adsabs/AstroCLIMB huggingface dataset:
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: Water mass fractions calculated for the mass-buildup, steady state, and mass-settling phases assuming three different disk lifetimes. The median value for each curve is indicated by the vertical lines. For visualization, water fractions of zero are reported as 10−2.5. Unless the disk lifetime is very short (panel (A)) compared to the settling timescales, the water mass fractions in the mass-buildup and steady-state phases are very similar. The inferred parent bodies are more likely to present as dry in the mass-settling phase.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: A selection of fits for the absorption lines for WD 0145+234. The red line shows the modeled spectrum, while the blue line shows the fit with the labeled element (listed as ﹩\mathrm{log}{\rm{(}}X/H)﹩ in each panel) removed. Species identified in red indicate ground-state transitions; these may be due to the ISM.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: A selection of fits for the absorption lines for WD J0649−7624 for the case of the spectroscopic solution. Colored lines and labels are as described in the caption of Figure 1. See Section 2.5 for a discussion of interstellar medium absorption and how limits are assessed for C and S.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: Evolution of the inferred water mass fraction calculated over time for two example WDs assuming a disk lifetime of 105 yr. Water fractions with propagated errors are shown at various times during the evolving accretion process. The shaded gray region shows the 1σ water mass fraction calculated for the accretion phase indicated in each plot panel. The arrows show the times at which we sample water mass fractions in the mass-buildup, steady state, and mass-settling phases of accretion. The ranges of settling timescales for each WD are shown by the horizontal bars.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: Water mass fractions (﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩) calculated from O excesses for the H-WDs described in Section 2, according to the approach outlined in Section 3. The ranges of settling timescales for the observed elements on each WD are labeled, and the resulting ranges of buildup, steady state, and settling phases are shown from left to right as the shaded regions.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: A selection of fits for the absorption lines in WD 0842+572. Colored lines and labels are as described in the caption of Figure 1.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: The distributions of abundance ratios calculated for the population of WDs in this study at mass-buildup, steady state, and mass-settling times, assuming a disk lifetime of 105 yr. Abundance ratios for Al, Si, and O are largely unchanged at all accretion phases.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: From left to right: density maps of HD, MHD-T, and MHD-P at the end of the simulations, t = 7 days. The top row shows the midplane view, and the bottom row shows an azimuthal slice at the collision angle. The location of the azimuthal slice is marked as a gray dashed line on the midplane view panels. The original ballistic orbit is overplotted in green in the top MHD-T panel.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Mass accretion rate measured at r = 3rs as a function of time since the first stream self-intersection.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Total mass outflow rate measured at r = 400rs as a function of time since the first stream self-intersection. The dotted lines show the unbound gas.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Reynolds (left) and Maxwell (right) stresses averaged within 10° from the midplane, over the azimuth, and over the last 2 days of the simulation, normalized by the average of the sum of gas and radiation pressures.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Total accreted energy per unit time (black) and its components: kinetic energy (green), radiative energy (orange), magnetic energy (pink), and internal energy (red) for MHD-T, HD, and MHD-P, from left to right.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Magnetic field strength at the end of the runs for MHD-T (left) and MHD-P (right). The streamlines show the projected magnetic field lines. The top row shows the midplane view, and the bottom row shows an azimuthal slice at the collision angle.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Total outflowing energy per unit time (black) at r = 400rs and its components: kinetic energy (green), luminosity (orange), magnetic energy (pink), and internal energy (red) for MHD-T, HD, and MHD-P, from left to right.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: The ratio, shown as a mean of eight GALPROP models “c”, of the percentage of the element that each isotope represents to that of the solar system, as represented by the protosolar abundances in Table 4 of K. Lodders (2021). A high abundance of 2H, representing primary 2H at the source, is required to fit the observed 2H energy spectrum. The source abundances of Li and Be were set to zero in all models. The uncertainty is taken to be the variance, σ, of the values from the eight models, defined as ﹩\sqrt{(}\sum {({x}_{i}-\mu )}^{2}/7)﹩, where xi is one of the model values and μ is the mean. Note that this quantity is larger than the uncertainty of the mean by a factor of ﹩\sqrt{8}﹩ and was chosen to better represent the spread of the data than would be the uncertainty of the mean.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: The results of a calculation where the source elemental abundances of S, Ar, Sc, Ti, V, Co, Cr, and Mn are normalized to the solar system values (K. Lodders 2021), model 4022d, keeping other elemental abundances and propagation parameters unchanged (as in model 4022c). The deviations of the calculated spectra of elements Sc and V do not exceed 2σ. The calculated spectra of elements S, Ar, and Co show large deviations. The intermediate case is presented by elements Ti, Cr, and Mn, which show mild deviations at higher energies, and larger deviations in the two lowest-energy bins. Note that this calculation includes the primary components for 2H and B. The GALPROP “d” model energy spectra and propagation parameters are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available in the online article.)
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: The results of a calculation where the source isotopic abundances within an element (6 ≤ Z ≤ 14) are normalized to the solar system values (K. Lodders 2021), model 4022d, keeping the elemental abundances and propagation parameters unchanged (as in model 4022c). The deviations of the calculated spectra of isotopes 13C, 15N, 17,18O, and 20,21Ne do not exceed ∼2σ, while 22Ne shows a large deviation, which is expected (W. R. Binns et al. 2005). Note that this calculation includes the primary components for 2H and B. The GALPROP “d” model energy spectra are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available in the online article.)
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: GCR elemental source abundances from the mean of eight GALPROP models “c” relative to those of the solar system (protosolar; Table 3 in K. Lodders 2021). Also shown for comparison are the GCR elemental abundances from ACE-CRIS (M. H. Israel et al. 2018) and Ulysses (M. A. Duvernois & M. R. Thayer 1996), the latter of which has been renormalized to the same solar system abundances as the others. A high abundance of B, representing a primary contribution of B at the source, is required to fit the observed energy spectrum of B. The uncertainties are represented by the variance as defined in the caption of Figure 16. Note that in this work the elemental source abundances of Li and Be were set to zero in all models.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Elemental spectra of H-F calculated in models “a” with no primary 2H and B (orange curves) compared with V1 (blue circles) and AMS-02 data (black diamonds). The black dashed lines show GALPROP-HelMod VLISM spectra (M. J. Boschini et al. 2020, 2021a, 2022a, 2022b) tuned to AMS-02 data where available, otherwise they are tuned to ACE-CRIS and HEAO-3-C2 measurements. Red curves over AMS-02 data points show spectra modulated with HelMod (M. J. Boschini et al. 2020, 2021a, 2022a, 2022b) and corresponding to the period of data taking.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: (Top) V1 B/C ratio together with eight models “a” that have no primary B. (Bottom) Same as top but with models “c” that have primary B. The points are plotted at the B energies, with a power-law interpolation to get the C intensities at those energies.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Elemental spectra of Ne-Ar calculated in models “a” with no primary 2H and B (orange curves) compared with V1 (blue circles) and AMS-02 data (black diamonds). For details see the caption of Figure 20.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Elemental spectrum of Ni calculated in models “a” with no primary 2H and B (orange curves) compared with V1 (blue circles) and AMS-02 data (black diamonds). For details see the caption of Figure 20.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Elemental spectra K-Co calculated in models “a” with no primary 2H and B (orange curves) compared with V1 (blue circles) and AMS-02 data (black diamonds). For details see the caption of Figure 20.
Paper: Pulsed Gamma-Ray Emission of PSR J0447+2447
Authors: Liancheng Zhou, Li Zhang, Jun Fang, Z. L. Yang, Yi Yan, J. L. Han
Figure caption: The analysis results of PSR J0447+2447. (A) The polarization position angle (PA) curve, represented by black dots and including data with errors within 5∘, is plotted twice: once using the original PA values and again with the PA values adjusted by adding 180∘. The vertical dashed lines at phases 0.59 and 0.61 denote the locations where the 90∘ jumps take place. (B) Integrated polarization profiles. The total intensity I, linear polarization L, and circular polarization V are represented by curves colored purple, green, and blue, respectively. (C) The weighted γ-ray pulse profile divided into 50 phase bins is depicted. The opaque orange curve represents the best-fitting template pulse profile of the γ-ray pulsations. The light black curves illustrate the uncertainty in the pulse profile, showing templates randomly drawn from the MCMC samples. The red dashed horizontal line represents the estimated background level. (D) A two-dimensional phaseogram from MJD 54682 to 60687 is depicted. Each photon was assigned a weight, which indicates the probability of its originating from the target source, as represented by the color bar at the left side. (E) The image illustrates the cumulative weighted H-test value curve for the LAT data, which is consistent with the time span presented in panel (D).
Paper: Balmer Absorption in Iron Low-ionization Broad Absorption Line Quasars
Authors: Karen M. Leighly, Sarah C. Gallagher, Hyunseop Choi, 현섭 최, Donald M. Terndrup, Julianna R. Voelker, Gordon T. Richards, Leah K. Morabito
Figure caption: The results of the Spearman rank correlation analysis for the 12-object subsample that covers Hα (left), and for the full 14-object sample (right). The size and color of each marker indicate the sign and p-value of the correlation. Anticorrelations are shown in blue, and correlations are shown in red. The shade of the color of each point indicates the significance of the correlation as a continuous variable, while the discrete sizes of the points characterize a range of p-values: p > 0.05, 0.05 > p > 0.005, 0.005 > p > 0.0005, and 0.0005 > p. The circular markers show the results for the full sample. Most of the strongest positive correlations are trivial, including those between measures of opacity, and Lbol vs. the Eddington ratio. The stars mark the physically interesting correlations that survive the one-out criterion (see the text for details).
Paper: Balmer Absorption in Iron Low-ionization Broad Absorption Line Quasars
Authors: Karen M. Leighly, Sarah C. Gallagher, Hyunseop Choi, 현섭 최, Donald M. Terndrup, Julianna R. Voelker, Gordon T. Richards, Leah K. Morabito
Figure caption: An illustration of partial covering models in SDSS 1635+1439. The black line shows the unconstrained model fit in which the relative Balmer optical depths were allowed to vary independently, yielding an excellent fit but an unphysical model. The blue line shows the best-fitting step-function partial covering model. The Hα line is truncated because the absorption on the continuum is saturated, and it is not black because the partially covered broad-line region fills it in. The magenta line shows an illustration of a SimBAL model. SimBAL uses power-law partial covering (e.g., K. M. Leighly et al. 2018, 2019), which allows the line to largely retain its shape and yields an overall better fit. We note that this is not formally a SimBAL model fit; those will be presented in H. Choi et al. (2025, in preparation).
Paper: Open Cluster Study Using Gaia. I. Membership and Cluster Properties
Authors: Anindya Ganguly, Prasanta K. Nayak, Sourav Chatterjee
Figure caption: Same as Figure 9 but showing the effect of adopted Pmem,c on the estimated cluster properties tage, [Fe/H], Av, and D. The different colors denote different adopted Pmem,c (see legend). We find that the adopted Pmem,c (within reason) does not affect the final posterior distributions of cluster properties.
Paper: Pulsed Gamma-Ray Emission of PSR J0447+2447
Authors: Liancheng Zhou, Li Zhang, Jun Fang, Z. L. Yang, Yi Yan, J. L. Han
Figure caption: Post-fit timing residuals with phase-connected timing solutions for PSR J0447+2447. The black and green error bars represent the observations from Fermi-LAT in the 0.1–300 GeV range and FAST in the 1.0–1.5 GHz range, respectively.
Paper: Pulsed Gamma-Ray Emission of PSR J0447+2447
Authors: Liancheng Zhou, Li Zhang, Jun Fang, Z. L. Yang, Yi Yan, J. L. Han
Figure caption: The γ-ray energy spectrum of PSR J0447+2447 spans from 0.1 to 300 GeV. The LP and PLEC4 models are depicted by blue solid and green dashed lines, respectively. The error ranges for the LP and PLEC4 models are indicated by the light blue and green regions. Three data points with TS values ≥4 are retained, while the remaining points are represented by their 95% flux upper limits.
Paper: The Altered Chaplygin Model as a Model for Dark Energy
Authors: Yi-Syuan Wu, 宜軒 吳, Chuan-Jui Li, 傳睿 李, W. F. Kao, 文芳 高
Figure caption: Posterior constraints from the Pantheon+ data set (D. Brout et al. 2022), including SNe Ia in the redshift range 0.001 < z < 2.26 with Cepheid-calibrated distances. The marginalized posterior estimates of the Hubble constant H0, the present-day matter density parameter, the present-day effective equation-of-state parameter ω0, the transition redshift z⋆, and the age of the Universe t0 for the ΛCDM model are summarized in Table 2.
Paper: The Altered Chaplygin Model as a Model for Dark Energy
Authors: Yi-Syuan Wu, 宜軒 吳, Chuan-Jui Li, 傳睿 李, W. F. Kao, 文芳 高
Figure caption: Same as Figure 1, but for the ACG model. The corresponding parameters are also summarized in Table 2.
Paper: The Altered Chaplygin Model as a Model for Dark Energy
Authors: Yi-Syuan Wu, 宜軒 吳, Chuan-Jui Li, 傳睿 李, W. F. Kao, 文芳 高
Figure caption: Same as Figure 1, but for the GCG model. The corresponding parameters are also summarized in Table 2.
Paper: The Altered Chaplygin Model as a Model for Dark Energy
Authors: Yi-Syuan Wu, 宜軒 吳, Chuan-Jui Li, 傳睿 李, W. F. Kao, 文芳 高
Figure caption: Same as Figure 1, but for the MCG model. The corresponding parameters are also summarized in Table 2.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Real (left panels) and imaginary (right panels) part of the dynamical sound speed squared for the QMC-RMF3 EOS. For the real part, the equilibrium sound speed squared is used as a reference. The black dashed line represents the difference between adiabatic and equilibrium squared sound speeds. The upper two panels correspond to fixed temperature T = 5 MeV while varying frequency ω = [200, 400, 1000, 2000] s−1; the bottom two panels represent fixed frequency ω = 1000 s−1 while varying temperature from 3 to 7 MeV. Note the different scales of the y-axes in the real and imaginary parts.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: The dashed contour shows the maximum (across all densities) of the imaginary part of the dynamical sound speed squared for QMC-RMF3 (top) and IOPB-I (bottom). The dark blue region corresponds to the resonant peak, where bulk viscosity is most effective at damping oscillations. The horizontal brown and red bands represent typical f-mode and g1-mode frequencies (at zero temperature) for NSs of various masses, with the central line corresponding to a 1.4 M⊙ NS.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Left (main) panel shows the beta equilibration relaxation rate γ defined in Equation (7) for QMC-RMF3, IUFSU, and IOPB-I EOSs at temperatures T = 1 MeV (dotted–dashed) and T = 3  MeV (dashed). The solid (dashed) lines in the top right panel represent the g-mode (f-mode) frequency of cold NSs with various central baryon densities ﹩{n}_{{\rm{B}}}^{c}﹩. The sharp jump in the rate is due to the onset of the direct Urca threshold.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Same as Figure 2, but for the IOPB-I EOS.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Real and imaginary parts of the frequencies of the fundamental and the first three overtone g-modes for a 1.4M⊙ NS vs. varying temperature for the QMC-RMF3 EOS. The imaginary part of the full GR calculation (dotted) largely overlaps with that of the calculation with Cowling approximation (dashed), and the real parts of the full GR calculation (dashed–dotted) and Cowling approximation (solid) are also very similar. We define the ordering of g-modes by their smooth asymptotic eigenmode at zero temperature.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Real part of the radial displacement field ξr(r) for the fundamental g1-mode (left panels) and first overtone g2-mode (right panels) as a function of the temperature, for three different EOSs: QMC-RMF3 (top row), IUFSU (middle row), and IOPB-I (bottom row). The curves are labeled by the temperature in MeV. Zoomed-in insets show the displacement field at the outer edge of the star for both modes using the QMC-RMF3 EOS—since many curves are overlapping in the insets, only some curves are labeled.