adsabs/AstroCLIMB huggingface dataset:
Paper: Evidence for Evolved Stellar Binary Mergers in Observed B-type Blue Supergiants
Authors: Athira Menon, Andrea Ercolino, Miguel A. Urbaneja, Daniel J. Lennon, Artemio Herrero, Ryosuke Hirai, Norbert Langer, Abel Schootemeijer, Emmanouil Chatzopoulos, Juhan Frank, Sagiv Shiber
Figure caption: Evolutionary tracks of a 31.6﹩\,{{\rm{M}}}_{\odot }﹩(primary) + 3.2﹩\,{{\rm{M}}}_{\odot }﹩ (secondary) binary that merges when the primary is a 30﹩\,{{\rm{M}}}_{\odot }﹩ star, with two core-penetration limits: ﹩{f}_{{\rm{c}},max}=\,0.28﹩ (system 1, green line) and ﹩{f}_{{\rm{c}}}=0﹩ (system 2, brown line). The direction of post-merger evolution is indicated by open triangle symbols. Tick marks separated by 0.1 Myr indicate the duration of the core He-burning phase (light blue shading). Also plotted are the ZAMS position of the primary (gray closed point), start (gray open point) and end of the merger (green and brown open points), core He-depletion (filled diamond), and core C-depletion BSG (blue star) or RSG (red star), close to their respective pre-explosion positions. The RSG core C-depletion position is connected by a red dotted line to its core He-burning phase. The secondary star is barely evolved from ZAMS and is not shown here.
Paper: Evidence for Evolved Stellar Binary Mergers in Observed B-type Blue Supergiants
Authors: Athira Menon, Andrea Ercolino, Miguel A. Urbaneja, Daniel J. Lennon, Artemio Herrero, Ryosuke Hirai, Norbert Langer, Abel Schootemeijer, Emmanouil Chatzopoulos, Juhan Frank, Sagiv Shiber
Figure caption: Log number ratios of N/C and N/O of our considered binary-merger and born-alone stellar models. The sample is marked according to the three groups as discussed in Section 4.1, along with the nebular abundances of the BSG progenitor of SN 1987A (dark orange open triangle; Lundqvist & Fransson 1996) and He-rich stars (Y ≥ 0.12). The gray dashed and solid lines depict the boundaries for the ON and CN cycle, respectively, using the analytical approximations of Maeder et al. (2014).
Paper: Evidence for Evolved Stellar Binary Mergers in Observed B-type Blue Supergiants
Authors: Athira Menon, Andrea Ercolino, Miguel A. Urbaneja, Daniel J. Lennon, Artemio Herrero, Ryosuke Hirai, Norbert Langer, Abel Schootemeijer, Emmanouil Chatzopoulos, Juhan Frank, Sagiv Shiber
Figure caption: Number fractions of C, N, O, and He expressed in log units as explained in Section 2 for merger models, classical blue loops, and TAMS stars, along with our sample groups (as plotted in Figure 2). Y abundance of Sk-69°202 is taken from France et al. (2011). Dotted lines in each panel represent the initial abundances: ϵ(C, i) = 7.75, ϵ(N, i) = 6.90, ϵ(O, i) = 8.35, and Y i = 0.087.
Paper: Evidence for Evolved Stellar Binary Mergers in Observed B-type Blue Supergiants
Authors: Athira Menon, Andrea Ercolino, Miguel A. Urbaneja, Daniel J. Lennon, Artemio Herrero, Ryosuke Hirai, Norbert Langer, Abel Schootemeijer, Emmanouil Chatzopoulos, Juhan Frank, Sagiv Shiber
Figure caption: Composition of the primary star at the onset of merger (left) and of the post-merger star at the end of the merger (right), corresponding to system 1 in Section 3.2.
Paper: Evidence for Evolved Stellar Binary Mergers in Observed B-type Blue Supergiants
Authors: Athira Menon, Andrea Ercolino, Miguel A. Urbaneja, Daniel J. Lennon, Artemio Herrero, Ryosuke Hirai, Norbert Langer, Abel Schootemeijer, Emmanouil Chatzopoulos, Juhan Frank, Sagiv Shiber
Figure caption: Distribution of post-merger and blue-loop single-star models, along with the observed sample in the bolometric luminosity (log L/L⊙) and spectroscopic luminosity space (log ﹩{ \mathcal L }﹩/﹩{{ \mathcal L }}_{\odot }﹩). Symbols for stellar models are as explained in Figures 2 and 4.
Paper: Can the Gravitational Wave Background Feel Wiggles in Spacetime?
Authors: Gen Ye, Alessandra Silvestri
Figure caption: Full numerical results of the energy spectrum of GW with and without (fiducial) resonance for different resonance starting times k  c  τ  i . The amplitude of the background wiggle is ψ 0 = 0.1. A scale-invariant initial GW spectrum and radiation dominance are assumed. In panel (b) we plot the analytic approximation, from the second line of Equations (9) and (8), of the highest peak (i.e., the k  c  τ  i  = 1 case) as a red solid line for comparison.
Paper: Can the Gravitational Wave Background Feel Wiggles in Spacetime?
Authors: Gen Ye, Alessandra Silvestri
Figure caption: Integrated power excess signal ﹩\tfrac{{\rm{\Delta }}{\rho }_{\mathrm{GW}}}{{\rho }_{\mathrm{GW},\mathrm{fid}}}﹩ induced by GW resonance with background wiggles of amplitude ψ 0 = 0.1, in the logarithmic frequency bin centered at k  c . NANOGrav 15 yr data detect possible GWB signal up to bin 8 (Agazie et al. 2023a), corresponding to the max frequency resolution ﹩{\rm{\Delta }}\mathrm{ln}k\simeq \mathrm{ln}(8/7)/2\simeq 0.07﹩, which is indicated by dashed gray lines in the plots. The black dashed line in the left panel indicates the result for a Gaussian peak with the same peak height and half-width as the k τ  i  = 1 resonant peak (thick black solid line).
Paper: The Strength and Shapes of Contact Binary Objects
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Plots showing the populations of binary asteroids, asteroid pairs, and contact binaries, plotting (a) the primary’s rotation period as a function of size ratio and (b) the primary’s rotation period as a function of the primary’s elongation. Doubly synchronous binary asteroids are plotted separately as an open black circle.
Paper: Can the Gravitational Wave Background Feel Wiggles in Spacetime?
Authors: Gen Ye, Alessandra Silvestri
Figure caption: 68% and 95% posterior distributions of the resonance signal template parameters ﹩\{{\mathrm{log}}_{10}{A}_{\mathrm{GWB}},{\gamma }_{\mathrm{GWB}},{\psi }_{0},{f}_{c}\}﹩ fitted to NANOGrav 15 yr data.
Paper: Can the Gravitational Wave Background Feel Wiggles in Spacetime?
Authors: Gen Ye, Alessandra Silvestri
Figure caption: Resonance signal in the GW energy spectrum with a color coding for the variance of the random phase factor. “Completely aligned phase” corresponds to phase variance = 0 (reddish color), while “completely random phase” corresponds to phase variance → ∞ (greenish color).
Paper: The Strength and Shapes of Contact Binary Objects
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Plots showing the required cohesion and friction as a function of the size ratio of two spheres with equal densities. (a) Cohesion for various friction angles and (b) required friction for cohesionless spheres. The solid line corresponds to the secondary and the dashed line to the primary,
Paper: The Strength and Shapes of Contact Binary Objects
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The polyhedral shape model (top) and the ellipsoidal model (bottom) for 1999 JV6.
Paper: The Strength and Shapes of Contact Binary Objects
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The polyhedral shape model (top) and the ellipsoidal model (bottom) for Itokawa.
Paper: Roaring to Softly Whispering: X-Ray Emission after ∼3.7 yr at the Location of the Transient AT2018cow and Implications for Accretion-powered Scenarios 
Authors: Giulia Migliori, R. Margutti, B. D. Metzger, R. Chornock, C. Vignali, D. Brethauer, D. L. Coppejans, T. Maccarone, L. Rivera Sandoval, J. S. Bright, T. Laskar, D. Milisavljevic, E. Berger, A. J. Nayana
Figure caption: Temporal evolution of AT 2018cow at X-ray energies (0.3–10 keV), as captured by Swift-XRT, XMM-Newton, and Chandra. X-rays are modeled with a power-law spectrum. In the top panel the measured X-ray photon indexes are reported: Γ ∼ 1.5 at early time, while the 218-day spectrum suggests a strong softening, Γ ∼ 2.9. No measurement of Γ was possible for the last XMM observation. The dotted line and gray shaded area are the averaged photon index at δ t ≲ 83 days and the relative uncertainty. In the bottom panel, the gray solid line is the best-fit broken power-law decay assuming that AT 2018cow has faded after δ t ≲ 218 days, the short-dashed gray lines being the uncertainties on the model parameters. The long-dashed brown line is the broken power law with the addition of a constant component, mimicking a late-time flattening of the light curve, under the hypothesis that the X-ray flux at δ t = 1349−1358 days is associated with AT 2018cow (see text). The five X-ray-detected FBOTs, CSS 161010 (Coppejans et al. 2022), AT 2020xnd (Ho et al. 2022a; Bright et al. 2022), AT 2020mrf (Yao et al. 2022), AT 2022tsd (Matthews et al. 2023), and AT 2023fhn (Chrimes et al. 2024), are also shown for comparison.
Paper: Roaring to Softly Whispering: X-Ray Emission after ∼3.7 yr at the Location of the Transient AT2018cow and Implications for Accretion-powered Scenarios 
Authors: Giulia Migliori, R. Margutti, B. D. Metzger, R. Chornock, C. Vignali, D. Brethauer, D. L. Coppejans, T. Maccarone, L. Rivera Sandoval, J. S. Bright, T. Laskar, D. Milisavljevic, E. Berger, A. J. Nayana
Figure caption: Left panel: AT 2018cow radio-to-X-ray SED at δ t ∼ 217–234 days. The red solid line is the best-fit broken power-law model for the radio data (GMRT and VLA from Nayana & Chandra 2021 and D. L. Coppejans et al. 2024, in preparation, respectively). The bow tie is the best-fit power-law model (Γ ∼ 2.9) from the X-ray spectral analysis of Obs3. Gray points are data taken at δ t ∼ 1100–1440 days. Right panel: optical/UV-to-X-ray SED at δ t ∼ 700–1440 days. While for the modeling we formally associate the X-ray flux of Obs4 with AT 2018cow, this assumption is relaxed in the discussion on the nature of the accretor (see the text). The optical/UV fluxes (colored squares) are the HST data from Chen et al. (2023a, 2023b). Triangles are NuSTAR data. Gray points are data acquired at δ t ∼ 217–234 days. In both panels, the long-dashed line is a standard Shakura–Sunyaev (T ∝ r −3/4) disk modeling the HST and soft X-rays (blue circle) at δ t ∼ 1350–1435 days, while the thin black line assumes a disk temperature evolution as T ∝ r −1/2 (i.e., Shakura & Sunyaev 1973 “windy” solution, or disks where radiation is trapped within the inflow and advected onto the accretor). In addition, at δ t ∼ 220 days, we added a power law (Γ ∼ 2.0) with an exponential cutoff at ≈3 keV, mimicking a fading Comptonized component.
Paper: Roaring to Softly Whispering: X-Ray Emission after ∼3.7 yr at the Location of the Transient AT2018cow and Implications for Accretion-powered Scenarios 
Authors: Giulia Migliori, R. Margutti, B. D. Metzger, R. Chornock, C. Vignali, D. Brethauer, D. L. Coppejans, T. Maccarone, L. Rivera Sandoval, J. S. Bright, T. Laskar, D. Milisavljevic, E. Berger, A. J. Nayana
Figure caption: Mosaic of the 0.2–4.5 keV images of AT 2018cow in the three EPIC cameras for Obs3 (left panel) and Obs4 (right panel). Color intensity scales logarithmically with the number of counts. The cyan circle (r = 20″) marks the XMM-Newton detection.
Paper: Unveiling Luminous Lyα Emitters at z ≈ 6 through JWST/NIRCam Imaging in the COSMOS Field
Authors: Yuanhang Ning, Zheng Cai, Xiaojing Lin, Zhen-Ya Zheng, Xiaotong Feng, Mingyu Li, Qiong Li, Daniele Spinoso, Yunjing Wu, Haibin Zhang
Figure caption: Lyα luminosity (top panel), UV slope (middle panel), and half-light radius (bottom panel) as a function of the absolute UV magnitude at rest-frame 1500 Å. The stars indicate the 14 LAEs at z ≈ 5.7 in this work. Note that the larger stars with thick edges mark the merging/interacting systems and the smaller open ones mark their individual components. The green squares represent the LBGs (luminous in Lyα) at z ≃ 6 from Ning et al. (2023). The open circles correspond to the LBGs at z ≃ 6 (green) and LAEs at z ≈ 5.7 (blue) and 6.5 (red) from Jiang et al. (2013b). The gray crosses represent the LBGs at z ∼ 6 from Finkelstein et al. (2012). In the bottom panel, the gray dashed line with an uncertainty region indicates an average R  e  for galaxies at z ≈ 5.7, which is obtained from the size–evolution results of Ormerod et al. (2024).
Paper: Unveiling Luminous Lyα Emitters at z ≈ 6 through JWST/NIRCam Imaging in the COSMOS Field
Authors: Yuanhang Ning, Zheng Cai, Xiaojing Lin, Zhen-Ya Zheng, Xiaotong Feng, Mingyu Li, Qiong Li, Daniele Spinoso, Yunjing Wu, Haibin Zhang
Figure caption: Lyα–UV spatial offset Δd Lyα  as a function of NB magnitude, Lyα luminosity, rest-frame UV magnitude, and Lyα equivalent width. The stars indicate the 14 LAEs at z ≈ 5.7 in this work, while the larger ones with thick red edges mark the merging/interacting systems and the red filled ones mark the two LAEs (z6lae-091 and z6lae-101) probably hosting AGNs. In the top left panel, the Δd Lyα  are plotted in units of arcsec with the shaded regions of measurement uncertainty for the NB imaging detection. In the other panels, the Δd Lyα  are plotted in units of physical kpc (pkpc) with 1σ  error bars converted from the 1σ  curve shown in the top left panel. The orange dotted and dashed lines indicate the best-fit linear functions. We also make the merger and AGN symbols shallower to highlight, by contrast, the LAEs used in the linear fitting.
Paper: Unveiling Luminous Lyα Emitters at z ≈ 6 through JWST/NIRCam Imaging in the COSMOS Field
Authors: Yuanhang Ning, Zheng Cai, Xiaojing Lin, Zhen-Ya Zheng, Xiaotong Feng, Mingyu Li, Qiong Li, Daniele Spinoso, Yunjing Wu, Haibin Zhang
Figure caption: The SFR–M * and size–M * distributions of our LAE sample. The stars indicate our sample of 14 LAEs at z ≈ 5.7; the smaller open ones mark the components of the merging/interacting systems. In the left panel, the blue lines represent the best-fit MS power-law relation from Rinaldi et al. (2022). In the right panel, the orange dashed line is the best-fit linear relation for our LAEs at z ≈ 5.7. The purple line gives the mass–size relation for galaxies at z = 4–10 from Langeroodi & Hjorth (2023).
Paper: Unveiling Luminous Lyα Emitters at z ≈ 6 through JWST/NIRCam Imaging in the COSMOS Field
Authors: Yuanhang Ning, Zheng Cai, Xiaojing Lin, Zhen-Ya Zheng, Xiaotong Feng, Mingyu Li, Qiong Li, Daniele Spinoso, Yunjing Wu, Haibin Zhang
Figure caption: SED fitting for our LAE sample with Bagpipes. In each panel, the observed and best-fit photometric data are shown by red circles and blue squares with error bars, respectively. The best-fit model SED is plotted as a gray line with a shaded region indicating 1σ  uncertainty. Note that the best-fit model SEDs cannot match the observed SEDs for the two little red dots, z6lae-091 and z6lae-101, which imply probably additional AGN components.
Paper: Can the Gravitational Wave Background Feel Wiggles in Spacetime?
Authors: Gen Ye, Alessandra Silvestri
Figure caption: Numeric results of theory (A1). (a) Scalar field energy fraction. (b) Tensor power spectrum. Vertical dashed lines in panel (b) mark the position of resonance k  c  and the conformal Hubble scale k  H  at which the spectrum is plotted.
Paper: Unveiling Luminous Lyα Emitters at z ≈ 6 through JWST/NIRCam Imaging in the COSMOS Field
Authors: Yuanhang Ning, Zheng Cai, Xiaojing Lin, Zhen-Ya Zheng, Xiaotong Feng, Mingyu Li, Qiong Li, Daniele Spinoso, Yunjing Wu, Haibin Zhang
Figure caption: (a) Our LAE sample covered by the COSMOS-Web observations. The stars represent the 14 LAEs, in which the larger ones with thick edges indicate the merging/interacting systems (Section 4.1), while the red filled ones indicate the little red dots with AGN features (Section 4.2). The magenta pentagons correspond to all other z ≈ 5.7 LAEs spectroscopically confirmed by our M2FS spectroscopic survey. The visit tiles covering our sample have a darker edge with the observation IDs (Column (5) in Table 1). The big circles represent the M2FS pointings. (b) The lower panel gives the redshift–Lyα luminosity distribution of the LAEs. The symbols are the same as those in panel (a). Note that two LAEs, z6lae-072 and z6lae-076, overlap each other in the parameter space. The corresponding number distributions are plotted shown in the upper panel. (c) The 14 LAEs detected in the four JWST/NIRCam bands (1.″5 × 1.″5; north is up and east to left) with pseudo-color images (after PSF matching; blue: F115W+F150W; green: F277W; red: F444W). The central plus signs mark the Lyα centroids detected from the NB816 images.
Paper: Chandra’s Insights into SN 2023ixf
Authors: Poonam Chandra, Roger A. Chevalier, Keiichi Maeda, Alak K. Ray, Nayana A. J.
Figure caption: Evolution of column density (left) and 0.3–10 keV unabsorbed luminosity (right). The first red data point on day 4 in the column density plot is the NuSTAR data point (Grefenstette et al. 2023). The purple data point on the luminosity evolution plot is the Swift-XRT data point. While the column density evolves faster between day 4 and 13 before starting to follow the standard t −1 evolution, the 0.3–10  keV luminosity initially rises and then follows t −1 evolution.
Paper: Chandra’s Insights into SN 2023ixf
Authors: Poonam Chandra, Roger A. Chevalier, Keiichi Maeda, Alak K. Ray, Nayana A. J.
Figure caption: Left: contour plot of the best-fit parameter values of the column density and the plasma temperature for the 2023 May Chandra spectrum. The column density is well constrained while the temperature is not. Right: contour plot of the best-fit values of the Gaussian line energy and the column density. Both parameters are well constrained.
Paper: Chandra’s Insights into SN 2023ixf
Authors: Poonam Chandra, Roger A. Chevalier, Keiichi Maeda, Alak K. Ray, Nayana A. J.
Figure caption: Left: 2023 May best-fit spectrum of SN 2023ixf. The model is fit with an absorbed plasma with a Gaussian profile. Right: 2023 August best-fit spectrum of SN 2023ixf. The 6.4 Fe Kα line is no longer detected.
Paper: Chandra’s Insights into SN 2023ixf
Authors: Poonam Chandra, Roger A. Chevalier, Keiichi Maeda, Alak K. Ray, Nayana A. J.
Figure caption: Contour plot of the best-fit parameter values for the column density and the plasma temperature for the 2023 August Chandra spectrum. The column density is well constrained while the temperature is not.
Paper: JWST Observations of K2-18b Can Be Explained by a Gas-rich Mini-Neptune with No Habitable Surface
Authors: Nicholas F. Wogan, Natasha E. Batalha, Kevin J. Zahnle, Joshua Krissansen-Totton, Shang-Min Tsai, Renyu Hu
Figure caption: The climate of a plausible Hycean K2-18b. (a) shows the incoming short-wave (red) and outgoing long-wave radiation (black) as a function of surface temperature computed with the climate model in Photochem. Calculations assume 1 bar of H2 with H2O at saturation in the troposphere. The solid red line is the incoming short-wave radiation for K2-18b’s full stellar insolation (1368 W m−2), which cannot be balanced by outgoing long-wave energy below the critical point of H2O (<647 K). The dashed red line considers a 30% smaller insolation to crudely represent high-altitude clouds reflecting away starlight, which would allow for a stable ∼320 K climate. (b) The P–T profile for the stable climate in panel (a), which we adopt for the Hycean photochemical simulations.
Paper: JWST Observations of K2-18b Can Be Explained by a Gas-rich Mini-Neptune with No Habitable Surface
Authors: Nicholas F. Wogan, Natasha E. Batalha, Kevin J. Zahnle, Joshua Krissansen-Totton, Shang-Min Tsai, Renyu Hu
Figure caption: Climate and photochemical simulation of K2-18b as a mini-Neptune with no habitable surface (model 3 in Table 1). The black dashed line is the computed P–T profile, which is referenced to the upper x-axis. The horizontal gray line at 1 bar divides the lower and upper atmosphere as discussed in Section 2.1. Solid colored lines are predicted atmospheric composition from our photochemical model. For comparison, the dotted lines in the lower atmosphere are chemical equilibrium composition. If K2-18b is a 100× solar mini-Neptune with a solar C/O ratio, then we predict the observable upper atmosphere should have ∼4% CH4 and nearly 0.1% CO2, which is in reasonable agreement with recent JWST observations (Madhusudhan et al. 2023b).
Paper: JWST Observations of K2-18b Can Be Explained by a Gas-rich Mini-Neptune with No Habitable Surface
Authors: Nicholas F. Wogan, Natasha E. Batalha, Kevin J. Zahnle, Joshua Krissansen-Totton, Shang-Min Tsai, Renyu Hu
Figure caption: Transmission spectra of Hycean and mini-Neptune models of K2-18b compared to JWST NIRISS and NIRSpec data from Figure 3 in Madhusudhan et al. (2023b). Panels (a), (b), and (c) show simulated clear-sky transmission spectra of models 1, 2, and 3, respectively. Colored shading shows the effect of molecules on the spectrum. The reported ﹩{\chi }_{r}^{2}﹩ values each have 64 degrees of freedom. The JWST data strongly rules out a lifeless Hycean world (model 1, ﹩{\chi }_{r}^{2}=3.22﹩), but allows for either an inhabited Hycean (model 2) or mini-Neptune (model 3) model of K2-18b (﹩{\chi }_{r}^{2}=1.51﹩).
Paper: JWST Observations of K2-18b Can Be Explained by a Gas-rich Mini-Neptune with No Habitable Surface
Authors: Nicholas F. Wogan, Natasha E. Batalha, Kevin J. Zahnle, Joshua Krissansen-Totton, Shang-Min Tsai, Renyu Hu
Figure caption: Photochemical simulations of K2-18b as a habitable Hycean world. Panels (a) and (b) correspond to models 1 and 2, respectively, described in Table 1. Both panels include the surface CH4 flux in molecules cm−2 s−1 required to sustain the CH4 concentration. Panel (a) shows that only parts-per-billion-level methane can accumulate photochemically (i.e., abiotically). Panel (b) shows that methane is predicted to build up to percent levels assuming a biological surface CH4 flux of 5 × 1010 molecules cm−2 s−1, which is about half of the modern Earth’s biological flux (Jackson et al. 2020).
Paper: Collisional Shaping of Nuclear Star Cluster Density Profiles
Authors: Sanaea C. Rose, Morgan MacLeod
Figure caption: The peak wavelength of each star in our sample 4.64 × 109 yr into our Rauch99 α = 1.75 simulation. Peak wavelength, a proxy for color, is plotted vs. distance from the SMBH. We also color code the stars in the sample by bolometric luminosity. The left panel shows the stars without collisions, the same as the gray points in the lower right plot of Figure 2, while the right panel shows the simulated population with collisions. Collision-induced mergers cause a population of brighter, bluer stars to form, stars that would not otherwise exist in a population of the same age. We also include the population of collisionally stripped stars, though the luminosity, color, and general appearance of these stars are uncertain.
Paper: Restoration of the Tully–Fisher Relation by Statistical Rectification
Authors: Hai Fu
Figure caption: The distribution of ALFALFA-SDSS galaxies in the plane of i-band absolute magnitude vs. H I line width. This is the input ﹩\tilde{\phi }(\tilde{x},\tilde{y})﹩ function, which will be rectified by the Lucy algorithm to statistically remove the effects from random disk orientations and random measurement errors. Here and in most of the subsequent figures, the main panel shows the 2D distribution, and the side panels show the marginalized distributions over each axis.
Paper: Backscattering of Ions Impacting Ganymede’s Surface as a Source for Energetic Neutral Atoms
Authors: Paul S. Szabo, Andrew R. Poppe, Andreas Mutzke, Lucas Liuzzo, Shane R. Carberry Mogan
Figure caption: (a) Globally averaged backscattered H ENA fluxes (solid lines) are compared to the sputtered atomic ENA fluxes (from dissociation in an ENA instrument, dashed lines, based on the calculations by Pontoni et al. 2022) at three different ice abundances. Given uncertainties in the emission of high-energy H2, the dotted line depicts sputtered fluxes with the H2 component excluded. (b) The relative contribution of backscattered H ENAs to the total H ENA environment (backscattered + sputtered, including the H2 component) is plotted based on the data shown in (a).