adsabs/AstroCLIMB huggingface dataset:
Paper: Remarkable Correspondence of the Sagittarius A* Submillimeter Variability with a Stellar-wind-fed Accretion Flow Model
Authors: Lena Murchikova, Christopher J. White, Sean M. Ressler
Figure caption: Sgr A*'s simulated and observed light curves. Excerpts from simulated data for the SANE torus, MAD torus, and MAD winds are plotted in red, gray, and green, respectively. Solid points represent finely sampled high-cadence light curves, and empty points represent coarsely sampled data obtained with the fast-light approximation (Section 4). Excerpts from observational data are plotted in black—the sample of ALMA data for project 2018.1.01124.S observed in 2019 June. The total length of the simulated data is about 30 hr for torus models and 56 hr for wind models. The total length of the observational data from all sources used here is greater than about 100 hr.
Paper: Revisiting a Disky Origin for the Faint Branch of the Sagittarius Stellar Stream
Authors: Pierre-Antoine Oria, Rodrigo Ibata, Pau Ramos, Benoit Famaey, Raphaël Errani
Figure caption: Evolution of the faint branch selection, from spirals at the start of the simulation 3 Gyr ago (top-left panel, in the initial disk plane, close to the yz MW plane) to the present time (bottom-right panel). The evolution is seen in the xz MW plane, close to the Sgr orbital plane. Particles that will make up the final leading arm are shown in red and the final trailing arm in blue. The black curve represents the progenitor's orbit, and the orange ball represents the Sun. Pericentric passages of the Sgr occur around t ≃ −2.3 Gyr and t ≃ −1.1 Gyr. Similar plots for every snapshot of the simulation and the corresponding video are available in the shared data.
Paper: Revisiting a Disky Origin for the Faint Branch of the Sagittarius Stellar Stream
Authors: Pierre-Antoine Oria, Rodrigo Ibata, Pau Ramos, Benoit Famaey, Raphaël Errani
Figure caption: Fraction of disk particles that end up in the faint branch for a given disk inclination i. Each inclination angle is probed by a holed disk made of the 2 × 104 outermost test particles, with the holed disk rotated as explained in Section 2 around the x-axis (Sun‒MW center axis) for the top panels and around the y-axis for the bottom panels. The arrow points to our best model.
Paper: Revisiting a Disky Origin for the Faint Branch of the Sagittarius Stellar Stream
Authors: Pierre-Antoine Oria, Rodrigo Ibata, Pau Ramos, Benoit Famaey, Raphaël Errani
Figure caption: Comparison of the faint branch (probability ≥80%) from the Gaia EDR3 Sgr sample of Ramos et al. (2021, gray) with the faint branch selection in our N-body model including self-gravity (red for the leading arm, blue for the trailing arm). From top to bottom: proper motions in ﹩{\tilde{{\rm{\Lambda }}}}_{\odot }﹩, in ﹩{\tilde{\beta }}_{\odot }﹩, and line-of-sight velocities (heliocentric reference frame). For comparison, the bottom panel shows bright branch members (probability ≥80%, yellow).
Paper: Revisiting a Disky Origin for the Faint Branch of the Sagittarius Stellar Stream
Authors: Pierre-Antoine Oria, Rodrigo Ibata, Pau Ramos, Benoit Famaey, Raphaël Errani
Figure caption: The Gaia EDR3 Sgr sample from Ramos et al. (2021) in the background (gray), with our selection of faint branch test particles from our simulations from Section 3.1.1 overplotted (red for leading arm, blue for trailing arm). The remnant of the progenitor lies in the 275° ≤ R. A. ≤ 300° region.
Paper: Revisiting a Disky Origin for the Faint Branch of the Sagittarius Stellar Stream
Authors: Pierre-Antoine Oria, Rodrigo Ibata, Pau Ramos, Benoit Famaey, Raphaël Errani
Figure caption: Final snapshot of the simulation (at present time) of our model with massive particles replacing some stellar particles of V21's initial model. Top panel: the faint branch (red for the leading arm, blue for the trailing arm) is well populated, overplotted on V21's particles (green). Bottom panel: density plot of all stream stars (V21's stellar particles plus our faint branch particles).
Paper: A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae
Authors: Mikhail M. Meskhi, Noah E. Wolfe, Zhenyu Dai, Carla Fröhlich, Jonah M. Miller, Raymond K. W. Wong, Ricardo Vilalta
Figure caption: The distance from the mean for each EOS and each population for D KL (top) and D TV (bottom) for BHs (left) and isolated NSs (right). Error bars show 95% confidence intervals.
Paper: A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae
Authors: Mikhail M. Meskhi, Noah E. Wolfe, Zhenyu Dai, Carla Fröhlich, Jonah M. Miller, Raymond K. W. Wong, Ricardo Vilalta
Figure caption: Probability density functions of BHs (top) and NS (bottom) for simulated (color) and observed (black; dashed for isolated and dotted for double NS) distributions.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: 90% credible region for slices of the χ eff distribution at four different values of redshift for the three different prior choices in Table 7 (1–3 from top to bottom).
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: Posteriors for the mixture fraction in Equation (12) obtained for GWTC-3 events under the first prior choice in Table 7. The solid black line shows the mean, while the dashed black lines show the 90% credible region.
Paper: Stability Constrained Characterization of the 23 Myr Old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains?
Authors: Roberto Tejada Arevalo, Daniel Tamayo, Miles Cranmer
Figure caption: Posterior distribution of orbital configurations for the inner two planets, c and d, based on the two observed period ratios shown in blue in the bottom panels. The left panel shows configurations where the planets are in the 3:2 MMR, and the right panel shows nonresonant configurations. See the end of Section 2.1 for variable definitions. Red configurations go unstable in N-body integrations within ≈225 yr (104 orbits) upon sampling a mass and orbit for planet b from RV observations (Section 3). The dashed histograms trace all of the configurations, while the solid histograms are the stability constrained distributions, i.e., weighted by each configuration’s probability of stability as evaluated by the Stability of Orbital Configurations Klassifier (SPOCK; red points have SPOCK probability = 0). The blue solid lines mark the 99.7th percentile upper limit for each parameter. The lower panels show period ratio time series for a 100 random samples, passing through the observations, marked as blue points with their (small) error bars. See the text for discussion.
Paper: Stability Constrained Characterization of the 23 Myr Old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains?
Authors: Roberto Tejada Arevalo, Daniel Tamayo, Miles Cranmer
Figure caption: For the resonant configurations on the left side of Figure 1, we plot the 3:2 resonant island for planets c and d, bounded by the “cat’s eye” separatrix trajectory (solid black line). The x-axis is the 3:2 resonant angle, and the y-axis is the period ratio’s deviation from 3/2. The resonance region varies for each configuration (points) since it depends on the masses and orbital parameters, so the period ratio deviation has been normalized so that the separatrix extends from ≈ [−1, 1] for all points (see the Appendix). The left panel shows the original posterior samples (both black and red points in Figure 1), with the color bar denoting the total planet mass m  c  + m  d . The right panel applies stability constraints by setting an opacity to each point given by the SPOCK probability of stability. As expected, stability preferentially removes configurations near the separatrix, but it also imposes additional structure.
Paper: Stability Constrained Characterization of the 23 Myr Old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains?
Authors: Roberto Tejada Arevalo, Daniel Tamayo, Miles Cranmer
Figure caption: Stability constraints on planet b; masses and eccentricities were drawn from the Suárez Mascareño et al. (2021) RV posteriors (blue histograms), assuming the posteriors are Gaussian. Coloring and opacity scheme of the main panel follows the same as in Figure 1. Stability (orange histograms) strongly constrains the orbital eccentricity. The black dashed lines represent the 99.7th percentile upper limits from stability while the green dashed line depicts the RV Gaussian 3σ upper limit on the eccentricity (also shown in Table 2). The RV measured mass of 0.64 ± 0.19 is within a factor of 2 from the instability region even at zero eccentricity.
Paper: A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae
Authors: Mikhail M. Meskhi, Noah E. Wolfe, Zhenyu Dai, Carla Fröhlich, Jonah M. Miller, Raymond K. W. Wong, Ricardo Vilalta
Figure caption: An overview of our methodology. Different equations of state lead to differences in simulated outcomes of core collapse.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: Posteriors for ﹩{\delta }{\rm{log}}{{\sigma }}_{{m}_{1}},{\delta }{\rm{log}}{{\sigma }}_{z}﹩ obtained under the model allowing for both redshift and primary mass correlations with χ eff, for two different simulated populations. The dark purple shows the results for the population with a simulated redshift correlation, ﹩{\delta }{\rm{log}}{{\sigma }}_{z}=0.85﹩, while the light purple shows the results for the population with a simulated primary mass correlation, ﹩{\delta }{\rm{log}}{{\sigma }}_{{m}_{1}}=0.15﹩. The shading indicates the 1, 2, and 3σ 2D credible regions and the dashed lines on the individual histograms show the 1D 1σ credible interval. While the posterior for the redshift-correlated population is consistent with primary mass being the sole source of correlation, the opposite is not true.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: Spin hyperparameter posteriors obtained for GWTC-3 events when allowing for redshift correlations only. The colors indicate the 1, 2, and 3σ 2D credible regions, the dashed lines on the individual histograms show the 1D 1σ credible interval, and the median and 1σ credible interval are printed above each histogram.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: Spin hyperparameter posteriors obtained for GWTC-3 events when allowing for a correlation between χ eff and both primary mass and redshift. The colors indicate the 1, 2, and 3σ 2D credible regions, the dashed lines on the individual histograms show the 1D 1σ credible interval, and the median and 1σ credible interval are printed above each histogram.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: 90% credible region for slices of the χ eff distribution at four different values of redshift (top) and primary mass (bottom) for the simulated population with a correlation between the width of the χ eff distribution and redshift.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: Posteriors for the mean, μ  χ , and standard deviation, σ  χ , of the binary black hole effective spin distribution as a function of redshift obtained for GWTC-3 events. The solid black line shows the mean, while the dashed black lines show the 90% credible region.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: 90% credible region for slices of the χ eff distribution at four different values of redshift.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: Spin hyperparameter posteriors obtained for GWTC-3 events when allowing for a correlation between χ eff and primary mass only. The colors indicate the 1, 2, and 3σ 2D credible regions, the dashed lines on the individual histograms show the 1D 1σ credible interval, and the median and 1σ credible interval are printed above each histogram.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: 90% credible region for slices of the χ eff distribution at four different values of primary mass.
Paper: The Binary Black Hole Spin Distribution Likely Broadens with Redshift
Authors: Sylvia Biscoveanu, Thomas A. Callister, Carl-Johan Haster, Ken K. Y. Ng, Salvatore Vitale, Will M. Farr
Figure caption: 90% credible region for slices of the χ eff distribution at four different values of redshift (top) and primary mass (bottom) for the simulated population with no correlations.
Paper: Remarkable Correspondence of the Sagittarius A* Submillimeter Variability with a Stellar-wind-fed Accretion Flow Model
Authors: Lena Murchikova, Christopher J. White, Sean M. Ressler
Figure caption: Structure functions of simple harmonics sources described by Equation (A3). Solid line: single-mode source with A = 1, ω = 2π/50,000, B = ν = 0. Dashed line: two-mode source with the same A, ω as above and B = 0.15, ν = 2π/5000. The ﹩{ \mathcal S }{ \mathcal F }﹩ is multiplied by the factor of 0.55 to align with single-mode ﹩{ \mathcal S }{ \mathcal F }.﹩ Universal scaling ∼ τ 1.0 is plotted with a dotted line.
Paper: The Local Stellar Halo is Not Dominated by a Single Radial Merger Event
Authors: Thomas Donlon II, Heidi Jo Newberg, Bokyoung Kim, Sebastien Lépine
Figure caption: Heat maps of kinematic properties of an isotropic halo model (left column) and the Gaia sample of local dwarf stars (three right columns, separated by metallicity as labeled at the top). The top row shows v  r,⊥ vs. L  z , and the bottom row shows ﹩\widetilde{E}﹩ vs. L  z . Arrows and labels identify substructure. At low metallicities, the dwarf star population in the solar region appears similar to an isotropic halo background plus a nonrotating (L  z  ∼ 0) RME at higher energies. At intermediate metallicities, the isotropic component is still evident, but at high energies, the population is dominated by a retrograde RME, and at low energies, there are an excess of prograde stars and an overdensity at L  z  = −1000 kpc km s−1. At high metallicities, the dwarf stars are primarily made up of the L  z  = −1000 kpc km s−1 overdensity plus a crescent of disk/Splash stars bleeding up to positive L  z . The missing semicircle of data at v  r,⊥ = 0 and L  z  = −1500 kpc km s−1 is due to the proper motion cut that removes disk stars.
Paper: The Local Stellar Halo is Not Dominated by a Single Radial Merger Event
Authors: Thomas Donlon II, Heidi Jo Newberg, Bokyoung Kim, Sebastien Lépine
Figure caption: Metallicity and radial velocity of the low-energy structures. The top, middle, and bottom rows present results for the low-energy RME (a.k.a. Cronus), the low-energy halo, and the metal-poor halo, respectively. Purple boxes show two samples in regions where an excess has been identified, yellow boxes the halo, and red boxes the disk (solid line) and a region with opposite velocity (dashed line). The middle panels in the top and middle rows show the MDFs of the overdense region (purple line), the estimated total background (dashed black line), and the difference between them (solid black line, corresponding to Cronus and the low-energy halo). The bottom middle panel shows the MDF of the halo and disk comparison regions. The rightmost column shows the v  r,⊥ distributions for each substructure, using only stars with −1.5 < [Fe/H] < −1. The top-right panel shows the radial velocity distributions for stars with the v  ϕ  range of the Cronus excess region (purple line) and the halo region with an opposite v  ϕ,⊥ (yellow line). The yellow distribution is artificially high at large ∣v  r,⊥∣ due to the VRM velocity lobes. The solid black line shows the difference between the purple and yellow distributions, which represents the Cronus v  r,⊥ distribution. A dashed black line shows a Gaussian that has been normalized to the solid black distribution; the depletion near v  r,⊥ = 0 in the solid black distribution compared to the Gaussian suggests that Cronus is associated with an RME. The right panel in the center row shows the velocity distribution of the low-energy halo; the Gaussian is not fit on the left side due to the apparent pollution of the data by VRM stars. The bottom-right panel shows the radial velocity distribution of halo stars within the v  ϕ  range of the dashed red box and a Gaussian fit to it. Also shown is the v  r,⊥ distribution for stars with the v  ϕ  range of the solid yellow box, which includes halo in the center plus VRM lobes on each side.
Paper: The Local Stellar Halo is Not Dominated by a Single Radial Merger Event
Authors: Thomas Donlon II, Heidi Jo Newberg, Bokyoung Kim, Sebastien Lépine
Figure caption: Kinematic properties of the various structures identified in this work. The dark red and purple dashed lines indicate the extent of the nonrotating and retrograde high-energy RMEs, respectively. The solid yellow line indicates the extent of the low-energy RME, and the dashed light-blue line surrounds the isotropic halo background. The light-red ellipse indicates the location of the Nyx Stream, the green and blue dashed lines show the extent of Splash and disk stars, respectively. Contours in the bottom row show the 95%, 75%, and 50% levels of stars within the VRM, Nereus, and Cronus selections in the top row. The stars in the center of the top panels have low velocity, and therefore lower energy since the stars in the solar neighborhood have similar potential energies.
Paper: The Local Stellar Halo is Not Dominated by a Single Radial Merger Event
Authors: Thomas Donlon II, Heidi Jo Newberg, Bokyoung Kim, Sebastien Lépine
Figure caption: Properties of the Nyx Stream. The left panel shows a heat map of velocities in our polar sample. A solid white outline marks the velocity extent of the excess that has been associated with the Nyx Stream. A dashed white outline marks an adjacent background region of similar size. The right panel shows the MDF for the excess region, the background region, and their difference, which represents the distribution of the Nyx Stream stars.
Paper: The Local Stellar Halo is Not Dominated by a Single Radial Merger Event
Authors: Thomas Donlon II, Heidi Jo Newberg, Bokyoung Kim, Sebastien Lépine
Figure caption: Fit MDFs for the two high-energy RMEs. The purple line corresponds to the VRM, and the red line corresponds to a low-metallicity, nonrotating (collection of) RME(s). The two structures contribute roughly similar numbers of stars to the nearby stellar halo.
Paper: Onset of Particle Acceleration during the Prompt Phase in Gamma-Ray Bursts as Revealed by Synchrotron Emission in GRB 160821A
Authors: Felix Ryde, Shabnam Iyyani, Björn Ahlgren, Asaf Pe'er, Vidushi Sharma, Christoffer Lundman, Magnus Axelsson
Figure caption: Evolution of the main episode of GRB 160821A. The yellow shaded regions represent the three time bins that are analyzed and correspond to time intervals where the polarization measurements are made using AstroSat CZTI data. (a) The high-resolution (0.01 s) light curve (blue) and the Bayesian block binned light curve (black line), with a false-alarm probability to compute the prior, p 0 = 0.01. The y-axis represents the probability density, which gives the counts per bin divided by the width of the bin. The polarization fraction, PF, and the polarization angle, PA, obtained by Sharma et al. (2019) are shown in magenta star and blue diamonds, respectively. The temporal variation of the derived physical parameters, assuming Γ = 300 and z = 0.4, are shown: (b) the number of radiating electrons, N e; (c) the comoving magnetic field, B, and (d) the magnetization, σ.
Paper: Onset of Particle Acceleration during the Prompt Phase in Gamma-Ray Bursts as Revealed by Synchrotron Emission in GRB 160821A
Authors: Felix Ryde, Shabnam Iyyani, Björn Ahlgren, Asaf Pe'er, Vidushi Sharma, Christoffer Lundman, Magnus Axelsson
Figure caption: Spectral distributions of electrons and gamma rays. Left panel: electron energy spectrum used in fits to the three time intervals. Because the fits are translationally degenerate, the energy scale is arbitrary (see, e.g., Burgess et al. 2014). The physical quantities are later derived in Appendix A.3. Right panel: ν F  ν  spectrum from the three time intervals, being the best fits to the data.
Paper: Onset of Particle Acceleration during the Prompt Phase in Gamma-Ray Bursts as Revealed by Synchrotron Emission in GRB 160821A
Authors: Felix Ryde, Shabnam Iyyani, Björn Ahlgren, Asaf Pe'er, Vidushi Sharma, Christoffer Lundman, Magnus Axelsson
Figure caption: Draws from the posterior distribution of the model conditioned on the data in the three intervals. The 50 thin lines correspond to random draws from the posterior distribution, and the dashed line corresponds to the MAP. The data and model have been rebinned to bins containing at least 20 counts. The blue, orange, green, red, and purple colors correspond to the NaI6, NaI7, NaI9, BGO 1, and LAT/LLE data, respectively.
Paper: Onset of Particle Acceleration during the Prompt Phase in Gamma-Ray Bursts as Revealed by Synchrotron Emission in GRB 160821A
Authors: Felix Ryde, Shabnam Iyyani, Björn Ahlgren, Asaf Pe'er, Vidushi Sharma, Christoffer Lundman, Magnus Axelsson
Figure caption: The relative Lorentz factor Γr across the shock vs. the bulk Lorentz factor, Γ. The colored lines are given by ﹩{{\rm{\Gamma }}}_{{\rm{r}}}=0.55{\sigma }_{{\rm{d}}}^{-1/2}({\rm{\Gamma }})﹩, where σ d(Γ) is the measured magnetization for different Γ. The lines are for the three intervals in GRB 160820A (same colors as in Figure 2). The black line is for Γr = Γ; therefore, only parameter values below this line are allowed. The lines cross each other at Γ = 420, 510, and 770, as marked by the dashed lines. This gives the estimate of the Lorentz factor to be 420 < Γ < 770. A redshift of z = 0.4 is assumed.
Paper: Onset of Particle Acceleration during the Prompt Phase in Gamma-Ray Bursts as Revealed by Synchrotron Emission in GRB 160821A
Authors: Felix Ryde, Shabnam Iyyani, Björn Ahlgren, Asaf Pe'er, Vidushi Sharma, Christoffer Lundman, Magnus Axelsson
Figure caption: Corner plot of the posterior probability distribution of free model parameters, as well as the derived values of the break energies in the photon spectra. The blue, green, and red colors correspond to intervals 1, 2, and 3, respectively, and the light and dark contours represent the 68% and 95% credible regions.