adsabs/AstroCLIMB huggingface dataset:
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: 3D structure of California from multiple viewing angles. Small arrows show the orientation of each angle. The bubble described previously and marked in Figure 1 is visible in multiple panels. Color scales are as in Figure 1.
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: Extinction as a function of distance for three LOSs toward California as shown in Figure 3 (solid lines with 1σ uncertainties as shaded area), plus those from Green et al. (2019) (dashed lines). A typical uncertainty in Green et al. (2019) is about 0.02 mag in this range. The predicted distances for gray and blue LOSs agree fairly well in both maps, while the red curve from Green et al. (2019) is missing the second peak in our map.
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: Density predictions as a function of distance for mock data set explained in Appendix B. The vertical red lines demonstrate the “true” distances and widths of the clouds.
Paper: On the Potential of Bright, Young Pulsars to Power Ultrahigh Gamma-Ray Sources
Authors: Emma de Oña Wilhelmi, Rubén López-Coto, Elena Amato, Felix Aharonian
Figure caption: Maximum electron energy derived from the LHAASO spectra vs. spin-down power of the co-located pulsars. The right y-axis shows the corresponding gamma-ray energy. The colored area shows the values for η  e  η  B  1/2 ranging from 0.01 to 1, with the red line indicating the limiting value corresponding to maximally efficient acceleration η  e  = 1 and η B = 1. The dotted black line marks the upper limit to the maximum energy for young pulsars with a large magnetic field of 100 μG. The blue dashed horizontal lines show the predicted values for PWNe associated with Geminga and N157B.
Paper: A New Member of the Milky Way’s Family Tree: Characterizing the Pontus Merger of Our Galaxy
Authors: Khyati Malhan
Figure caption: Action–energy ( J , E) space of the Milky Way showing stars that form part of our halo sample (see Sections 2 and 3). The left panel shows J  ϕ (≡L  z ) vs. J  R , where stars are colored by their J  z  values. The right panel shows J  ϕ  vs. E, which is represented by a 2D histogram colored by the logarithm of the number of stars per bin. In both panels, the boxes describe the dynamical volumes occupied by different mergers per Malhan et al. (2022). Stars belonging to Pontus possess low energy (E ∼ −1.65 × 105  km2 s−2) and slightly retrograde motion (J  ϕ  ∼ 200 kpc km s−1).
Paper: A New Member of the Milky Way’s Family Tree: Characterizing the Pontus Merger of Our Galaxy
Authors: Khyati Malhan
Figure caption: Phase-space distribution of the Pontus stars (in magenta) in Galactocentric coordinates. The top panels show the spatial distribution of stars, and the bottom panels show the velocity distribution. The “star” markers correspond to the member globular clusters of Pontus. For comparison, we show the halo sample (in gray) and also the Gaia-Sausage/Enceladus stars (in blue).
Paper: Origin of Intense Electron Heating in Relativistic Blast Waves
Authors: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet
Figure caption: Drift Lorentz factors (top) and temperatures (bottom) for ions (blue) and electrons (red) of the background plasma, extracted from our three reference PIC simulations with parameters: (a) γ ∞ = 100 and r = 25, (b) γ ∞ = 100 and r = 100, and (c) γ ∞ = 10 and r = 100. In the top panels, the solid gray lines plot the Lorentz factor of the Weibel frame as extracted from each simulation (see text).
Paper: A New Member of the Milky Way’s Family Tree: Characterizing the Pontus Merger of Our Galaxy
Authors: Khyati Malhan
Figure caption: The CMD of the Pontus stars. Panel (a) shows Pontus stars in magenta and the halo population in gray. We also plot a stellar population model that is similar to the average metallicity of Pontus. Panel (b) is similar to panel (a), except Pontus stars are now colored by their [Fe/H] values. To make this plot, we also cross-match our Pontus sample with the LAMOST DR5 data set (Zhao et al. 2012; Xiang et al. 2019).
Paper: Origin of Intense Electron Heating in Relativistic Blast Waves
Authors: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet
Figure caption: Close-up of the precursor of an unmagnetized electron–ion collisionless shock in the PIC simulation frame. The upstream plasma is injected from the right-hand side with a Lorentz factor γ ∞ = 100, proper temperatures T e = T i = 0.01m e, and mass ratio r = m  i /m  e  = 100. The top (middle and bottom) panel shows the magnetic field (ion density and electron energy fraction) profile at time ﹩t=870\,{\omega }_{\mathrm{pi}}^{-1}﹩. The shock front, located at x = 0, separates the unshocked plasma (x > 0) from the shocked plasma (x < 0).
Paper: A New Member of the Milky Way’s Family Tree: Characterizing the Pontus Merger of Our Galaxy
Authors: Khyati Malhan
Figure caption: Analyzing chemical abundances of Pontus stars using the APOGEE data set. Panel “a” shows the [Fe/H] vs. [α/Fe] distribution. The background shows 2D histograms constructed using the entire APOGEE data set (the darker the bin, the higher the number of stars in that bin). The bars at the bottom of the panel indicate the median error at that [Fe/H]. For comparison, we also show the Gaia-Sausage/Enceladus stars. Panel (b) shows the [Fe/H] vs. [Mg/Fe] distribution, and panel (c) shows the [Fe/H] vs. [Al/Fe] distribution.
Paper: Origin of Intense Electron Heating in Relativistic Blast Waves
Authors: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet
Figure caption: (a) Estimate of the coherent mean electric potential −∫〈E  x 〉 y  dx weighted by the electron density (solid curves) and in the range of ±1σ variation (shaded area). The different colors respectively correspond to the three PIC simulations with (r, γ ∞) = (100, 10) (blue), (25, 100) (black), and (100, 100) (red). The dotted–dashed lines correspond to the electrostatic potential reconstructed from the Monte Carlo-Poisson integration of our theoretical model. (b) Charge density of the beam component as measured in the PIC simulations with the same color code as in panel (a). The suprathermal beam is defined as the ensemble of particles moving with longitudinal velocity β  x  > 0. The dotted lines show the relationship between the (apparent) beam charge density ρ b and γ w, as extracted from Equation (1), namely, ﹩{\rho }_{{\rm{b}}}\propto \,{\gamma }_{\infty }{n}_{\infty }\,e/{\gamma }_{{\rm{w}}}^{2}﹩, which matches well the observed profile.
Paper: Origin of Intense Electron Heating in Relativistic Blast Waves
Authors: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet
Figure caption: Comparison of the drift Lorentz factor (top) and temperature (bottom) between the PIC simulation with the respective (r, γ ∞) = (25, 100), (100, 100), (100, 10) (gray) and the MCP solution to the transport equation for the ions (blue) and electrons (red). The transport equation is integrated using the scattering frequency given by Equation (5) with ν 0∣w  ≃  6, 6, 0.2 ϵ B/k ⊥. The light red and blue curves in the middle panel correspond to the solution to the transport equation ignoring the contribution of the electrostatic field; while they globally reproduce the observed amount of ion heating, they indicate insufficient electronic heating. We thus find that the shock dynamics is correctly reproduced for ν 0∣w  ∼  ϵ B/k ⊥ when accounting for the electrostatic field contribution.
Paper: Origin of Intense Electron Heating in Relativistic Blast Waves
Authors: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet
Figure caption: Comparison of the drift Lorentz factor (top) and temperature (bottom) between the PIC simulation with (r, γ ∞) = (100, 100) (gray) and the MCP solution to the transport equation (including the electric field contribution) for the ions (blue) and the electrons (red). The transport equation is integrated using the scattering frequency given by Equation (5) with, from left to right, ν 0∣w = 0.6, 6, 60 ϵ B/k ⊥.
Paper: Origin of Intense Electron Heating in Relativistic Blast Waves
Authors: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet
Figure caption: Longitudinal profile of the transverse Fourier modes of the out-of-plane (B  z ) magnetic field across the shock precursor for (r, γ ∞) = (25, 100), (100, 100), (100, 10) (from left to right). The two horizontal dotted lines correspond to the electron (top) and ion (bottom) plasma scales. The black line follows the dominant transverse wavenumber across the precursor, which is used to estimate the scattering frequency ν 0∣w.
Paper: Origin of Intense Electron Heating in Relativistic Blast Waves
Authors: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet
Figure caption: Left: out-of-plane magnetic field component (B  z ) in the simulation plane, for (r, γ ∞) = (25, 100), (100, 100), (100, 10) (from top to bottom). Right: one-dimensional profile along the shock normal of the magnetic energy fraction ϵ B, for the three simulations. This profile is used in the estimate of ν 0∣w.
Paper: Origin of Intense Electron Heating in Relativistic Blast Waves
Authors: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet
Figure caption: In shaded bands, distributions of the electron (red) and ion (blue) scattering frequencies across the shock precursor as extracted from the MCP solution to the transport equation using the continuous formula (5) with (r, γ ∞) = (100, 100). For comparison, we overlay the scattering frequencies in the trapped (dotted lines) and untrapped (solid lines) limits as extracted from the corresponding PIC simulation using Equations (34) and (35) of Lemoine et al. (2019c).
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Histograms of measured abundances of Th (left), Eu (as a proxy for U; middle), and K (right) for our samples of stars described in Appendix A.4. The total number of stars in each sample is noted. Best fits assuming a lognormal distribution are shown in red, with the average value and 95% confidence interval shown for each element in each panel.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Interpolated color maps of average (middle), lower (left), and upper (right) 95% confidence interval bounds on the mantle degassing lifetime for stagnant-lid exoplanets as a function of planet mass and age of the system. The data interpolated are represented by crosses with averages and confidence intervals being determined by 50,000 random samplings of our parameter space (see Appendix A). We define the cessation of degassing as occurring when the degassing rate drops below 10% of the Earth’s current value, scaled linearly by planet surface area (see Appendix A).
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Initial mantle abundances (left), initial radiogenic heat budget (Q 0; middle), and fraction of total heat budget (right) for a cosmochemically Earth-like planet as a function of the time of planet formation from Frank et al. (2014) and adopting the current Earth HPE abundances of Palme & O’Neill (2003) for 40K (yellow), 238U (blue), 235U (green), and Th (red). The time of Earth formation (t = 8 Gyr) is shown for reference.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Planet age when degassing ceases (present = 12.5 Gyr) as a function of planetary mass and current system age adopting the average (middle) and lower (left) and upper (right) bounds of our 95% confidence intervals of degassing lifetime for planets of a given mass and time of formation (Figure 2 of main text). Those 17 planets with measured mass, radius, and system age and density consistent with being rocky are included for reference (Table A2). Uncertainties represent the reported 1σ error bars in both mass and age. The TRAPPIST-1 planets are highlighted, adopting the system ages of Burgasser & Mamajek (2017) and planet masses of Agol et al. (2021).
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Age when degassing ends for a 1 M ⊕ planet as a function of the initial heat budget for an HPE X (Q  X  0) relative to the initial heat budget for the same element for the Earth (﹩{Q}_{0-\mathrm{Earth}}^{X};﹩ see Table A3) for restricted ranges of mantle reference viscosity: μ ref < 1020 (first row), 1021 (second row), 1022 (third bottom row), and 1023 (fourth row) Pa s. Models were run assuming that planets formed at the same time as the Earth (t = 8 Gyr). The average (red line) and 95% confidence intervals in the degassing cessation age (red band) are included for reference. In each plot, only 2000 models are shown to reduce the density of the data points.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Age when degassing ends for 1 M ⊕ (colors) as a function of reference viscosity and the initial radiogenic heat budget for formation times 12.4 (left) and 4.5 (right) Gyr into the past. The figure was created using 50,000 random samples as described above. For comparison, the Earth’s reference viscosity is ∼1021 Pa s.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Same as Figure A6 but for a 6 M ⊕ planet.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Degassing lifetime as a function of initial radiogenic heat budget (left), reference viscosity (middle), and initial mantle temperature (right) for 1 (top) and 6 (bottom) M ⊕ planets with Earth-like CMFs (0.33) that formed at the same time as the Earth (t = 8 Gyr).
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Best-fit average (red) and upper (blue) and lower (black) limits of the 95% confidence interval of Age﹩{}_{\max }﹩ assuming that 40K is arbitrarily halved (dotted), left Earth-like (solid), and doubled (dashed) in Equation (A37) for 25,000 model iterations for each curve.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Histograms of the degassing lifetime for 1 (left) and 6 (right) M ⊕ planets with CMFs of 0.25 (red) and 0.45 (blue) for a planet forming at the same time as the Earth (t = 8 Gyr). The average of our CMF = 0.33 models (Figure 2 of main text) for each mass is shown as a black dashed line. These histograms were derived from 200,000 random samplings of our parameters, as described above.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Probability that the host-star/planet age is ﹩\leqslant {\mathrm{Age}}_{\max }^{\mathrm{Avg}}﹩ (left) and ≤Age﹩{}_{\max }^{\mathrm{UL}95 \% \mathrm{CI}}﹩ (right) for the 17 planets in our sample (Table A2) as a function of their mass and system age. Planets with probabilities greater than 1σ (67%) confidence are labeled, and TRAPPIST-1 is included for reference. We define active degassing as having degassing rates greater than 10% of the Earth’s current value, scaled linearly by planet surface area (see Appendix A).
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Change in Age﹩{}_{\max }^{\mathrm{Avg}}﹩ in comparison to a dry-planet baseline as a function of mantle water content. Three different values of the viscosity water dependence exponent, r, are used: r = 0.7 (dotted line), 1 (solid line), and 1.2 (dashed line). Results for 1 (a) and 6 (b) M ⊕ are presented. The lower bound on the mantle water concentration for each curve is determined by the mantle water concentration where the dry and wet olivine flow laws are equal. This crossover point depends on r, which is why curves with different r do not start at the same point in terms of mantle water concentration. The vertical gray line denotes Earth’s mantle’s estimated water content.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Left: mass percentage of bulk K and 40K in the gas for a 15 M ⊙ progenitor. Right: 40K/K vs. mass fraction of 40K in the gas for the same progenitor (Ellinger et al. 2012). The Sun’s primordial 40K/K is shown for reference (Lodders 2003).
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Histograms of the age when planetary degassing ends for 1 (left) and 6 (right) M ⊕ planets with our default solidus (blue) and the solidus decreased arbitrarily by 100 (gray) and 200 (red) Kelvin. These histograms represent 200,000 random samplings of our parameters as described in Appendix A.5.
Paper: Mantle Degassing Lifetimes through Galactic Time and the Maximum Age Stagnant-lid Rocky Exoplanets Can Support Temperate Climates
Authors: Cayman T. Unterborn, Bradford J. Foley, Steven J. Desch, Patrick A. Young, Gregory Vance, Lee Chiffelle, Stephen R. Kane
Figure caption: Cross section of ejecta in a mildly bipolar explosion of a 15 M ⊙ star. Axes are in units of solar radii. The color bar represents the log of the mass ratio of 40K to total K. The peak 40K/Ktot occurs in areas of large overdensity near the base of the Rayleigh–Taylor fingers. These clumps persist out to large radii during the remnant phase of the supernova.
Paper: Signature of Supersonic Turbulence in Galaxy Clusters Revealed by AGN-driven Hα Filaments
Authors: Haojie Hu, 豪杰 胡, Yu Qiu, 宇 邱, Marie-Lou Gendron-Marsolais, Tamara Bogdanović, Julie Hlavacek-Larrondo, Luis C. Ho, Kohei Inayoshi, Brian R. McNamara
Figure caption: Left: line-of-sight velocity distribution of the Hα nebula in the Perseus cluster (Gendron-Marsolais et al. 2018, with the systemic velocity shifted to 5264 km s−1), divided into nine azimuthal regions. Only pixels with velocity errors < 30 km s−1 are plotted and used in the VSF calculation. The arc in Region 2 separates the inner filament complex lacking a radial gradient, and the outer horseshoe filament. An X-ray shock front is detected across Regions 4 and 5, which also indicates supersonic flows (Fabian et al. 2003a). Right: the VSF calculated from pixels in each region. The scaling relations of v ∝ l 1/3 (subsonic), v ∝ l 1/2 (supersonic), and v ∝ l 1 (gradient) are plotted for comparison. The VSF of the entire nebula from Li et al. (2020), which represents an average of all nine regions, is shown by the solid black line. Data points below the velocity error threshold (30 km s−1) and the seeing limit (0.4 kpc) are marked with shaded regions.
Paper: Signature of Supersonic Turbulence in Galaxy Clusters Revealed by AGN-driven Hα Filaments
Authors: Haojie Hu, 豪杰 胡, Yu Qiu, 宇 邱, Marie-Lou Gendron-Marsolais, Tamara Bogdanović, Julie Hlavacek-Larrondo, Luis C. Ho, Kohei Inayoshi, Brian R. McNamara
Figure caption: Line-of-sight VSF of the simulated cold gas from different viewing angles (θ; between the sight line and the initial outflow direction, indicated by the different line colors), for outflows with different initial velocities (v out = 1500, 1000, or 500  km s−1), at two epochs of evolution (t = 20 and 30  Myr). The scaling relations of v ∝ l 1/3 and v ∝ l 1/2 are plotted for comparison. The lines representing the scaling relations are shifted in each column to approximately bracket the VSF lines. An additional scaling of v ∝ l 1 is plotted in the lower middle panel, which shows that the VSF is dominated by the velocity gradient at large separations. Note that the cutoff of the lines at separations beyond a few kiloparsecs is constrained by the size of each filament complex, without the contribution from nearby filaments at separations beyond 10 kpc, as shown in Figure 3.
Paper: Signature of Supersonic Turbulence in Galaxy Clusters Revealed by AGN-driven Hα Filaments
Authors: Haojie Hu, 豪杰 胡, Yu Qiu, 宇 邱, Marie-Lou Gendron-Marsolais, Tamara Bogdanović, Julie Hlavacek-Larrondo, Luis C. Ho, Kohei Inayoshi, Brian R. McNamara
Figure caption: The spatial distribution of the projected Hα emissivity (columns 1, 3, and 5) and the emissivity-weighted line-of-sight velocity (columns 2, 4, and 6) for the three simulation runs with different initial outflow velocity, v out, projected along θ = 90° (viewing angle θ between the sight line and the initial outflow direction). The initial outflow direction and the length scale are shown in the two bottom right panels. The top, middle, and bottom rows show three representative evolution epochs at t = 20, 30, and 40  Myr, respectively. A horseshoe-shaped outer shell consisting of Hα-emitting gas is produced for the outflow with v out = 1500 km s−1 at t = 20 Myr (albeit smaller in size compared to the Perseus horseshoe filament; Conselice et al. 2001).