adsabs/AstroCLIMB huggingface dataset:
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: JWST (blue), HST (blue), VLT (red and magenta), and ALMA (yellow) composite image of NGC 1300. SN 2022acko lies in a star-forming region in a spiral arm northeast of the nucleus and is marked in both the image and the inset with white ticks. Image adapted from M. Hakan Özsaraç and Alyssa Pagan, NASA, ESA, ESO-Chile, ALMA, NAOJ, NRAO; north is up, and east is right.
Paper: Deuterium Escape on Photoevaporating Sub-Neptunes
Authors: Pin-Gao Gu, Howard Chen
Figure caption: Dependence of D/H evolution on the free parameters η, K  zz , and T  h . The solid curves illustrate the typical evolution with the fiducial parameters shown in Figure 1, while the dashed and dotted curves present those with other values of free parameters. The curve for η = 0.75 in the case of f env = 0.005 is not plotted in the upper left panel due to the unphysical radius anomaly in the simulation. The evolution is insensitive to the free parameters except in extreme cases for the high photoevaporation efficiency η = 0.75 shown in the lower left panel, where the D/H value of the massive sub-Neptune with an initial thin atmosphere (e.g., f env = 0.005 and M  p  = 10 M ⊕) can be more enhanced at t = 7.5 Gyr due to the faster diffusive escapes of both H and D during the late stage, when t ≳ 1–2 Gyr.
Paper: IXPE and Multiwavelength Observations of Blazar PG 1553+113 Reveal an Orphan Optical Polarization Swing
Authors: Riccardo Middei, Matteo Perri, Simonetta Puccetti, Ioannis Liodakis, Laura Di Gesu, Alan P. Marscher, Nicole Rodriguez Cavero, Fabrizio Tavecchio, Immacolata Donnarumma, Marco Laurenti, Svetlana G. Jorstad, Iván Agudo, Herman L. Marshall, Luigi Pacciani, Dawoon E. Kim, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Beatriz Agís-González, Alfredo Sota, Carolina Casadio, Juan Escudero, Ioannis Myserlis, Albrecht Sievers, Pouya M. Kouch, Elina Lindfors, Mark Gurwell, Garrett K. Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sang-Hyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Emmanouil Angelakis, Alexander Kraus, 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, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Alessandro Di Marco, 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, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, 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: Multiwavelength radio and optical observations of PG 1553+113. Panel (a) shows the brightness in magnitudes, panel (b) the polarization degree, panel (c) the polarization angle, and panel (d) the γ-ray light curve in the 0.1–100 GeV range. The gray shaded areas mark the two intervals of IXPE observations. The error bars represent 1σ uncertainties. Pink boxes identify the ψ X best-fit value and its 1σ uncertainty as derived using IXPE. Panel (d) displays the photon flux observed by the Fermi Area Telescope during the IXPE monitoring of the source. The photon flux is in units of 10−7 photons s−1 cm−2 (see Abdollahi et al. 2023, for details of the Fermi light curve).
Paper: IXPE and Multiwavelength Observations of Blazar PG 1553+113 Reveal an Orphan Optical Polarization Swing
Authors: Riccardo Middei, Matteo Perri, Simonetta Puccetti, Ioannis Liodakis, Laura Di Gesu, Alan P. Marscher, Nicole Rodriguez Cavero, Fabrizio Tavecchio, Immacolata Donnarumma, Marco Laurenti, Svetlana G. Jorstad, Iván Agudo, Herman L. Marshall, Luigi Pacciani, Dawoon E. Kim, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Beatriz Agís-González, Alfredo Sota, Carolina Casadio, Juan Escudero, Ioannis Myserlis, Albrecht Sievers, Pouya M. Kouch, Elina Lindfors, Mark Gurwell, Garrett K. Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sang-Hyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Emmanouil Angelakis, Alexander Kraus, 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, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Alessandro Di Marco, 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, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, 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 and XMM-Newton data and corresponding residuals. On the left, we show the model const×polconst×logpar fitting the I Stokes spectra, while on the right the best-fit Q and U Stokes spectra are shown. Bottom panels: regions accounting for 68%, 90%, and 99% confidence levels computed using the full IXPE 2–8 keV data (bottom left) or taking into account the IXPE I, Q, and U Stokes spectra only in the 2–5.5 keV range.
Paper: IXPE and Multiwavelength Observations of Blazar PG 1553+113 Reveal an Orphan Optical Polarization Swing
Authors: Riccardo Middei, Matteo Perri, Simonetta Puccetti, Ioannis Liodakis, Laura Di Gesu, Alan P. Marscher, Nicole Rodriguez Cavero, Fabrizio Tavecchio, Immacolata Donnarumma, Marco Laurenti, Svetlana G. Jorstad, Iván Agudo, Herman L. Marshall, Luigi Pacciani, Dawoon E. Kim, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Beatriz Agís-González, Alfredo Sota, Carolina Casadio, Juan Escudero, Ioannis Myserlis, Albrecht Sievers, Pouya M. Kouch, Elina Lindfors, Mark Gurwell, Garrett K. Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sang-Hyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Emmanouil Angelakis, Alexander Kraus, 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, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Alessandro Di Marco, 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, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, 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 PG 1553+113. Fluxes F IXPE, F Soft, and F Hard are computed in the 2–8, 0.5–2, and 2–10 keV bands, respectively, and are displayed in units of 10−11 erg cm−2 s−1. “HR” is the hardness ratio, defined as (F Hard − F Soft)/(F Hard + F Soft). Gray shaded areas mark the durations of the two IXPE observations, intervals a (left) and b (right). Black data points account for the different quantities measured by IXPE and quoted in Table 2.
Paper: A Broken “α–intensity” Relation Caused by the Evolving Photosphere Emission and the Nature of the Extraordinarily Bright GRB 230307A
Authors: Yun Wang, Zi-Qing Xia, Tian-Ci Zheng, Jia Ren, Yi-Zhong Fan
Figure caption: Observational data and parameter evolution of GRB 220307A. The first panel shows the light curve of GRB 060614, the well-known long-short burst (i.e., a long-duration GRB from a compact object merger). The second panel shows the light curves of GRB 220307A and the Bayesian block in the black and red solid line, respectively. The next three panels are the evolution of α, E p, and energy flux (1–10,000 keV), where orange represents the Band-model results and blue represents the CPL-model results. The slashed region in each panel indicates the time interval of TTE data losses.
Paper: A Broken “α–intensity” Relation Caused by the Evolving Photosphere Emission and the Nature of the Extraordinarily Bright GRB 230307A
Authors: Yun Wang, Zi-Qing Xia, Tian-Ci Zheng, Jia Ren, Yi-Zhong Fan
Figure caption: The α–F relation (left panel) and the F–E p relation (right panel) for the CPL-model samples of GRB 230307A. In the left panel: the Fermi-GBM samples with α exceeding the synchrotron limit (α = − 2/3, the gray dashed line) are marked in purple, and the others are in blue. The Konus-Wind data point, measured at the peak time, is marked in orange. The black/red/green lines correspond to the best-fit log-linear/broken log-linear/smoothly broken PL model for the α–F relation, respectively. In the right panel: the black line corresponds to the best-fit PL model we obtained for the α–F relation.
Paper: A Broken “α–intensity” Relation Caused by the Evolving Photosphere Emission and the Nature of the Extraordinarily Bright GRB 230307A
Authors: Yun Wang, Zi-Qing Xia, Tian-Ci Zheng, Jia Ren, Yi-Zhong Fan
Figure caption: The ν F  ν  spectra of GRB 230307A at three special time intervals. From left to right in the top row panel, the photon spectrum used in the first two time intervals is the mBB+PL model, and the last one is the CPL model. The distributions of posterior parameters for each model are presented in the bottom panels.
Paper: ExoGemS Detection of a Metal Hydride in an Exoplanet Atmosphere at High Spectral Resolution
Authors: Laura Flagg, Jake D. Turner, Emily Deibert, Andrew Ridden-Harper, Ernst de Mooij, Ryan J. MacDonald, Ray Jayawardhana, Neale Gibson, Adam Langeveld, David Sing
Figure caption: The CCFs at the predicted k  p  (in purple) for WASP-31b along with the 99% and 99.9% ranges for 							the bootstrap sampling, with GRACES on the left and UVES on the right. 							On the top row, we plot the raw CCF values, which shows the nature of 							the systematics for each instrument, while the bottom row shows the CCF 							values with the median from the bootstrap sample at each specific 								v sys subtracted. Assuming a Gaussian distribution, these are 							equivalent to 3.9σ and 3.5σ detection respectively on their own, and a 								5.6σ detection when the probabilities 							are combined.
Paper: ExoGemS Detection of a Metal Hydride in an Exoplanet Atmosphere at High Spectral Resolution
Authors: Laura Flagg, Jake D. Turner, Emily Deibert, Andrew Ridden-Harper, Ernst de Mooij, Ryan J. MacDonald, Ray Jayawardhana, Neale Gibson, Adam Langeveld, David Sing
Figure caption: The S/N of the injected signal in the ΔCCF matrix as a function of 							components removed for GRACES (top) and UVES (bottom). The plus signal 							indicates additional components removed after the barycentric correction 							to better remove the stellar signal.
Paper: ExoGemS Detection of a Metal Hydride in an Exoplanet Atmosphere at High Spectral Resolution
Authors: Laura Flagg, Jake D. Turner, Emily Deibert, Andrew Ridden-Harper, Ernst de Mooij, Ryan J. MacDonald, Ray Jayawardhana, Neale Gibson, Adam Langeveld, David Sing
Figure caption: The CCF matrices from GRACES (top), the first transit with UVES (middle, 							left), the second transit with UVES (middle, right), and both UVES 							transits combined (bottom). For the three transits, we detect CrH at a 								3.9σ, 3.7σ, and 3.6σ level, 							respectively, while CrH is detected at a 4.2σ level for the UVES combined data set. The white dashed 							lines, indicating the systemic velocity of the system and the expected 							velocity amplitude of the planet (Table 1), cross at the expected location of the 							planet’s signal. The red lines indicate the peaks’ center positions.
Paper: ExoGemS Detection of a Metal Hydride in an Exoplanet Atmosphere at High Spectral Resolution
Authors: Laura Flagg, Jake D. Turner, Emily Deibert, Andrew Ridden-Harper, Ernst de Mooij, Ryan J. MacDonald, Ray Jayawardhana, Neale Gibson, Adam Langeveld, David Sing
Figure caption: The original (top) and filtered CrH template (bottom). The wavelength 							range use, chosen because of the relatively strong CrH lines with 							minimal telluric contamination, is highlighted in purple.
Paper: ExoGemS Detection of a Metal Hydride in an Exoplanet Atmosphere at High Spectral Resolution
Authors: Laura Flagg, Jake D. Turner, Emily Deibert, Andrew Ridden-Harper, Ernst de Mooij, Ryan J. MacDonald, Ray Jayawardhana, Neale Gibson, Adam Langeveld, David Sing
Figure caption: Cross-correlating our template with the spectra of a very low-mass star 							yields a clear signal in orders where CrH is expected to be present (red 							lines, covering wavelengths longer than 860 nm) and not the orders where 							it would not be present (blue lines).
Paper: ExoGemS Detection of a Metal Hydride in an Exoplanet Atmosphere at High Spectral Resolution
Authors: Laura Flagg, Jake D. Turner, Emily Deibert, Andrew Ridden-Harper, Ernst de Mooij, Ryan J. MacDonald, Ray Jayawardhana, Neale Gibson, Adam Langeveld, David Sing
Figure caption: One order of the reduced spectra from GRACES (top), with the main stellar and 						telluric signal divided out (middle), and after SVD processing (bottom).
Paper: First Detection of X-Ray Polarization from the Accreting Neutron Star 4U 1820−303
Authors: Alessandro Di Marco, Fabio La Monaca, Juri Poutanen, Thomas D. Russell, Alessio Anitra, Ruben Farinelli, Guglielmo Mastroserio, Fabio Muleri, Fei Xie, Matteo Bachetti, Luciano Burderi, Francesco Carotenuto, Melania Del Santo, Tiziana Di Salvo, Michal Dovčiak, Andrea Gnarini, Rosario Iaria, Jari J. E. Kajava, Kuan Liu, Riccardo Middei, Stephen L. O'Dell, Maura Pilia, John Rankin, Andrea Sanna, Jakob van den Eijnden, Martin C. Weisskopf, Anna Bobrikova, Fiamma Capitanio, Enrico Costa, Philip Kaaret, Alessio Marino, Paolo Soffitta, Francesco Ursini, Filippo Ambrosino, Massimo Cocchi, Sergio Fabiani, Herman L. Marshall, Giorgio Matt, Sara Elisa Motta, Alessandro Papitto, Luigi Stella, Antonella Tarana, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, 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, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, 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: Polar plot of the X-ray polarization in 4U 1820−303. (a) Contours at 99% CL in the 2–4 keV energy bin, for the first (red) and the second (green) observations. (b) Same as (a), but in the 4–8 keV energy bin. (c) Combined data in the three energy bins 2–4, 4–7, and 7–8 keV. The contours correspond to 50%, 95%, and 99% CL.
Paper: First Detection of X-Ray Polarization from the Accreting Neutron Star 4U 1820−303
Authors: Alessandro Di Marco, Fabio La Monaca, Juri Poutanen, Thomas D. Russell, Alessio Anitra, Ruben Farinelli, Guglielmo Mastroserio, Fabio Muleri, Fei Xie, Matteo Bachetti, Luciano Burderi, Francesco Carotenuto, Melania Del Santo, Tiziana Di Salvo, Michal Dovčiak, Andrea Gnarini, Rosario Iaria, Jari J. E. Kajava, Kuan Liu, Riccardo Middei, Stephen L. O'Dell, Maura Pilia, John Rankin, Andrea Sanna, Jakob van den Eijnden, Martin C. Weisskopf, Anna Bobrikova, Fiamma Capitanio, Enrico Costa, Philip Kaaret, Alessio Marino, Paolo Soffitta, Francesco Ursini, Filippo Ambrosino, Massimo Cocchi, Sergio Fabiani, Herman L. Marshall, Giorgio Matt, Sara Elisa Motta, Alessandro Papitto, Luigi Stella, Antonella Tarana, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, 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, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, 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: Swift-XRT HR in time bins of 100 s during the first (left, we used ObsIDs: 00014980028, 00014980029, 00014980030, and 00014980031) and the second (right, we used ObsIDs: 00014980055, 00014980056, and 00014980057) IXPE coordinated observations. The horizontal gray band reports the average 99% CL HR interval during the two observations; the vertical bands and/or horizontal arrows report the time intervals when observations by other observatories were performed.
Paper: First Detection of X-Ray Polarization from the Accreting Neutron Star 4U 1820−303
Authors: Alessandro Di Marco, Fabio La Monaca, Juri Poutanen, Thomas D. Russell, Alessio Anitra, Ruben Farinelli, Guglielmo Mastroserio, Fabio Muleri, Fei Xie, Matteo Bachetti, Luciano Burderi, Francesco Carotenuto, Melania Del Santo, Tiziana Di Salvo, Michal Dovčiak, Andrea Gnarini, Rosario Iaria, Jari J. E. Kajava, Kuan Liu, Riccardo Middei, Stephen L. O'Dell, Maura Pilia, John Rankin, Andrea Sanna, Jakob van den Eijnden, Martin C. Weisskopf, Anna Bobrikova, Fiamma Capitanio, Enrico Costa, Philip Kaaret, Alessio Marino, Paolo Soffitta, Francesco Ursini, Filippo Ambrosino, Massimo Cocchi, Sergio Fabiani, Herman L. Marshall, Giorgio Matt, Sara Elisa Motta, Alessandro Papitto, Luigi Stella, Antonella Tarana, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, 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, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, 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: Top: normalized Stokes parameters Q/I and U/I in different energy bins as measured with PCUBE in IXPEOBSSIM. Bottom: polar plot of the X-ray polarization in 4U 1820−303 when 1 keV binning is applied. Contours are reported at 68% CL. A trend of polarization growing with energy is visible in both plots.