adsabs/AstroCLIMB huggingface dataset:
Paper: Potential Subpopulations and Assembling Tendency of the Merging Black Holes
Authors: Yuan-Zhu Wang, Yin-Jie Li, Jorick S. Vink, Yi-Zhong Fan, Shao-Peng Tang, Ying Qin, Da-Ming Wei
Figure caption: The reconstructed astrophysical primary mass distribution for the OnePL model. The shaded areas indicate the 90% credible regions for different components.
Paper: Potential Subpopulations and Assembling Tendency of the Merging Black Holes
Authors: Yuan-Zhu Wang, Yin-Jie Li, Jorick S. Vink, Yi-Zhong Fan, Shao-Peng Tang, Ying Qin, Da-Ming Wei
Figure caption: Posterior distribution of all the parameters obtained by the OnePL and the TwoPL models; the dashed lines in the marginal distribution represent the 90% credible intervals.
Paper: Potential Subpopulations and Assembling Tendency of the Merging Black Holes
Authors: Yuan-Zhu Wang, Yin-Jie Li, Jorick S. Vink, Yi-Zhong Fan, Shao-Peng Tang, Ying Qin, Da-Ming Wei
Figure caption: Posterior distributions of parameters of the spin model described by Equation (15); the dashed lines represent the 90% credible intervals.
Paper: Failed Solar Eruption of a Multithermal Flux Rope
Authors: Leping Li, Hongqiang Song, Hardi Peter, Lakshmi Pradeep Chitta
Figure caption: General information of the failed multithermal FR eruption. (a)–(b) and (g) SDO/AIA 94, (c) 211, (d) 193, and (e)–(f) 171 Å images, enhanced by the MGN technique, and (h) a composite of 94, 211, and 171 Å images. The red rectangles in (b), (f), and (g), and green and purple rectangles in (c) and (g) enclose regions for the DEM curves in Figures 4(a), (d), (b), (e), and (f). The pink rectangles in (b), (f), and (g), and blue and black rectangles in (c) and (g) mark the locations where the background emissions are measured. The green solid arrows in (c)–(e) denote the warm channel fine structures. The blue, purple, and green lines AB, CD, and EF in (e) and (f) separately show the positions of time slices in Figures 3(a1)–(d1), (a2)–(d2), and (a3)–(d3). In (g), the AIA 94 Å image in the yellow rectangle is enlarged in the white rectangle. The HC, WC, BF, and CS mean the hot channel, warm channel, bright front, and current sheet, respectively.
Paper: Failed Solar Eruption of a Multithermal Flux Rope
Authors: Leping Li, Hongqiang Song, Hardi Peter, Lakshmi Pradeep Chitta
Figure caption: Temperature and EM of the failed FR eruption. (a)–(d) DEM curves for the FR regions enclosed by the red rectangles separately in Figures 1(b), 1(g), 2(a)–(f), and 1(f). (e)–(f) Similar to (a)–(d), but for the compression front and current sheet regions enclosed by the green and purple rectangles in Figures 1(c) and (g). The black lines are the best-fit DEM distributions, and the red, green, and blue rectangles separately represent the regions containing 50%, 51%–80%, and 81%–95% of the Monte Carlo solutions.
Paper: Failed Solar Eruption of a Multithermal Flux Rope
Authors: Leping Li, Hongqiang Song, Hardi Peter, Lakshmi Pradeep Chitta
Figure caption: Temporal evolution of the failed FR eruption. (a1)–(d1), (a2)–(d2), and (a3)–(d3) Time slices of AIA 94, 211, and 171 Å images and their composites along the blue, purple, and green lines AB, CD, and EF in Figures 1(e) and (f), respectively. The red lines in (a1)–(d1) and (a2) show the GOES-15 1–8 Å soft X-ray flux. The pink arrows in (a1)–(a2) mark the hot channel. The blue arrows in (b1)–(c1) and (b3)–(c3) denote the compression front. The green and cyan arrows in (b1)–(b3) and (c1)–(c3) mark the warm channel. The red and black arrows in (b2)–(c2) and (b3)–(c3) denote the loops.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. 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, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, 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, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Top: dependence of the normalized flux in the 2–8 keV energy band (blue points) on the pulse phase in the bright state of Cen X-3. The contribution from two single-pole components, C1 and C2, derived by Kraus et al. (1996) are shown with green and red dashed lines (see Section 4.3). Middle: dependence of the PD on phase from the spectropolarimetric analysis (blue points). The red dashed line represents the relative contributions of one of the poles (C2) to the total flux. Bottom: dependence of the PA on the pulse phase. The orange line corresponds to the best-fit rotating vector model (RVM; see Section 4.2).
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. 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, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, 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, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Corner plot of posterior distribution for the RVM parameters for the pulsar inclination angle i p fixed at the orbital inclination value of 70.°2. The contours correspond to two-dimensional 1σ, 2σ, and 3σ confidence levels. The histograms show normalized one-dimensional distribution for a given parameter derived from the posterior samples. The mean value and 1σ confidence interval for the derived parameters are presented above the corresponding histogram.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. 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, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, 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, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Schematic view of the system with the polarization mechanisms considered in this work. Different roman numerals correspond to (i) the intrinsic polarization from the hot spot, (ii) reflection from the NS surface, (iii) reflection from the accretion curtain, (iv) reflection from the accretion disk, (v) scattering by the stellar wind, and (vi) reflection by the optical companion.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. 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, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, 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, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Top: pulse time arrival delays with respect to constant period. Bottom: residuals for the best-fit models assuming ephemerides by Raichur & Paul (2010) in orange and the final timing solution obtained in this work for the second IXPE observation in blue.
Paper: On the Injection Scale of the Turbulence in the Partially Ionized Very Local Interstellar Medium
Authors: Siyao Xu, 思遥 徐, Hui Li, 晖 李
Figure caption: Illustration for turbulent eddies in super-Alfvénic (a) and sub-Alfvénic (b), (c) turbulence. Strong MHD turbulence is indicated by shaded regions. With anisotropic injection scale of turbulence in (c), the entire turbulent cascade can be in the strong turbulence regime. The blue line indicates the magnetic field.
Paper: Evidence of a Nonorthogonal X-line in Guide-field Magnetic Reconnection
Authors: Neha Pathak, R. E. Ergun, Y. Qi, S. J. Schwartz, T. Vo, M. E. Usanova, M. Hesse, T. D. Phan, J. F. Drake, S. Eriksson, N. Ahmadi, A. Chasapis, F. D. Wilder, J. E. Stawarz, J. L. Burch, K. J. Genestreti, R. B. Torbert, R. Nakamura
Figure caption: A zoomed-in view of the magnetic reconnection event. (a)  B  in LMN coordinates (written below the figure). (b)  V  Ion. (c)  V  Elc. (d)  J  derived from electron and ion distributions. (e)  E . (f) Electromagnetic energy transfer. (g) The electron density derived from the electron distribution.
Paper: Evidence of a Nonorthogonal X-line in Guide-field Magnetic Reconnection
Authors: Neha Pathak, R. E. Ergun, Y. Qi, S. J. Schwartz, T. Vo, M. E. Usanova, M. Hesse, T. D. Phan, J. F. Drake, S. Eriksson, N. Ahmadi, A. Chasapis, F. D. Wilder, J. E. Stawarz, J. L. Burch, K. J. Genestreti, R. B. Torbert, R. Nakamura
Figure caption: Overview of a magnetotail reconnection event on 2018 August 27. From top to bottom: (a)  B  in GSE coordinates, (b)  V  Ion, (c)  E , (d) omnidirectional ion flux from 70 to 600 keV, (e) differential ion energy flux from 3 eV to 25 keV, (f) omnidirectional electron flux from 60 to 500 keV, and (g) differential electron energy flux from 6 eV to 25 keV.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. 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, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, 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, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Variations of the phase-resolved normalized Stokes parameters q and u with pulsar phase in the 2–8 keV energy band averaged over all DUs (gray circles and arrows) measured in the bright state of Cen X-3. Each circle corresponds to a specific pulse phase, numbered following the binning shown in Figure 5. The circle size represents the uncertainty value. The phase-averaged values for the bright and low states are shown in red and blue, respectively.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. 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, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, 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, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Background-corrected light curves of Cen X-3 in the 2–8 keV energy bands summed over three modules of IXPE. Vertical dashed lines define good time intervals applied for the polarimetric analysis (see text for details). Times of eclipses of XRP by the optical companion are marked with vertical shaded regions. Observations performed in 2022 January and July are shown in the left and right panels, respectively.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. 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, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, 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, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Dependence of the phase-averaged normalized Stokes parameters q and u on energy in the bright state of Cen X-3. Solid, dashed, and dashed–dotted lines correspond to the 1σ, 2σ, and 3σ confidence levels, respectively. Data from the three telescope units were summed together.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. 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, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, 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, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Polarization vectors of Cen X-3 based on the spectral fitting of the pulse phase-resolved data in the bright state as a function of the phase. In each plot, the PD and PA confidence level contours at 1σ, 2σ, and 3σ (in red, green, and blue, respectively) are shown in polar coordinates for 10 different phase intervals.