adsabs/AstroCLIMB huggingface dataset:
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption: Inclination-corrected velocity width vs. axis ratio (b/a). Gray and blue dots are for normal dwarf galaxies and HUDGs (without b/a cut), respectively. Curves represent the median values. The distribution of the b/a ratios and the inclination-corrected velocity width are presented on the top and right sides. The offset between normal dwarf galaxies and HUDGs is caused by their different mass distributions.
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption: Half-light radius in Tully–Fisher relation diagram. Left: HUDGs. Right: G20 dwarf galaxies. Colored as half-light radii (r  e ), the gray/blue/red dashed lines indicated the luminosity limits of minimal/50%/90% size of HUDGs by 3σ of background.
Paper: Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants
Authors: Elias R. Most, Eliot Quataert
Figure caption: Flaring process at the surface (red) of the neutron star merger remnant. Shown in color are the magnetic field, the entropy per baryon s (indicating heating inside the flare). The times t are stated relative to the time of merger t mer. (Left) Buildup of magnetic stresses due to buoyancy of field lines from the star. (Center) Inflation of the connected flux tube due to strong differential rotation at the surface of the star, where both footpoints are anchored. (Right) Detachment of the flare within ≃1 ms of its creation. In our simulations, this cycle repeats quasiperiodically until a steady outflow is launched.
Paper: Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants
Authors: Elias R. Most, Eliot Quataert
Figure caption: Magnetic field strength, B, in the hypermassive neutron star around the time of the onset of flaring. The solid red line approximately marks the surface of the star. The field close to the surface has been amplified to high field strengths due the use of a subgrid dynamo model, mimicking the effect of small-scale field amplification during merger. Shown are high (top) and low (bottom) magnetization cases.
Paper: Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants
Authors: Elias R. Most, Eliot Quataert
Figure caption: Propagation of the flares away from the merger site. Several flaring episodes are visible in the center panel. Shown in color is the magnetization σ = b 2/ρ, where b 2 is the comoving magnetic field energy density, and ρ is the baryon rest-mass density. All times, t, are stated relative to the time of merger, t mer.
Paper: Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants
Authors: Elias R. Most, Eliot Quataert
Figure caption: Same as Figure 3 (right panel), but showing the entropy s per baryon and vertical velocity component Γv  z  of the outflow. Shown are target magnetizations σ = 0.01 (left) and σ = 0.001 (right) for the models using the DD2 equation of state. A distinct quasiperiodic substructure is visible in the mildly relativistic outflows for both models.
Paper: Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants
Authors: Elias R. Most, Eliot Quataert
Figure caption: Electromagnetic luminosity ﹩{{ \mathcal L }}_{\mathrm{EM}}﹩ (i.e., Poynting flux) relative to the time of first electromagnetic outburst, t EM, extracted at a radius r = 236 km from the stellar remnant. Solid lines refer to high-magnetization models, σ = 0.01; dashed lines refer to low-magnetization models, σ = 0.001. Times, t, are stated relative to the time t EM of the first flare launch. For the high-magnetization cases, black hole formation is indicated by a vertical black line.
Paper: Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants
Authors: Elias R. Most, Eliot Quataert
Figure caption: Frequency spectrum (logarithmic power spectral density, PSD) of the electromagnetic (EM) and gravitational-wave (GW) luminosities. Note that the units of the PSDs have been rescaled and shifted relative to each other to aid a direct comparison.
Paper: IXPE Observations of the Quintessential Wind-accreting X-Ray Pulsar Vela X-1
Authors: Sofia V. Forsblom, Juri Poutanen, Sergey S. Tsygankov, Matteo Bachetti, Alessandro Di Marco, Victor Doroshenko, Jeremy Heyl, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Alexander A. Mushtukov, Maura Pilia, Daniele Rogantini, Valery F. Suleimanov, Roberto Taverna, Fei Xie, Iván Agudo, Lucio A. Antonelli, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Rashid A. Sunyaev, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Silvia Zane
Figure caption: Stokes I, Q, and U energy distributions for the combined data set of Vela X-1 with the best-fit model superimposed for IXPE’s DUs (upper larger panels in rows 1 and 3). The residuals between the best-fit model and the data are shown in the lower narrow panels of rows 2 and 4. Two upper and two lower rows correspond to the first and second observations, respectively, and are shown separately for clarity.
Paper: IXPE Observations of the Quintessential Wind-accreting X-Ray Pulsar Vela X-1
Authors: Sofia V. Forsblom, Juri Poutanen, Sergey S. Tsygankov, Matteo Bachetti, Alessandro Di Marco, Victor Doroshenko, Jeremy Heyl, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Alexander A. Mushtukov, Maura Pilia, Daniele Rogantini, Valery F. Suleimanov, Roberto Taverna, Fei Xie, Iván Agudo, Lucio A. Antonelli, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Rashid A. Sunyaev, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Silvia Zane
Figure caption: Phase-resolved analysis of Vela X-1 for the combined data set in the 2–7 keV range, combining data from all DUs. (a) Pulse profile. Panels (b) and (c) display the dependence of the Stokes q and u parameters, respectively, on the pulse phase, obtained for the phase-resolved polarimetric analysis utilizing the PCUBE algorithm. Panels (d) and (e) show the dependence of the PD and PA, respectively, on the pulse phase, obtained from the phase-resolved spectropolarimetric analysis using XSPEC. Upper limits (arrows) to the PD in panel (d) are at 99.73% (3σ) confidence level and are computed using a χ 2 with 1 degree of freedom.
Paper: IXPE Observations of the Quintessential Wind-accreting X-Ray Pulsar Vela X-1
Authors: Sofia V. Forsblom, Juri Poutanen, Sergey S. Tsygankov, Matteo Bachetti, Alessandro Di Marco, Victor Doroshenko, Jeremy Heyl, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Alexander A. Mushtukov, Maura Pilia, Daniele Rogantini, Valery F. Suleimanov, Roberto Taverna, Fei Xie, Iván Agudo, Lucio A. Antonelli, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Rashid A. Sunyaev, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Silvia Zane
Figure caption: Energy dependence of the normalized Stokes parameters q and u for the phase-averaged data of the combined data set, obtained with the PCUBE algorithm.
Paper: IXPE Observations of the Quintessential Wind-accreting X-Ray Pulsar Vela X-1
Authors: Sofia V. Forsblom, Juri Poutanen, Sergey S. Tsygankov, Matteo Bachetti, Alessandro Di Marco, Victor Doroshenko, Jeremy Heyl, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Alexander A. Mushtukov, Maura Pilia, Daniele Rogantini, Valery F. Suleimanov, Roberto Taverna, Fei Xie, Iván Agudo, Lucio A. Antonelli, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Rashid A. Sunyaev, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Silvia Zane
Figure caption: Background-corrected light curves of Vela X-1 in the 2–8 keV energy bands summed over the three DUs of IXPE for the first and second observations, shown in the left and right panels, respectively. The light-curve time bin value was set to ∼250 s. The time of the eclipse is marked by the blue shaded area.
Paper: IXPE Observations of the Quintessential Wind-accreting X-Ray Pulsar Vela X-1
Authors: Sofia V. Forsblom, Juri Poutanen, Sergey S. Tsygankov, Matteo Bachetti, Alessandro Di Marco, Victor Doroshenko, Jeremy Heyl, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Alexander A. Mushtukov, Maura Pilia, Daniele Rogantini, Valery F. Suleimanov, Roberto Taverna, Fei Xie, Iván Agudo, Lucio A. Antonelli, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Rashid A. Sunyaev, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Silvia Zane
Figure caption: Polarization vector of Vela X-1 from the results of the phase-averaged spectropolarimetric analysis of the combined data set. Contours at 68.3%, 95.45%, and 99.73% confidence are shown in blue, purple, and red, respectively.
Paper: IXPE Observations of the Quintessential Wind-accreting X-Ray Pulsar Vela X-1
Authors: Sofia V. Forsblom, Juri Poutanen, Sergey S. Tsygankov, Matteo Bachetti, Alessandro Di Marco, Victor Doroshenko, Jeremy Heyl, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Alexander A. Mushtukov, Maura Pilia, Daniele Rogantini, Valery F. Suleimanov, Roberto Taverna, Fei Xie, Iván Agudo, Lucio A. Antonelli, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Rashid A. Sunyaev, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Silvia Zane
Figure caption: Pulse profiles of Vela X-1 as seen by IXPE in two different energy bands for the first and second observations, combined for DU1–3.
Paper: IXPE Observations of the Quintessential Wind-accreting X-Ray Pulsar Vela X-1
Authors: Sofia V. Forsblom, Juri Poutanen, Sergey S. Tsygankov, Matteo Bachetti, Alessandro Di Marco, Victor Doroshenko, Jeremy Heyl, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Alexander A. Mushtukov, Maura Pilia, Daniele Rogantini, Valery F. Suleimanov, Roberto Taverna, Fei Xie, Iván Agudo, Lucio A. Antonelli, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Rashid A. Sunyaev, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Silvia Zane
Figure caption: Polarization vectors of Vela X-1 from the results of the phase-resolved spectropolarimetric analysis of the combined data set. Contours at 68.3%, 95.45%, and 99.73% confidence are shown in blue, purple, and red, respectively.
Paper: Insights on the Sun Birth Environment in the Context of Star Cluster Formation in Hub–Filament Systems
Authors: Doris Arzoumanian, Sota Arakawa, Masato I. N. Kobayashi, Kazunari Iwasaki, Kohei Fukuda, Shoji Mori, Yutaka Hirai, Masanobu Kunitomo, M. S. Nanda Kumar, Eiichiro Kokubo
Figure caption: Schematic figure summarizing the importance of HFSs in the understanding of the impact of stellar feedback on the surrounding matter and the formation of stellar systems. (a) Formation of an HFS through the merging of multiple filaments forming low- to intermediate-mass stars (Sections 3.1 and 3.2). (b) High-mass star formation in the dense hub. The feedback from massive stars during their formation and evolution (outflow and wind) compresses the dense filaments (see Zavagno et al. 2020) and flow away into the ISM through the interfilamentary diffuse medium, forming bipolar-shaped H II regions (Section 4.1). (c) At the end of their lives, high-mass stars go through a WR phase followed, for some of them, by a supernova explosion (Section 4.2). During these later stages of high-mass star evolution, SLRs (such as 26Al) present in the WR winds and supernova ejecta (Section 2) are injected into the filament and the cores embedded in them. These cores are additionally supplied with SLR-rich gas and dust by streamers throughout the different protostellar evolutionary phases (Section 3.3) until the formation of planetary systems (d). (a) and (b) are adapted from Kumar et al. (2020).
Paper: Insights on the Sun Birth Environment in the Context of Star Cluster Formation in Hub–Filament Systems
Authors: Doris Arzoumanian, Sota Arakawa, Masato I. N. Kobayashi, Kazunari Iwasaki, Kohei Fukuda, Shoji Mori, Yutaka Hirai, Masanobu Kunitomo, M. S. Nanda Kumar, Eiichiro Kokubo
Figure caption: Fraction of ejecta mass, ﹩{M}_{\mathrm{tot}}^{\mathrm{ejecta}\mbox{--}\mathrm{to}\mbox{--}\mathrm{fil}}/{M}_{\mathrm{ejecta}}﹩, intercepted by the filament against the distance of the filament from the exploding star. The three curves correspond to three estimates of the filament cross section, S fil = w fil l fil for l fil = w fil, 2w fil, and 3w fil, where l fil is the longitudinal extent and w fil = W fil = 0.1 pc is the radial extent (see Section 3.1).
Paper: Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts
Authors: Daichi Hiramatsu, Edo Berger, Brian D. Metzger, Sebastian Gomez, Allyson Bieryla, Iair Arcavi, D. Andrew Howell, Ryan Mckinven, Nozomu Tominaga
Figure caption: Optical luminosity limits (in the g, c, r, o, i, and z bands from the top to bottom rows) with respect to the temporally closest FRB detection for our sample of eight repeating FRBs (including the Galactic SGR 1935+2154). Representative limits are shown for the targeted high-speed observations (TNT i and i + z, MAGIC U, Tomo-e open) in the panels with the closest filter effective wavelength, and similarly for LCO R and BOOTES Z and clear bands. A typical luminosity error in each band for SGR 1935+2154 (due to the large extinction and distance uncertainties) is shown as the magenta vertical bar. Our KeplerCam and LCO limits for FRB 20220912A (enclosed by the black rectangle) are the deepest among the simultaneous observations of extragalactic FRBs. Optical data sources: KeplerCam (this work for FRB 20220912A), LCO (this work and Lin et al. 2020 for FRBs 20200120E and 20220912A in griz, and SGR 1935+2154 in R, respectively), Binospec (this work for FRB 20220912A), ZTF (Andreoni et al. 2020, 2021 for FRBs 20200120E and 20180916B, respectively), ZTF forced-photometry service (Masci et al. 2019 and this work for all the FRBs), ATLAS forced photometry server (Shingles et al. 2021 and this work for all the FRBs), APO (Kilpatrick et al. 2021 for FRB 20180916B), TNT (Hardy et al. 2017 for FRB 20121102A), MAGIC (MAGIC Collaboration et al. 2018 for FRB 20121102A), Tomo-e (Niino et al. 2022 for FRB 20190520B), and BOOTES (Lin et al. 2020 for SGR 1935+2154).(The data used to create this figure are available.)