adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Probability distribution functions of spatially resolved D4000 (left panel) and mean quenched fraction (﹩{\bar{f}}_{{\rm{q}}}﹩, right panel) for our galaxy sample. In the left panel, we show the result for D4000 of spaxels within 1.5R e and the gray dashed line indicating D4000th = 1.55. In the right panel, ﹩{\bar{f}}_{{\rm{q}}}﹩ is calculated with D4000th = 1.55.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: The sSFR vs. M q/M * for QCCs. The sSFR is measured within the whole galaxy rather than within the QCC.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: The black circles show the predicted M BH vs. M * relation for FQGs (left) and the predicted M BH vs. M q relation for QCCs (right). The M BH is calculated using Equation (8). The yellow bands show the predicted M BH–M * relation (Equation (10)) and its 1-Δ uncertainty based on the best fit of the QGSR. The color-coded symbols and lines show the observational data (BH2 sample) with dynamically measured black hole masses and their best fits, taken from Graham & Sahu (2023). The red circles are elliptical galaxies, pink triangles are ES/S0 galaxies, and blue squares are spiral galaxies. The left panel shows M BH vs. M * while the right panel shows M BH vs. M sph, where M sph is the mass of the spheroid component in a galaxy, derived using the decomposition technique. The purple/red/pink/blue lines show the best fit for early-type (elliptical+ES/S0), elliptical, ES/S0, and spiral galaxies, respectively. We convert their Kroupa (Kroupa 2002) IMF to our Salpeter (Salpeter 1955) IMF by adding 0.30 dex in the stellar mass (see Table 2 in Bernardi et al. 2010).
Paper: Simple Convective Accretion Flows (SCAFs): Explaining the ≈ −1 Density Scaling of Hot Accretion Flows around Compact Accretors
Authors: Wenrui Xu, 文睿 许
Figure caption: Slope of the self-similar density profile −α  ρ  for different choices of the adiabatic index γ. All runs in this figure have r acc = 2 × 10−3 r 0 (﹩{l}_{\max }=8﹩). There are three main regimes. At intermediate values of γ, we see behavior similar to our fiducial γ = 5/3 runs, with approximately constant α  ρ . At large γ, turbulence is weaker and α  ρ  is set by marginal convective instability, α  ρ  = −1/(γ − 1) (Section 4.3). At small γ (open markers), a small disk resembling a CDAF forms spontaneously around the accretor (Section 4.4). The slopes are estimated using the mean density profile for r/r acc ∈ [1, 20] for runs exhibiting SCAFs (solid markers) and r/r acc ∈ [1, 5] for runs exhibiting spontaneous disk formation (open markers; this range corresponds to the self-similar disk portion of the flow). Markers and error bars show the median and 16th/84th percentiles of local density slope ﹩d\mathrm{log}\bar{\rho }/d\mathrm{log}r﹩, respectively.
Paper: Simple Convective Accretion Flows (SCAFs): Explaining the ≈ −1 Density Scaling of Hot Accretion Flows around Compact Accretors
Authors: Wenrui Xu, 文睿 许
Figure caption: Radial profile of our fiducial simulations (γ = 5/3, smooth sink). Each column shows results from a different r acc, and results from other r acc are plotted in light gray lines for comparison. The rows show density ρ, density compensated by r −0.8, temperature P/ρ, radial velocity v  r  2, tangential velocity ﹩{v}_{\perp }^{2}﹩, and the normalized Bernoulli parameter B/∣Φ∣. Here the Bernoulli parameter B is defined as B = E tot + P + Φ, with E tot being the total (kinetic + thermal) energy and Φ = −GM ρ/r being the gravitational energy. Temperature and velocities are normalized by ﹩{v}_{{\rm{K}}}^{2}﹩. The shaded area shows the variability of the flow, with the shade spanning between 16th and 84th percentiles. Solid lines mark regions in a steady state, which we define as where the integration time is longer than 100× the local dynamical timescale r/v  r,rms. The profiles are relatively insensitive to r acc and becomes approximately self-similar at small radii.
Paper: Simple Convective Accretion Flows (SCAFs): Explaining the ≈ −1 Density Scaling of Hot Accretion Flows around Compact Accretors
Authors: Wenrui Xu, 文睿 许
Figure caption: Comparison between runs with different inner boundary conditions (marked by colors) and different r acc. Top panel: compensated radial density profiles similar to those in Figure 2. Colored and gray lines show the parts of the flow that have and have not reached a steady state, respectively; runs with different r acc are marked by different line styles. For small r acc, we see a tendency of convergence toward α  ρ  ≈ −0.8. Bottom panel: accretion rates. Dots show the mean accretion rate, error bars the 16th and 84th percentiles, and shaded areas the distribution. For small r acc, the accretion rate is consistent with a power-law scaling of ﹩{\alpha }_{\dot{M}}\approx 0.7﹩.
Paper: Simple Convective Accretion Flows (SCAFs): Explaining the ≈ −1 Density Scaling of Hot Accretion Flows around Compact Accretors
Authors: Wenrui Xu, 文睿 许
Figure caption: Left and center: density and azimuthal velocity of a snapshot taken from our γ = 4/3 run with r acc = 2 × 10−3 r 0 (﹩{l}_{\max }=8﹩), showing a disk/torus resembling a CDAF at the center. We pick an epoch when the disk angular momentum is approximately in the y-direction. Right: flow properties in disk coordinates, averaged over spherical surfaces and over time. Here the r, θ, ϕ directions are defined separately for each snapshot and each radius, with the pole aligned with the total angular momentum within this radius. At r ≲ few times 10−2 r 0, the flow is supported by rotation (together with pressure) and the velocity is mainly in the azimuthal (ϕ) direction. The amplitude of the azimuthal velocity agrees well with the CDAF theory, which predicts ﹩{v}_{\phi }^{2}/{v}_{{\rm{K}}}^{2}=0.77﹩ for γ = 4/3 (Quataert & Gruzinov 2000, Equation A15).
Paper: Simple Convective Accretion Flows (SCAFs): Explaining the ≈ −1 Density Scaling of Hot Accretion Flows around Compact Accretors
Authors: Wenrui Xu, 文睿 许
Figure caption: Contribution of different sources to the evolution of kinetic energy ∂ t  E  k  (with ﹩{E}_{k}\equiv \tfrac{1}{2}\overline{\rho {v}^{2}}﹩), normalized by E  k ΩK. Each line corresponds to a term in Equation (8) and is marked with a different color. Solid/dashed lines represent positive/negative contributions. Buoyancy (convection) is the main source of kinetic energy. This figure combines data from three simulations: r acc ≈ 3 × 10−5 r 0 (﹩{l}_{\max }=14﹩) for r/r 0 < 10−2, r acc ≈ 2 × 10−4 r 0 (﹩{l}_{\max }=11﹩) for 10−2 < r/r 0 < 10−1, and r acc ≈ 2 × 10−3 r 0 (﹩{l}_{\max }=8﹩) for r/r 0 > 10−1. This produces minor discontinuities at the intersections.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: The black circles show the predicted M BH vs. σ in for FQGs (left) and QCCs (right). The M BH is calculated using Equation (8). The yellow bands show the predicted M BH–σ in relation (Equation (9)) and its 1-Δ uncertainty based on the best-fitting of the QGSR. The red circles show the observational data (BH1 sample) with dynamically measured black hole masses, taken from Saglia et al. (2016). The solid red lines show the best fit of the BH1 sample, also taken from Saglia et al. (2016).
Paper: Simple Convective Accretion Flows (SCAFs): Explaining the ≈ −1 Density Scaling of Hot Accretion Flows around Compact Accretors
Authors: Wenrui Xu, 文睿 许
Figure caption: A snapshot taken from our fiducial simulation (γ = 5/3, smooth sink) with r acc = 3.1 × 10−5 r 0 (﹩{l}_{\max }=14﹩). First row: a slice at z = 0 showing the density profile at different scales; the circles mark r = r 0 and r = r acc. Each panel is a 50× zoom-in of the previous one. Second row: the same slice mapped into polar coordinates. Last two rows: same as the first two rows, but showing the radial velocity normalized by ﹩{v}_{{\rm{K}}}\equiv \sqrt{{GM}/r}﹩. The flow shows strong, large-scale turbulence.
Paper: Hybrid Simulation and Quasi-linear Theory of Bi-Kappa Proton Instabilities
Authors: R. A. López, P. H. Yoon, A. F. Viñas, M. Lazar
Figure caption: Growth rates of the proton-cyclotron instability (quasi-parallel propagation) and mirror-mode instability, computed using the full-spectrum dispersion solver DIS-k (López 2023; top) and the approximations according to Equations (5) and (8) (normalized using Equations (9) and (10)) in the bottom panel, respectively. Quasi-parallel modes correspond to the proton-cyclotron mode, while the oblique mode is the mirror mode.
Paper: High-energy Neutrino Constraints on Cosmic-Ray Reacceleration in Radio Halos of Massive Galaxy Clusters
Authors: Kosuke Nishiwaki, Katsuaki Asano, Kohta Murase
Figure caption: The LFs for radio (1.4 GHz) and neutrino (100 TeV) emissions in the fiducial model. The LFs are multiplied by the luminosity. The redshift evolution from z = 1 to zero (every 0.2, from red to blue) is shown. The vertical dashed lines show the luminosities corresponding to the mass M 500 = 1013, 1014, and 1015 M ⊙ calculated with the LM relation at z = 0. The black dashed line in the right panel shows the LF averaged within ﹩z\lt {z}_{\max }﹩, where the sources produce 99% of the total neutrino background of the model.
Paper: Hybrid Simulation and Quasi-linear Theory of Bi-Kappa Proton Instabilities
Authors: R. A. López, P. H. Yoon, A. F. Viñas, M. Lazar
Figure caption: Snapshots of the total magnetic power spectra for the three cases from the 2D hybrid code simulations (upper panel) and QL theory (bottom panel). Similar to Figure 1, a few contour levels (solid lines) at γ/Ω i  = [0.01, 0.04, 0.08, 0.12, 0.16], are indicated in order to distinguish between spectra of EMIC and Proton Fire Hose (PFH) instabilities. Plots are normalized to the maximum value for the case of κ = 2 in each case.
Paper: High-energy Neutrino Constraints on Cosmic-Ray Reacceleration in Radio Halos of Massive Galaxy Clusters
Authors: Kosuke Nishiwaki, Katsuaki Asano, Kohta Murase
Figure caption: Time evolution of synchrotron luminosity at 1.4 GHz (red line, left axis) and neutrino luminosity at 100 TeV (blue line, right axis). We consider a Coma-like cluster with a mass of M 500 = 8.5 × 1014 M ⊙ and adopt a reacceleration timescale of t acc = 330 Myr. The spectral index of the primary CRPs is α inj = 2.45. Those trends are modeled with g(t R). The reacceleration starts at t R = 0 and ends at ﹩{t}_{{\rm{R}}}={t}_{{\rm{R}}}^{\mathrm{peak}}﹩ (dashed line).
Paper: Hybrid Simulation and Quasi-linear Theory of Bi-Kappa Proton Instabilities
Authors: R. A. López, P. H. Yoon, A. F. Viñas, M. Lazar
Figure caption: The 1D Kappa distribution function, ﹩F(v)\propto {\left(1+{v}^{2}/\kappa {\alpha }^{2}\right)}^{-\kappa -1}﹩, vs. normalized speed, ﹩\sqrt{m/(2T)}v﹩, where T is defined either as T  κ  = [κ/(κ − 1.5)](m α 2/2) (left), or as T = m α 2/2 (right). In the present analysis, we adopt the definition corresponding to the right-hand side.
Paper: Hybrid Simulation and Quasi-linear Theory of Bi-Kappa Proton Instabilities
Authors: R. A. López, P. H. Yoon, A. F. Viñas, M. Lazar
Figure caption: Temporal evolution of the macroscopic quantities for the three cases, κ = ∞ , 4, and 2, in black, blue, and red, respectively, calculated via 2D hybrid simulation (left) and QL theory (right).
Paper: Hybrid Simulation and Quasi-linear Theory of Bi-Kappa Proton Instabilities
Authors: R. A. López, P. H. Yoon, A. F. Viñas, M. Lazar
Figure caption: Temporal evolutions of the total magnetic power spectra in terms of (normalized) wavenumber v  A  k/Ω p  and angle θ, as obtained from 2D hybrid simulations (upper panels) and from QL theory (lower panels), for bi-Maxwellian (κ → ∞, left column) and bi-Kappa distributions, with κ = 4 (middle column) and κ = 2 (right column).
Paper: Effects of Coronal Magnetic Field Configuration on Particle Acceleration and Release during the Ground Level Enhancement Events in Solar Cycle 24
Authors: Wenlong Liu, Xiangliang Kong, Fan Guo, Lulu Zhao, Shiwei Feng, Feiyu Yu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: Large-scale magnetic configuration around the AR11476 with selected field lines traced through the PFSS model. Closed field lines are plotted in magenta, positive open field lines in red, and negative open field lines in green. The footpoint of the Parker spiral connecting to the Earth at 2.5 R ☉ is shown with the blue square, and the corresponding field line further traced down to the solar surface is also plotted in blue. In panels (c) and (d), the yellow ellipsoids show the evolution of shock fronts at the time of shock formation and the GLE release time when the shock apex reaches 2.4 R ☉, respectively. The direction of the shock apex in panel (d) is indicated by an arrow in gold color. The small solid circles in panel (d) represent the highest-energy SEPs, which are mainly accelerated at the top of closed loops and released when the shock moves through the streamer cusp region.
Paper: Effects of Coronal Magnetic Field Configuration on Particle Acceleration and Release during the Ground Level Enhancement Events in Solar Cycle 24
Authors: Wenlong Liu, Xiangliang Kong, Fan Guo, Lulu Zhao, Shiwei Feng, Feiyu Yu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: The same as Figure 6, for the 2017 September 10 event. In panel (d), the shock apex reaches 3.7 R ☉ at the GLE particle release time, with the direction indicated with an arrow in gold color. The small solid circles illustrate the highest-energy SEPs released to the field line connecting to Earth.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: We plot the images and contours of three typical clusters in three panels. In the first panel, 240 × 240 pixel images of a typical GC in the g and i bands are displayed in the first row, while zoomed-in 54 × 54 pixel images are shown in the second row. Adjacent to these images, contour plots are shown on the same scale. We exhibit another known GC with a comparatively smaller size in the second panel. A known star cluster from Johnson et al. (2012) is shown in the third panel.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The PAndAS g-band images (top panels) and HST images (bottom panels) of five possible cluster candidates in our 54 visually checked candidates. The HST images were taken using the following filters: F475W, F814W, F814W, F275W, and F127M, respectively. Upon examining the HST images, we eliminated Sources 2–5 from our final catalog of candidates. In both sets of panels, the green dashed circles indicate a radius of 1″, with the center aligned to the J2000 position of each respective source.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The distribution of the P GC of the galaxies and GCs with a simbad type in our extended sources (P ext > 0.5). The blue histogram shows the fraction of known galaxies, while the orange histogram shows the fraction of known GCs.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: PAndAS g-band images and contours of six typical types of sources in the extended sources with P GC > 0.25, including a known GC, GC candidates, an elliptical galaxy, a spiral galaxy, a QSO, and a star. The first column shows 240 × 240 pixel images, while the third column shows the zoomed-in 54 × 54 pixel images. The second and fourth columns display the contours of Column 1 and Column 3, respectively.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The distribution of the magnitude difference of the LAMOST stars between the predicted G-band magnitude, G pre, and the Gaia G magnitude. The red shadow shows a range of 90% confidence. The red dashed line indicates the median of ﹩{G}_{\mathrm{pre}}-G﹩.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The flow chart of Section 3.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: Slow body sausage mode 1. (a), (b): Re( v  −) vs. k z R. (c), (d): γ vs.k z R. (e), (f): ﹩\gamma /\tilde{\mu }﹩ vs. k z R, where ﹩\tilde{\mu }=\tilde{\zeta }﹩. The left and right columns show the ﹩\tilde{\mu }﹩ dependent behavior for  U / v  si=1.0 and 1.2, respectively.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: Slow surface sausage mode. (a), (b): Re(Ω−) vs. k z R. (c), (d): γ vs. k z R. (e), (f): ﹩\gamma /\tilde{\mu }﹩ vs. k z R, where ﹩\tilde{\mu }=\tilde{\zeta }﹩. The left and right columns show the ﹩\tilde{\mu }﹩ dependent behavior for  U / v  si = 1.5 and 1.6, respectively.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: (a) Real and (b) imaginary parts of  v  − and (c) their ratio γ (=Im( v  −)/Re( v  −)) for the backward slow body sausage mode 1 vs. k z R where ﹩\tilde{\mu }=\tilde{\zeta }={10}^{-4}﹩. The real and imaginary parts of the phase speeds change their sign at k z R ≈ 0.6 when  U / v  si = 0.9.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: The dependence of ﹩\gamma /\tilde{\mu }﹩ on ﹩\tilde{\zeta }﹩. The left (right) column represents the slow surface mode (slow body mode 1) with  U / v  si=1.6 (1.2). The panels (a) and (b) are for ﹩\tilde{\mu }={10}^{-6}﹩ and (c) and (d) are for ﹩\tilde{\mu }={10}^{-4}﹩.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: (a) Doppler-shifted real and (b) imaginary parts of  v  − and (c) the ratio γ (=Im( v  −)/Re( v  −)) of the backward slow surface sausage mode vs. k z R where ﹩\tilde{\mu }=\tilde{\zeta }={10}^{-4}﹩.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: The critical speed  U   c  and dispersion curve of the slow body sausage (sbs) mode 1 vs. k z R.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: (a)  v  − and (b) Ω− of the backward slow body sausage mode 1 (sbs 1) vs. k z R. Inset in (b) illustrates the turning behavior of dispersion curve at  U / v  si ≈ 0.9.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: (a) Phase speed  v  − and (b) Doppler-shifted phase speed Ω− of the backward slow surface sausage mode vs. k z R.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: The characteristic function ﹩{ \mathcal C }﹩ of the slow surface sausage (sss) mode vs. k z R.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: Fits to the background spectra extracted from the regions shown in Figure 2. The top and bottom panels show the spectra from FPMA and FPMB, respectively. The order from left to right is A665 (first observation), A665 (second observation), and A2146. Each region is represented by a different color. Solar contributions produce the background at softer energies (<5 keV) which is combined with the model that includes instrumental background lines present at all energies. The undeflected cosmic X-ray background (CXB) that passes through the aperture stops dominates between 10 and 20 keV, while the CXB that is focused through the optics (fCXB) is ∼10× fainter. ICM emission from the cluster produces the steeper spectral models in this energy range. At higher energies, cosmic-ray-induced activation and fluorescence lines dominate, along with a flat continuum component representing the overall instrumental background level. For plotting purposes, adjacent bins are grouped until they have a significant detection at least as large as 10σ, with maximum 15 bins.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: The residual CIB (left) and tSZ (right) signals compared to the expected kSZ level of D  ℓ  = 3 μK2 in the MV CMB/kSZ maps from different experiments considered in this work.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: This figure shows the fixed redshift vs. offset temperature relation between five clusters. The green line is our best-fit line to the data, while the black line is the x = y line showing a 1:1 relation for reference and comparison to Figure 13. The fixed redshift temperatures are further from the offset values than in the other case.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: This figure shows the free redshift vs. offset temperature relation between five clusters. The green line represents our best-fit line to the data, while the black line represents the x = y line showing a 1:1 relation for reference and comparison to Figure 14. The free redshift temperatures are closer to the offset values than in the other case