adsabs/AstroCLIMB huggingface dataset:
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Similar to Figure 15 but for fixed α  M  = 0.1 and varying K  x .
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Same as Figure 10, but for the AdSI in dust-poor disk with ϵ = 0.2 (run E02eta0am01).
Paper: The Relation between the Optical Fe II Emission and the Dimensionless Accretion Rate for Active Galactic Nuclei
Authors: Yan-Sheng Liu, Wei-Hao Bian
Figure caption: Left: R Fe vs. ﹩\dot{{\mathscr{M}}}﹩. The green line and black line are the best linear fittings for the SDSS subsample (blue points) and the RM subsample (red points). The blue triangles represent the mean R Fe in bins of ﹩{\rm{\Delta }}\mathrm{log}\dot{{\mathscr{M}}}=0.6\,\mathrm{dex}﹩, and the error bars represent the standard deviations. The green solid line shows the best fit to the binned data with a second-order polynomial function. The purple squares denote 44 RM SDSS AGN from the RM subsample. The r  s  and p null for the RM subsample are the ones excluding the SDSS RM AGN. Right: v Fe vs. ﹩\dot{{\mathscr{M}}}﹩ for the SDSS subsample. The green line and black line are the best linear fittings for the inflow AGN (v Fe > 0, red points and red contours) and the outflow AGN (v Fe < 0, blue points and blue contours).
Paper: The Relation between the Optical Fe II Emission and the Dimensionless Accretion Rate for Active Galactic Nuclei
Authors: Yan-Sheng Liu, Wei-Hao Bian
Figure caption: Left: f FWHM vs. FWHM H β . The black line and orange line are the best linear fittings for the SDSS subsample (blue points) and the RM subsample (red points and triangles). The triangles show 44 RM AGN from the SDSS. The red points show other 76 compiled RM AGN excluding 44 RM AGN from the SDSS. The pink line is the relation given by Yu et al. (2020b). Right: f FWHM vs. σ Hβ  for the subsample of 120 RM AGN from the mean spectrum. The symbols are the same as in the left panel. The Spearman correlation coefficient and the probability of the null hypothesis are shown in panels. The blue is for the SDSS subsample; the purple is for 44 RM AGN from the SDSS; the red is for the RM subsample excluding 44 RM AGN from the SDSS; the orange is for the RM subsample.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Top panels: best-fit measured temperature vs. the true (simulated) temperature for different band combinations as noted, using simulated measurement uncertainties of 0.05 magnitudes and log-uniform priors. The solid lines denote the ensemble median best-fit temperature, and the shaded regions denote the 16th–84th ensemble percentile. Results for both methods are shown. Bottom panels: same as top, but for the difference between the measured and true temperatures. The mean ensemble upper and lower fit uncertainties are shown in dotted lines.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Example MCMC fits to simulated magnitudes of a 30,000 K, 1000 R ⊙ blackbody (black circles) assuming 0.05 magnitude photometric uncertainties, using only optical (in red) vs. optical+ultraviolet (in blue) bands (100 random models drawn from the posterior distribution are shown). The insets show the corner plots for each MCMC fit, with contour lines denoting 90% bounds, and dotted lines denoting the true values. The top and bottom plots are two different realizations of simulated data, each fit also with a different method (see the text for details). Including ultraviolet data reduces both the errors and the uncertainties significantly.
Paper: The Relation between the Optical Fe II Emission and the Dimensionless Accretion Rate for Active Galactic Nuclei
Authors: Yan-Sheng Liu, Wei-Hao Bian
Figure caption:  L Bol/L Edd vs. ﹩\dot{{\mathscr{M}}}﹩ for the subsample of 4037 SDSS quasars (blue points) and the subsample of 120 RM AGN (red points). The black and orange solid lines are the best linear fittings for the SDSS subsample and the RM subsample.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Median (of 100-realization ensembles) best-fit measured temperature vs. the true (simulated) temperature for different methods, priors, and band combinations as noted, using photometric uncertainties of 0.05 magnitudes. The fits using log-uniform priors (solid lines) produce more precise median temperatures compared to those using uniform priors (dashed lines), when using optical data alone (left panel). When adding space-based ultraviolet data (right panel), both priors perform equally well.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Blackbody spectra at various temperatures (denoted in kilo-Kelvin), normalized to their flux at 6000 Å. Swift uvw1 (abbreviated as w1), uvm2 (m2), and uvw2 (w2) filter response curves are shown at the bottom together with those of the optical-infrared ugriz (solid lines) and UBVRI (dotted lines) bands. Blackbodies at temperatures ≳30,000 K all appear very similar in the optical to near-infrared regime.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Same as Figure 4 but using simulated photometric uncertainties of 0.1 magnitudes.
Paper: The Spiderweb Protocluster is Being Magnetized by Its Central Radio Jet
Authors: Craig S. Anderson, Christopher L. Carilli, Paolo Tozzi, G. K. Miley, S. Borgani, Tracy Clarke, Luca Di Mascolo, Ang Liu, Tony Mroczkowski, Maurilio Pannella, L. Pentericci, H. J. A. Rottgering, A. Saro
Figure caption: Maps of peak-P (X plus Ka band), source-frame RM (X plus Ka band; note that values saturate at RM = ±2000 rad m−2 to better reveal low ∣RM∣ structure throughout the jet), intrinsic sky-projected magnetic field orientation (Ka-band only), and fractional polarization (Ka-band only) across the Spiderweb radio jet (rows (a)–(d), respectively). The eastern and western jet components (see Figure 1) are shown in the left-hand and right-hand columns, respectively. Coordinates are shared between axes in the same way as in Figure 1. The effective synthesized beam areas (see Section 3) are shown in the lower-left corner of the right-hand column of panels in white. The location of the X-ray AGN core (Tozzi et al. 2022) is indicated with blue concentric circles. The maps have been masked at full-band polarized signal-to-noise levels of 7σ (for their respective frequency band coverage). The map of fractional polarization has been masked at a full-Ka-band signal to noise of 10σ in the total intensity. The green “x” markers on the RM map mark the positions at which RMs were extracted for values presented in Table 2. The uncertainties in RM (row (b)), intrinsic magnetic field orientation (row (c)), and fractional polarization (row (d)) typically lie in the range 100–400 rad m−2 , 0°–5°, and 0–0.03, respectively.
Paper: The Spiderweb Protocluster is Being Magnetized by Its Central Radio Jet
Authors: Craig S. Anderson, Christopher L. Carilli, Paolo Tozzi, G. K. Miley, S. Borgani, Tracy Clarke, Luca Di Mascolo, Ang Liu, Tony Mroczkowski, Maurilio Pannella, L. Pentericci, H. J. A. Rottgering, A. Saro
Figure caption: MFS maps of the Spiderweb radio jet and lobes at the S band (row (a)), X band (row (b)), and Ka band (row (c)). The full source is shown for scale and perspective. All maps are shown on the same coordinate scale. The X- and Ka-band images are presented with square-root-stretched color scales. The S-band image is presented with a logarithmic color scale to emphasize detail over a larger dynamic range. For all images, the sensitivity is ~5 μJy beam−1. The synthesized beam areas are indicated at the bottom-left in the right-hand column of plots. The position of the X-ray AGN core (Tozzi et al. 2022) is indicated with blue concentric circles. The angular scale is identical between images; the white scale bar indicates a projected span of 50 kpc at z = 2.16 for the adopted cosmology.
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Time evolution of the maximum dust density perturbation for simulations listed in Table 1. The upper and lower panels correspond to ϵ = 3 and 0.2, respectively. The left, middle, and right columns corresponds to ﹩\widetilde{\eta }=0﹩ (no pressure gradient), 0.005, and 0.05, respectively. Within each panel we show vary the applied torque or Maxwell stress α  M  = 0 (green, no accretion flow), α  M  = 0.01 (blue), and α  M  = 0.1 (red). The horizontal dashed–dotted line corresponds to the clumping condition, Equation (25).
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Dust density snapshots of the AdSI (ϵ = 3, ﹩\widetilde{\eta }=0﹩, α  M  = 0.1, run E3eta0am01). The top panel shows the linear growth phase, the middle panel shows the first saturated turbulent state, and the lower panel shows a second saturated state of the system with fewer vertical filaments (after merging) but with higher dust densities.
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Outcome of our main simulation with ϵ = 3 for different Maxwell stresses, α  M , and global radial pressure gradients, ﹩\widetilde{\eta }﹩. Turbulent cases that meet the clumping criterion (Equation (25)) are symbolized by “C”. Cases that are turbulent but do not meet the clumping condition are marked by “T”. The case with ﹩\widetilde{\eta }={\alpha }_{M}=0﹩ remains stable.
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Dust density snapshots of the classic SI (ϵ = 3, ﹩\widetilde{\eta }=0.05﹩, α  M  = 0; run E3eta005am0). The top panel shows the linear growth phase, while the middle and lower panels show the saturated state of the system.
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Similar to Figure 1, but for runs with ϵ = 0.2.
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Autocorrelation function of the gas velocity fluctuations for runs the classic SI (left, run E3eta005am0) and the AdSI (right, run E3eta0am01). Black, red, and blue lines denote the x, y, and z velocity components, respectively. Circles are the half-life points for each component of the velocity fluctuations, which defines the correlation times t  c,i .
Paper: Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks
Authors: Chun-Yen Hsu (徐峻彥), Min-Kai Lin (林明楷)
Figure caption: Spectra of the vertically averaged gas kinetic energy density for the classic SI (top, run E3eta005am0) and the AdSI (bottom, run E3eta0am01). The red dashed lines mark a slope of −5/3.
Paper: Investigating the Asymmetry of Magnetic Field Profiles of “Simple” Magnetic Ejecta through an Expansion-modified Flux Rope Model
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Florian Regnault, Antoinette Galvin
Figure caption: Wind measurements and fitting results for the ME interval (vertical black dashed lines) from 1996 July 1 18:00 UT to July 2 10:30 UT for a Type 1 event. The panels show B total, the three B components in GSE coordinates, the proton velocity, proton density, proton temperature (the red line is the expected temperature), Alfvén mach number, and β  p , from top to bottom, respectively. In the top four panels, the black lines indicate the observations, the red lines indicate the fit with the Lundquist model, and the green lines indicate the fit with the Exp-Lundquist model.
Paper: Survival of Terrestrial N2–O2 Atmospheres in Violent XUV Environments through Efficient Atomic Line Radiative Cooling
Authors: Akifumi Nakayama, Masahiro Ikoma, Naoki Terada
Figure caption: Estimated lifetime of the 1 bar N2–O2 Earth-like atmosphere. We have estimated the lifetime, dividing the mass of the present-day Earth’s atmosphere by the mass-loss rate with (red) and without (blue) major hydrogen species (H and H+) for each XUV irradiation flux. The red line is exactly the same as the lifetime shown in Figure 8.
Paper: Survival of Terrestrial N2–O2 Atmospheres in Violent XUV Environments through Efficient Atomic Line Radiative Cooling
Authors: Akifumi Nakayama, Masahiro Ikoma, Naoki Terada
Figure caption: Temperature (left panel) and compositional (right panel) profiles for present Earth conditions. The solid lines are the profiles derived by our model. The dashed lines represent empirical profiles derived by Picone et al. (2002).
Paper: Investigating the Asymmetry of Magnetic Field Profiles of “Simple” Magnetic Ejecta through an Expansion-modified Flux Rope Model
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Florian Regnault, Antoinette Galvin
Figure caption: Wind: 2004 July 27 02:00:00–2004 July 27 15:30:00 (Type 1). The same format as Figure 1.
Paper: Investigating the Asymmetry of Magnetic Field Profiles of “Simple” Magnetic Ejecta through an Expansion-modified Flux Rope Model
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Florian Regnault, Antoinette Galvin
Figure caption: Wind: 2001 March 20 00:00:00–2001 March 22 00:00:00 (Type 2). The same format as Figure 1.
Paper: Chemical Diversity in Protoplanetary Disks and Its Impact on the Formation History of Giant Planets
Authors: Elenia Pacetti, Diego Turrini, Eugenio Schisano, Sergio Molinari, Sergio Fonte, Romolo Politi, Patrick Hennebelle, Ralf Klessen, Leonardo Testi, Ugo Lebreuilly
Figure caption: Normalized elemental ratios in the final atmosphere of the planet (top two panels) and in the disk (bottom four panels) in the reset scenario with high ionization. The top two panels show results for the six migration scenarios, corresponding to initial semimajor axes of 5, 12, 19, 50, 100, and 130 au. The increasing size of the markers maps the increasing distance traveled by the planet in the six migration scenarios. Linking lines are shown only for visual ease. The plot on the left (with empty markers) describes a gas-dominated giant planet, while the plot on the right (filled markers) is for solid-enriched ones. The bottom four panels show the trends of the elemental ratios on the disk for the gas (dashed lines) and the solid (solid lines) phases. The black, dashed, horizontal line at 1 indicates the reference stellar value in all plots.
Paper: Chemical Diversity in Protoplanetary Disks and Its Impact on the Formation History of Giant Planets
Authors: Elenia Pacetti, Diego Turrini, Eugenio Schisano, Sergio Molinari, Sergio Fonte, Romolo Politi, Patrick Hennebelle, Ralf Klessen, Leonardo Testi, Ugo Lebreuilly
Figure caption: Normalized elemental ratios in the final atmosphere of the planet (top two panels) and in the disk (bottom four panels) in the inheritance scenario with low ionization. The top two panels show results for the six migration scenarios, corresponding to initial semimajor axes of 5, 12, 19, 50, 100, and 130 au. The increasing size of the markers maps the increasing distance traveled by the planet in the six migration scenarios. Linking lines are shown only for visual ease. The plot on the left (with empty markers) describes a gas-dominated giant planet, while the plot on the right (filled markers) is for solid-enriched ones. The bottom four panels show the trends of the elemental ratios on the disk for the gas (dashed lines) and the solid (solid lines) phases. The gray, dashed, vertical lines, from left to right, indicate the position of the snowlines of H2O (2.5 au), refractory organic carbon (3 au), NH3 (9.4 au), CO2 (10.5 au), and CH4 (105 au). The black, dashed, horizontal line at 1 indicates the reference stellar value in all plots.
Paper: Chemical Diversity in Protoplanetary Disks and Its Impact on the Formation History of Giant Planets
Authors: Elenia Pacetti, Diego Turrini, Eugenio Schisano, Sergio Molinari, Sergio Fonte, Romolo Politi, Patrick Hennebelle, Ralf Klessen, Leonardo Testi, Ugo Lebreuilly
Figure caption: Elemental abundances of C, O, N, and S in the disk, normalized to their respective stellar value, for the gas (dashed lines) and the solid (solid lines) phases (the latter includes rocks, organics, and ices). The trends are extracted from the radial profiles of molecular abundances in the four chemical scenarios. The gray, dashed, vertical lines in the top four panels indicate, from left to right, the locations of the snowlines of H2O (2.5 au), refractory organic carbon (3 au), NH3 (9.4 au), CO2 (10.5 au), and CH4 (105 au). Such snowlines are unequivocally defined only in the inheritance scenario with a low ionization level, and for that reason they are omitted in the other scenarios. The black, dashed, horizontal line at 1 indicates the reference stellar value in all plots.
Paper: Chemical Diversity in Protoplanetary Disks and Its Impact on the Formation History of Giant Planets
Authors: Elenia Pacetti, Diego Turrini, Eugenio Schisano, Sergio Molinari, Sergio Fonte, Romolo Politi, Patrick Hennebelle, Ralf Klessen, Leonardo Testi, Ugo Lebreuilly
Figure caption: Elemental ratios C/O*, C/N*, N/O*, and S/N* normalized to their respective stellar value in the four chemical scenarios. The data are the same as in the top two panels of Figures 4–7, here being plotted together to be more easily compared with each other. The blue points refer to the inheritance scenarios, while the red ones refer to the reset scenarios. Specifically, the light-blue octagons and the light-red hexagons indicate low ionization level, while the dark-blue, downward triangles and the dark-red, upward triangles indicate high ionization level. The results are plotted for the six migration scenarios, corresponding to initial semimajor axes of 5, 12, 19, 50, 100, and 130 au. The increasing size of the markers maps the increasing distance traveled by the planet in the six migration scenarios. Trends for both the accretion scenarios are shown: filled markers for solid-enriched and empty markers for gas-dominated giant planets. The black, dashed, horizontal line at 1 indicates the reference value for giant planets whose chemical composition matches that of their host star.
Paper: Chemical Diversity in Protoplanetary Disks and Its Impact on the Formation History of Giant Planets
Authors: Elenia Pacetti, Diego Turrini, Eugenio Schisano, Sergio Molinari, Sergio Fonte, Romolo Politi, Patrick Hennebelle, Ralf Klessen, Leonardo Testi, Ugo Lebreuilly
Figure caption: Normalized elemental ratios in the final atmosphere of the planet (top two panels) and in the disk (bottom four panels) in the reset scenario with low ionization. The top two panels show results for the six migration scenarios, corresponding to initial semimajor axes of 5, 12, 19, 50, 100, and 130 au. The increasing size of the markers maps the increasing distance traveled by the planet in the six migration scenarios. Linking lines are shown only for visual ease. The plot on the left (with empty markers) describes a gas-dominated giant planet, while the plot on the right (filled markers) is for solid-enriched ones. The bottom four panels show the trends of the elemental ratios on the disk for the gas (dashed lines) and the solid (solid lines) phases. The black, dashed, horizontal line at 1 indicates the reference stellar value in all plots.
Paper: Chemical Diversity in Protoplanetary Disks and Its Impact on the Formation History of Giant Planets
Authors: Elenia Pacetti, Diego Turrini, Eugenio Schisano, Sergio Molinari, Sergio Fonte, Romolo Politi, Patrick Hennebelle, Ralf Klessen, Leonardo Testi, Ugo Lebreuilly
Figure caption: Comparison between pairs of normalized elemental ratios in the planet’s atmosphere. Results are shown for the four analyzed chemical scenarios. Each point on the plots represents one of the six analyzed simulations, describing a planet that starts its migration at 5, 12, 19, 50, 100, and 130 au from the star. Color maps and increasing size of markers are used to distinguish between short-scale (light colors, small markers) and large-scale (dark colors, big markers) migrations. The blue markers (hexagons) indicate gas-dominated giant planets, while the red ones (circles) are for solid-enriched ones. The gray, dashed lines indicate stellar values. Their intersection identifies four quadrants in which the elemental ratios can assume sub- or superstellar values. The yellow shaded areas indicate regions of the parameter space that are forbidden in our simulations.
Paper: Chemical Diversity in Protoplanetary Disks and Its Impact on the Formation History of Giant Planets
Authors: Elenia Pacetti, Diego Turrini, Eugenio Schisano, Sergio Molinari, Sergio Fonte, Romolo Politi, Patrick Hennebelle, Ralf Klessen, Leonardo Testi, Ugo Lebreuilly
Figure caption: Normalized elemental ratios in the final atmosphere of the planet (top two panels) and in the disk (bottom two panels) in the inheritance scenario with high ionization. The top two panels show results for the six migration scenarios, corresponding to initial semimajor axes of 5, 12, 19, 50, 100, and 130 au. The increasing size of the markers maps the increasing distance traveled by the planet in the six migration scenarios. Linking lines are shown only for visual ease. The plot on the left (with empty markers) describes a gas-dominated giant planet, while the plot on the right (filled markers) is for solid-enriched ones. The bottom four panels show the trends of the elemental ratios on the disk for the gas (dashed lines) and the solid (solid lines) phases. The black, dashed, horizontal line at 1 indicates the reference stellar value in all plots.
Paper: Chemical Diversity in Protoplanetary Disks and Its Impact on the Formation History of Giant Planets
Authors: Elenia Pacetti, Diego Turrini, Eugenio Schisano, Sergio Molinari, Sergio Fonte, Romolo Politi, Patrick Hennebelle, Ralf Klessen, Leonardo Testi, Ugo Lebreuilly
Figure caption: Comparison between the C/N* and the S/N* ratios of solid-enriched giant planets in the inheritance low scenario. The trends are taken from Figure 4 and shown in linear scale to highlight the differences. The black, dashed, horizontal line at 1 indicates the reference stellar value.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Ratios between the measured and true bolometric luminosities at various temperatures for different SEDs as noted, using photometric uncertainties of 0.05 magnitudes (left) and 0.1 magnitudes (right). The solid lines use the bolometric luminosity calculated from the ensemble median best-fit temperature and radius, and the shaded regions denote the ensemble 16th–84th percentile range.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Distributions of the true temperatures (up to the limit of what was simulated—80,000 K) that lead to various measured temperatures (in 5000 K bins) when a blackbody is fit to gri-band data with 0.05 magnitude photometric uncertainties with the lightcurve_fitting method. Above the measured temperatures of 25,000 K, the real temperature uncertainty becomes large.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Same as Figure 4 but for Johnson–Cousins bands and using simulated measurement uncertainties of 0.1 magnitudes.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Same as Figure 4 but for Johnson–Cousins bands.