adsabs/AstroCLIMB huggingface dataset:
Paper: Quasiperiodic Oscillation in Short Gamma-Ray Bursts from Black Hole–Neutron Star Mergers
Authors: Yan Li, 彦 李, Rong-Feng Shen, 荣锋 申, Bin-Bin Zhang, 彬彬 张
Figure caption: Predicted sGRB light curve with the appearance of the QPO. We compute four different sets of θ obs, θ bd, and θ  c  (i.e., the half opening angle of the jet core), whose exact values are shown in the legend. ϕ obs and ϕ jet,0 are set to 0 and 0.3π, respectively. The precession period is set to 0.1 s. The starting time for the wind ejection, i.e., the appearance time for the QPO, is set to 0.4 s. We adopt a Gaussian jet with Γ c  = 100. The intrinsic intensity (Equation (19)) is normalized to 1 (gray dashed line).
Paper: Quasiperiodic Oscillation in Short Gamma-Ray Bursts from Black Hole–Neutron Star Mergers
Authors: Yan Li, 彦 李, Rong-Feng Shen, 荣锋 申, Bin-Bin Zhang, 彬彬 张
Figure caption: Schematic diagram for the evolution of the accretion rate (black solid line) after a compact binary merger. After reaching the maximum accretion rate at t = t 0 (gray solid line), the accretion rate starts to decrease with time as ﹩{\dot{M}}_{\mathrm{acc}}\propto {t}^{-\eta }﹩. Initially, as the accretion rate is higher than ﹩{\dot{M}}_{\mathrm{ign}}﹩ (black dashed line), the disk stays in the neutrino-cooled state. Once the accretion rate evolves to be lower than ﹩{\dot{M}}_{\mathrm{ign}}﹩, the disk enters into the ADAF state and a viscosity-driven wind is ejected. The intersection between the black solid and black dashed lines shows the starting time of the ejection of the disk wind, which is denoted as t w and marked by the gray dashed line. Due to the ejection of the wind, the accretion rate for the ADAF state drops more sharply compared with that for the NDAF state. The gray dashed–dotted line (t jet) denotes the launching time of the relativistic jet.
Paper: Quasiperiodic Oscillation in Short Gamma-Ray Bursts from Black Hole–Neutron Star Mergers
Authors: Yan Li, 彦 李, Rong-Feng Shen, 荣锋 申, Bin-Bin Zhang, 彬彬 张
Figure caption: Schematic illustration of the geometry of the model. The blue dashed–dotted line represents the axis of the deflected jet, which is inclined to the Z-axis (equivalent to the spin axis of the BH) with an angle roughly equal to θ bd. θ obs denotes the angle between the LOS and the spin axis of the BH. ϕ obs (ϕ jet) denotes the angle between the projection of the LOS (axis of the deflected jet) and the arbitrary X-axis. θ v represents the angle between the LOS and the jet axis, which varies with time due to the periodic change in ϕ jet.
Paper: Quasiperiodic Oscillation in Short Gamma-Ray Bursts from Black Hole–Neutron Star Mergers
Authors: Yan Li, 彦 李, Rong-Feng Shen, 荣锋 申, Bin-Bin Zhang, 彬彬 张
Figure caption: Schematic illustration for the configuration of the BH–disk system (edge-on view) right after a BH–NS merger. Initially, the jet aligns with the BH spin,  J  BH, but the ejection of the wind (blue) from the disk (red) deflects and collimates the jet, causing it to align with the momentum of the disk,  J  disk. θ bd represents the angle between  J  BH and  J  disk, and is also the angle between  J  BH and the deflected jet.
Paper: Quasiperiodic Oscillation in Short Gamma-Ray Bursts from Black Hole–Neutron Star Mergers
Authors: Yan Li, 彦 李, Rong-Feng Shen, 荣锋 申, Bin-Bin Zhang, 彬彬 张
Figure caption: Observed isotropic-equivalent energies normalized to their corresponding maximum values as a function of the viewing angle θ v for the Gaussian jet model (red and blue lines). The blue and red lines correspond to Γ c  = 100 and 300, respectively. The half opening angle of the jet core θ  c  is set to 5°. The normalized intrinsic energy profile for the Gaussian jet, i.e., ﹩{e}^{-{\left(\theta /{\theta }_{{\rm{c}}}\right)}^{2}}﹩, is shown as the dashed line for comparison.
Paper: Quasiperiodic Oscillation in Short Gamma-Ray Bursts from Black Hole–Neutron Star Mergers
Authors: Yan Li, 彦 李, Rong-Feng Shen, 荣锋 申, Bin-Bin Zhang, 彬彬 张
Figure caption: Precession period of the accretion disk varying with ζ. The outer radii for the dashed, solid, and dotted–dashed lines are 15R S, 10R S, and 5R S, respectively. The mass and spin of the BH are set to 5M ⊙ and 0.8, respectively.
Paper: Quasiperiodic Oscillation in Short Gamma-Ray Bursts from Black Hole–Neutron Star Mergers
Authors: Yan Li, 彦 李, Rong-Feng Shen, 荣锋 申, Bin-Bin Zhang, 彬彬 张
Figure caption: Two typical sGRB light curves with the appearance of the QPO. The black solid line represents the scenario that the early main burst of an off-axis sGRB could be invisible but followed by an observable QPO due to the precessing jet. The light curve of an on-axis sGRB with an observable main burst (gray dashed line), which is the same as the green line in Figure 6, is shown for comparison.
Paper: Modeling of the High-velocity Jet Powered by the Massive Star MWC 349A
Authors: Antonio Martínez-Henares, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Alejandro Báez-Rubio
Figure caption: Centroid maps of the H30α emission of MWC 349A from ALMA (dots with error bars) and the model (line). (a) The model in Báez-Rubio et al. (2013); (b) we incorporate a jet; (c) half of the outflow Keplerian rotation is removed; (d) the deceleration parameter b  v  = −0.05 is included. The red star symbol is located at the (0, 0) position, i.e., the peak of the continuum emission.
Paper: Modeling of the High-velocity Jet Powered by the Massive Star MWC 349A
Authors: Antonio Martínez-Henares, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Alejandro Báez-Rubio
Figure caption: Sketches that illustrate the geometry and kinematics of the model. The two diagrams share common features: the ionized gas is located inside the cone delimited by the layer of thickness θ  d , corresponding to the Keplerian ionized disk. The neutral disk is located beyond this layer. The disk is tilted an angle θ  i  with respect to the plane of the sky, and the jet orientation is represented as (θ jet, φ jet). Left: shaded gray areas inside the double cone represent the jet velocity, with darker tones indicating higher velocity values. The jet has a certain collimation; hence the velocity decreases with the angular distance to the jet axis (θ jet, φ jet). Right: kinematic components of the model. We show a vertical cut of the northern cone. The dotted line at small radius from the central star indicates the launching radius of the outflow at ∼24 au from the star (Báez-Rubio et al. 2014). Large colored arrows surrounded by the dotted curve correspond to the jet expansion velocity ﹩{\vec{v}}_{\mathrm{jet}}﹩, which becomes lower with larger angular distances from the jet orientation due to collimation. Darker blue (red) colors indicate a higher projection of the blueshifted (redshifted) jet expansion along the line of sight. Straight black arrows represent the wind expansion velocity ﹩{\vec{v}}_{\mathrm{wind}}﹩ and are smaller at larger radial distances to account for the radial deceleration b  v ; curved black arrows represent the wind rotation velocity component ﹩{\vec{v}}_{\mathrm{rot}}﹩ and are smaller in the ionized wind than in the disk, because in the former the wind rotates at half the Keplerian velocity in our model (Section 3.2). Neither of the diagrams is to scale.
Paper: Modeling of the High-velocity Jet Powered by the Massive Star MWC 349A
Authors: Antonio Martínez-Henares, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Alejandro Báez-Rubio
Figure caption: Line profile of the H30α (left panels) and H26α (right panels) from observations (blue) and the final model (red). Each lower panel is a zoom-in of the panel above at the lower intensity values. The double peak traces emission from the ionized disk, while the weaker features at higher radial velocities (the “wing humps”) arise from the outflow. The minimum intensity of the double peak is located at the systemic velocity of the source, 8 km s−1.
Paper: Modeling of the High-velocity Jet Powered by the Massive Star MWC 349A
Authors: Antonio Martínez-Henares, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Alejandro Báez-Rubio
Figure caption: Band 6 217 GHz and band 7 342 GHz continuum maps from ALMA (black contours) and the model (red contours). The ellipse in the lower left part of each image represents the synthesized beam of observations. Contour levels are [10, 30, 50, 70, 100, 200, 300, 500] times the rms noise of the maps (0.48 mJy beam−1 for band 6 and 1.4 mJy beam−1 for band 7).
Paper: Modeling of the High-velocity Jet Powered by the Massive Star MWC 349A
Authors: Antonio Martínez-Henares, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Alejandro Báez-Rubio
Figure caption: Rotation curves of the H30α (top) and H26α (bottom) centroids. The distance from the center is calculated as ﹩\sqrt{{\rm{\Delta }}{\alpha }^{2}+{\rm{\Delta }}{\delta }^{2}}﹩. Observations are represented with circles, while the model result is represented by the colored line.
Paper: Modeling of the High-velocity Jet Powered by the Massive Star MWC 349A
Authors: Antonio Martínez-Henares, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Alejandro Báez-Rubio
Figure caption: Observed H30α centroids (colored points with error bars) and an identification of the terms used in the discussion to describe the different parts of the map. Redder (bluer) colors represent more redshifted (blueshifted) emission. The centroid positions are located in the plane of the sky, where north is up and east is left: we have not shown the axes for clarity. See, e.g., Figure 4 to see the axes. The red star symbol is located at the (0, 0) position, i.e., the peak of the continuum emission.
Paper: Modeling of the High-velocity Jet Powered by the Massive Star MWC 349A
Authors: Antonio Martínez-Henares, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Alejandro Báez-Rubio
Figure caption: Centroid map of the H26α emission of MWC 349A from ALMA (dots with error bars) and the final model (line). The red star symbol is located at the (0, 0) position.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Histograms of the cosine of the relative angles between parental clump rotation axis Ω 0 and the integrated angular momentum ﹩{{\boldsymbol{L}}}_{\mathrm{core}}﹩, for all bound cores formed in different models. The black line shows the expected distribution for an isotropic orientation of ﹩{{\boldsymbol{L}}}_{\mathrm{core}}﹩. In the legends, the orientation parameter ﹩{S}_{L,{\rm{\Omega }}}=(3\langle {\cos }^{2}\measuredangle [{{\boldsymbol{L}}}_{\mathrm{core}},{{\boldsymbol{\Omega }}}_{0}]\rangle -1)/2﹩ for each model is shown, and values with S  L,Ω > 0.25 are indicated in bold. θ 0 = 0° cases are shown in the first row, while θ 0 = 45° cases are shown in the second row. In all models with weak turbulence (indicated by blue lines), there is a clear tendency for ﹩{{\boldsymbol{L}}}_{\mathrm{core}}﹩ and Ω 0 to align. On the other hand, in the strong turbulence models (indicated by red lines), the angles are close to being isotropically distributed and no tendency for alignment is observed.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Histograms of the cosine of the relative angle between the initial magnetic field  B  0 and the mean magnetic field within the core, ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩, for bound cores formed in different models. The black line shows the expected distribution for an isotropic orientation of ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩. In the legends, the orientation parameter ﹩{S}_{B,{B}_{0}}=(3\langle {\cos }^{2}\measuredangle [{{\boldsymbol{B}}}_{\mathrm{core}},{{\boldsymbol{B}}}_{0}]\rangle -1)/2﹩ for each model is shown, and values with ﹩{S}_{L,{B}_{0}}\gt 0.25﹩ are indicated in bold. Rotation setup models with θ 0 = 0° are shown in the top panel, while θ 0 = 45° models are shown in the middle panel. w/o Setup models are shown in the bottom panel. Generally, in models with strong magnetic fields (indicated by dashed lines), the strong alignment of ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩ with  B  0 is observed.
Paper: Evolutionary Origins of Binary Neutron Star Mergers: Effects of Common Envelope Efficiency and Metallicity
Authors: Monica Gallegos-Garcia, Christopher P. L. Berry, Vicky Kalogera
Figure caption: Final outcomes for the simulations at a fixed donor mass of M donor = 8 M ⊙ as a function of NS companion mass and initial orbital period at subsolar metallicity 0.1Z ⊙ and α CE = 1. We show only the prescription following Tauris et al. (2015) to determine ECSNe. With an NS mass of M NS = 2.0 M ⊙, we find a nonzero BNS merger fraction following only stable MT.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Cosine of the relative orientation angles of ﹩{{\boldsymbol{L}}}_{\mathrm{core}}﹩ pairs as a function of their separation distances. The data are averaged in various separation distance bins, with the size of the circle representing the number of samples in each distance bin. The black dashed line indicates ﹩\cos \,45^\circ ﹩. The models with θ 0 = 0° and 45◦ are presented together. Rotation Setup is shown in the top panel and w/o Setup in the bottom panel. In the Rotation Setup, a stronger alignment of ﹩{{\boldsymbol{L}}}_{\mathrm{core}}﹩ pairs is observed, especially when the turbulence is weak (﹩{ \mathcal M }=1.5﹩).
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Sample map from simulations considered in this study. The column density, as viewed along the z-axis, is shown. The top two rows display one of the Rotation Setup models (Rot-M5-B10P) at 0.0 and 0.32 Myr. The orientation of the rotation axis of the clump is indicated by the symbol “⨂” pointing in the direction of the z-axis. The bottom two rows display one of the Collision Setup models (Col-M5-B10P) at 0.0 and 0.17 Myr. In the Collision Setup, the initial clump does not have an overall rotational velocity. However, after the collision, the two clumps rotate around their center due to the off-center configuration. The positions of bound cores identified in simulations are additionally plotted as red open circles.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Cosine of the relative orientation angles of ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩ pairs as a function of their separation distances. The presentation method is similar to Figure 3. Models with strong magnetic fields (B 0 = 100 μ G) have a higher degree of alignment of ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩ pairs compared to models with weak magnetic fields (B 0 = 10 μ G).
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Cumulative distribution function of the cosine of the relative angle between the mean magnetic field ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩ and the angular momentum ﹩{{\boldsymbol{L}}}_{\mathrm{core}}﹩, compared to the expected CDF (black lines) for a completely uniform distribution. Rotation Setup models with θ 0 = 0° are shown in the top panel, while θ 0 = 45° models are shown in the middle panel. The bottom panel shows the results of w/o Setup. In most models, suggesting random distributions of ﹩\measuredangle [{{\boldsymbol{L}}}_{\mathrm{core}},{{\boldsymbol{B}}}_{\mathrm{core}}]﹩.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Same as Figure 2 except for Collision Setup models. Fast collision velocity cases with θ 0 = 0° are shown in the top panel and those of θ 0 = 45° are shown in the middle panel. Slow collision velocity cases are shown in the bottom panel. For all models in the Collision Setup, the angles are close to being isotropically distributed and no tendency for alignment is observed.
Paper: Properties of Electron-scale Magnetic Reconnection at a Quasi-perpendicular Shock
Authors: Ao Guo, Quanming Lu, San Lu, Shimou Wang, Rongsheng Wang
Figure caption: Evolution of different physical values at a traced X point from Ω i0 t = 11.27–11.93. (a) Electron current in the z-direction. (b) The magnetic flux between the traced X and O points Δψ = ψ  X  − ψ  O . (c) Reconnection electric field E  R  (blue line) and the gradient of the magnetic flux ﹩\tfrac{d{\rm{\Delta }}\psi }{{dt}}﹩(orange line). (d) The conversion efficiency of electromagnetic energy in z-direction at the X point E  R  J  ez . (e) Distance between the X point and the shock front (﹩x^{\prime} ﹩).
Paper: Crossing the Rubicon of Reionization with z ∼ 5 QSOs
Authors: Andrea Grazian, Konstantina Boutsia, Emanuele Giallongo, Stefano Cristiani, Fabio Fontanot, Manuela Bischetti, Angela Bongiorno, Giorgio Calderone, Guido Cupani, Valentina D'Odorico, Chiara Feruglio, Fabrizio Fiore, Francesco Guarneri, Matteo Porru, Ivano Saccheo
Figure caption: The G − R vs. I − Z color selection criterion for z ∼ 5 QSO candidates in the HSC-Udeep survey. The black dots are all the objects with magnitude magZ ≤ 20.0, and the red asterisks show the known QSOs with 4.5 ≤ z spec ≤ 5.2 drawn from SDSS DR17 (Abdurro’uf et al. 2022). The dark-green open pentagons are the known very bright QSOs with 4.5 ≤ z spec ≤ 5.0 from the QUBRICS survey (Grazian et al. 2022), for which synthetic HSC photometry is derived starting from the observed SkyMapper photometry through SED fitting at their fixed spectroscopic redshift. The big blue circles are the three confirmed QSOs with 4.5 ≤ z spec ≤ 5.2 in the HSC-Udeep area, while the big dark-green circles indicate known QSOs at 3.5 < z spec < 4.5. The cyan circle is a confirmed low-redshift object. The green lines indicate the color criteria for selecting bona fide z ∼ 5 QSO candidates, while the green squares are the QSO candidates identified in the HSC-Udeep region. Bona fide stars are identified through accurate measurements of parallaxes and proper motions by Gaia DR3 and are marked by magenta stars. The gray tracks are the simulated colors of synthetic QSOs in the redshift range 4.5 < z < 5.2.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Median profile (black line) and standard deviation (red line) of the 141 draped magnetic field profiles. The 141 individual profiles are plotted as thinner gray lines.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Temporal variations of model simulated profiles. (a) Profiles of ion velocity. The profiles for t = 0 s, 50 s, and 100 s are divided by 50, 3, and 3, respectively, to compare with others. (b) Profiles of magnetic field strength.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Similar to Figure 8, but showing profiles of simulated vertical ion velocity W  i  with different oscillation periods (T) of undulating magnetic fields at the upper boundary. W  i  is positive for upward-moving ions. (a) T = 104 s; (b) T = 5 × 103 s; (c) T = 2 × 103 s; (d) T = 103 s; (e) T = 5 × 102 s; (f) T = 2 × 102 s.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Observational and modeled density and temperature profiles during the MAVEN DD2 period. (a) Median profiles of ﹩{{\rm{O}}}_{2}^{+}﹩, O+, and CO2 + density from MAVEN observations. The dashed line is a fitted curve for total ion density using the function from Sánchez-Cano et al. (2013). (b) Profiles of neutral species (CO2, O, N2, CO) from Wu et al. (2021). (c) Electron, ion, and neutral temperature from Wu et al. (2021). (d) Calculated timescales of magnetic field diffusion, transport, and ﹩{{\rm{O}}}_{2}^{+}﹩ recombination.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Simulated magnetic field profiles with different oscillation periods (T) of undulating magnetic fields at the upper boundary. (a) T = 104 s; (b) T = 5 × 103 s; (c) T = 2 × 103 s; (d) T = 103 s; (e) T = 5 × 102 s; (f) T = 2 × 102 s; (g) T = 102 s; (h) T = 10 s; (i) T = 1 s.
Paper: Crossing the Rubicon of Reionization with z ∼ 5 QSOs
Authors: Andrea Grazian, Konstantina Boutsia, Emanuele Giallongo, Stefano Cristiani, Fabio Fontanot, Manuela Bischetti, Angela Bongiorno, Giorgio Calderone, Guido Cupani, Valentina D'Odorico, Chiara Feruglio, Fabrizio Fiore, Francesco Guarneri, Matteo Porru, Ivano Saccheo
Figure caption: The best-fit SED (left) and the χ 2(z phot) at different redshifts (right) for three known QSOs at z spec ∼ 5 in the HSC-Udeep survey.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Altitudinal profiles of the standard deviation of the simulated magnetic field. The profiles in each panel of Figure 8 are used to calculate the standard deviation for different oscillation periods (T) at the upper boundary.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Gaussian-smoothed (using a 7.″38 radius Gaussian; left) and adaptively smoothed (right) background-subtracted and exposure-corrected composite X-ray images in the 0.7–7 keV energy range, with 1.4 GHz VLA FIRST (green) and 150 MHz TGSS (cyan) radio contours.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: X-ray image (left) showing the region used to plot the azimuthal surface brightness profile (right) across the eastern NAT source, to highlight the decreased X-ray emission surrounding the NAT, discussed in Section 3.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Optical image from DSS, with the 1.4 GHz (green) and 150 MHz (blue) radio contours, as well as black contours showing the X-ray emission from the adaptively smoothed image. The red ellipses mark the point sources detected by wavdetect. The magenta “x” marks the peak of the X-ray emission.