adsabs/AstroCLIMB huggingface dataset:
Paper: Estimating Coronal Mass Ejection Mass and Kinetic Energy by Fusion of Multiple Deep-learning Models
Authors: Khalid A. Alobaid, Yasser Abduallah, Jason T. L. Wang, Haimin Wang, Shen Fan, Jialiang Li, Huseyin Cavus, Vasyl Yurchyshyn
Figure caption: Comparison between DeepCME and its three component models. Left column: performance metric values, displayed by bar charts, obtained by the four models in estimating the mass of CMEs. Right column: performance metric values obtained by the four models in estimating the kinetic energy of CMEs.
Paper: Estimating Coronal Mass Ejection Mass and Kinetic Energy by Fusion of Multiple Deep-learning Models
Authors: Khalid A. Alobaid, Yasser Abduallah, Jason T. L. Wang, Haimin Wang, Shen Fan, Jialiang Li, Huseyin Cavus, Vasyl Yurchyshyn
Figure caption: Scatterplots showing DeepCME’s predicted values vs. ground truth values in estimating the mass and kinetic energy, respectively, of CMEs.
Paper: Estimating Coronal Mass Ejection Mass and Kinetic Energy by Fusion of Multiple Deep-learning Models
Authors: Khalid A. Alobaid, Yasser Abduallah, Jason T. L. Wang, Haimin Wang, Shen Fan, Jialiang Li, Huseyin Cavus, Vasyl Yurchyshyn
Figure caption: Reliability assessment of DeepCME showing the performance of the model on reliable test data and unreliable test data, respectively.
Paper: Estimating Coronal Mass Ejection Mass and Kinetic Energy by Fusion of Multiple Deep-learning Models
Authors: Khalid A. Alobaid, Yasser Abduallah, Jason T. L. Wang, Haimin Wang, Shen Fan, Jialiang Li, Huseyin Cavus, Vasyl Yurchyshyn
Figure caption: Training and validation learning curves showing DeepCME is a well-fit model in estimating the mass and kinetic energy, respectively, of CMEs.
Paper: XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
Authors: María Claudia Ramírez-Tannus, Arjan Bik, Lars Cuijpers, Rens Waters, Christiane Göppl, Thomas Henning, Inga Kamp, Thomas Preibisch, Konstantin V. Getman, Germán Chaparro, Pablo Cuartas-Restrepo, Alex de Koter, Eric D. Feigelson, Sierra L. Grant, Thomas J. Haworth, Sebastián Hernández, Michael A. Kuhn, Giulia Perotti, Matthew S. Povich, Megan Reiter, Veronica Roccatagliata, Elena Sabbi, Benoît Tabone, Andrew J. Winter, Anna F. McLeod, Roy van Boekel, Sierk E. van Terwisga
Figure caption: Comparison between the gas line luminosities and spectral index n 13–25 of XUE 1 and the Spitzer sample studied by Banzatti et al. (2020) and the CO emission from Banzatti et al. (2022) (black circles). The y-axis shows the 17 μm H2O luminosity. From left to right the x-axis shows the ratio of HCN, C2H2, CO2, and CO to H2O luminosities. The x-axis of the rightmost panel shows the spectral index n 13–25, where the shaded region shows the location of disks with large gaps and/or cavities. The measurements for the JWST spectrum of XUE 1 are shown with the orange stars. The upper limits from Banzatti et al. (2020) and Banzatti et al. (2022) are indicated with gray arrows, and the open circles show the sources with upper limits in both the numerator and denominator. The yellow plus signs show the location of the MIRI spectra published to date: GW Lup (Grant et al. 2023), EX Lup (Kóspál et al. 2023), and PDS 70 (Perotti et al. 2023).
Paper: XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
Authors: María Claudia Ramírez-Tannus, Arjan Bik, Lars Cuijpers, Rens Waters, Christiane Göppl, Thomas Henning, Inga Kamp, Thomas Preibisch, Konstantin V. Getman, Germán Chaparro, Pablo Cuartas-Restrepo, Alex de Koter, Eric D. Feigelson, Sierra L. Grant, Thomas J. Haworth, Sebastián Hernández, Michael A. Kuhn, Giulia Perotti, Matthew S. Povich, Megan Reiter, Veronica Roccatagliata, Elena Sabbi, Benoît Tabone, Andrew J. Winter, Anna F. McLeod, Roy van Boekel, Sierk E. van Terwisga
Figure caption: Continuum-subtracted MIRI spectrum of XUE 1 (black) with the best-fit slab models. Molecules are shown with colors, and the purple shaded area shows the total model spectrum. Top: region between 4.9 and 5.35 μm including CO (brown) and H2O (blue). Bottom: region between 13 and 16 μm including H2O (blue), C2H2 (green), HCN (orange), and 12CO2 (red).
Paper: XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
Authors: María Claudia Ramírez-Tannus, Arjan Bik, Lars Cuijpers, Rens Waters, Christiane Göppl, Thomas Henning, Inga Kamp, Thomas Preibisch, Konstantin V. Getman, Germán Chaparro, Pablo Cuartas-Restrepo, Alex de Koter, Eric D. Feigelson, Sierra L. Grant, Thomas J. Haworth, Sebastián Hernández, Michael A. Kuhn, Giulia Perotti, Matthew S. Povich, Megan Reiter, Veronica Roccatagliata, Elena Sabbi, Benoît Tabone, Andrew J. Winter, Anna F. McLeod, Roy van Boekel, Sierk E. van Terwisga
Figure caption: MIRI MRS spectrum of XUE 1. The most prominent dust features are labeled. The insets show the P-branch transitions of the CO rovibrational fundamental band, the water emission around 7 μm, and the 13–15 μm region featuring C2H2, HCN, and 12CO2.
Paper: XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
Authors: María Claudia Ramírez-Tannus, Arjan Bik, Lars Cuijpers, Rens Waters, Christiane Göppl, Thomas Henning, Inga Kamp, Thomas Preibisch, Konstantin V. Getman, Germán Chaparro, Pablo Cuartas-Restrepo, Alex de Koter, Eric D. Feigelson, Sierra L. Grant, Thomas J. Haworth, Sebastián Hernández, Michael A. Kuhn, Giulia Perotti, Matthew S. Povich, Megan Reiter, Veronica Roccatagliata, Elena Sabbi, Benoît Tabone, Andrew J. Winter, Anna F. McLeod, Roy van Boekel, Sierk E. van Terwisga
Figure caption: Left: HST/ACS F850LP band image of the target position for XUE 1. The three point-like objects are marked by green circles with radii of 0.″1. The cyan circle on A1 marks the position of the Gaia DR3 source 5976051168205228416. The magenta circle (0.″5 radius) marks the position of the Chandra X-ray source. A grid of J2000 coordinates is shown. Right: MIRI F560W image (log intensity scale) of the target position for XUE 1. The white box marks the observed field of view with MRS. The optical positions of the three point-like objects A1, A2, and B are marked by green circles with radii of 0.″1.
Paper: XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
Authors: María Claudia Ramírez-Tannus, Arjan Bik, Lars Cuijpers, Rens Waters, Christiane Göppl, Thomas Henning, Inga Kamp, Thomas Preibisch, Konstantin V. Getman, Germán Chaparro, Pablo Cuartas-Restrepo, Alex de Koter, Eric D. Feigelson, Sierra L. Grant, Thomas J. Haworth, Sebastián Hernández, Michael A. Kuhn, Giulia Perotti, Matthew S. Povich, Megan Reiter, Veronica Roccatagliata, Elena Sabbi, Benoît Tabone, Andrew J. Winter, Anna F. McLeod, Roy van Boekel, Sierk E. van Terwisga
Figure caption: Rotation diagrams for the v = 1−0 (circles), v = 2−1 (triangles) bands. The dashed and dotted lines show linear fits to each vibrational level.
Paper: J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467
Authors: Shuo Huang, Ryohei Kawabe, Kotaro Kohno, Toshiki Saito, Shoichiro Mizukoshi, Daisuke Iono, Tomonari Michiyama, Yoichi Tamura, Christopher C. Hayward, Hideki Umehata
Figure caption: A multiwavelength view of J0107a: (a) the integrated 1D spectra of J0107a from ALMA Band 3/4 data. The channel widths are 50 km s−1. (b) Left: JWST/NIRCam color composite image (red: F356W; green: F200W; blue: F150W) of J0107a. Middle: F356W image with ALMA Band 7 continuum of J0107a (dark orange) and the zeroth-moment map of the Band 3 emission line from the z = 1.186 southwest (SW) spiral galaxy (magenta) overlaid. The insert panel shows the Band 3 spectrum of the SW spiral galaxy, with the line’s central frequency of 105.458 GHz marked with the gray dashed line. Right: Chandra ACIS-S 0.5–10 keV count image smoothed with a 0.″5 FWHM circular Gaussian kernel. Contours show the zeroth-moment maps of J0107a’s emission lines, with white, red, and blue for CO(3–2), CO(4–3), and [CI](1–0), respectively. Each panel is 5″ × 5″ in size. ALMA beam sizes are shown with the same colors as the contours. Contour levels are −2, 2, 4, 6, 8, 10... in the middle panel and −2, 2, 4, 8, 16... in the right panel.
Paper: J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467
Authors: Shuo Huang, Ryohei Kawabe, Kotaro Kohno, Toshiki Saito, Shoichiro Mizukoshi, Daisuke Iono, Tomonari Michiyama, Yoichi Tamura, Christopher C. Hayward, Hideki Umehata
Figure caption: Left: (a) 3″ × 3″ F444W cutout of J0107a displayed in the −2σ to 80σ range; (b) the ellipse isophote fit to J0107a (cyan); (c) the best-fit 2D parametric model of J0107a; (d) the residual of the best-fit model. During modeling processes, the two neighboring galaxies are masked. Right: radial surface brightness (SB, top), ellipticity (middle), and position angle (PA, bottom) distributions of J0107a. The vertical dashed line marks the spatial resolution in the F444W band.
Paper: The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX)
Authors: Chenxu Liu, Xinlei Chen, Xinzhong Er, Gregory R. Zeimann, József Vinkó, J. Craig Wheeler, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Karl Gebhardt, Helong Guo, Gary J. Hill, Lindsay House, Wolfram Kollatschny, Fanchuan Kong, Brajesh Kumar, Xiangkun Liu, Sarah Tuttle, Michael Endl, Parker Duke, William D. Cochran, Jinghua Zhang, Xiaowei Liu
Figure caption: The two-dimensional maps of the diffuse ISM extinction (E(B − V)ISM, top left panel), O abundance derived from the metal-rich branch of the R 23 method (middle left panel), and the surface density of the star formation rate (﹩\mathrm{log}{{\rm{\Sigma }}}_{\mathrm{SFR}}﹩, bottom left panel) centered on SN 2023ixf. Pixels with fiber coverage but not shown are because their nebular emission lines are not strong enough for reliable measurements of the extinction, O abundance, and the star formation rates, see contexts for details. Their variations as a function of the separations from SN 2023ixf are shown in the right panels. Data points in the right panels are associated with the individual pixels with measurements within the red circles in the left panels. The blue, orange, and green dashed lines in the right panels mark the median values of E(B − V)ISM, ﹩12+\mathrm{log}{({\rm{O}}/{\rm{H}})}_{\mathrm{upper}}﹩, and ﹩\mathrm{log}{{\rm{\Sigma }}}_{\mathrm{SFR}}﹩ of pixels within r < 1″, 3″, and 4.″5, respectively. The median values are also labeled in the upper left corners. The red solid lines in the right panels are simple linear fits to all pixels within r < 5.″5 (the red circles in the left panels) given to guide the eye to radial trends. In the middle right panel, both the O abundances derived from the metal-rich branch of the R 23 method (the solid upper triangles) and those derived from the metal-poor branch (open lower triangles) are shown.
Paper: The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX)
Authors: Chenxu Liu, Xinlei Chen, Xinzhong Er, Gregory R. Zeimann, József Vinkó, J. Craig Wheeler, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Karl Gebhardt, Helong Guo, Gary J. Hill, Lindsay House, Wolfram Kollatschny, Fanchuan Kong, Brajesh Kumar, Xiangkun Liu, Sarah Tuttle, Michael Endl, Parker Duke, William D. Cochran, Jinghua Zhang, Xiaowei Liu
Figure caption: The spectrum of the HETDEX pixel closest to SN 2023ixf. The top panel shows the spectrum in the full HETDEX wavelength range with the black data points. The red line is our best-fit spectrum consisting of the best-fit stellar continuum using BC03 templates and the best-fit emission lines. The blue dashed lines mark the emission lines. The six panels in the second and third rows show the subregions of the six emission lines: [O II] λ3727, Hδ, Hγ, Hβ, [O III] λ4959, and [O III] λ5007. The green lines are the best-fit stellar continuum in all seven panels. The gray curves in all panels of the bottom two rows are the HETDEX spectrum in each wavelength range. The black data points in the bottom two rows show the continuum-subtracted spectra. The magenta lines are the best-fit emission line profiles.
Paper: The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX)
Authors: Chenxu Liu, Xinlei Chen, Xinzhong Er, Gregory R. Zeimann, József Vinkó, J. Craig Wheeler, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Karl Gebhardt, Helong Guo, Gary J. Hill, Lindsay House, Wolfram Kollatschny, Fanchuan Kong, Brajesh Kumar, Xiangkun Liu, Sarah Tuttle, Michael Endl, Parker Duke, William D. Cochran, Jinghua Zhang, Xiaowei Liu
Figure caption: Color–magnitude diagram plotting 8 and 9 Myr PARSEC stellar evolutionary isochrones along with our progenitor candidate. The cyan point is the color–magnitude position measured from CFHTLS images. The solid lines present the isochrones of solar metallicity Z ☉ (the gas metallicity derived from the metal-rich branch using the R 23 method). The dashed lines present those of 0.25Z ☉ (the gas metallicity derived from the metal-poor branch using the R 23 method).
Paper: The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX)
Authors: Chenxu Liu, Xinlei Chen, Xinzhong Er, Gregory R. Zeimann, József Vinkó, J. Craig Wheeler, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Karl Gebhardt, Helong Guo, Gary J. Hill, Lindsay House, Wolfram Kollatschny, Fanchuan Kong, Brajesh Kumar, Xiangkun Liu, Sarah Tuttle, Michael Endl, Parker Duke, William D. Cochran, Jinghua Zhang, Xiaowei Liu
Figure caption: The CFHTLS image cutouts centered on SN 2023ixf. The six panels in the top two rows show the six individual z-band images. The bottom panels show the z-band coadded, the z-band background subtracted coadded, and the i-band background subtracted coadded images from left to right. The z-band observations were taken on 2006 June 7. The i-band observations were taken on 2005 May 11. The green and red circles mark the r < 1.″5 and r < 5.″5 regions of SN 2023ixf, respectively.
Paper: The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX)
Authors: Chenxu Liu, Xinlei Chen, Xinzhong Er, Gregory R. Zeimann, József Vinkó, J. Craig Wheeler, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Karl Gebhardt, Helong Guo, Gary J. Hill, Lindsay House, Wolfram Kollatschny, Fanchuan Kong, Brajesh Kumar, Xiangkun Liu, Sarah Tuttle, Michael Endl, Parker Duke, William D. Cochran, Jinghua Zhang, Xiaowei Liu
Figure caption: The ±30″ HETDEX image cutout centered on SN 2023ixf taken in the year of 2020. The image is created from the integrated flux within the wavelength range of [3550, 5450] Å. The pixel size is 1″ × 1″. The red circle shows the region of r < 5.″5, which is selected for the study of the local environments.
Paper: The First X-Ray Polarization Observation of the Black Hole X-Ray Binary 4U 1630–47 in the Steep Power-law State
Authors: Nicole Rodriguez Cavero, Lorenzo Marra, Henric Krawczynski, Michal Dovčiak, Stefano Bianchi, James F. Steiner, Jiri Svoboda, Fiamma Capitanio, Giorgio Matt, Michela Negro, Adam Ingram, Alexandra Veledina, Roberto Taverna, Vladimir Karas, Francesco Ursini, Jakub Podgorný, Ajay Ratheesh, Valery Suleimanov, Romana Mikušincová, Silvia Zane, Philip Kaaret, Fabio Muleri, Juri Poutanen, Christian Malacaria, Pierre-Olivier Petrucci, Ephraim Gau, Kun Hu, Sohee Chun, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, 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, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Paolo Soffitta, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, 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
Figure caption: Fits of 4U 1630–47 NICER and NuSTAR X-ray spectra for Period 1 (blue) and Period 2 (green): (a) Disk blackbody assumed as seed radiation for the power-law component (Fit 1). (b) Single temperature blackbody assumed as seed radiation for the power-law component (Fit 2). Unfolded spectra around the best-fitting model in F  E  representation, the total model (solid), the kerrbb contribution (dashed), and nthcomp (dotted) contribution for each data set are shown in the top panels while the data-model residuals in σ are shown in the bottom panels.
Paper: The First X-Ray Polarization Observation of the Black Hole X-Ray Binary 4U 1630–47 in the Steep Power-law State
Authors: Nicole Rodriguez Cavero, Lorenzo Marra, Henric Krawczynski, Michal Dovčiak, Stefano Bianchi, James F. Steiner, Jiri Svoboda, Fiamma Capitanio, Giorgio Matt, Michela Negro, Adam Ingram, Alexandra Veledina, Roberto Taverna, Vladimir Karas, Francesco Ursini, Jakub Podgorný, Ajay Ratheesh, Valery Suleimanov, Romana Mikušincová, Silvia Zane, Philip Kaaret, Fabio Muleri, Juri Poutanen, Christian Malacaria, Pierre-Olivier Petrucci, Ephraim Gau, Kun Hu, Sohee Chun, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, 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, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Paolo Soffitta, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, 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
Figure caption: (a) PD and (b) PA as a function of energy in the IXPE 2–8 keV energy range. Comparison of the 4U 1630–47 polarization properties in the HSS (black), reported in Paper I, and in the SPL Period 1 (blue) and Period 2 (green) discussed in this paper. Linear fits for PD and constant fit for PA are also shown in dotted lines (see the text for the fit details).
Paper: The First X-Ray Polarization Observation of the Black Hole X-Ray Binary 4U 1630–47 in the Steep Power-law State
Authors: Nicole Rodriguez Cavero, Lorenzo Marra, Henric Krawczynski, Michal Dovčiak, Stefano Bianchi, James F. Steiner, Jiri Svoboda, Fiamma Capitanio, Giorgio Matt, Michela Negro, Adam Ingram, Alexandra Veledina, Roberto Taverna, Vladimir Karas, Francesco Ursini, Jakub Podgorný, Ajay Ratheesh, Valery Suleimanov, Romana Mikušincová, Silvia Zane, Philip Kaaret, Fabio Muleri, Juri Poutanen, Christian Malacaria, Pierre-Olivier Petrucci, Ephraim Gau, Kun Hu, Sohee Chun, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, 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, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Paolo Soffitta, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, 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
Figure caption: Measured PD and PA of 4U 1630–47 in 5 logarithmic energy bins: 2.0–2.6, 2.6–3.5, 3.5–4.6, 4.6–6.1, and 6.1–8.0 keV. The black line and transparent contours show the polarization in the HSS reported in Paper I. The red solid line and solid contours show the polarization in the SPL state (this paper). The shaded and unshaded ellipses show their 68.3% and 99.7% confidence regions, respectively. Errors on PD and PA computed by IXPEOBSSIM are derived from the Q and U Gaussian errors according to the formalism developed by Kislat et al. (2015).