure depicts a comparison of the SNR for BNS mergers as a function of redshift (z) across various configurations of GW detectors. The colors represent different ranges for sky localization areas, indicating the precision with which the location of the GW sources can be pinpointed.
Paper: The Critical Role of LIGO-India in the Era of Next-generation Observatories
Authors: Shiksha Pandey, Ish Gupta, Koustav Chandra, Bangalore S. Sathyaprakash
Figure caption: This figure depicts the relative uncertainty in luminosity distance as a function of 90% credible sky area in square degrees for BNS mergers for different GW detector configurations. The color denotes the signal’s network SNR.
Paper: High Optical-to-X-Ray Polarization Ratio Reveals Compton Scattering in BL Lacertae’s Jet
Authors: Iván Agudo, Ioannis Liodakis, Jorge Otero-Santos, Riccardo Middei, Alan Marscher, Svetlana Jorstad, Haocheng Zhang, Hui Li, Laura Di Gesu, Roger W. Romani, Dawoon E. Kim, Francesco Fenu, Herman L. Marshall, Luigi Pacciani, Juan Escudero Pedrosa, Francisco José Aceituno, Beatriz Agís-González, Giacomo Bonnoli, Víctor Casanova, Daniel Morcuende, Vilppu Piirola, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, Callum McCall, Helen E. Jermak, Iain A. Steele, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Emmanouil Angelakis, Alexander Kraus, Dmitry Blinov, Siddharth Maharana, Rumen Bachev, Jenni Jormanainen, Kari Nilsson, Vandad Fallah Ramazani, Carolina Casadio, Antonio Fuentes, Efthalia Traianou, Clemens Thum, José L. Gómez, Lucio Angelo Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Sequence of 43 GHz VLBA images of BL Lac from the BEAM-ME program at 0.1 mas angular resolution. Contours represent total flux density from 0.01 Jy beam−1 (the lowest contour on every image) to 5.50 Jy beam−1 (the highest contour). There are 10 logarithmically equally spaced total flux contours from those minimum and maximum levels. The short sticks symbolize the direction of the electric vector polarization angle.
Paper: High Optical-to-X-Ray Polarization Ratio Reveals Compton Scattering in BL Lacertae’s Jet
Authors: Iván Agudo, Ioannis Liodakis, Jorge Otero-Santos, Riccardo Middei, Alan Marscher, Svetlana Jorstad, Haocheng Zhang, Hui Li, Laura Di Gesu, Roger W. Romani, Dawoon E. Kim, Francesco Fenu, Herman L. Marshall, Luigi Pacciani, Juan Escudero Pedrosa, Francisco José Aceituno, Beatriz Agís-González, Giacomo Bonnoli, Víctor Casanova, Daniel Morcuende, Vilppu Piirola, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, Callum McCall, Helen E. Jermak, Iain A. Steele, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Emmanouil Angelakis, Alexander Kraus, Dmitry Blinov, Siddharth Maharana, Rumen Bachev, Jenni Jormanainen, Kari Nilsson, Vandad Fallah Ramazani, Carolina Casadio, Antonio Fuentes, Efthalia Traianou, Clemens Thum, José L. Gómez, Lucio Angelo Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Results of the Swift-XRT monitoring campaign of BL Lac. Fluxes F 0.5−2 keV and F 2−10 keV are displayed in units of 10−12 erg cm−2 s−1 and 10−11 erg cm−2 s−1, respectively. The label “HR” stands for hardness ratio, which we define as (F 2−10 keV − F 0.5−2 keV)/(F 2−10 keV + F 0.5−2 keV). Gray shaded areas mark the duration of the IXPE pointing.
Paper: High Optical-to-X-Ray Polarization Ratio Reveals Compton Scattering in BL Lacertae’s Jet
Authors: Iván Agudo, Ioannis Liodakis, Jorge Otero-Santos, Riccardo Middei, Alan Marscher, Svetlana Jorstad, Haocheng Zhang, Hui Li, Laura Di Gesu, Roger W. Romani, Dawoon E. Kim, Francesco Fenu, Herman L. Marshall, Luigi Pacciani, Juan Escudero Pedrosa, Francisco José Aceituno, Beatriz Agís-González, Giacomo Bonnoli, Víctor Casanova, Daniel Morcuende, Vilppu Piirola, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, Callum McCall, Helen E. Jermak, Iain A. Steele, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Emmanouil Angelakis, Alexander Kraus, Dmitry Blinov, Siddharth Maharana, Rumen Bachev, Jenni Jormanainen, Kari Nilsson, Vandad Fallah Ramazani, Carolina Casadio, Antonio Fuentes, Efthalia Traianou, Clemens Thum, José L. Gómez, Lucio Angelo Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Top panels: best fit to the IXPE, XMM-Newton, and NuSTAR data and corresponding residuals. On the left, the model tbabs × const × polconst × po fitting the I Stokes spectra is shown, while the right panel displays the best-fit Q and U Stokes spectra. Bottom panel: confidence regions corresponding to 68%, 90%, and 99% uncertainties derived using the full IXPE 2–8 keV data.