adsabs/AstroCLIMB huggingface dataset:
Paper: The Dark Energy Survey: Cosmology Results with ∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set
Authors: DES Collaboration: T. M. C. Abbott, M. Acevedo, M. Aguena, A. Alarcon, S. Allam, O. Alves, A. Amon, F. Andrade-Oliveira, J. Annis, P. Armstrong, J. Asorey, S. Avila, D. Bacon, B. A. Bassett, K. Bechtol, P. H. Bernardinelli, G. M. Bernstein, E. Bertin, J. Blazek, S. Bocquet, D. Brooks, D. Brout, E. Buckley-Geer, D. L. Burke, H. Camacho, R. Camilleri, A. Campos, A. Carnero Rosell, D. Carollo, A. Carr, J. Carretero, F. J. Castander, R. Cawthon, C. Chang, R. Chen, A. Choi, C. Conselice, M. Costanzi, L. N. da Costa, M. Crocce, T. M. Davis, D. L. DePoy, S. Desai, H. T. Diehl, M. Dixon, S. Dodelson, P. Doel, C. Doux, A. Drlica-Wagner, J. Elvin-Poole, S. Everett, I. Ferrero, A. Ferté, B. Flaugher, R. J. Foley, P. Fosalba, D. Friedel, J. Frieman, C. Frohmaier, L. Galbany, J. García-Bellido, M. Gatti, E. Gaztanaga, G. Giannini, K. Glazebrook, O. Graur, D. Gruen, R. A. Gruendl, G. Gutierrez, W. G. Hartley, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, B. Jain, D. J. James, N. Jeffrey, E. Kasai, L. Kelsey, S. Kent, R. Kessler, A. G. Kim, R. P. Kirshner, E. Kovacs, K. Kuehn, O. Lahav, J. Lee, S. Lee, G. F. Lewis, T. S. Li, C. Lidman, H. Lin, U. Malik, J. L. Marshall, P. Martini, J. Mena-Fernández, F. Menanteau, R. Miquel, J. J. Mohr, J. Mould, J. Muir, A. Möller, E. Neilsen, R. C. Nichol, P. Nugent, R. L. C. Ogando, A. Palmese, Y.-C. Pan, M. Paterno, W. J. Percival, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, B. Popovic, A. Porredon, J. Prat, H. Qu, M. Raveri, M. Rodríguez-Monroy, A. K. Romer, A. Roodman, B. Rose, M. Sako, E. Sanchez, D. Sanchez Cid, M. Schubnell, D. Scolnic, I. Sevilla-Noarbe, P. Shah, J. Allyn. Smith, M. Smith, M. Soares-Santos, E. Suchyta, M. Sullivan, N. Suntzeff, M. E. C. Swanson, B. O. Sánchez, G. Tarle, G. Taylor, D. Thomas, C. To, M. Toy, M. A. Troxel, B. E. Tucker, D. L. Tucker, S. A. Uddin, M. Vincenzi, A. R. Walker, N. Weaverdyck, R. H. Wechsler, J. Weller, W. Wester, P. Wiseman, M. Yamamoto, F. Yuan, B. Zhang, Y. Zhang
Figure caption: Constraints for the full DES-SN5YR data set (cyan), when excluding low-z SNe (z < 0.1; gray dashed line), and when excluding high-z SNe (z > 0.85; brown dotted–dashed line). In flat wCDM (left), the contours shift primarily along the degeneracy line (and in opposite directions for the low-z and high-z cuts) but also slightly perpendicular to the degeneracy direction. In combination with the CMB prior, this pushes the result closer to w = −1 in the no-low-z case. The flat w 0 w  a CDM model (right) best fit sees no significant shifts with subsample selection.
Paper: Neglected Silicon Dioxide Polymorphs as Clouds in Substellar Atmospheres
Authors: Sarah E. Moran, Mark S. Marley, Samuel D. Crossley
Figure caption: The expected silica polymorphs that form at 1 bar and elevated temperature (indicated by shading according to the legend). Also shown are condensation curves of cloud species for multiple atmospheric metallicities (dashed lines), along with temperature–pressure profiles (solid lines) of the hot Jupiters WASP-107 b (teal; A. Dyrek et al. 2024) and WASP-17 b (blue; G23) and an L4.5 brown dwarf (gold; M. S. Marley et al. 2021). Where a solid curve crosses a dashed curve of the corresponding color, cloud particles will condense. To the left of a condensation curve but before the cristobalite stability region, liquid cloud droplets should form. Quartz, as previously invoked in observational studies, is not the expected first crystalline polymorph of silica to form at warm substellar upper atmospheric conditions.
Paper: Neglected Silicon Dioxide Polymorphs as Clouds in Substellar Atmospheres
Authors: Sarah E. Moran, Mark S. Marley, Samuel D. Crossley
Figure caption: (a) Atmospheric models of WASP-17 b using the Mie coefficients of different silica polymorphs, using the best-fit sedimentation efficiency and eddy diffusivity of the PICASO-Virga nested sampling analysis of G23. Shown in light blue is the spectrum without the contribution from Al2O3 clouds. (b) The same as (a) but focused on the MIRI/LRS wavelength region as highlighted in (a) by the dotted gray box. Atmospheric models that account for the appropriate polymorph density in addition to optical properties are shown as dotted lines. (c) Particle size distributions for each SiO2 polymorph using appropriate polymorph densities. Accounting for silica polymorphs results in differentiable effects on the observable transmission spectrum of WASP-17 b.
Paper: Neglected Silicon Dioxide Polymorphs as Clouds in Substellar Atmospheres
Authors: Sarah E. Moran, Mark S. Marley, Samuel D. Crossley
Figure caption: Optical properties of silica polymorphs. The (a) real and (b) imaginary refractive indices and (c) the extinction efficiencies of various silica polymorphs. Cristobalite and tridymite refractive indices were calculated as described in the text. The extinction efficiencies are shown for a particle radius of 32 nm. The different SiO2 crystalline forms have distinct scattering and absorption features that should be separable with the precision of JWST’s MIRI instrument.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Neglected Silicon Dioxide Polymorphs as Clouds in Substellar Atmospheres
Authors: Sarah E. Moran, Mark S. Marley, Samuel D. Crossley
Figure caption: (a) Virga atmospheric models of WASP-17 b using tridymite Mie coefficients and differing sedimentation efficiencies (f sed), with no alumina cloud layer. Dark blue lines show f sed = 0.3, consistent with the best-fit Virga models of G23; light blue shows f sed = 3. (b) Particle size distributions for the two different f sed values, where f sed = 0.3 is dark blue and f sed = 3 is light blue. (c) The same as (a) but focused on Hubble wavelengths. (d) The same as (a) but focused on JWST/MIRI LRS wavelengths. With different sedimentation efficiency, silica clouds alone can explain observations of WASP-17 b in Virga models without the need for a lower Al2O3 cloud deck.
Paper: Neglected Silicon Dioxide Polymorphs as Clouds in Substellar Atmospheres
Authors: Sarah E. Moran, Mark S. Marley, Samuel D. Crossley
Figure caption: Emission spectra for Sonora Bobcat brown dwarf atmospheric models with an effective temperature of 1700 K and surface gravity log(g) = 5.0, postprocessed with clouds generated with different Mie coefficients for silica polymorph cloud particles. In addition to affecting planetary transmission spectra, different polymorphs of crystalline silica clouds could also be differentiable with JWST/MIRI in emission for a wide range of warm substellar objects.
Paper: Neglected Silicon Dioxide Polymorphs as Clouds in Substellar Atmospheres
Authors: Sarah E. Moran, Mark S. Marley, Samuel D. Crossley
Figure caption: Additional polymorph models for WASP-17 b. We show here that the choice of whether to use the optical properties derived from E. R. Lippincott et al. (1958) or M. Sitarz et al. (2000) impacts the observed SiO2 feature. All models use the best-fit values for the P–T profile, chemistry, and cloud parameters as in G23. The main text uses only the M. Sitarz et al. (2000) values, as these measurements were taken at elevated temperature. These differences highlight the need for careful, precise laboratory measurements of this polymorph.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Climate Bistability at the Inner Edge of the Habitable Zone due to Runaway Greenhouse and Cloud Feedbacks
Authors: Bowen Fan, Da Yang, Dorian S. Abbot
Figure caption: The size of bistability is controlled by the runaway greenhouse effect and cloud parameters. For each parameter, the base case (panel (a), same as Figure 2(d)) is adjusted. The change in bistability size is quantified by the temperature (T 1) and stellar flux (S 1) at which the model transitions from the cold state to the hot state (runaway greenhouse) as well as the temperature (T 2) and stellar flux (S 2) at which the model transitions from the hot state to the cold state (runaway condensation). T 1 and T 2 are controlled by T emis (panel (b)) and T end (panel (c)), respectively, the temperatures at which the runaway greenhouse process begins and ends. S 1 and S 2 are controlled by k  c  (panel (d)) and F NC (panel (e)), respectively. k  c  describes the relationship between convection and cloud fraction, while F NC is the decrease in OLR on the nightside if the nightside is completely covered with clouds. Circles indicate parameter values in the base case (Figure 2(d)).
Paper: Climate Bistability at the Inner Edge of the Habitable Zone due to Runaway Greenhouse and Cloud Feedbacks
Authors: Bowen Fan, Da Yang, Dorian S. Abbot
Figure caption: The climate bistability can be understood by considering energy balance between OLR (solid line) and ASR (dashed lines). Each panel represents the corresponding simulation from Figure 2. Each intersection represents an equilibrium climate state, where blue closed circles represent stable, cold climates; red closed circles represent stable, hot climates; and the open circle represents an unstable climate during the runaway greenhouse transition.
Paper: Erratum: “Electron–Ion Heating Partition in Imbalanced Solar-wind Turbulence” (2023, ApJL, 957, L30)
Authors: Jonathan Squire, Romain Meyrand, Matthew W. Kunz
Figure caption: Frequency spectrum of the magnetic field ﹩{{ \mathcal E }}_{\delta {B}_{\perp }}(\omega )﹩ normalized by ω −2 (top) and the ratio of the density spectrum and the magnetic-field spectrum ﹩{{ \mathcal E }}_{\delta n}/{{ \mathcal E }}_{\delta {B}_{\perp }}﹩ (bottom). Various times are shown, with spectra computed over intervals ±2τ A about the labeled times.
Paper: Climate Bistability at the Inner Edge of the Habitable Zone due to Runaway Greenhouse and Cloud Feedbacks
Authors: Bowen Fan, Da Yang, Dorian S. Abbot
Figure caption: Climate bistability at the inner edge of the HZ due to the runaway greenhouse effect. The figure shows the evolution of mean surface temperature with mean stellar flux. The blue results represent simulations with a cold start, and the red results represent simulations with a hot start. Solid and dashed lines represent results from our two-column model, while colored dots represent results from GCMs (J. Yang et al. 2013; M. Turbet et al. 2023). Panels show (a) YA14 settings (YA14); (b) addition of runaway greenhouse effect to YA14 with dayside cloud fraction fixed; (c) addition of runaway greenhouse effect to YA14; and (d) addition of nightside cloud feedback to (c).
Paper: Climate Bistability at the Inner Edge of the Habitable Zone due to Runaway Greenhouse and Cloud Feedbacks
Authors: Bowen Fan, Da Yang, Dorian S. Abbot
Figure caption: Schematic representation of the two-column model. Gray boxes represent the free atmosphere (pressure < 1 bar). Blue boxes represent the short-wave extinction layer (pressure ∼ 1 bar). Orange arrows represent short-wave radiative fluxes, blue arrows represent OLR to space, and black arrows represent atmospheric heat advection. The dayside column consists of a cloudy part and a clear-sky part; we also include an optional stratospheric (<0.1 bar) nightside cloud that blocks nightside long-wave emission. The ovals indicate modules that have been updated from YA14.
Paper: Physical Conditions That Led to the Detection of the Pair Annihilation Line in the Brightest-of-all-time GRB 221009A
Authors: Asaf Pe'er, Bing Zhang
Figure caption: Rate of pair annihilation as a function of the Lorentz factor, Γ, from Equations (19) and (24). At low Γ, the system is in the high-optical-depth-to-pair-production regime, and the rate of annihilation is proportional to Γ−2, while at higher values of Γ (the low optical depth regime), it sharply decays as Γ−17. Solid lines are for A = 1, while dashed lines are for A = 8 (note that A = 10 would result in lines overlapping).
Paper: Physical Conditions That Led to the Detection of the Pair Annihilation Line in the Brightest-of-all-time GRB 221009A
Authors: Asaf Pe'er, Bing Zhang
Figure caption: Temporal evolution of the line luminosity. Left: the full data set. Right: the zoomed-in version. Figure made from data taken from the tables given M. Edvige Ravasio et al. (2024) and Y.-Q. Zhang et al. (2024).
Paper: Physical Conditions That Led to the Detection of the Pair Annihilation Line in the Brightest-of-all-time GRB 221009A
Authors: Asaf Pe'er, Bing Zhang
Figure caption: Temporal evolution of the line energy. Left: the full data set. Right: the zoomed-in version. Figure made from data taken from the tables given in M. Edvige Ravasio et al. (2024) and Y.-Q. Zhang et al. (2024).
Paper: Nonlinear Alfvén-wave Dynamics and Premerger Emission from Crustal Oscillations in Neutron Star Mergers
Authors: Elias R. Most, Yoonsoo Kim, Katerina Chatziioannou, Isaac Legred
Figure caption: Minimum required perturbation that becomes nonlinear within the orbital light cylinder. The launching time, t launch, is given for black hole (BH)–neutron star (NS) and binary neutron star (NS–NS) systems relative to the time of merger t merger. We adopt m 2 = 1.4 M ⊙, r NS = 12 km and vary Q = 1 (NS–NS) to Q = 4 (BH–NS). Shaded regions correspond to the expected time window of the crust–core interface mode resonance from Equation (1).
Paper: Nonlinear Alfvén-wave Dynamics and Premerger Emission from Crustal Oscillations in Neutron Star Mergers
Authors: Elias R. Most, Yoonsoo Kim, Katerina Chatziioannou, Isaac Legred
Figure caption: Initial wave packet of Alfvén waves launched from the neutron star (gray disk) for the aligned configuration, θ  B  = 0. The orbital angular momentum points along the positive z-axis. Shown is the out-of-plane magnetic field component B  ϕ , rescaled to the surface magnetic field strength B NS, as well as the relative surface perturbation velocity δ v  ϕ .
Paper: Nonlinear Alfvén-wave Dynamics and Premerger Emission from Crustal Oscillations in Neutron Star Mergers
Authors: Elias R. Most, Yoonsoo Kim, Katerina Chatziioannou, Isaac Legred
Figure caption: Alfvén-wave propagation in a compact binary spacetime with aligned magnetic fields, θ  B  = 0°, in a frame corotating with the binary. (Top) Neutron star (NS)–black hole (BH). (Bottom) NS–NS. In the NS–NS case, the companion NS has an antialigned magnetic field. Shown are three different times, t, stated relative to the time of launch, t launch. Colors denote the out-of-plane magnetic, B  ϕ , and electric, E  ϕ , fields normalized to the poloidal magnetic field, B  P , and the field strength at the surface, B NS, respectively.
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: Proposed reaction pathways for the formation of organosulfur gases observed in this study. Dashed arrows are multistep pathways that are not speculated upon here. (a) Initial photolysis of CH4, H2S, and CO2 and the corresponding photochemical products important for the proposed pathways. (b) Pathways and products that are favored without CO2 or in more reducing conditions. (c) The proposed pathway that produces CH3SH, which is formed under all conditions in this study. (d) The pathway to OCS formation, which only occurs with CO2 present. (e) The pathway to CS2 formation, which occurs at higher sulfur levels (20 ppmv H2S).
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: (a) Example chromatogram of organosulfur gas-phase products from starting conditions of 0.1% CH4, 20 ppmv H2S, in N2 (red curve, left axis) and the DMS standard (blue curve, right axis). (b) Example chromatogram of gas-phase organosulfur products from starting conditions of 0.1% CH4, 20 ppmv H2S, with 0.1% CO2 in N2 (red curve, left axis) and the DMS/OCS standards (blue and orange lines, respectively, right axis). The inset included in panel (b) is a magnified portion of the chromatogram of the H2S and OCS peaks.
Paper: Nonlinear Alfvén-wave Dynamics and Premerger Emission from Crustal Oscillations in Neutron Star Mergers
Authors: Elias R. Most, Yoonsoo Kim, Katerina Chatziioannou, Isaac Legred
Figure caption: Late-stage compact magnetosphere evolution for a binary neutron star system with magnetic field inclination angle θ  B  = 60° in the meridional plane. Shown in color are the current sheets, in terms of the dissipative current J  i , the drift Lorentz factor γ  d , and the radial Poynting flux ﹩{S}_{\mathrm{EM}}^{r}﹩ normalized to its maximum value, ﹩{S}_{\mathrm{EM},\mathrm{flare}}﹩, in the outgoing flare.
Paper: Nonlinear Alfvén-wave Dynamics and Premerger Emission from Crustal Oscillations in Neutron Star Mergers
Authors: Elias R. Most, Yoonsoo Kim, Katerina Chatziioannou, Isaac Legred
Figure caption: Conversion efficiency η of the initial Alfvén wave into the final flare. Shown are results for black hole (BH)–neutron star (NS) and NS–NS systems. Solid lines correspond to waves with a drift Lorentz factor γ  d  > 5, which approximately filters out the fast wave component, whereas dashed lines correspond to the entire energy in the final outflow. Error bars quantify the uncertainty in choosing the cutoff on γ  d .
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: Voronoi diagrams of estimated mixing ratios (given in ppmv) of the organosulfur photochemical products for each condition. The values given are the average of the two values calculated using the DMS and OCS standards. Note that for the 5 ppmv H2S and 0.1% CO2 condition, only the OCS standard was available, and thus only the OCS standard was used to estimate the mixing ratios shown. For a conservative precision estimate, the values were rounded to one significant figure, and consequently values may not sum to 5 or 20 ppmv exactly. The values used to calculate the averages are given in Table B1 in the Appendix.
Paper: Nonlinear Alfvén-wave Dynamics and Premerger Emission from Crustal Oscillations in Neutron Star Mergers
Authors: Elias R. Most, Yoonsoo Kim, Katerina Chatziioannou, Isaac Legred
Figure caption: Same as Figure 3 but showing the final times t − t launch = 2.2 ms for different initial magnetic field inclinations, θ  B . We do not repeat the θ  B  = 0° case, as it is overall similar to θ  B  = 30°. In all cases, Alfvén waves drive flares detaching from the compact binary magnetosphere.
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: Illustration of the general methodology. “Sorg” is for “organosulfur gases,” “GC” is for “gas chromatograph,” and “SCD” is for “sulfur chemiluminescence detection.”
Paper: A Far-ultraviolet-detected Accretion Shock at the Star–Disk Boundary of FU Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Kevin France, Gregory J. Herczeg
Figure caption: The COS spectrum of FU Ori with the regions selected to represent continuum highlighted in light blue. Regions in black represent those masked out due to observed or potential line emission. The pink points with error bars mark the binned-down continuum points we fit in Section 4. The vertical cyan lines mark the locations of prominent H2 features in typical CTTS spectra (K. France et al. 2023), while identified bright or well-known (but marginally detected) atomic emission lines are marked and labeled in maroon. The vertical shaded regions denote masked geocoronal emission.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Far-ultraviolet-detected Accretion Shock at the Star–Disk Boundary of FU Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Kevin France, Gregory J. Herczeg
Figure caption: The FUV and NUV STIS spectra (dark blue) and the continuum points we derived from the COS spectrum (pink circles with error bars). Our combined disk + shock model fit is shown (light blue) along with the individual model components, with the disk model in green and the 16,275 K blackbody component in maroon. Notice the sharp transition from the disk-dominated spectrum to the excess-emission-dominated spectrum at the 2060 Å continuum break. The model components have all been reddened to our adopted A  V  = 1.5 mag and using the D. C. B. Whittet et al. (2004) extinction curve, which has a weaker 2200 Å bump than the commonly used J. A. Cardelli et al. (1989) curve. The effect of the bump can be seen as an undulation from 2000 to 2800 Å in the otherwise featureless reddened excess component blackbody spectrum.
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: Chromatogram of gas-phase organosulfur products from 0.1% CH4, 20 ppmv H2S, with 0.1% CO2 in N2 with the OCS standard spiked into the sample at a 7:3 sample-to-standard ratio by volume (red curve, left axis). The peak at ∼1 minute increased in magnitude compared to the unspiked sample (Figure 2(b)), providing evidence that it should be assigned as OCS and resolves the OCS peak from the H2S peak at ∼0.9 minutes. The OCS standard measured separately is also provided (orange curve, right axis).
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: Example chromatogram of sample from lamp-off conditions of the 20 ppmv H2S, 0.1% CH4, and 0.1% CO2 in N2 gas mixture. The lone peak at ∼0.9 minutes is H2S as it is the only sulfur gas present in the mixture.
Paper: Abiotic Production of Dimethyl Sulfide, Carbonyl Sulfide, and Other Organosulfur Gases via Photochemistry: Implications for Biosignatures and Metabolic Potential
Authors: Nathan W. Reed, Randall L. Shearer, Shawn Erin McGlynn, Boswell A. Wing, Margaret A. Tolbert, Eleanor C. Browne
Figure caption: Chromatogram of organosulfur photochemical products from the 5 ppmv H2S, 0.1% CH4, and 0.1% CO2 in N2 gas mixture (red curve, left axis) as well as the OCS standard (orange curve, right axis).
Paper: A Far-ultraviolet-detected Accretion Shock at the Star–Disk Boundary of FU Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Kevin France, Gregory J. Herczeg
Figure caption: The corner plot for our MCMC fit for the FU Ori FUV excess. Our adopted best-fit values are marked by the navy vertical lines, showing the medians of the histograms. The modal values, marked by light blue dotted lines, are identical to the median values. The contours in the 2D histogram mark the 0.5σ, 1.0σ, 1.5σ, and 2.0σ levels, while the vertical dashed lines mark the 16th and 84th percentiles in the 1D histograms.