adsabs/AstroCLIMB huggingface dataset:
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 3000 keV H+ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 100 keV O++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 300 keV H+ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 10 keV O++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 100 keV H+ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 50 keV O++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 5 keV O++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 50 keV H+ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: Does the Lockstep Growth between Black Holes and Bulges Create Their Mass Relation?
Authors: Guang Yang, 光 杨, W. N. Brandt, David M. Alexander, Médéric Boquien, Qingling Ni, Casey Papovich, Justin S. Spilker, Fabio Vito, Jonelle L. Walsh, Chengpeng Zhang
Figure caption: Schematic diagram of the two scenarios tested in this work. The blue and red stars represent the bulge formation redshift and z = 0, respectively. The black arrows indicate the evolution paths. The dashed line represents the observed BH–bulge mass relation in the local universe. The determining factor between the two scenarios is the amount of cold gas that is available after bulge formation (see Section 1 for details).
Paper: Does the Lockstep Growth between Black Holes and Bulges Create Their Mass Relation?
Authors: Guang Yang, 光 杨, W. N. Brandt, David M. Alexander, Médéric Boquien, Qingling Ni, Casey Papovich, Justin S. Spilker, Fabio Vito, Jonelle L. Walsh, Chengpeng Zhang
Figure caption:  μ = M gas/M star vs. redshift. The stars and squares are the values estimated using α CO = 4.3 (default) and α CO = 0.8, respectively. The downward-pointing arrows indicate 3σ upper limits. The dashed line indicates μ = 1. The two blue data points represent two bulge-dominated galaxies at z = 2–2.5 from Barro et al. (2016). The gas content of the bulge-dominated galaxies is generally low (μ < 1 in most cases), insufficient to support significant bulge/BH growth.
Paper: Does the Lockstep Growth between Black Holes and Bulges Create Their Mass Relation?
Authors: Guang Yang, 光 杨, W. N. Brandt, David M. Alexander, Médéric Boquien, Qingling Ni, Casey Papovich, Justin S. Spilker, Fabio Vito, Jonelle L. Walsh, Chengpeng Zhang
Figure caption: SED fits of our ALMA sources using CIGALE. The black curve represents the best-fit SED model, while the blue, orange, and red curves indicate AGN, galaxy, and mbb (if present) components, respectively. The redshift and reduced χ 2 are labeled on each panel.
Paper: Does the Lockstep Growth between Black Holes and Bulges Create Their Mass Relation?
Authors: Guang Yang, 光 杨, W. N. Brandt, David M. Alexander, Médéric Boquien, Qingling Ni, Casey Papovich, Justin S. Spilker, Fabio Vito, Jonelle L. Walsh, Chengpeng Zhang
Figure caption: Left: HST H-band 7″ × 7″ cutouts, with contours of CO emission. The contours are at the 2σ, 3σ, 5σ, and 8σ levels. The beam profile is displayed in the bottom left corner. There is no contour for CANDELS 23845, due to the weak signal of its CO line map. Right: CO spectrum for each source. The red dashed curve represents the best-fit Gaussian model (only displayed for CO-detected sources). The horizontal and vertical dotted lines indicate zero flux and velocity, respectively. The orange shaded region indicates the integrated velocity range for the line flux measurement. The measured line flux and its uncertainty (or upper limit) is labeled. We consider the line to be detected if S/N > 3; we adopt the 3σ uncertainties as upper limits for undetected sources (see Table 2).
Paper: Does the Lockstep Growth between Black Holes and Bulges Create Their Mass Relation?
Authors: Guang Yang, 光 杨, W. N. Brandt, David M. Alexander, Médéric Boquien, Qingling Ni, Casey Papovich, Justin S. Spilker, Fabio Vito, Jonelle L. Walsh, Chengpeng Zhang
Figure caption: The fraction of star-forming galaxies (M star > 1010.2 M ⊙) as a function of redshift. The red data points represent bulge-dominated galaxies and the blue ones are for the other galaxies that are not bulge-dominated. The error bars represent 1σ binomial uncertainties calculated with the “binom_conf_interval” function of ASTROPY. The star-forming fraction is low (≈0.2–0.3 at z ≈ 0.5–2) for bulge-dominated galaxies, indicating that gas replenishment is not common for them.
Paper: Does the Lockstep Growth between Black Holes and Bulges Create Their Mass Relation?
Authors: Guang Yang, 光 杨, W. N. Brandt, David M. Alexander, Médéric Boquien, Qingling Ni, Casey Papovich, Justin S. Spilker, Fabio Vito, Jonelle L. Walsh, Chengpeng Zhang
Figure caption:  τ dep vs. τ grow. The red stars and squares are values estimated using α CO = 4.3 (default) and α CO = 0.8, respectively. The downward-pointing arrows indicate 3σ upper limits. The black dashed lines indicate τ dep = τ grow. Except for CANDELS 25998 (α CO = 4.3), the other data points are all below the τ dep = τ grow line.
Paper: Does the Lockstep Growth between Black Holes and Bulges Create Their Mass Relation?
Authors: Guang Yang, 光 杨, W. N. Brandt, David M. Alexander, Médéric Boquien, Qingling Ni, Casey Papovich, Justin S. Spilker, Fabio Vito, Jonelle L. Walsh, Chengpeng Zhang
Figure caption: HST H-band 7″ × 7″ cutouts with contours of CO emission, for the four CO-detected sources. The blue and red contours are from the blue and red halves of the line, respectively. The contours are at the 2σ, 3σ, 5σ, and 8σ levels. The beam profile is displayed in the bottom left corner.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Schematic illustration of the interstellar scattering at a thin screen that imparts random phase fluctuations. The paths of two rays, differing in polarization, are shown, indicating the slight difference in the refractive deflection angles θ ±. The source–screen (R) and screen–observer (D) distances are indicated.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Collision histories of two planets from debris-loss cases. Each collision is represented by a set of colored dots and lines. Unfilled dots represent the CMF of the bodies that collide, and the filled squares represent the bodies that remain after the collision. The “largest remnant” is the most massive (and only, for most collisions) embryo that remains. Some collisions have two remaining embryos (see Table 3), and in this case the second embryo is called the “second-largest remnant.” All of the dots for one collision are connected by a solid, colored line. Dashed lines represent the body’s CMF over time between giant collisions. CMF change between giant collisions is due to debris accretion. The path of the main embryo that becomes the planet is bolded. Top: the planet has a final CMF of 0.49. It experiences only one erosive collision, but other collisions it experiences close to the end of its life keep the planet’s CMF high (i.e., hit’n’run, hit’n'spray), and debris reaccretion does not bring its CMF down as much. Bottom: final planet CMF of ∼0.35. Even though it experiences two erosive collisions that significantly increase its CMF, the final CMF of the planet is actually quite close to the initial of 0.33 because of debris reaccretion and other collisions that bring the planet’s CMF down, mainly graze’n’merge.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Final CMF of each planet with respect to the number of each type of collision it experienced in its lifetime. The planets are color coded by f erosive, which is the fraction of the collisions in the planet’s history that were erosive collisions. Planets less than 0.1 M ⊕ are included as “×” in the plot. The black line is the initial CMF all embryos start with. Super-catastrophic collisions are not included because any embryo that experiences these will not become a planet. We exclude catastrophic disruption because it does not occur, and merge is not included but follows the same trend seen in the panels shown. For all collision types, a planet that experiences more collisions of that type will be more likely to have a final CMF that is closer to the initial CMF. The fewer collisions of a certain type the planet experiences, the wider a range of final CMFs it can occupy. For erosive collisions, this trend is not as strong, particularly since there are so few planets with more than two erosive collisions.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Comparison of the CMF distributions of the final planets in debris-loss runs to those without for this study and for planets from Scora et al. (2020). The distributions are achieved with a kernel density estimator (kde) to avoid binning effects. The excited disk simulations with 50% debris loss have a significantly wider distribution than the others, and therefore a higher average CMF. The maximum CMF reached is higher for planets in this study than in Scora et al. (2020), but the maximum CMF is roughly the same for both debris-loss and non-debris-loss runs.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Relationship between the final CMF and mass of planets for runs with 0% and 50% debris loss. The points are color coded by the number of giant collisions experienced in their lifetime. The color bar is on a log scale from 0 to 100. The dashed line shows the initial CMF given to all planets, and the solid black line with error bars shows the mass-binned average CMF. The vertical gray lines show the bins, and the error bars show the 1σ spread in CMF in each bin. The gray ×’s are planets that are smaller than 0.1 M ⊕. We see a strong correlation between the planet mass and the range of CMFs that it can have, with more massive planets that have experienced more collisions having lower CMFs.
Paper: Does the Gamma-Ray Binary LS I + 61°303 Harbor a Magnetar?
Authors: Arthur G. Suvorov, Kostas Glampedakis
Figure caption: Characteristic strains h 0 from Equation (20) as a function of the poloidal-to-total magnetic energy ratio, Λ, using the dipolar Tolman-VII model (Equation (21)) of Mastrano et al. (2011) for LSI. The colored bands represent the prediction for different B  p , with the lower curves having M ⋆ = 1.4 M ⊙ and R ⋆ = 10 km and the upper curves having M ⋆ = 2 M ⊙ and R ⋆ = 14 km. Overlaid are the detection thresholds for aLIGO and ET for a variety of different observation times T obs, as indicated by the labeled dashed lines.
Paper: Does the Gamma-Ray Binary LS I + 61°303 Harbor a Magnetar?
Authors: Arthur G. Suvorov, Kostas Glampedakis
Figure caption: “Strong-field” spin period evolutions: P(t) tracks for LSI permitting large polar field strengths, B  p  ≳ 1014 G, as shown in the panel legends. Larger braking indices allow for ﹩\dot{P}﹩ to be relatively small at early times t ≤ 5 kyr (see insets, which display ﹩\dot{P}﹩ as in Figure 2). Propeller torques may activate at this fiducial switching time for an accretion rate ﹩{10}^{-6}\leqslant \dot{M}/{\dot{M}}_{\mathrm{Edd}}\leqslant {10}^{-5}﹩ (left panel) or the surface field may decay to a dipole-like configuration with 2.5 ≤ n ≤ 3 (right panel) to account for a large ﹩\dot{P}﹩ shortly after t = 5 kyr. We fix α = 0.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Pericenter fraction (f peri = (r  GC  − r peri)/(r apo − r peri) of observed dSphs (black) and subhalos (blue) from six MW-like N-body cosmological simulations. We exclude LMC dSphs and dSphs with large uncertainties from the observed sample (see text). For the observed sample, the bins are made from the Monte Carlo chains of each satellite. In both samples there are “excesses” of satellites near the pericenter and apocenter as the radial velocity is zero there and thus satellites spend relatively more time there.
Paper: GRB 220426A: A Thermal Radiation–Dominated Gamma-Ray Burst
Authors: Yun Wang, Tian-Ci Zheng, Zhi-Ping Jin
Figure caption: Correlations and statistical distributions. For comparison, purple and green represent GRB 220426A and GRB 090902B, respectively. The black dashed line is the range of the 1σ confidence interval of GRB 220426A in the E  γ,iso–E  p,z  correlation. (a) is the intrinsic spectral peak energy (E  p,z ) and isotropic equivalent gamma-ray radiation energy (E  γ,iso) correlation diagram. Blue and red dashed lines represent the best-fit correlations for the type-I and type-II GRB samples, respectively. The trajectory indicate GRB 220426A in different redshift values (from 0.1 to 5). (b) is the T 90,z –EH diagram, and the trajectories is calculated at different redshift from 0.001 to 5. (c) and (d) give the E  p  and HR, respectively, and the comparison with other GRBs in the Fermi-GBM catalog.
Paper: The Stellar Mass Function in CANDELS and Frontier Fields: The Buildup of Low-mass Passive Galaxies since z ∼ 3
Authors: Paola Santini, Marco Castellano, Adriano Fontana, Flaminia Fortuni, Nicola Menci, Emiliano Merlin, Amanda Pagul, Vincenzo Testa, Antonello Calabrò, Diego Paris, Laura Pentericci
Figure caption: Upper panels: mass counts of passive galaxies in different redshift bins in the CANDELS deep and wide sample (i.e., all CANDELS except the HUDF area, turquoise), in HUDF (orange), in the HFF data set (magenta), and in the total sample (black). Lower panels: observational completeness of passive galaxies calculated by means of simulations for the different data sets (same color coding as above). The horizontal dotted lines mark the 75% completeness above which the SMF is computed.
Paper: GRB 220426A: A Thermal Radiation–Dominated Gamma-Ray Burst
Authors: Yun Wang, Tian-Ci Zheng, Zhi-Ping Jin
Figure caption: The first three panels from top to bottom are the evolution diagrams of the posterior parameters of different models. The red dashed line in the first panel is the limit of the synchrotron shock model, also known as the “Line of Death” (Preece et al. 1998, 2002). The green dashed line in the second panel represents the typical value of high-energy photon spectral index (β ∼ 2) (Preece et al. 2000). The bottom panel is the evolution of the bulk Lorentz factor Γ and the radius of the photosphere R ph.
Paper: GRB 220426A: A Thermal Radiation–Dominated Gamma-Ray Burst
Authors: Yun Wang, Tian-Ci Zheng, Zhi-Ping Jin
Figure caption: Upper panel: spectral analysis results of time-integrated spectrum ([T 0 − 0.05, T 0 + 7.79 s]). Upper left: the observed photon count spectra (scatter of different colors) and the photon spectra (brown dashed line) obtained by the mBB+PL model folded response file of each detector. Upper middle: the corresponding ν F  ν  spectra. Upper right: the posterior parameter distribution of the mBB+PL model. Lower panel: spectral analysis results of a time-resolved spectrum slice ([T 0 + 2.61, T 0 + 2.99 s]). The description is consistent with upper panel except that the model is a single mBB.
Paper: GRB 220426A: A Thermal Radiation–Dominated Gamma-Ray Burst
Authors: Yun Wang, Tian-Ci Zheng, Zhi-Ping Jin
Figure caption: Upper panel: Γ–L diagram for for the bursts given by Lü et al. (2012; excluding those with a Γ in dispute, for example GRB 090510 and GRB 090328A) and for the time-resolved thermal radiation of GRB 090902B and GRB 220426A. The black dashed line represents the fitting result of 1σ prediction interval, which is ﹩\mathrm{log}{\rm{\Gamma }}={2.42}_{-0.06}^{+0.06}+{0.28}_{-0.06}^{+0.06}\mathrm{log}L﹩. Lower panel: E  p –L diagram for the bursts investigated in Zhang et al. (2012). Consistent with the above, the black dashed line represents the fitting result of 1σ prediction interval, which is ﹩\mathrm{log}{E}_{{\rm{p}}}={2.47}_{-0.05}^{+0.05}+{0.40}_{-0.05}^{+0.04}\mathrm{log}L﹩.
Paper: GRB 220426A: A Thermal Radiation–Dominated Gamma-Ray Burst
Authors: Yun Wang, Tian-Ci Zheng, Zhi-Ping Jin
Figure caption: Observational of GRB 220426A. (a) is the light curve of each energy band in different detectors. The bin size is set to 32 ms. (b) is the T 90 calculation. Upper panel of (b) shows the light curve of the NaI detector with an energy range of 50–300 keV with the bin size of 64 ms. The solid red line and dashed magenta line are the Bayesian block and the background, respectively. The bottom panel of (b) shows the photon count accumulation curve. The green dashed line represents the range of values between 5% and 95% of the cumulative photon count.
Paper: GRB 220426A: A Thermal Radiation–Dominated Gamma-Ray Burst
Authors: Yun Wang, Tian-Ci Zheng, Zhi-Ping Jin
Figure caption: Calculation of spectral lags in multiband light curves. Left panel: the multiband light curve is from the Fermi-GBM n0 detector, and the interval in red dashed line are used to calculate the spectral lags. Right panel: the spectral lags between high energy bands and the lowest energy band (10–20 keV), 1σ error bars calculated from Monte Carlo simulations.