adsabs/AstroCLIMB huggingface dataset:
Paper: NICER, NuSTAR, and Insight-HXMT Views to the Newly Discovered Black Hole X-Ray Binary Swift J1727.8-1613
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Peng-Ju Wang, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan
Figure caption: The simultaneous broadband spectrum of Swift J1727.8–1613 is observed from NICER (black), NuSTAR/FPMA (red), NuSTAR/FPMB (green), Insight-HXMT/ME (blue), and Insight-HXMT/HE (cyan). Left panel: spectral fitting residuals for model 2. The bottom panel is the residual of model 2 after removing compTT. Right panel: spectral fitting residuals for model 3. The bottom panel is the residual of model 3 after removing cutoffpl.
Paper: NICER, NuSTAR, and Insight-HXMT Views to the Newly Discovered Black Hole X-Ray Binary Swift J1727.8-1613
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Peng-Ju Wang, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan
Figure caption: Spectral fitting residuals for different models. The black, red, green, and blue points represent spectral residuals from NuSTAR FPMA, FPMB and Insight-HXMT ME, HE respectively.
Paper: NICER, NuSTAR, and Insight-HXMT Views to the Newly Discovered Black Hole X-Ray Binary Swift J1727.8-1613
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Peng-Ju Wang, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan
Figure caption: The MAXI HID of Swift J1727.8–1613 with time bin 1 day, where the hardness is defined as the ratio of 4–10 keV to 2–4 keV count rate. The red dot is the time of the observation in Table 1.
Paper: NICER, NuSTAR, and Insight-HXMT Views to the Newly Discovered Black Hole X-Ray Binary Swift J1727.8-1613
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Peng-Ju Wang, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan
Figure caption: An illustration of one- and two-dimensional projections of the posterior probability distributions derived from the MCMC analysis for the parameters in M1*.
Paper: NICER, NuSTAR, and Insight-HXMT Views to the Newly Discovered Black Hole X-Ray Binary Swift J1727.8-1613
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Peng-Ju Wang, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan
Figure caption: An illustration of one- and two-dimensional projections of the posterior probability distributions derived from the MCMC analysis for the parameters in M1.
Paper: Dependences of Energetic Neutral Atoms Energy on the Solar Wind Energy and Solar Zenith Angle Observed by the Chang’E-4 Rover
Authors: Tianhua Zhong, Lianghai Xie, Aibing Zhang, Xiaocheng Guo, Lei Li, Wenjing Wang, Martin Wieser, Xiaoping Zhang, Yazhou Yang, Hong Tang, Yiteng Zhang, Chi Wang
Figure caption: (a) The dependence of the energy loss rate (R  E ) on the solar wind energy (E SW); (b) the dependence of the energy loss rate (R  E ) on the solar zenith angle (SZA). Red dots represent the results of ASAN observations, with red lines obtained from the power fitting. Green dots and lines indicate the results of SDTrimSP simulations, with an SZA of 63.63°" in (a) and an E SW of 776 eV in (b). The blue lines are derived from the empirical function proposed by Futaana et al. (2012).
Paper: Dependences of Energetic Neutral Atoms Energy on the Solar Wind Energy and Solar Zenith Angle Observed by the Chang’E-4 Rover
Authors: Tianhua Zhong, Lianghai Xie, Aibing Zhang, Xiaocheng Guo, Lei Li, Wenjing Wang, Martin Wieser, Xiaoping Zhang, Yazhou Yang, Hong Tang, Yiteng Zhang, Chi Wang
Figure caption: Black circles: the normalized hydrogen ENA energy spectrum observed by the ASAN during 09:31–10:36 UTC on 2019 May 30. Dotted line: the 90% confidence sensitivity limit below which a signal can not be distinguished from background. Red squares: the normalized ENA energy spectrum measured by CENA (Futaana et al. 2012). Green and blue diamonds: the normalized ENA energy spectrum observed by IBEX-Hi and IBEX-Lo, respectively (Allegrini et al. 2013). Vertical line: division line at 150 eV relative to the ASAN spectrum.
Paper: Dependences of Energetic Neutral Atoms Energy on the Solar Wind Energy and Solar Zenith Angle Observed by the Chang’E-4 Rover
Authors: Tianhua Zhong, Lianghai Xie, Aibing Zhang, Xiaocheng Guo, Lei Li, Wenjing Wang, Martin Wieser, Xiaoping Zhang, Yazhou Yang, Hong Tang, Yiteng Zhang, Chi Wang
Figure caption: SDTrimSP simulation results: (a) green, red, and blue lines indicate the dependences of the total, nuclear, and electronic energy losses per unit depth, respectively, on the depth, with an incident energy of 1000 eV and an SZA of 60°; (b) red and blue dots indicate the dependences of the mean path length and the mean implantation depth, respectively, on the incident H ions energy, with an SZA of 63.63°"; (c) red and blue dots indicate the dependences of the mean path length and the mean implantation depth, respectively, on the SZA, with an incident energy of 956.13 eV. Note that the Y-axis scales are not starting at 0.
Paper: Dependences of Energetic Neutral Atoms Energy on the Solar Wind Energy and Solar Zenith Angle Observed by the Chang’E-4 Rover
Authors: Tianhua Zhong, Lianghai Xie, Aibing Zhang, Xiaocheng Guo, Lei Li, Wenjing Wang, Martin Wieser, Xiaoping Zhang, Yazhou Yang, Hong Tang, Yiteng Zhang, Chi Wang
Figure caption: The dependence of the mean ENA energy on the solar wind energy. Red dots and blue dots represent the mean ENA energies measured in the local morning and in the local afternoon, respectively, with a lower energy limit of 150 eV. Different colored lines represent the fitting lines of different measurements.
Paper: Evidence for a Redshifted Excess in the Intracluster Light Fractions of Merging Clusters at z ∼ 0.8
Authors: Yolanda Jiménez-Teja, Renato A. Dupke, Paulo A. A. Lopes, Paola Dimauro
Figure caption: Rest-frame ICL fractions of ACT0102 (black squares) and CL0152 (black diamonds), compared with those of dynamically active, intermediate-redshift clusters (red symbols). The electromagnetic spectrum is split into six intervals according to the emission peaks of the different stellar types, labeled with gray letters on the top. Black lines indicate the error-weighted mean for each subsample and the shaded regions represent the mean of the errors, calculated within each stellar type interval (the K-type interval has been divided in two given its width and the number of measurements that are located in it).
Paper: Evidence for a Redshifted Excess in the Intracluster Light Fractions of Merging Clusters at z ∼ 0.8
Authors: Yolanda Jiménez-Teja, Renato A. Dupke, Paulo A. A. Lopes, Paola Dimauro
Figure caption: Rest-frame ICL fractions of ACT0102 (black squares) and CL0152 (black circles), compared with those of intermediate-redshift clusters. The comparison sample spans the redshift interval 0.18 < z < 0.57 and gathers the ICL fractions calculated by Jiménez-Teja et al. (2018, 2021) and de Oliveira et al. (2022). Clusters represented with blue symbols are characterized by its passive dynamical stage, while those plotted with red markers are merging systems. Shadowed regions indicate the error-weighted average of the ICL fractions for the two subsamples of relaxed and merging clusters.
Paper: Evidence for a Redshifted Excess in the Intracluster Light Fractions of Merging Clusters at z ∼ 0.8
Authors: Yolanda Jiménez-Teja, Renato A. Dupke, Paulo A. A. Lopes, Paola Dimauro
Figure caption: ICL spatial distribution in the F105W band (rest frame ∼5750 Å at z = 0.85). We plot the ICL isocontours over the original HST mosaics of ACT0102 (left) and CL0152 (right) in the F105W band.
Paper: 4FGL J1318.2+6754: A Long Orbital-period Redback Candidate
Authors: Jie Lin, Hailiang Chen, Bojun Wang, Renxin Xu
Figure caption: The TESS light curves for J1318 from 2019 July to 2022 February. The Lomb–Scargle periodogram of the entire data set for TESS, showing a clear peak around 4.13 days.
Paper: 4FGL J1318.2+6754: A Long Orbital-period Redback Candidate
Authors: Jie Lin, Hailiang Chen, Bojun Wang, Renxin Xu
Figure caption: The Digitized Sky Survey (DSS) image of 4FGL J1318.2+6754. The red and blue ellipses show a 68% error ellipse and 95% error ellipse of the 4FGL catalog, respectively. The small pink plus is the position determined by the SB1 of Gaia DR3, which is located at a 95% confidence level of 4FGL J1318.2+6754.
Paper: 4FGL J1318.2+6754: A Long Orbital-period Redback Candidate
Authors: Jie Lin, Hailiang Chen, Bojun Wang, Renxin Xu
Figure caption: The Lomb–Scargle periodogram of the TESS light curve for different epochs. The dashed blue line is the orbital period obtained by he entire data set, while the dashed green line is the harmonic of the orbital period.
Paper: 4FGL J1318.2+6754: A Long Orbital-period Redback Candidate
Authors: Jie Lin, Hailiang Chen, Bojun Wang, Renxin Xu
Figure caption: TESS optical photometry of J1318 in 2019 August. The red lines show the best-fit ELC code model. Bottom panel shows residuals for the difference between the observed and calculated magnitudes.
Paper: 4FGL J1318.2+6754: A Long Orbital-period Redback Candidate
Authors: Jie Lin, Hailiang Chen, Bojun Wang, Renxin Xu
Figure caption: Top: the mid-resolution LAMOST spectra of the blue arms are shown. Middle: the mid-resolution LAMOST spectra of the red arms are shown. Bottom: a model spectrum in the blue arms using the atmospheric parameters derived from iSpec is shown in green.
Paper: 4FGL J1318.2+6754: A Long Orbital-period Redback Candidate
Authors: Jie Lin, Hailiang Chen, Bojun Wang, Renxin Xu
Figure caption: The observed radial velocities for J1318 as a function of the orbital phase obtained in four epochs from LAMOST, with the radial-velocity solution of Gaia DR3 plotted.
Paper: 4FGL J1318.2+6754: A Long Orbital-period Redback Candidate
Authors: Jie Lin, Hailiang Chen, Bojun Wang, Renxin Xu
Figure caption: The best-fitting SED model for J1318 after fixing the extinction parameters A v = 0. The black curve is the best-fitting model. The green pluses and circles are the retrieved photometric measures. The blue diamonds are synthetic photometry.
Paper: Semimajor-axis Jumps as the Activity Trigger in Centaurs and High-perihelion Jupiter-family Comets
Authors: Eva Lilly, Peter Jevčák, Charles Schambeau, Kat Volk, Jordan Steckloff, Henry Hsieh, Yanga R. Fernandez, James Bauer, Robert Weryk, Richard J. Wainscoat
Figure caption: Orbital history of two active Centaurs at the opposite edges of Centaur region—167P (top panel) and LD2 (bottom panel). The left y-axis shows the semimajor axis, and the right y-axis shows perihelion distance. Both nominal orbit and clones are depicted with lines of the same color. LD2 has experienced multiple close encounters with Jupiter, leading to substantial orbital changes, and is an example of a Centaur with prominent a-jumps. Such close encounters introduce chaos leading to clone divergence and difficulty in assessing the orbital parameters of LD2 before ∼1800 and after ∼2125. Bottom panel: the dynamical evolution of 167P in the past 5000 years for the nominal orbit (orange) and 50 orbital clones (blue). The clones of 167P follow essentially identical evolution down to 1800 yr ago, when they diverge owing to a wider encounter with Saturn, after which the semimajor axis started to drift inward. 167P is an example of a “drifter” Centaur. The arrow denotes part of the orbital history where the heliocentric distance R  o  is determined.
Paper: Semimajor-axis Jumps as the Activity Trigger in Centaurs and High-perihelion Jupiter-family Comets
Authors: Eva Lilly, Peter Jevčák, Charles Schambeau, Kat Volk, Jordan Steckloff, Henry Hsieh, Yanga R. Fernandez, James Bauer, Robert Weryk, Richard J. Wainscoat
Figure caption: (a) Surface temperature evolution, (c) evolution of the interior’s temperature profile, and (e) the interior radial profile for temperature during three different perihelion passages of 167P—just before its 1898 a-jump, in 1938, and during its last perihelion passage in 2003 April, before its 2004 August discovery while active. The light-blue shaded region displays the AWI crystallization temperature regime (∼90–160 K) containing all three temperature profiles for 167P. Right column: same quantities as in left column, but for LD2. A more pronounced temperature change can be seen for LD2 owing to the more significant a-jump (panel (b)). The temperatures reached for LD2's interior are higher owing to its orbit being closer to and now interior to Jupiter’s (panel (d)). The shaded regions in panel (f) indicate thermal regimes for different proposed activity drivers: AWI crystallization between 90 and 160 K (light blue), beginnings of water-ice sublimation at ∼170 K (coral), and beginnings of vigorous water-ice sublimation at ∼180 K (light red). The temperature evolution displayed pre− and post−a-jump may display a transition between activity-driving mechanisms in play for LD2.
Paper: Semimajor-axis Jumps as the Activity Trigger in Centaurs and High-perihelion Jupiter-family Comets
Authors: Eva Lilly, Peter Jevčák, Charles Schambeau, Kat Volk, Jordan Steckloff, Henry Hsieh, Yanga R. Fernandez, James Bauer, Robert Weryk, Richard J. Wainscoat
Figure caption: (a) Most recent a-jumps—changes in semimajor axis accompanied by changes in eccentricity (panel (b)) evident in the orbital evolution of selected known active Centaurs compared to a typical recent evolution of two inactive Centaurs (2013 JX14 and 2003 QD112) without the a-jump feature (black dotted lines). Some objects can undergo several a-jumps in a row. Time is relative to the epoch of orbit for integration. Only nominal orbits are shown for clarity. (c) Percent change in the average per-orbit insolation of active Centaurs caused by the object’s most recent a-jump as a function of its pre−a-jump perihelion distance. (d) Percent changes in the average per-orbit insolation of inactive Centaurs caused by the object’s largest variation in semimajor axis and eccentricity as a function of its pre−a-jump perihelion distance.
Paper: Semimajor-axis Jumps as the Activity Trigger in Centaurs and High-perihelion Jupiter-family Comets
Authors: Eva Lilly, Peter Jevčák, Charles Schambeau, Kat Volk, Jordan Steckloff, Henry Hsieh, Yanga R. Fernandez, James Bauer, Robert Weryk, Richard J. Wainscoat
Figure caption: Left panels: percent change in semimajor axis from an object’s most recent a-jump as a function of its post−a-jump perihelion distance, where the gray horizontal region signifies the average amplitude of variations in a for known inactive Centaurs (top); percent changes in eccentricity and semimajor axis (middle); percent changes in perihelion distance and semimajor axis (bottom). Right panels, top to bottom: distribution of percent change in semimajor axis, eccentricity, and perihelion distance for active and inactive Centaurs and high-perihelion JFCs. All depicted changes were fueled by the object’s most recent a-jump in case of active bodies, or the highest amplitude change in the given element over the inspected time period.
Paper: Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1
Authors: Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Matteo Bachetti, Sara Elisa Motta, Alessandro Papitto, Maura Pilia, Fei Xie, Stefano Bianchi, Anna Bobrikova, Enrico Costa, Wei Deng, Ming-Yu Ge, Giulia Illiano, Shu-Mei Jia, Henric Krawczynski, Eleonora Veronica Lai, Kuan Liu, Guglielmo Mastroserio, Fabio Muleri, John Rankin, Paolo Soffitta, Alexandra Veledina, Filippo Ambrosino, Melania Del Santo, Wei Chen, Javier A. Garcia, Philip Kaaret, Thomas D. Russell, Wen-Hao Wei, Shuang-Nan Zhang, Chao Zuo, Zaven Arzoumanian, Massimo Cocchi, Andrea Gnarini, Ruben Farinelli, Keith Gendreau, Francesco Ursini, Martin C. Weisskopf, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, 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, Kinwah Wu
Figure caption: Bartlett (1948)–like periodogram from the last 805 s of NICER ObsID 6689010102, obtained by averaging 100 periodograms from 8 s segments of the light curve, normalized as in Leahy et al. (1983) in gray and rebinned geometrically (factor 1.02) to improve the signal-to-noise ratio at high frequencies (black). In blue, we plot the best-fit model consisting of a Poisson noise level, significantly below 2 due to dead time; a power-law red-noise component at low frequencies; and a QPO.
Paper: Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1
Authors: Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Matteo Bachetti, Sara Elisa Motta, Alessandro Papitto, Maura Pilia, Fei Xie, Stefano Bianchi, Anna Bobrikova, Enrico Costa, Wei Deng, Ming-Yu Ge, Giulia Illiano, Shu-Mei Jia, Henric Krawczynski, Eleonora Veronica Lai, Kuan Liu, Guglielmo Mastroserio, Fabio Muleri, John Rankin, Paolo Soffitta, Alexandra Veledina, Filippo Ambrosino, Melania Del Santo, Wei Chen, Javier A. Garcia, Philip Kaaret, Thomas D. Russell, Wen-Hao Wei, Shuang-Nan Zhang, Chao Zuo, Zaven Arzoumanian, Massimo Cocchi, Andrea Gnarini, Ruben Farinelli, Keith Gendreau, Francesco Ursini, Martin C. Weisskopf, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, 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, Kinwah Wu
Figure caption: Spectral residuals in the energy range 5.5–7.5 keV for the Sco X-1 observations with NuSTAR-FPMA (top), NICER (center), and IXPE-DU1 (bottom), when the spectral model which represents the continuum, without any component describing the Fe line complex. The NuSTAR and NICER data show an excess compatible with a broad iron line, indistinguishable in the IXPE spectrum due to its limited spectral capabilities.
Paper: Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1
Authors: Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Matteo Bachetti, Sara Elisa Motta, Alessandro Papitto, Maura Pilia, Fei Xie, Stefano Bianchi, Anna Bobrikova, Enrico Costa, Wei Deng, Ming-Yu Ge, Giulia Illiano, Shu-Mei Jia, Henric Krawczynski, Eleonora Veronica Lai, Kuan Liu, Guglielmo Mastroserio, Fabio Muleri, John Rankin, Paolo Soffitta, Alexandra Veledina, Filippo Ambrosino, Melania Del Santo, Wei Chen, Javier A. Garcia, Philip Kaaret, Thomas D. Russell, Wen-Hao Wei, Shuang-Nan Zhang, Chao Zuo, Zaven Arzoumanian, Massimo Cocchi, Andrea Gnarini, Ruben Farinelli, Keith Gendreau, Francesco Ursini, Martin C. Weisskopf, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, 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, Kinwah Wu
Figure caption: In these plots, the Sco X-1 polarization in different energy bins, as measured with PCUBE in IXPEOBSSIM, is reported. (a) Normalized Stokes parameters plane in 1 keV energy bins: Q/I vs. U/I. (b) Polar plot of the X-ray polarization when 1 keV binning is applied; contours are given at 68% CL. No trend of polarization varying with energy is visible in either (a) or (b). (c) Polar plot of the X-ray polarization in the 3–8 keV energy band; contours correspond to 50%, 95%, and 99% CL. The detection significance of the energy averaged polarization is at ∼7σ CL.