adsabs/AstroCLIMB huggingface dataset:
Paper: Grain Growth and Dust Segregation Revealed by Multiwavelength Analysis of the Class I Protostellar Disk WL 17
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Jaehan Bae, Patrick Sheehan
Figure caption: DIANA dust absorption opacities used for radiative transfer modeling. The 15 adopted opacities and ﹩{a}_{\max }﹩ = 1 μm opacities have different line colors and styles depending on ﹩{a}_{\max }﹩ and q. Two gray dashed vertical lines correspond to ALMA Band 3 (3.1 mm) and 7 (0.87 mm) wavelengths. For comparison, the opacity computed in Beckwith et al. (1990) is indicated by a black dashed–dotted line. Note that this widely used opacity is particularly similar to the DIANA opacity with ﹩{a}_{\max }﹩c = 1 cm and q = 3.5.
Paper: Grain Growth and Dust Segregation Revealed by Multiwavelength Analysis of the Class I Protostellar Disk WL 17
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Jaehan Bae, Patrick Sheehan
Figure caption: Part of the 15 best-fit models depending on ﹩{a}_{\max }﹩ and q. The top two panels are the same as the Band 3 and 7 data shown in Figures 1 and 2(b). The red star indicates the position of the protostar. The remaining panels are the model images. From the left, the first column shows the three Band 3 model images depending on ﹩{a}_{\max }﹩ and q, the second column shows their residual maps obtained by subtracting individual models from the Band 3 observational image, the third column shows the Band 7 model images, and the fourth column shows their residual maps obtained by subtracting individual models from the Band 7 observational image. Contour levels in the Band 3 and 7 residual maps are {−3, 3}, where σ B3 = 33 μJy beam−1, and {−3, 3, 9, 15}, where σ B7 = 0.4 mJy beam−1, respectively. Note that only these three models, mainly populated by centimeter-sized large grains, reproduce well the central hole in Band 7.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Similar to Figure 5, but for the conditions used to generate Figure 9 (left), Figure 10 (middle), and Figure 11 (right). The discussion in Section 7.1 applies in these cases as well. In the middle panels where Γ s  is increased, the curvature of the spectrum is inside the detector window, and the excess of bursts with α 2 ∼ − 2 vanishes. Furthermore, the spectral indices are more clustered around the values expected in marginally fast cooling synchrotron emission.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Similar to Figure 4, but using the conditions for the reverse shock instead of the forward shock in Equations (B7) and (B8). The resulting spectra has lower values of E peak and are softer, with α reaching ∼ − 1.5 in a few cases in the delayed acceleration scenario.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Similar to Figure 4, but generated from the higher-order initial parameter distribution given in Table 4. A higher initial value of Γ s  has a small effect on α but increases the observed peak energy.
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: Left: the SSMF for individual groups in the ELVES Survey where each curve represents the SSMF for one Local Volume group surveyed in ELVES. We forward model completeness in Section 4.3 but do not correct it here. The shaded regions associated with each curve show the 1σ uncertainty of the number of satellites, taking into account the “unconfirmed/candidate” satellites (see text). The groups are listed in the legend sorted by their K-band magnitude (with NGC 3379 having the brightness group K-band magnitude of M  K,NGC3379 = −25.37 mag and NGC 4517 having the faintest group K-band magnitude of M  K,NGC4517 = −22.16 mag. The legend also lists the radial coverage (in projected kiloparsecs from the group central galaxy) of the survey imaging used to find candidate satellites. Right: the combined SSMF for the 27 groups used in the analysis (excluding the NGC 3379, NGC 3627, and M81 groups). In total, the black curve shows 279 ± 4 satellite galaxies and are used in the analysis.
Paper: Prospects for Cryovolcanic Activity on Cold Ocean Planets
Authors: Lynnae C. Quick, Aki Roberge, Guadalupe Tovar Mendoza, Elisa V. Quintana, Allison A. Youngblood
Figure caption: Total internal heating, H Total, for the cold ocean planets in our study compared to H Total for Europa, Earth, and Io. Every planet that we have considered receives more heating from tidal and radiogenic sources than Europa, which is cryovolcanically and tectonically active, and maintains an ocean beneath its icy shell. OGLE 2005-BLG-390-Lb receives approximately the same amount of internal heating as Io, the most volcanically active body in our solar system. Internal heating rates for Kepler 1652 b, Kepler 1544 b, Kepler 441 b, Kepler 296 f, LHS 1140 b, Proxima Cen b, Kepler 1229 b, HD33793 c, and GJ 514 b exceed that of Io. This suggests that all planets in our study receive enough internal heating to maintain internal oceans and cryovolcanic activity at their surfaces. 1 Watt = 107 erg s−1.
Paper: Prospects for Cryovolcanic Activity on Cold Ocean Planets
Authors: Lynnae C. Quick, Aki Roberge, Guadalupe Tovar Mendoza, Elisa V. Quintana, Allison A. Youngblood
Figure caption: Total internal heating, H Total, for the cold ocean planets in our study compared to H Total for Earth, Io, and the geologically active ocean worlds in our solar system. Compared to volcanic activity rates on Earth and Io, and cryovolcanic activity rates on Europa and Enceladus, all of the cold ocean planets considered here are likely to be cryovolcanically active. Cold ocean planets in the blue shaded region may exhibit very high rates of cryovolcanism with frequent eruptions of large geyser-like plumes that vent water and its constituent molecules into space. Cold ocean planets in the green shaded region are also likely to exhibit cryovolcanism with explosive venting of geyser-like plumes but may have slightly smaller, less frequent eruptions. 1 Watt = 107 erg s−1.
Paper: Prospects for Cryovolcanic Activity on Cold Ocean Planets
Authors: Lynnae C. Quick, Aki Roberge, Guadalupe Tovar Mendoza, Elisa V. Quintana, Allison A. Youngblood
Figure caption: The initiation of cryovolcanism on cold ocean worlds. (a) Cryovolcanism may be initiated on cold ocean planets with thin (approximately <10 km thick) ice shells by the exsolution of volatiles from water-filled fractures connected to a subsurface ocean. (b) Water erupted during explosive cryovolcanic eruptions on cold ocean planets that have relatively thick ice shells, such as OGLE-2005-BLG-390-Lb and Trappist-1h, may be sourced from salty water pockets that are perched in their ice shells, rather than directly from the subsurface oceans. Figures after Fagents (2003).
Paper: Prospects for Cryovolcanic Activity on Cold Ocean Planets
Authors: Lynnae C. Quick, Aki Roberge, Guadalupe Tovar Mendoza, Elisa V. Quintana, Allison A. Youngblood
Figure caption: Geometry for the solidification of the subsurface ocean on a cold ocean planet. Here the ice shell is represented as a solid layer at a single, constant surface temperature (T  S ), while the subsurface ocean is represented as a layer of liquid. The boundary between the ice shell and ocean has a constant temperature, T melt = 273 K. Here h out represents conductive heat loss that causes the solidification front, S(t), to advance. S(t) measures the position of the ice–water interface over time, which defines the instantaneous thickness (D) of the ice shell in response to the gradual cooling of the ocean. H Total represents basal heating added into the system from tidal dissipation and radiogenic sources.
Paper: Prospects for Cryovolcanic Activity on Cold Ocean Planets
Authors: Lynnae C. Quick, Aki Roberge, Guadalupe Tovar Mendoza, Elisa V. Quintana, Allison A. Youngblood
Figure caption: Explosive cryovolcanism in the form of geyser-like plumes on two of our solar system’s ocean worlds. Left: Cryovolcanic eruptions at the south pole of Saturn’s moon Enceladus (credit: NASA/JPL-Caltech/SSI). Right: Hubble Space Telescope UV observations of cryovolcanic eruptions at the south pole of Jupiter’s moon Europa (credit: NASA/L. Roth). By facilitating the transport of liquid water and energy between their interiors and surfaces, similar activity could create habitable environments on cold ocean planets.
Paper: A Magnetically Driven Disk Wind in the Inner Disk of PDS 70 
Authors: Justyn Campbell-White, Carlo F. Manara, Myriam Benisty, Antonella Natta, Rik A. B. Claes, Antonio Frasca, Jaehan Bae, Stefano Facchini, Andrea Isella, Laura Pérez, Paola Pinilla, Aurora Sicilia-Aguilar, Richard Teague
Figure caption: X-Shooter and an example HARPS spectra of PDS70 Hα profile. Flux is normalized and continuum subtracted.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Histograms obtained by fitting a CPL function to 150 synthetic photospheric spectra, using the method described in Sections 4.2 and 4.3. The mean and standard deviations for the input RMS and KRA parameters are given in Table 2, which in turn are obtained from the higher-order initial parameter distributions given in Table 1. Top panels show α, and bottom panels show E peak, for the early acceleration scenario (left) and the delayed acceleration scenario (right), as also indicated in the panels. The solid dark green lines show the distributions found for the CPL parameters in a time-resolved catalog of bright Fermi GRBs during the first 4 yr of observations (Yu et al. 2016). It is evident that, unless collimation shocks delay the acceleration, the distribution obtained is harder than most observed bursts. All panels are made with χ = 1, and z = 1.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Photospheric KRA spectra generated using Komrad in the internal collision framework for Γ s  = 101.5, τ  s  = 101.5, and ψ = 10 in the early acceleration scenario (red, r 0 = 107  cm, Γ0 = 1.5) and in the delayed acceleration scenario (green, r 0 = 1010  cm, Γ0 = 4). The spectra are shown prior to the forward-folding through the Fermi response. The shaded area is a rough indication of the Fermi GBM sensitivity range, with lighter shading implying less sensitivity (Meegan et al. 2009). The parameter values obtained in the early acceleration scenario are τ θ = 4.2 (τ = 95, θ  r  = 0.045), R = 27, y  r =3.76, and Γ = 100. In the delayed acceleration scenario, they are τ θ = 5.1 (τ = 97, θ  r  = 0.053), R = 220, y  r =2.1, and Γ = 100.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Histograms obtained by fitting a 2SBPL function to 150 synthetic photospheric spectra in the delayed acceleration scenario, obtained using the method described in Sections 4.2 and 4.3. The insets show the subset with ΔAIC < 0. Left panel shows the low-energy indices α 1 and α 2, and the right panel shows the ratio of the peak energy to the break energy. The lines are smoothed kernels of each distribution. The excess of fits with α 2 ∼ − 2 is due to bursts where the hardening of the spectrum is below the detector energy window (see main text). These spectra are not better described by 2SBPL function compared to a CPL function as evident from the inset. When the Lorentz factor increases, more of the curvature is visible in the detector, and the excess disappears, which can be seen in the top middle panel of Figure 12. Both panels are made with χ = 1, and z = 1.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Figure showing ﹩{\theta }_{r}^{v}﹩ (left axis, blue line) and ﹩{\bar{\epsilon }}_{r}﹩ (right axis, red line) as a function of optical depth for a simulation. The effective electron temperature ﹩{\theta }_{r}^{v}﹩ initially grows as the Compton temperature in the shock grows. It tends to its steady-state value θ  r , which is indicated by the horizontal dotted line. As expected, the average photon energy in the RMS, ﹩{\bar{\epsilon }}_{r}﹩, remains at all times constant and equal to ﹩{\bar{\epsilon }}_{d}﹩, which is indicated by the horizontal dashed line. The vertical dotted–dashed line shows our estimate of τ ss calculated using Equation (5). It slightly underestimates when equilibrium is reached, which is expected since Equation (5) assumes a constant energy gain per scattering of 4θ  r , while the true energy gain per scattering is equal to ﹩4{\theta }_{r}^{v}﹩, which is initially lower than 4θ  r . Adiabatic cooling is not included. Parameter values are τ θ = 5, θ  r  = 0.1, R = 500, y  r  = 1.5.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Count spectrum (top) and ν F  ν  spectrum (bottom) obtained by fitting a CPL function to the (forward-folded) photospheric spectrum in the delayed acceleration scenario from Figure 2. As the hardening of the input spectrum at low energies is outside of the GBM sensitivity range (indicated by the shaded area), the fit is adequate. In the bottom panel, the unfolded photospheric spectrum from Figure 2 has been overlaid for comparison. Best-fit parameters are α = − 0.92 ± 0.05, and ﹩{E}_{\mathrm{peak}}={150}_{-12}^{+13}\,﹩ keV.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Left: evolution of the RMS spectrum in a simulation. Ten snapshot spectra are shown, taken at even intervals of τ ranging from the initial value τ = 50 (black) until the shock has crossed the upstream, at τ = 25 (red). Initially, the shock contains a Wien thermal photon distribution with mean energy ﹩{\bar{\epsilon }}_{d}﹩. As the shock evolves, the initial peak moves to higher energies and broadens, while new cold photons enter the shock from the upstream. At τ ≈ 33 (snapshot seven), steady state has been reached and the final spectra are overlapping. This corresponds well with the estimate shown in Figure 6. Right: similar to the left panel but for the downstream spectrum. This time the spectra range from τ = 50 all the way up until the photosphere, at τ = 1 (from darker to brighter green). Note that the spectrum for τ = 50 is not visible since the downstream does not contain any photons at the start of the simulation. For this specific choice of parameters, the optical depth was large enough to erase all signatures of the shock formation in the final spectrum. Adiabatic cooling and the broadening effects explained in Appendix C are not included. Parameter values are the same as in Figure 6.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: A schematic of the subphotospheric internal collision framework. Two fireballs are accelerated from the base in a conical outflow, starting at radius r 0 and with an initial Lorentz factor Γ0. The slower of the two fireballs has a bulk Lorentz factor Γ s , and the faster fireball has a Lorentz factor Γ f  = ψΓ s . The collision occurs at an optical depth (as measured for the slower fireball) τ  s , with the requirement τ  s  > 5 to avoid the dynamical changes that occur in the RMS at small optical depths.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Similar to Figure 4, but generated from the higher-order initial parameter distribution given in Table 3. This choice of initial parameters results in higher values of τ  i  on average, leading to harder spectra. Many of these bursts would likely be missed in observations due to the increase in adiabatic degrading and decrease in luminosity.
Paper: Observational Characteristics of Radiation-mediated Shocks in Photospheric Gamma-Ray Burst Emission
Authors: Filip Samuelsson, Felix Ryde
Figure caption: Two spectra before (solid lines) and after (dashed lines) the broadening effects have been added. The solid lines correspond to comoving spectra at the photosphere, and the dashed lines to the shapes of the observed spectra, but shifted down in energy to have the same average photon energy as the corresponding comoving spectrum (see the text for details). Both initial spectra have been normalized such that θ  u,K = 1. The red spectrum has a smaller ratio between the peaks (R = 50) than that of the green (R = 1000). It is evident that the effect of the broadening scheme is most important for the narrower spectrum. Other parameter values are τ θ = 5, and y  r  = 1.5.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Temperature slices in the xy-plane through the Hydro (left) and MHD (right) simulations after 9 Gyr of evolution. The virial radius of the simulation is shown by a black circle. The white X shows the position of the example sight line shown in Figure 4. Each simulation ran for 9 Gyr, which we show in the lower left of each panel.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Component turbulent measure, b turb, in the large-scale simulations as a function of distance from the center of the simulation, ρ. Results through the Hydro box are shown on the top panel, while the MHD results are on the bottom. Each column corresponds to a different axis being probed by the sight lines, where y is along the axis of rotation and x and z are perpendicular to it. Sight lines along the x-axes and y-axes are a subset of those along the z-axes, so fewer points are present in these panels.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Turbulent measures in the small-scale simulations as a function of injected σ 1D, where the top panels show b turb and the bottom panels are σ LOS. Each column is labeled with the nL drive of the box the results are through. The coloring and symbol in the top panel indicate the ion being shown, with blue circles for C IV, yellow triangles for Si IV, red diamonds for O VI, and cyan stars for Si II. The dashed black line in each panel shows the 1-to-1 line in each panel.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Example spectrum of Si IV (top) and C IV (bottom) through the large-scale MHD simulation with ρ = 50 kpc is shown in the left panel. The position of this example sight line is shown in Figure 3 as a white X. The resulting Voigt profile fits from RBVFit are shown in the right panels.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Temperature slices in the xy-plane through the nL drive = 1020 cm−2 density small-scale simulations. The injected σ 1D is shown in the lower left of each panel. The upper left shows the amount of time each simulation was run for.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Temperature slices in the xy-plane through each simulation with σ 1D  = 46 km s−1. The upper left of each panel shows the nL drive of the simulation being shown.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Sight line turbulent measure, σ LOS, in the Hydro simulation as a function of distance from the center of the simulation, ρ. Our measured values are shown as blue circles, while the red triangles show the measurements after applying the line of best fit from the nL drive = 1021 cm−2 small-scale simulation. The errors on σ LOS were smaller than the point sizes, so they are not shown. Each column corresponds to a different ion, which is labeled at the top, while each row corresponds to a different axis being probed by the sight lines. The “true” σ LOS is shown in each panel as a black line as defined in the text.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Same as Figure 7 except for the measurements through the MHD simulation.
Paper: Constraining Circumgalactic Turbulence with QSO Absorption Line Measurements
Authors: Brad Koplitz, Edward Buie II, Evan Scannapieco
Figure caption: Comparing σ LOS (Si II) measured through the large-scale simulations to the COS-Halos observational survey as a function of impact parameter normalized by the virial radius, ρ / R vir. Blue circles show our measurements through the Hydro and MHD simulations on the left and right panels, respectively, while values derived from COS-Halos measurements (Werk et al. 2013) are shown as cyan diamonds.
Paper: Constraining Inputs to Realistic Kilonova Simulations through Comparison to Observed r-process Abundances
Authors: Marko Ristić, Erika M. Holmbeck, Ryan T. Wollaeger, Oleg Korobkin, Elizabeth Champion, Richard O'Shaughnessy, Chris L. Fryer, Christopher J. Fontes, Matthew R. Mumpower, Trevor M. Sprouse
Figure caption: Unscaled mass fractions X as a function of atomic number Z for all single-Y  e  compositions considered in this work. The labels pertaining to the dynamical ejecta compositions considered in this work indicate the nuclear mass model, fission model, and electron fraction Y  e  used to generate the respective composition. The remaining labels indicate the solar and wind compositions. The wind1 and wind2 compositions do not extend to higher atomic numbers Z owing to their higher electron fractions Y  e  = 0.37 and Y  e  = 0.27, respectively.
Paper: Constraining Inputs to Realistic Kilonova Simulations through Comparison to Observed r-process Abundances
Authors: Marko Ristić, Erika M. Holmbeck, Ryan T. Wollaeger, Oleg Korobkin, Elizabeth Champion, Richard O'Shaughnessy, Chris L. Fryer, Christopher J. Fontes, Matthew R. Mumpower, Trevor M. Sprouse
Figure caption: Unified Modeling Language (UML) diagram describing the large-scale steps taken in creating the r-process mass prior and using it during parameter inference to generate the red posteriors in Figure 8. Per standard UML definition, rectangles represent processes, cylinders represent databases, hexagons represent data preparation steps, and ovals represent terminators, or final products.