adsabs/AstroCLIMB huggingface dataset:
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Compilation of estimates for the parameters associated with the progenitor of SN 2023ixf, including progenitor mass, CSM extent, and mass-loss rate. The techniques used to obtain the plotted estimates are indicated with distinct hatch patterns, such as pre-explosion progenitor identification, optical and UV observations, radio/X-ray observations, and hydrodynamical light-curve modeling. The horizontal solid lines, shown in different colors, represent our estimates derived from hydrodynamical light-curve modeling. Various wind velocities were assumed in different studies when estimating mass-loss rates, which are noted here for clarity: 10 km s−1 (J. E. Jencson et al. 2023; R. S. Teja et al. 2023a; M. C. Bersten et al. 2024; J. M. M. Neustadt et al. 2024; E. A. Zimmerman et al. 2024), 50 km s−1 (W. V. Jacobson-Galan et al. 2023; C. D. Kilpatrick et al. 2023; M. D. Soraisam et al. 2023; Y.-J. Qin et al. 2024), 70 km s−1 (D. Xiang et al. 2024), 115 km s−1 (E. Berger et al. 2023; D. Hiramatsu et al. 2023; Z. Niu et al. 2023; N. Smith et al. 2023; L. Martinez et al. 2024), and 150 km s−1 (K. A. Bostroem et al. 2023).
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Schematic illustration of the geometry (as viewed face-on by the observer) proposed for the CSM around the progenitor of SN 2023ixf depicted by its equatorial dense CSM and a clumpy, low-density extended CSM. The illustration on the left-hand side highlights the flash-ionized phase resulting from interaction with the dense CSM. On the right-hand side, we see an aspherical shock front arising after shock breaking out from the confined dense CSM and the continued interaction with the low-density extended CSM. CSM shows a projected major-to-minor axis ratio of 1.2, assuming an oblate geometry.
Paper: Joint Observation of a Series of Magnetic Holes by Tianwen-1 and MAVEN on Mars
Authors: T. Y. Zhou, H. S. Fu, Z. Z. Guo, J. B. Cao, Y. M. Wang, W. D. Fu, Z. Wang, M. Ge
Figure caption: Overview of measurements from the two satellites, Tianwen-1 and Mars Atmosphere and Volatile Evolution (MAVEN), on 2021 December 16. (a) The total magnetic field measured by Tianwen-1; (b) the B  y  component measured by Tianwen-1; (c) the B  x  component measured by Tianwen-1; (d) the B  z  component measured by Tianwen-1; (e) the ion spectrum measured by Tianwen-1; (f) the total magnetic field measured by MAVEN; (g) the B  y  component measured by MAVEN; (h) the B  x  component measured by MAVEN; (i) the B  z  component measured by MAVEN; (j) the ion density measured by MAVEN; (k) the ion spectrum measured by MAVEN. MSO represents the Mars Solar Orbital joints. The X MSO is directed from the center of the planet toward the center of the Sun, Y MSO points opposite to the direction of Mars’s orbital velocity component perpendicular to X MSO, and Z MSO completes the right-handed system.
Paper: Joint Observation of a Series of Magnetic Holes by Tianwen-1 and MAVEN on Mars
Authors: T. Y. Zhou, H. S. Fu, Z. Z. Guo, J. B. Cao, Y. M. Wang, W. D. Fu, Z. Wang, M. Ge
Figure caption: The positions of the two satellites, comparison of the MH signals, and schematic illustrations of the satellites crossing MHs. (a) The locations of MAVEN and Tianwen-1 in the X MSO–Z MSO plane; (b) the locations of MAVEN and Tianwen-1 in the X MSO–Y MSO plane; (c) the locations of MAVEN and Tianwen-1 in the X MSO–ρ MSO plane, ρ = (Y 2 + Z 2)1/2; (d) the V  x , V  y , and V  z  components of the proton velocity; (e) the total magnetic field measured by MAVEN; (f) the total magnetic field measured by Tianwen-1; (g), (h), (i) schematic illustrations of the satellites crossing MHs, where the red arrows represent the trajectory of MAVEN and the blue arrows represent the trajectory of Tianwen-1.
Paper: Joint Observation of a Series of Magnetic Holes by Tianwen-1 and MAVEN on Mars
Authors: T. Y. Zhou, H. S. Fu, Z. Z. Guo, J. B. Cao, Y. M. Wang, W. D. Fu, Z. Wang, M. Ge
Figure caption: Polarization analyses of the magnetic field fluctuation and electronic distribution, measured by MAVEN. (a) ∣B∣. (b) Spectrogram of ∣B∣, where the black curve denotes low frequency and the pink curve denotes 0.1 times electron cyclotron frequency. (c) Wave normal angle (WNA). (d) Planarity of waves. (e) Ellipticity of waves. The WNA varies from 0° to 90°. 90° denotes that the waves propagate perpendicular to the ambient magnetic field, and 0° denotes that the waves propagate parallel or antiparallel to the ambient magnetic field. The value of planarity varies between 0 and 1, with values close to 1 indicating that the other polarization parameters calculated by the SVD method are reliable. The value of ellipticity varies between −1 and 1, with 1 denoting right-hand polarization, −1 denoting left-hand polarization, and 0 denoting linear polarization. (f) The electronic spectra. (g) The parallel PSD and the perpendicular PSD as a function of electron energy inside the MH region. (h) The parallel PSD and the perpendicular PSD as a function of electron energy in the background solar wind. (i) Electronic distribution inside the MH region. (j) Electron distribution inside the solar wind region.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Backward orbit integrations of And III around M31 over the last 6 Gyr for a low-mass (M vir = 1.5 × 1012 M ⊙) and high-mass (M vir = 2 × 1012 M ⊙) M31 model, shown in solid and dashed lines, respectively. The black orbits adopt the HST + Sats M31 proper motion, while the red orbits assume a weighted average with M31's EDR3 proper motion. Andromeda’s disk lies along the X–Y plane, while the Milky Way lies along the negative X-axis.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Correction to absolute proper motions as given by EDR3 stars (left panel) and galaxies (middle panel); each of the two ACS chip catalogs is as indicated. The right panel shows the weighted averages as computed in Table 2. The symbols with large error bars in this panel correspond to the EDR3-based values. Note the difference in scale between the first two panels and the rightmost one.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: Top: turns parameter T  w  at t = 8 hr 12 minutes; the black contour shows the length-weighted twist parameter τ  w  = 6 identifying the flux rope. Bottom: Q; the flux rope is shaded yellow.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Overlap between the 1999 WFPC2 exposures (red symbols) and the modern 2014/2021 ACS/WFC exposures (blue symbols). Coordinates are a gnomonic projection of R.A. and decl. with the tangent point (ξ, η) = (0, 0) at And III’s center (A. W. McConnachie 2012).
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Spatial distribution, proper motions, and CMD of our two catalogs, for stars with proper-motion uncertainties ≤ 0.5 mas yr−1. The vector in the first panel marks the proper motion of And III with respect to M31 and its cone of uncertainty. M31's proper motion is the weighted average with the EDR3 proper motion from M. S. Pawlowski & S. T. Sohn (2021), see also Section 6.1.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Formal proper-motion uncertainty as a function of instrumental magnitude in F814W for the ACS chip 1 catalog. Two groups are highlighted: stars that have a 7 yr and a 22 yr baseline. A moving median is represented with a black line for each sample. For reference, the horizontal branch of And III is at magF814W ∼ 21.4, where a higher stellar density is apparent.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: Schematic summary of pseudostreamer CMEs combining our latest results with previous observational and simulation studies. Top row: low-expansion, jet-like CME events. Bottom row: high-expansion, fan-shaped CME events.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Distribution of formal proper-motion uncertainties in the two catalogs, corresponding to each ACS chip. Here we show uncertainties in μ  α ; we obtain a similar distribution for μ  δ .
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: Top row shows example snapshots of the observed vertical magnetic field B  r  (a), vertical electric current density J  r  (b), and the horizontal twisting electric field components ﹩{E}_{\theta }^{\mathrm{Tw}}﹩ (c), and ﹩{E}_{\phi }^{\mathrm{Tw}}﹩ (d) at the lower boundary at 23:47 UT on 2011 February 14, about 1.9 hr before the onset of the observed X-class flare. The bottom row shows a snapshot of the ξ field (e) for generating the random electric field ﹩{{\boldsymbol{E}}}_{h}^{\mathrm{random}}﹩ in Equation (8), and the resulting random electric field components ﹩{E}_{\theta }^{\mathrm{random}}﹩ (f), and ﹩{E}_{\phi }^{\mathrm{random}}﹩ (g) produced at the lower boundary when the ξ field is used with the B  r  given in panel (a).
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: (a) The observed vertical magnetic field B  r  and (b) the vertical electric current density J  r  measured from the vector magnetogram, compared with (c) the vertical electric current density J  r  obtained at the lower boundary of the simulation domain at time t = 1.506 hr, about the time of the onset of the first eruption in the simulation.
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: The top two panels show selected 3D magnetic field lines of the pre-eruption magnetic field just before the onset of the eruption at t = 1.51 hr, with the field lines colored in current density J (a) and in twist rate α (b). The middle row panels show the synthetic AIA 131 Å image (c) and synthetic AIA 94 Å image (d) at the same time. The bottom panels show in comparison the observed AIA 131 Å image (e) and 94 Å image (f) at, respectively, 2011 February 15 01:45:35 UT and 2011 February 15 01:46:28, which are about the time for the onset of the observed X2.2 flare.
Paper: The Role of Magnetic Skeleton in Solar Flare Filaments Activity
Authors: Juan Guo, Huaning Wang, Jingxiu Wang, Xiaoshuai Zhu, Jing Huang, Shanqiang Chen, Bingxian Luo, Siqing Liu, Yuanyong Deng, Jiaben Lin
Figure caption: Magnetic skeleton and flare filament activity. Panels (a) and (e) are local regions (marked by the dashed regions) of the AIA 171 Å image (panel (b)) and the AIA 1600 Å image (panel (f)), respectively. Panel (d) is the local HSOS Hα image in the same region as panels (a) and (e). The strong flare loops and patches marked by ellipses in panels (a), (d), and (e) are related to the small filament eruption. The weak flare patches marked with arrows in panels (d)–(e) are related to the large filament activity. The west boundaries of the large filament and flare ribbons are confined by the west closed fan (see panel (c) and panel (f)).
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: The 3D field lines of the magnetic field colored with the twist rate α (a) (see text for the definition of α), and the radial profiles of the horizontally averaged temperature (b), density (c), and the Alfvén and sound speeds (d) for the initial state of the simulation.
Paper: The Role of Magnetic Skeleton in Solar Flare Filaments Activity
Authors: Juan Guo, Huaning Wang, Jingxiu Wang, Xiaoshuai Zhu, Jing Huang, Shanqiang Chen, Bingxian Luo, Siqing Liu, Yuanyong Deng, Jiaben Lin
Figure caption: Magnetic skeleton and CME-like disturbance in AIA 193 Å difference images. The direction of the CME-like disturbance is in the ejection region of the magnetic skeleton. The field of view of the dashed line region is the same as that of Figure 3(c).
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: The simulation domain against the solar disk as viewed from the Earth perspective on 2011 February 15 at 02:00:00 UT. The gray scale image shows the full-disk SDO/HMI magnetogram of the normal magnetic field B  r .
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Ratio of the total carbon-burning reaction rate between E. Monpribat et al. (2022) and CF88 as a function of the temperature T 9 = T/109. The green line represents the HIN rates, whereas the HINRES rates are shown in red. The dashed blue line represents a ratio of 1. The shaded region depicts the range of typical temperatures characterizing 12C burning inside SAGB stars.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Distribution of the most important chemical elements for the M ZAMS = 7.50 M ⊙ models computed with the CF88 rate and different branching ratios (from upper left-hand side, in clockwise order, 50–50, 65–35, 90–10, and 80–20) at the beginning of the WD’s cooling path (∼105 K), pre- and post-Rayleigh–Taylor rehomogenization (upper panel, dashed and filled lines, respectively) and at the ZZ Ceti stage (∼12,000 K, lower panel). The gray region reflects the crystallized part of the star, with a crystallization level above 90%.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: The S* ratio of the alpha and proton channels. The measurements of K. U. Kettner et al. (1980), E. F. Aguilera et al. (2006), and T. Spillane et al. (2007) are shown as filled circles in the colors of dark green, red, and brown, respectively. The best fit, upper, and lower limits are shown as red lines. These limits are set at factors of 2.5 and 0.5 of the best fit, respectively.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Run of the maximum temperature of the flame (upper panel), the size of the CO core (middle panel), and the total 20Ne content left (lower panel) for all the reaction rates adopted for a M ZAMS = 8 M ⊙ model during the lapse of the carbon-burning phase.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Chemical structure for a 6.85 M ⊙ model computed with the CF88 reaction rate at the end of the C-burning phase. The flame is quenched before reaching the star’s center, leaving a core composed of CO surrounded by an ONe mantle.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Ratio of the 12C(12C, α)20 Ne to the 12C(12C, p)23 Na channel as a function of temperature. The color band indicates the region between the estimated upper and lower limits.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Chemical profiles for the most abundant elements at the end of the carbon-burning phase for an M ZAMS = 8 M ⊙ model for the three nuclear reaction rates adopted, namely, CF88 (solid lines), HINRES (dashed lines), and HIN (dotted lines). The branching ratio was set to 65% and 35% for the α- and p-channels, respectively. In this plot, X  i  is the element abundance per mass, whereas M  r  is the Lagrangian mass coordinate.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Chemical structure for a 7.50 M ⊙ model at the end of the C-burning phase for models adopting the CF88 reaction rate with [55/45], [65/35], and [90/10] branching ratios (dashed, dotted, and solid lines, respectively).
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption:  K X as a function of bolometric luminosity of type 2 AGN. The red square is J1714+6027 (the error bar is in 1σ). The orange and blue lines are the measurements (solid) and extrapolation (dotted) derived in E. Lusso et al. (2012) and F. Duras et al. (2020), respectively. The dashed lines correspond to the 1σ spread of the samples used in the two works. The bolometric luminosities of the type 2 AGN in their work span a range from 1042 erg s−1 to 2 × 1046 erg s−1. Beyond these bolometric luminosities, the K X-correction was extrapolated from the measured data following K X = a[1+(log(L BOL/L ☉)/b) c ]. a, b, c are coefficients that were measured to be constants as a function of the bolometric luminosity.
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: Best-fit SED fitting result from CIGALE and relative residual. The line styles for each module are listed in the key. Relative residual is defined as (Obs–Mod)/Obs, where Obs is the observation data and Mod is the model prediction.
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: X-ray spectra (in the observed frame) of J1714+6027 fitted using phenomenological, MYTorus (edge-on and face-on), and borus models. The black and red points correspond to NuSTAR and XMM-Newton data, respectively. The solid, dashed, and dotted lines correspond to the model predictions from the total, line-of-sight component, and reflection components, respectively.
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: The 2011 XMM-Newton observed X-ray spectrum (in observed frame) of J1714+6027 fitted using the phenomenological model described in Section 2.2.1. The spectra are grouped with a minimum of 2 counts per bin. The red points correspond to the data, and the solid line is the best-fit model prediction.
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: Contour of the 2–10 keV flux as a function of the line-of-sight column density of the 2011 (yellow) and 2021 (green) observations. We present the fitting results from the phenomenological model of both observations. The dark and light colors represent the 68% and 90% confidence levels, respectively.