adsabs/AstroCLIMB huggingface dataset:
Paper: A Need to Revise Stellar Opacities from Asteroseismology of δ Scuti Stars
Authors: Jadwiga Daszyńska-Daszkiewicz, Przemysław Walczak, Alexey Pamyatnykh, Wojciech Szewczuk, Wojciech Niewiadomski
Figure caption: The normalized histograms for the mixing-length parameter α MLT for seismic models computed with the OPAL opacities.
Paper: A Need to Revise Stellar Opacities from Asteroseismology of δ Scuti Stars
Authors: Jadwiga Daszyńska-Daszkiewicz, Przemysław Walczak, Alexey Pamyatnykh, Wojciech Szewczuk, Wojciech Niewiadomski
Figure caption: Seismic models of BP Peg, AE UMa, RV Ari, and SX Phe constructed with the three opacity databases: OPAL, OP, and OPLIB. The initial hydrogen abundance by mass was X 0 = 0.70, and the range of metallicity Z is given in each case.
Paper: A Need to Revise Stellar Opacities from Asteroseismology of δ Scuti Stars
Authors: Jadwiga Daszyńska-Daszkiewicz, Przemysław Walczak, Alexey Pamyatnykh, Wojciech Szewczuk, Wojciech Niewiadomski
Figure caption: The normalized histograms for the metallicity Z for seismic models computed with the OPAL opacities.
Paper: A Need to Revise Stellar Opacities from Asteroseismology of δ Scuti Stars
Authors: Jadwiga Daszyńska-Daszkiewicz, Przemysław Walczak, Alexey Pamyatnykh, Wojciech Szewczuk, Wojciech Niewiadomski
Figure caption: The normalized histograms for the current rotational velocity V rot for seismic models computed with the OPAL opacities.
Paper: A Need to Revise Stellar Opacities from Asteroseismology of δ Scuti Stars
Authors: Jadwiga Daszyńska-Daszkiewicz, Przemysław Walczak, Alexey Pamyatnykh, Wojciech Szewczuk, Wojciech Niewiadomski
Figure caption: The normalized histograms for the initial hydrogen abundance X 0 for seismic models computed with the OPAL opacities.
Paper: The Deformation of an Erupting Magnetic Flux Rope in a Confined Solar Flare
Authors: Ruisheng Zheng, Yihan Liu, Liang Zhang, Yang Liu, Changhui Rao, Qing Lin, Zhimao Du, Libo Zhong, Huadong Chen, Yao Chen
Figure caption: The overview of AR 12860 and its magnetic field evolution. ((a)–(f)) The orange and the pink dashed boxes separately outline the preceding sunspots and following sunspots, and the blue and red arrows points out the moving negative sunspots, NS1 and NS2. The green and orange arrows show the sigmoidal filament and the underlying threads. (g) Time–distance plot along the green line in panel (e), showing the movement of NS1 and NS2. The dotted lines are used to derive the attached speeds. (h) The negative (red) and positive (blue) magnetic flux evolution (between 12:00 on August 28 and 06:00 UT on August 29) in the AR center (red boxes in panels (d) and (f)). The green-shaded area represents the duration of the eruption.
Paper: The Deformation of an Erupting Magnetic Flux Rope in a Confined Solar Flare
Authors: Ruisheng Zheng, Yihan Liu, Liang Zhang, Yang Liu, Changhui Rao, Qing Lin, Zhimao Du, Libo Zhong, Huadong Chen, Yao Chen
Figure caption: The flare ribbons in Atmospheric Imaging Assembly (AIA) 1600 Å and their contours over Helioseismic and Magnetic Imager (HMI) magnetograms (left panels). (b) The intensity curves in AIA 1600, 304, and 94 Å for the eruption region (the red box in panel (a)) and the GOES SXR flux and its derivative for the flare. The vertical lines mark the two peak times of the flare. The yellow and cyan shades separately cover the flare impulsive phase in GOES SXR and AIA 94 Å. ((d) and (f)) the curves of the reconnected flux and the reconnection rate for the positive (blue) and negative (red) magnetic flux. (g) The radio dynamic spectra from CALLISTO, showing the type III radio bursts (white arrows).
Paper: The Deformation of an Erupting Magnetic Flux Rope in a Confined Solar Flare
Authors: Ruisheng Zheng, Yihan Liu, Liang Zhang, Yang Liu, Changhui Rao, Qing Lin, Zhimao Du, Libo Zhong, Huadong Chen, Yao Chen
Figure caption: Schematic drawings for the eruption and deformation of the MFR (red) below the confining cage (orange) based on the contours of positive and negative polarities from the HMI magnetogram at 00:00 UT on August 29. The green and blue lines represent the filed lines stretched by the rising MFR, and the green-blue lines show the postflare loops and the newly formed lines wrapping the rising MFR due to the inner magnetic reconnection. The underlying SA is indicated by the short black line, and the pink-black lines show the newly formed loops resulting from the external magnetic reconnection. The flare ribbons are outlined by the purple curves, and the two-step magnetic reconnection is indicated by star symbols.
Paper: Evidence for Enrichment of Niobium-92 in the Outer Protosolar Disk
Authors: Yuki Hibiya, Tsuyoshi Iizuka, Hatsuki Enomoto, Takehito Hayakawa
Figure caption: Nb–Zr isochron diagram for NWA 6704. The error bars reflect 2σ. Solid and dashed lines represent the isochron and error envelopes (at 95% confidence) based on the regression of the data, respectively. For the isochron regression, all 92Zr/90Zr were normalized to 92Zr/90Zr = 0.333383 for the standard solution, following previous studies (Schönbächler et al. 2002; Iizuka et al. 2016).
Paper: The Deformation of an Erupting Magnetic Flux Rope in a Confined Solar Flare
Authors: Ruisheng Zheng, Yihan Liu, Liang Zhang, Yang Liu, Changhui Rao, Qing Lin, Zhimao Du, Libo Zhong, Huadong Chen, Yao Chen
Figure caption: Two-step magnetic reconnection in EM maps at temperature range of 0.3–1 MK, 1–10 MK, and 10–25 MK. The yellow and pink arrows separately indicate the postflare loops and the flashings. The white arrows show the newly formed high-temperature loops.
Paper: The Deformation of an Erupting Magnetic Flux Rope in a Confined Solar Flare
Authors: Ruisheng Zheng, Yihan Liu, Liang Zhang, Yang Liu, Changhui Rao, Qing Lin, Zhimao Du, Libo Zhong, Huadong Chen, Yao Chen
Figure caption: The NLFFF extrapolated MFR (orange) and the overlying arcades (blue and red) before the eruption (00:00 UT) superposed on the HMI vector magnetogram in the side view (left) and on the contours of Q value at photospheric surface in the top view (right). The yellow and cyan dashed arrows show two kinds of slipping motions.
Paper: Evidence for Enrichment of Niobium-92 in the Outer Protosolar Disk
Authors: Yuki Hibiya, Tsuyoshi Iizuka, Hatsuki Enomoto, Takehito Hayakawa
Figure caption: Plot of ε 92Zr vs. 1/Zr for the whole-rock and mineral fractions of the NWA 6704 achondrite. Error bars represent 2σ, as listed in Table A1.
Paper: Clustered Formation of Massive Stars within an Ionized Rotating Disk
Authors: Roberto Galván-Madrid, Qizhou Zhang, Andrés Izquierdo, Charles J. Law, Thomas Peters, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Adam Ginsburg, Carlos Carrasco-González
Figure caption: Results from the radiative-transfer model fitting. Top row, left panel: continuum modeling. The top cut shows the ALMA data and the bottom cut shows the best-fit power-law model for the electron density. Top row, center and right panels: Keplerian disk best-fit and residuals. Middle row: ALMA H30α P–V diagram, along with the best-fit Keplerian model with radial motions and residuals. Bottom row: same as middle row for the Keplerian disk with Ulrich envelope. Residuals are defined as observational data minus model.
Paper: Clustered Formation of Massive Stars within an Ionized Rotating Disk
Authors: Roberto Galván-Madrid, Qizhou Zhang, Andrés Izquierdo, Charles J. Law, Thomas Peters, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Adam Ginsburg, Carlos Carrasco-González
Figure caption: Distribution of molecular and ionized gas in the dense cluster G10.6-0.4. (a) CH3OH line emission imaged with the SMA. Red, green, and blue show CH3OH with upper energies 35, 59, and 97 K (see Liu et al. 2011). The white square marks the region of the ALMA maps shown in the other panels. (b) Emission of the CH3CN J = 12–11 line (Jy beam−1 km s−1; see Law et al. 2021). (c) 1.3 mm continuum (Jy beam−1). (d) Integrated H30α line emission (Jy beam−1 km s−1). The spatial cut for the P–V diagrams is shown with a red line.
Paper: Clustered Formation of Massive Stars within an Ionized Rotating Disk
Authors: Roberto Galván-Madrid, Qizhou Zhang, Andrés Izquierdo, Charles J. Law, Thomas Peters, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Adam Ginsburg, Carlos Carrasco-González
Figure caption: Diagnostic plots for best fit of purely Keplerian model. The top-left panel shows the midplane ion density n ion = n  e , along with a cut in which the velocity field is measured. The top-right panel shows cartesian velocity components in the midplane z = 0 cut. The bottom-left panel shows the midplane density profile. The bottom-right panel shows the scale-height H profile.
Paper: Clustered Formation of Massive Stars within an Ionized Rotating Disk
Authors: Roberto Galván-Madrid, Qizhou Zhang, Andrés Izquierdo, Charles J. Law, Thomas Peters, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Adam Ginsburg, Carlos Carrasco-González
Figure caption: Same as Figure 4, but for the case of the case of a Keplerian disk with an exterior Ulrich envelope. Note that the Ulrich envelope has a divergence at the radius in which it settles into a disk (Ulrich 1976; Mendoza et al. 2004), which we smooth by averaging a few neighboring grid points.
Paper: Clustered Formation of Massive Stars within an Ionized Rotating Disk
Authors: Roberto Galván-Madrid, Qizhou Zhang, Andrés Izquierdo, Charles J. Law, Thomas Peters, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Adam Ginsburg, Carlos Carrasco-González
Figure caption: Corner plots of posterior probability distributions of the model parameters fitted by maximizing the log-likelihood χ 2 function defined in Equation (3). The top-left panels show the parameters labeled as “Density profile” in Table 1. The top-right panels correspond to the “Keplerian disk” modeling. The bottom-left panels are for the “Keplerian + radial” models. The bottom-right panels denote the “Keplerian + Ulrich” models.
Paper: Clustered Formation of Massive Stars within an Ionized Rotating Disk
Authors: Roberto Galván-Madrid, Qizhou Zhang, Andrés Izquierdo, Charles J. Law, Thomas Peters, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Adam Ginsburg, Carlos Carrasco-González
Figure caption: Same as Figure 4, but for the case of the case of a Keplerian disk with external radial motions.
Paper: X-Ray Polarization Observations of BL Lacertae
Authors: Riccardo Middei, Ioannis Liodakis, Matteo Perri, Simonetta Puccetti, Elisabetta Cavazzuti, Laura Di Gesu, Steven R. Ehlert, Grzegorz Madejski, Alan P. Marscher, Herman L. Marshall, Fabio Muleri, Michela Negro, Svetlana G. Jorstad, Beatriz Agís-González, Iván Agudo, Giacomo Bonnoli, Maria I. Bernardos, Víctor Casanova, Maya García-Comas, César Husillos, Alessandro Marchini, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, George A. Borman, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Andrey A. Vasilyev, Alexey V. Zhovtan, Carolina Casadio, Juan Escudero, Ioannis Myserlis, Antonio Hales, Seiji Kameno, Ruediger Kneissl, Hugo Messias, Hiroshi Nagai, Dmitry Blinov, Ioakeim G. Bourbah, Sebastian Kiehlmann, Evangelos Kontopodis, Nikos Mandarakas, Stylianos Romanopoulos, Raphael Skalidis, Anna Vervelaki, Joseph R. Masiero, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Georgia V. Panopoulou, Samaporn Tinyanont, Andrei V. Berdyugin, Masato Kagitani, Vadim Kravtsov, Takeshi Sakanoi, Ryo Imazawa, Mahito Sasada, Yasushi Fukazawa, Koji S. Kawabata, Makoto Uemura, Tsunefumi Mizuno, Tatsuya Nakaoka, Hiroshi Akitaya, Mark Gurwell, Ramprasad Rao, Niccoló Di Lalla, Nicoló Cibrario, Immacolata Donnarumma, Dawoon E. Kim, Nicola Omodei, Luigi Pacciani, Juri Poutanen, Fabrizio Tavecchio, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccoló Bucciantini, Fiamma Capitanio, Simone Castellano, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Alessandro Di Marco, Victor Doroshenko, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Vladimir Karas, 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, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Top panels: best fit to the May X-ray data set (on the left) and the IXPE-XMM-Newton data taken during 2022 July (right plots). In the middle and bottom subpanels, we report the residuals to the I, U, and Q spectra, respectively. Bottom plots: confidence regions of the model fits for the polarization angle and degree for the two observations.
Paper: X-Ray Polarization Observations of BL Lacertae
Authors: Riccardo Middei, Ioannis Liodakis, Matteo Perri, Simonetta Puccetti, Elisabetta Cavazzuti, Laura Di Gesu, Steven R. Ehlert, Grzegorz Madejski, Alan P. Marscher, Herman L. Marshall, Fabio Muleri, Michela Negro, Svetlana G. Jorstad, Beatriz Agís-González, Iván Agudo, Giacomo Bonnoli, Maria I. Bernardos, Víctor Casanova, Maya García-Comas, César Husillos, Alessandro Marchini, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, George A. Borman, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Andrey A. Vasilyev, Alexey V. Zhovtan, Carolina Casadio, Juan Escudero, Ioannis Myserlis, Antonio Hales, Seiji Kameno, Ruediger Kneissl, Hugo Messias, Hiroshi Nagai, Dmitry Blinov, Ioakeim G. Bourbah, Sebastian Kiehlmann, Evangelos Kontopodis, Nikos Mandarakas, Stylianos Romanopoulos, Raphael Skalidis, Anna Vervelaki, Joseph R. Masiero, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Georgia V. Panopoulou, Samaporn Tinyanont, Andrei V. Berdyugin, Masato Kagitani, Vadim Kravtsov, Takeshi Sakanoi, Ryo Imazawa, Mahito Sasada, Yasushi Fukazawa, Koji S. Kawabata, Makoto Uemura, Tsunefumi Mizuno, Tatsuya Nakaoka, Hiroshi Akitaya, Mark Gurwell, Ramprasad Rao, Niccoló Di Lalla, Nicoló Cibrario, Immacolata Donnarumma, Dawoon E. Kim, Nicola Omodei, Luigi Pacciani, Juri Poutanen, Fabrizio Tavecchio, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccoló Bucciantini, Fiamma Capitanio, Simone Castellano, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Alessandro Di Marco, Victor Doroshenko, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Vladimir Karas, 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, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Radio polarization vs. time for BL Lac object. Top: flux density; middle: polarization degree; bottom: polarization angle. The gray shaded areas demark the duration of IXPE observations 1 and 2.
Paper: X-Ray Polarization Observations of BL Lacertae
Authors: Riccardo Middei, Ioannis Liodakis, Matteo Perri, Simonetta Puccetti, Elisabetta Cavazzuti, Laura Di Gesu, Steven R. Ehlert, Grzegorz Madejski, Alan P. Marscher, Herman L. Marshall, Fabio Muleri, Michela Negro, Svetlana G. Jorstad, Beatriz Agís-González, Iván Agudo, Giacomo Bonnoli, Maria I. Bernardos, Víctor Casanova, Maya García-Comas, César Husillos, Alessandro Marchini, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, George A. Borman, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Andrey A. Vasilyev, Alexey V. Zhovtan, Carolina Casadio, Juan Escudero, Ioannis Myserlis, Antonio Hales, Seiji Kameno, Ruediger Kneissl, Hugo Messias, Hiroshi Nagai, Dmitry Blinov, Ioakeim G. Bourbah, Sebastian Kiehlmann, Evangelos Kontopodis, Nikos Mandarakas, Stylianos Romanopoulos, Raphael Skalidis, Anna Vervelaki, Joseph R. Masiero, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Georgia V. Panopoulou, Samaporn Tinyanont, Andrei V. Berdyugin, Masato Kagitani, Vadim Kravtsov, Takeshi Sakanoi, Ryo Imazawa, Mahito Sasada, Yasushi Fukazawa, Koji S. Kawabata, Makoto Uemura, Tsunefumi Mizuno, Tatsuya Nakaoka, Hiroshi Akitaya, Mark Gurwell, Ramprasad Rao, Niccoló Di Lalla, Nicoló Cibrario, Immacolata Donnarumma, Dawoon E. Kim, Nicola Omodei, Luigi Pacciani, Juri Poutanen, Fabrizio Tavecchio, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccoló Bucciantini, Fiamma Capitanio, Simone Castellano, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Alessandro Di Marco, Victor Doroshenko, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Vladimir Karas, 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, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Multimission light curve of BL Lac as observed in the 2–8 keV energy range. Different colors account for the various facilities. No significant intraobservation variability is observed during the first IXPE pointing, while, a flux decrease by a factor of ∼30% is observed during the second exposure.
Paper: X-Ray Polarization Observations of BL Lacertae
Authors: Riccardo Middei, Ioannis Liodakis, Matteo Perri, Simonetta Puccetti, Elisabetta Cavazzuti, Laura Di Gesu, Steven R. Ehlert, Grzegorz Madejski, Alan P. Marscher, Herman L. Marshall, Fabio Muleri, Michela Negro, Svetlana G. Jorstad, Beatriz Agís-González, Iván Agudo, Giacomo Bonnoli, Maria I. Bernardos, Víctor Casanova, Maya García-Comas, César Husillos, Alessandro Marchini, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, George A. Borman, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Andrey A. Vasilyev, Alexey V. Zhovtan, Carolina Casadio, Juan Escudero, Ioannis Myserlis, Antonio Hales, Seiji Kameno, Ruediger Kneissl, Hugo Messias, Hiroshi Nagai, Dmitry Blinov, Ioakeim G. Bourbah, Sebastian Kiehlmann, Evangelos Kontopodis, Nikos Mandarakas, Stylianos Romanopoulos, Raphael Skalidis, Anna Vervelaki, Joseph R. Masiero, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Georgia V. Panopoulou, Samaporn Tinyanont, Andrei V. Berdyugin, Masato Kagitani, Vadim Kravtsov, Takeshi Sakanoi, Ryo Imazawa, Mahito Sasada, Yasushi Fukazawa, Koji S. Kawabata, Makoto Uemura, Tsunefumi Mizuno, Tatsuya Nakaoka, Hiroshi Akitaya, Mark Gurwell, Ramprasad Rao, Niccoló Di Lalla, Nicoló Cibrario, Immacolata Donnarumma, Dawoon E. Kim, Nicola Omodei, Luigi Pacciani, Juri Poutanen, Fabrizio Tavecchio, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccoló Bucciantini, Fiamma Capitanio, Simone Castellano, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Alessandro Di Marco, Victor Doroshenko, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Vladimir Karas, 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, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Optical polarization time variations for BL Lac object. Top: magnitude; middle: polarization degree; bottom: polarization angle. The gray shaded areas demark the duration of the IXPE observations. The IXPE upper limits obtained in the two observations are also reported.