adsabs/AstroCLIMB huggingface dataset:
Paper: The First Polarimetric View on Quasiperiodic Oscillations in a Black Hole X-Ray Binary
Authors: Qing-Chang Zhao, Lian Tao, Han-Cheng Li, Shuang-Nan Zhang, Hua Feng, Ming-Yu Ge, Long Ji, Ya-Nan Wang, Yue Huang, Xiang Ma, Liang Zhang, Jin-Lu Qu, Yan-Jun Xu, Shu Zhang, Qian-Qing Yin, Qing-Cang Shui, Rui-Can Ma, Shu-Jie Zhao, Pan-Ping Li, Zi-Xu Yang, He-Xin Liu, Wei Yu
Figure caption: Left, middle, and right panels: the Stokes spectra of I, Q, and U for ObsID 02250901 of Swift J1727.8–1613. The solid lines represent the best fit of Const∗Polconst∗Powerlaw.
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Corner plot showing the constraints for AT 2019dsg for two different assumptions about the binding energy coefficient k that enters the fallback time (Equation (3)), with k = 0.8 in blue and k = 0.4 in orange.
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Corner plot showing the constraints for AT 2018hyz for two fits with the Gaussian rise and power-law pre–cooling envelope phenomenology in orange and blue, respectively.
Paper: Transverse MHD Waves as Signatures of Braiding-induced Magnetic Reconnection in Coronal Loops
Authors: A. Ramada C. Sukarmadji, Patrick Antolin
Figure caption: The top row shows the SJI 1330 and AIA 304 image with the slice (white line) for the time–distance diagram plots in the second and third rows. The white vertical line in the time–distance diagrams marks the time of the SJI and AIA image. The time–distance diagrams have the white circles marking the position of the oscillations that are selected based on an intensity threshold that separates the loop from its surrounding. The third row shows the combined oscillation data from SJI 1330 (first 232 s, in green) and AIA 304 (remaining 232 s, in blue) and the calculated upward-moving trend (red circles). Each point in the upward-moving trend is calculated by averaging a given point’s value with eight of its neighboring points. The IRIS and AIA points are subtracted by the global trend points to recover the detrended oscillations, shown in the bottom panel. We observe two clear periods before it damps.
Paper: The First Polarimetric View on Quasiperiodic Oscillations in a Black Hole X-Ray Binary
Authors: Qing-Chang Zhao, Lian Tao, Han-Cheng Li, Shuang-Nan Zhang, Hua Feng, Ming-Yu Ge, Long Ji, Ya-Nan Wang, Yue Huang, Xiang Ma, Liang Zhang, Jin-Lu Qu, Yan-Jun Xu, Shu Zhang, Qian-Qing Yin, Qing-Cang Shui, Rui-Can Ma, Shu-Jie Zhao, Pan-Ping Li, Zi-Xu Yang, He-Xin Liu, Wei Yu
Figure caption: Panel (a): the light curves of MAXI/Gas Slit Camera (GSC; 2–20 keV, red color) and Swift/BAT (15–50 keV, blue color) of Swift J1727.8–1613. The dashed purple line represents the state transition time, and the gray strip represents the first observation of IXPE. Panel (b): the hardness–intensity diagram (HID) of MAXI/GSC. The hardness ratio is defined as the count rate in the 4–10 keV band divided by that in the 2–4 keV band. The black diamond represents the location of IXPE's first observations. The purple star represents the location of state transition determined by the NICER data (Bollemeijer et al. 2023). Panel (c): the representative PDS from IXPE (2–8 keV). The Poisson noise was not subtracted.
Paper: The First Polarimetric View on Quasiperiodic Oscillations in a Black Hole X-Ray Binary
Authors: Qing-Chang Zhao, Lian Tao, Han-Cheng Li, Shuang-Nan Zhang, Hua Feng, Ming-Yu Ge, Long Ji, Ya-Nan Wang, Yue Huang, Xiang Ma, Liang Zhang, Jin-Lu Qu, Yan-Jun Xu, Shu Zhang, Qian-Qing Yin, Qing-Cang Shui, Rui-Can Ma, Shu-Jie Zhao, Pan-Ping Li, Zi-Xu Yang, He-Xin Liu, Wei Yu
Figure caption: Panels (a)–(c): the energy dependence of QPO fractional rms, PA, and PD, measured from the IXPE data of Swift J1727.8–1613.
Paper: X-Ray Polarized View of the Accretion Geometry in the X-Ray Binary Circinus X-1
Authors: John Rankin, Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Anna Bobrikova, Vadim Kravtsov, Fabio Muleri, Maura Pilia, Alexandra Veledina, Rob Fender, Philip Kaaret, Dawoon E. Kim, Andrea Marinucci, Herman L. Marshall, Alessandro Papitto, Allyn F. Tennant, Sergey S. Tsygankov, Martin C. Weisskopf, Kinwah Wu, Silvia Zane, Filippo Ambrosino, Ruben Farinelli, Andrea Gnarini, Iván Agudo, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, 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, Alan P. Marscher, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Fei Xie
Figure caption: Study of polarization binned in HR. (Top) HR trend with time (2000 s time binning); the colored bands identify the chosen binning for HR. (Middle) Polar plot of polarization, computed using the model-independent pcube algorithm from the IXPEOBSSSIM software (Baldini et al. 2022), for events in different intervals of HR reported in the top panel in the energy band 2–8 keV, where the shaded region indicates the direction of the jet (see discussion), and the black lines indicate this direction and its orthogonal direction. Contours are reported at 68%, 95%, and 99% CLs. (Bottom) Polarization in different energy bands. Contours are reported at a 90% CL.
Paper: X-Ray Polarized View of the Accretion Geometry in the X-Ray Binary Circinus X-1
Authors: John Rankin, Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Anna Bobrikova, Vadim Kravtsov, Fabio Muleri, Maura Pilia, Alexandra Veledina, Rob Fender, Philip Kaaret, Dawoon E. Kim, Andrea Marinucci, Herman L. Marshall, Alessandro Papitto, Allyn F. Tennant, Sergey S. Tsygankov, Martin C. Weisskopf, Kinwah Wu, Silvia Zane, Filippo Ambrosino, Ruben Farinelli, Andrea Gnarini, Iván Agudo, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, 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, Alan P. Marscher, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Fei Xie
Figure caption: Polar plot of polarization, computed using the pcube algorithm from the IXPEOBSSSIM software (Baldini et al. 2022), for the three phase intervals defined in Figure 1. (Top) Polarization in the entire IXPE energy band is reported. The shaded region indicates the direction of the jet (see discussion), and the black lines indicate this direction and its orthogonal direction. Contours are reported at the 68%, 95%, and 99% CLs. (Bottom) Polarization in different energy bands for the three phase intervals, with contours showing the 90% CL.
Paper: X-Ray Polarized View of the Accretion Geometry in the X-Ray Binary Circinus X-1
Authors: John Rankin, Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Anna Bobrikova, Vadim Kravtsov, Fabio Muleri, Maura Pilia, Alexandra Veledina, Rob Fender, Philip Kaaret, Dawoon E. Kim, Andrea Marinucci, Herman L. Marshall, Alessandro Papitto, Allyn F. Tennant, Sergey S. Tsygankov, Martin C. Weisskopf, Kinwah Wu, Silvia Zane, Filippo Ambrosino, Ruben Farinelli, Andrea Gnarini, Iván Agudo, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, 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, Alan P. Marscher, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Fei Xie
Figure caption: Evolution of the X-ray properties of Cir X-1. (Top) Rate obtained by MAXI (2–20 keV) and IXPE over two orbits binned in 180 s time bins. (Bottom) HR obtained from IXPE (Equation (1)) during the observations binned in 500 s time bins. There is a clear change in state from the hard to the soft at the beginning of the IXPE observation; based on this, we divide the analysis into the three phase intervals indicated in the plots by the colored regions.
Paper: X-Ray Polarized View of the Accretion Geometry in the X-Ray Binary Circinus X-1
Authors: John Rankin, Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Anna Bobrikova, Vadim Kravtsov, Fabio Muleri, Maura Pilia, Alexandra Veledina, Rob Fender, Philip Kaaret, Dawoon E. Kim, Andrea Marinucci, Herman L. Marshall, Alessandro Papitto, Allyn F. Tennant, Sergey S. Tsygankov, Martin C. Weisskopf, Kinwah Wu, Silvia Zane, Filippo Ambrosino, Ruben Farinelli, Andrea Gnarini, Iván Agudo, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, 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, Alan P. Marscher, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Fei Xie
Figure caption: Illustration of a possible accretion geometry in Cir X-1. (Left) Low accretion rate case, when there is a gap between the disk and the NS surface, and the full SL is developed. (Right) High accretion rate case, where the disk touches the NS surface, and the BL is emitting (with a PA almost perpendicular to the symmetry axis of the disk).
Paper: X-Ray Polarized View of the Accretion Geometry in the X-Ray Binary Circinus X-1
Authors: John Rankin, Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Anna Bobrikova, Vadim Kravtsov, Fabio Muleri, Maura Pilia, Alexandra Veledina, Rob Fender, Philip Kaaret, Dawoon E. Kim, Andrea Marinucci, Herman L. Marshall, Alessandro Papitto, Allyn F. Tennant, Sergey S. Tsygankov, Martin C. Weisskopf, Kinwah Wu, Silvia Zane, Filippo Ambrosino, Ruben Farinelli, Andrea Gnarini, Iván Agudo, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, 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, Alan P. Marscher, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Fei Xie
Figure caption: Spectral energy distribution of Cir X-1 during P2 (left) and P3 (right) in EF  E  representation using NICER and NuSTAR (FPMA and FPMB) data and showing the different model components.
Paper: X-Ray Polarized View of the Accretion Geometry in the X-Ray Binary Circinus X-1
Authors: John Rankin, Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Anna Bobrikova, Vadim Kravtsov, Fabio Muleri, Maura Pilia, Alexandra Veledina, Rob Fender, Philip Kaaret, Dawoon E. Kim, Andrea Marinucci, Herman L. Marshall, Alessandro Papitto, Allyn F. Tennant, Sergey S. Tsygankov, Martin C. Weisskopf, Kinwah Wu, Silvia Zane, Filippo Ambrosino, Ruben Farinelli, Andrea Gnarini, Iván Agudo, 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, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, 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, Alan P. Marscher, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Fei Xie
Figure caption: Hardness–intensity (left) and color–color (right) diagrams during the IXPE observations, binned in time bins of 180 s, with color highlighting the three phase intervals chosen for the subsequent analysis.
Paper: On the Source Contribution to the Galactic Diffuse Gamma Rays above 398 TeV Detected by the Tibet ASγ Experiment
Authors: S. Kato, D. Chen, J. Huang, T. Kawashima, K. Kawata, A. Mizuno, M. Ohnishi, T. Sako, T. K. Sako, M. Takita, Y. Yokoe
Figure caption: Expected number of gamma-ray events above 398 TeV that would be observed by the Tibet ASγ experiment from the 22 newly reported sub-PeV LHAASO sources. For more details, see the main text.
Paper: Empirically Constraining the Spectra of Stellar Surface Features Using Time-resolved Spectroscopy
Authors: David Berardo, Julien de Wit, Benjamin V. Rackham
Figure caption: Proof-of-concept for stellar spectra retrieved using time-resolved spectroscopy. Examples of retrieved spectral signals for a photosphere and three spot features on a synthetic star. Their parameters—temperature, size, latitude (θ), and longitude (ϕ) in radians—are given in the bottom left corner of each panel and are kept fixed in this first retrieval. Synthetic and retrieved spectra are in orange and blue, respectively, and residuals at the bottom. For this example, we purposely use a nonphysical emission spectrum for spot #3 to emphasize that the framework reliably retrieves the emission spectra empirically.
Paper: Empirically Constraining the Spectra of Stellar Surface Features Using Time-resolved Spectroscopy
Authors: David Berardo, Julien de Wit, Benjamin V. Rackham
Figure caption: On the information content of time-resolved spectroscopy. Left: synthetic stellar surface with two spot features, shown halfway through a stellar rotation (phase = 0.5). Middle: individual contribution of each component’s time-dependent signal (showing their contribution as the star rotates, as well as effects of limb darkening, size, and 2D-projection). Right: their summed contributions produce a single time-varying hemisphere-integrated spectrum. We show the deviation from median flux as a function of time, to illustrate the variations due to surface features.
Paper: The Thickness of Galaxy Disks from z = 5 to 0 Probed by JWST
Authors: Jianhui Lian, Li Luo
Figure caption: Redshift evolution of galaxy disk thickness. Small blue circles indicate the sech2 scale height measurements of individual edge-on galaxies with only a photometric redshift estimate and orange circles for those with spectroscopic redshift. Filled circles are the galaxies with a valid uncertainty estimate and empty circles are those without. The level of uncertainties is shown at the bottom in gray. Enlarged black squares and error bars show the median scale length and 1σ  scatter at each redshift bin with a bin width of 0.5 at z < 3 and a bin width of 1 at z > 3. The converted sech2 scale height of the Milky Way’s thick and thin disks are denoted by the dashed and dashed–dotted lines, respectively.
Paper: The Thickness of Galaxy Disks from z = 5 to 0 Probed by JWST
Authors: Jianhui Lian, Li Luo
Figure caption: The 1D point-spread function (PSF) that is used for modeling the vertical surface brightness profile of edge-on galaxies in our sample. The 1D PSF is constructed by convolving the 2D PSF of JWST F115W images with an infinitesimally thick disk model of a given size. The left panel shows the 1D PSF measured at one effective radius for disk models of different sizes. The right panel illustrates the 1D PSF measured at different positions relative to the center for the same disk model with an effective radius of 0.″2.
Paper: The Thickness of Galaxy Disks from z = 5 to 0 Probed by JWST
Authors: Jianhui Lian, Li Luo
Figure caption: JWST/F115W images and vertical surface brightness profiles of eight example galaxies from low redshift at the top left to high redshift at the bottom right. In the image, the two gray shaded regions cover the pixels within 0.5– 1.5 R e. The length of 1 kpc at each corresponding redshift is illustrated at the bottom right corner of the image. In the VSBP panel, the retrieved VSBP and best-fitted sech2 model are shown as blue points and an orange curve. The obtained sech2 scale length is presented at the bottom. The line spread function obtained in Section 2.2 is also included as reference.
Paper: The Thickness of Galaxy Disks from z = 5 to 0 Probed by JWST
Authors: Jianhui Lian, Li Luo
Figure caption: Scale height as a function of stellar mass for galaxies in eight redshift bins. Each panel shows edge-on galaxies in one redshift bin. The symbols are the same as in Figure 4.
Paper: The Thickness of Galaxy Disks from z = 5 to 0 Probed by JWST
Authors: Jianhui Lian, Li Luo
Figure caption: The distribution of stellar mass and redshift of our edge-on galaxy sample.
Paper: NICER, NuSTAR, and Insight-HXMT Views to the Newly Discovered Black Hole X-Ray Binary Swift J1727.8-1613
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Peng-Ju Wang, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan
Figure caption: The schematic of the corona/jet of Swift J1727.8–1613. Left: the jet has high speed and may as well be blocked by the extended corona underneath and thus provides less disk reflection. This configuration corresponds to the fitting results for models M1* and M2, as shown in the right panel of Figure 3 and the left panel of Figure 6. Right: reflection is mainly contributed by the low speed jet and the jet base/corona underneath is mostly edge-on with respect to the view of the disk and thus provides less reflection than the jet. This configuration corresponds to the fitting results for models M1 and M3, as shown in the left panel of Figure 3 and the right panel of Figure 6.
Paper: NICER, NuSTAR, and Insight-HXMT Views to the Newly Discovered Black Hole X-Ray Binary Swift J1727.8-1613
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Peng-Ju Wang, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan
Figure caption: The simultaneous broadband spectrum of Swift J1727.8–1613 is observed from NICER (black), NuSTAR/FPMA (red), NuSTAR/FPMB (green), Insight-HXMT/ME (blue), and Insight-HXMT/HE (cyan). Left panel: the spectrum of model 1, with a relatively high Γ and E cut for the reflection component. The bottom panel is the residual of model 1 after removing cutoffpl. Right panel: the spectrum of model 1, with a relatively low Γ and E cut for the reflection component. The bottom panel is the residual of model 1 after removing cutoffpl.