adsabs/AstroCLIMB huggingface dataset:
Paper: Photon Orbit Signatures in Spectra of Black Hole Accretion Disks
Authors: Daniel C. M. Palumbo, George N. Wong, Angelo Ricarte
Figure caption: Spectroscopy of the photon ring as predicted by a one-zone model viewed from two angles, tuned to approximate the size and compact flux of the M87* accretion flow. Top row: thermal electron energy distribution with Θe = 10 and ne = 3 × 104 cm−3. Bottom row: power-law electron energy distribution with ﹩p=3,{\gamma }_{min}=100,{\gamma }_{max}=\rm{10,000}﹩, and ne = 5 × 102cm−3. Both models have B = 30 G. Left: an example spectrum from the model chosen to accentuate the effect, for which the n = 1 image contributes a prominent spectral flattening beyond the turnover frequency. Middle: the range of ratios between the spectral peaks of each subimage as a function of the emission angles in each image. Right: same as the middle, but for the frequency offset between the peaks.
Paper: Photon Orbit Signatures in Spectra of Black Hole Accretion Disks
Authors: Daniel C. M. Palumbo, George N. Wong, Angelo Ricarte
Figure caption: Cross section of the one-zone, two-angle model for the spectroscopy of the n = 0 and n = 1 images. Blue lines indicate field lines, while red rays show the optical path. The same uniform plasma occupies both cells, but the two cells make different angles of incidence with the rays, and the reduced on-sky area of the n = 1 image is represented by shrinking one dimension of the cube by e−π. In this example for a 5M cube emitter, the n = 0 magnetic field incidence angle is 135°, while the n = 1 is 45°; rays passing through the n = 1 region still experience radiative transfer through the n = 0 region. Both regions are assumed to be at rest.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: Complete velocity profiles of the absorption lines of the two USMg II structures toward J1306+3150 at z = 4.87. System 1 at z = 4.8634 and System 2 at z = 4.8821 are plotted in blue and red shadow, respectively. The Voigt fitting profiles of the Fe II, Si II, Al II, Al III, and Zn II lines in these two systems are plotted with the green and orange dashed lines, respectively. The vertical dashed lines indicate the positions of the subcomponents in the fittings of the two systems. The quasar spectra were taken with Magellan/FIRE, with a spectral resolution of R ∼ 6000.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: Upper: comparison of VSMG II Lyα line flux with other DLA hosts. The DLA data points are color-coded by the velocity width v90 of the Si II (λ1808) line. The Mg II system (Wr = 2.033 ± 0.187 Å and v90(λ2796) = 355 km s−1) at z = 3.188 in the MAGG survey (M. Galbiati et al. 2024) is plotted as a red triangle. The column density of H I for the two Mg II systems, including our z = 4.8651 VSMG II system, is extrapolated from the Wr(Mg II)−N(H I) relation in T.-W. Lan & H. Mo (2018). Lower: EWs of LAEs detected in the MUSE Hubble Ultra Deep Field and JADES surveys at 2 < z < 8.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: CLOUDY modeling of two absorbing systems at z ∼ 4.9 along the sight line J1306+3150. The observed values of System 1 at z = 4.8634 and System 2 at z = 4.8821 are plotted as the blue dashed and red dashed–dotted lines, respectively. The modeling curves are plotted with different metallicities (log(Z/Z⊙)), ranging from −2.5 to 0. From the upper left to the lower right, we plot the column density ratio of Al II to Al III against the ionization parameter and the column densities of Zn II, Si II, and Fe II against the ionization parameter, respectively.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: Example of the H I gas column density distribution around one disk galaxy at z ∼ 3 from TNG100, selected based on the disklike galaxy criteria in J. Liang et al. (2025). The simulated galaxy has similar stellar mass, halo mass, SFR, and Re to our detected galaxy. The left and right panels show face-on and edge-on views, respectively, of the same galaxy on a 100 × 100 kpc scale. The zoom-in box shows the stellar+gas content of the galaxy on a 10 × 10 kpc scale. The red dashed line is the major axis of the galaxy. The blue and yellow arrows in the right panel indicate the angular momentum directions of the disk and H I gas, respectively.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: SED fitting of J0305M31-He1-2708 using BAGPIPES. We use photometry from the JWST/NIRCam F115W, F200W, and F356W bands and from the HST F105W, F125W, F160W, F606W, and F814W bands, shown as the blue and black points in the upper panel, respectively. The orange ovals and curve in the upper panel represent the modeled photometry in each observed band and the SED. The lower panel shows the likelihood distributions of the fitted SFR, galaxy age, stellar mass, and specific SFR, respectively. The black dashed lines mark the 16th, 50th, and 84th percentiles of the posterior.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: GALFIT fitting of galaxy J0305M31-He1-2708 in F200W (upper) and F356W (lower). We use GALFIT to measure the effective radius (Re), Sérsic index, axis ratio, and PA. The cyan dashed line marks the major axis. Each row shows (from left to right) the JWST image, GALFIT model, and residuals (data minus model).
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: Dynamical modeling for the He I line in J0305M31-He1-2708. We plot the galaxy’s F356W image and the He I grism spectra in the upper panel. In the lower panel, we show the rotation model of the line and the best-fit Sérsic model convolved with the PSF, following the method in Z. Li et al. (2023). In the last column of panels, we present the fitting residuals.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: The 2D and 1D spectra of the host galaxy of the VSMG II absorber. The cutout imaging size is 2″ × 2″.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: The JWST/NIRCam imaging of J0305M31-He1-2708 in the F115W, F200W, and F356W bands. The last panel shows the ALMA tapered imaging, to increase the S/N. All images are 5″ × 5″ in size.
Paper: Neural Enhancement of the Traditional Wang–Sheeley–Arge Solar Wind Relation
Authors: Prateek Mayank, Enrico Camporeale, Arpit K. Shrivastav, Thomas E. Berger, Charles N. Arge
Figure caption: Distributions of the seven empirical WSA parameters optimized for each of the 129 CRs. The points are color-coded with their PCC with in situ observations.
Paper: Neural Enhancement of the Traditional Wang–Sheeley–Arge Solar Wind Relation
Authors: Prateek Mayank, Enrico Camporeale, Arpit K. Shrivastav, Thomas E. Berger, Charles N. Arge
Figure caption: Comparison of solar wind speed profiles at sub-Earth latitudes for CR2065. All WSA variants are propagated from 0.1 to 1 au using the HUX model. Panels (a)–(c) show wind speed maps along the elliptic plane, while panels (d) and (e) present the corresponding in situ speeds at 0.1 and 1 au, respectively.
Paper: Neural Enhancement of the Traditional Wang–Sheeley–Arge Solar Wind Relation
Authors: Prateek Mayank, Enrico Camporeale, Arpit K. Shrivastav, Thomas E. Berger, Charles N. Arge
Figure caption: Schematic diagram of the undertaken method to optimize and generalize the WSA solar wind speed maps. PFSS is used to derive expansion factor and minimum angular distance maps from synoptic magnetograms. These 2D maps serve as input for both neural optimizer and neural network. The L-BFGS scheme is employed to generate optimized 2D WSA maps by fitting the WSA parameters to OMNI data. A Swin Transformer–based neural network is trained on these optimized WSA maps to learn how to produce them directly from the PFSS-derived input maps.
Paper: Neural Enhancement of the Traditional Wang–Sheeley–Arge Solar Wind Relation
Authors: Prateek Mayank, Enrico Camporeale, Arpit K. Shrivastav, Thomas E. Berger, Charles N. Arge
Figure caption: Comparison of model performance across 129 CRs. Panels (a1)–(a4) show CR-wise variations of RMSE, MAE, DTW, and PCC for WSA and WSA+ with respect to OMNI data. Panel (b) plots the FIT score of WSA+ with sunspot number and performance tier. Panels (c1)–(c3) show distribution histograms of DTW, RMSE, and FIT score.
Paper: Neural Enhancement of the Traditional Wang–Sheeley–Arge Solar Wind Relation
Authors: Prateek Mayank, Enrico Camporeale, Arpit K. Shrivastav, Thomas E. Berger, Charles N. Arge
Figure caption: Comparison of Carrington maps of solar wind speed at 0.1 au for three representative CRs: CR2049, CR2080, and CR2161, at different phases of the solar cycle. Each row corresponds to a different CR, while columns show outputs from default WSA (left), per-CR optimized WSA (middle), and WSA+ (right).
Paper: Neural Enhancement of the Traditional Wang–Sheeley–Arge Solar Wind Relation
Authors: Prateek Mayank, Enrico Camporeale, Arpit K. Shrivastav, Thomas E. Berger, Charles N. Arge
Figure caption: Metric-wise comparison of WSA+ against default WSA across training, validation, and test sets.
Paper: Neural Enhancement of the Traditional Wang–Sheeley–Arge Solar Wind Relation
Authors: Prateek Mayank, Enrico Camporeale, Arpit K. Shrivastav, Thomas E. Berger, Charles N. Arge
Figure caption: Evolution of training and validation losses over 300 epochs of WSA+ model training.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Chandra ACIS spectrum of the Perseus Cluster’s thermal emission. We find a two-temperature model with low-temperature (1.65 keV) and high-temperature (4.39 keV) VAPEC components to be the best description of the 0.5–7 keV spectrum.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Example of a flare in the IXPE data, with the DU3 light curve as a reference. Panel (a) shows the 2–8 keV light curve from a 1′ circle centered around 3C 84. The flare is not obvious. Panels (b) and (c) show the light curve from the same time frame, but from the Perseus Cluster from annular regions between 3′–5′ and 6′–8′, respectively. The flare is much more prominent in the absence of 3C 84. Panel (d) shows the 3′–5′ light curve in 2–8 keV, outside the science window. The flare is still visible, indicating a likely nonastrophysical origin. In our subsequent analysis, we reject the flare times.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Multiwavelength brightness and polarization observation during the IXPE observations. The top panel shows the flux density in optical (R band), the second panel shows the host-corrected optical (R band) and millimeter radio (225.5 GHz) polarization degree (%), the third panel shows the optical and radio polarization angle (degrees), and the bottom panel shows the γ-ray photon flux 3-day binned light curves. The gray shaded areas mark the IXPE exposures over the entire observation. The horizontal red shaded area marks the projected direction of the jet. The error bars correspond to the 68% (1σ) confidence interval.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Optical brightness and polarization measurements during the IXPE observations. The top panel shows the brightness in magnitudes for different optical bands (BVRI), the middle panel the host-corrected polarization degree (%, R band), and the bottom panel the polarization angle (degrees, R band). The gray shaded areas mark the IXPE exposures over the entire observation. The different optical bands are marked with different symbols and colors as shown in the legend. The horizontal red shaded area marks the projected direction of the jet. The error bars correspond to the 68% (1σ) confidence interval.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Surface brightness profiles of Perseus (blue) and two example point sources of different brightness, MCG –5-23-16 (orange) and NGC 2110 (green). Left panel: 8–10 keV surface brightness profiles. It demonstrates that the NXB levels are the same in all three IXPE observations. Right panel: the corresponding 2–8 keV surface brightness profiles. Even at distances as far away as 6′, Perseus is at least a factor of ∼6 brighter than the point sources. Together, these two panels imply that the cluster is observed throughout and the NXB is much less than the astrophysical background.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Spectropolarimetric fit between Swift/XRT, NuSTAR, and IXPE. The left panel shows the 0.5–50 keV spectral fit, with XRT in gray; IXPE DUs in magenta, blue, and green; and NuSTAR FPMA and FPMB in red and cyan, respectively. The best-fit model consists of an absorbed power law, a narrow Gaussian at Fe K energies, and a two-temperature thermal model based on our Chandra fit. The right panel shows the corresponding fit for the Q and U spectra. We have shown the fit for only the DU1 for greater clarity. We assumed a constant polarization model for the fit.