adsabs/AstroCLIMB huggingface dataset:
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Top: redshift dependence of average ILW, n, and ﹩{Z}_{d}^{{\prime} }﹩, computed at r = 0.1 Rvir, mass-weighted along the line of sight and averaged over all halos at a given redshift. Bottom: same as top, but for NH I and the product ﹩n\times {Z}_{d}^{\prime} /{I}_{{\rm{LW}}}﹩. The latter is proportional to ﹩{N}_{{{\rm{H}}}_{2},{\rm{p}}}/{N}_{{\rm{H}}\,{\rm\small{I}},{\rm{p}}}﹩ under optically thin conditions.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Top: radial median H I column density profiles using all halos at a given redshift. The shaded region shows that interquartile range for the z = 4 curve. Middle: as top, but for H2 column density, with dashed curves showing the 90th percentile. The red dashed lines correspond to the 2 × 1021 (top) and 2 × 1014 cm−2 (middle). Bottom: the normalized radius at which the radial H2 (H I) profiles drop below their respective thresholds. The extent of H I, as represented by rDLA clearly increases with redshift, while the extent of detectable H2 does not show a clear redshift dependence.
Paper: Shooting for the Stars: Jet-mode Feedback and AGN Jet Deceleration from Stellar Mass Loading
Authors: Talia M. O'Shea, Sebastian Heinz, Melinda Soares-Furtado, Zsofi Igo, Andrea Merloni
Figure caption: Comparison of the deceleration thresholds for top: fraction of kinetic power (i.e., Figure 5) in decelerated jets, and bottom: fraction of jets (i.e., Figure 4) that escape their hosts. On the left, we compare Methods (1) and (2) as listed in Section A.2, showing results for θ = 3°, Γj = 3,  and M* = 1011.7 M⊙. On the right, we vary the initial Γj for Method (2) only, still with θ = 3° and M* = 1011.7 M⊙. In both plots, we use the extrapolated incidence function from Z. Igo & A. Merloni (2025).
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Distributions of metallicity (left panel), redshift (middle panel), and NH I (right panel) for the observational sample, after removing proximate DLAs.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Two-dimensional maps of H2 column density (top left), H I column density (top left), mass-weighted average ILW, and ﹩{f}_{{{\rm{H}}}_{2}}={N}_{{{\rm{H}}}_{2}}/{N}_{{\rm{H}}\,{\rm\small{I}}}﹩, for halo A4 at z = 4 (halo mass 5 × 1011 M⊙, stellar mass 0.8 × 1010 M⊙, virial radius 50 kpc, and stellar half-mass radius 2.3 kpc). White contours show ﹩{N}_{{{\rm{H}}}_{2},{\rm{detec}}}=2\times 1{0}^{14}\ {{\rm{cm}}}^{-2}﹩, black contours show NH I,DLA = 2 × 1021 cm−2, the inner circle is the stellar half-mass radius, and the outer circle is the halo virial radius.
Paper: Long-term Monitoring of Scintillation in the Pulsar J0332+5434
Authors: Grayce C. Brown, Sofia Z. Sheikh, Luigi F. Cruz, Wael Farah, Vishal Gajjar, Christian Gilbertson, Brandon Grimaldo, Michael T. Lam, Sofia L. Marquez, Maura McLaughlin, Alexander W. Pollak, Andrew Siemion, Gurmehar Singh
Figure caption: Example 2DACF profiles from an observation of PSR J0332+5434 taken on MJD 60164, summed across the time axis from Figure 3 (shown in orange), and cropped to emphasize the central peak. The 2DACF profiles have a clear peak with definite width around a frequency lag of zero and are well-described by the best-fit Lorentzian curves. The stacked double-Lorentzian fits, as described in Section 3.3, and their associated errors, are shown overlaid in green. The purple dotted line depicts the first Lorentzian (﹩{\mathbb{L}}1﹩) that was subtracted from the profile to ensure a correct fit to the central peak with the second Lorentzian (﹩{\mathbb{L}}2﹩). Band 1 and Band 2 are centered at 1139.75 MHz and 1667.75 MHz, respectively.
Paper: Long-term Monitoring of Scintillation in the Pulsar J0332+5434
Authors: Grayce C. Brown, Sofia Z. Sheikh, Luigi F. Cruz, Wael Farah, Vishal Gajjar, Christian Gilbertson, Brandon Grimaldo, Michael T. Lam, Sofia L. Marquez, Maura McLaughlin, Alexander W. Pollak, Andrew Siemion, Gurmehar Singh
Figure caption: The daily average scattering delay Δτd (y-axis) over a year of observation (x-axis) of PSR J0332+5434. Band 1 is shown in purple (top panel), and Band 2 is shown in green (bottom panel). rms errors are shown via shading. The black line indicates the 10 day average, to emphasize longer timescale behavior. The long-term trends in Band 1—for example, having consistently higher delays from 60,050 to 60,200—seem to be mirrored, as expected, by Band 2, though the trends in Band 2 are obscured due to its lower S/N. The Spearman product-moment correlation coefficient is 0.51.
Paper: Long-term Monitoring of Scintillation in the Pulsar J0332+5434
Authors: Grayce C. Brown, Sofia Z. Sheikh, Luigi F. Cruz, Wael Farah, Vishal Gajjar, Christian Gilbertson, Brandon Grimaldo, Michael T. Lam, Sofia L. Marquez, Maura McLaughlin, Alexander W. Pollak, Andrew Siemion, Gurmehar Singh
Figure caption: Measurements of scintillation bandwidth Δνd (y-axis) over a year of observation (x-axis) of J0332+5434. Band 1 (1140 MHz) is shown in purple (top panel), and Band 2 (1668 MHz) is shown in green (bottom panel). We show 1σ errors on the measurements via vertical error bars.
Paper: Long-term Monitoring of Scintillation in the Pulsar J0332+5434
Authors: Grayce C. Brown, Sofia Z. Sheikh, Luigi F. Cruz, Wael Farah, Vishal Gajjar, Christian Gilbertson, Brandon Grimaldo, Michael T. Lam, Sofia L. Marquez, Maura McLaughlin, Alexander W. Pollak, Andrew Siemion, Gurmehar Singh
Figure caption: Example dynamic spectra for PSR J0332+5434 taken on MJD 60164, with time (in seconds) on the x-axis and frequency (in MHz) on the y-axis. The top plots show the lower frequencies (Band 1) while the bottom plots show the higher frequencies (Band 2). The plots on the left show the unmodified dynamic spectra, while the plots on the right show the same spectra “stretched” vertically to a Kolmogorov scaling index (α = 4.4) to normalize scintle size over the wide bandwidth with reference frequencies 1139.75 MHz and 1667.75 MHz for Band 1 and Band 2, respectively.
Paper: Long-term Monitoring of Scintillation in the Pulsar J0332+5434
Authors: Grayce C. Brown, Sofia Z. Sheikh, Luigi F. Cruz, Wael Farah, Vishal Gajjar, Christian Gilbertson, Brandon Grimaldo, Michael T. Lam, Sofia L. Marquez, Maura McLaughlin, Alexander W. Pollak, Andrew Siemion, Gurmehar Singh
Figure caption: An example 2DACF from an observation of PSR J0332+5434 taken on MJD 60164, cropped to emphasize the central peak. The 2DACFs look horizontally banded due to our ability to resolve scintles in frequency, but not in time. The scintillation bandwidth Δνd is extracted from the width of the bright stripe at a frequency lag of 0.
Paper: Long-term Monitoring of Scintillation in the Pulsar J0332+5434
Authors: Grayce C. Brown, Sofia Z. Sheikh, Luigi F. Cruz, Wael Farah, Vishal Gajjar, Christian Gilbertson, Brandon Grimaldo, Michael T. Lam, Sofia L. Marquez, Maura McLaughlin, Alexander W. Pollak, Andrew Siemion, Gurmehar Singh
Figure caption: Cumulative observing time of PSR J0332+5434. Excluding the pilot observation, there were 396 observations resulting in 63.79 hr of total observation. The blue dashed line marks where Version 2 of the observing campaign began. Most observations were around 10 minutes in length. On average, we observed PSR J0332+5434 every 1.25 days, over 306 days.
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: Map of the six regions overplotted on a stellar density map (for stars with J < 19 mag) of M31. Regions 1, 4, and 5 were specifically designed to contain the following major substructures: region 1 contains the Eastern Shelf, region 5 contains the Western Shelf, and region 4 contains NGC 205. Green polygons highlight the approximate positions of the stellar structures that are a part of the GSS, and the pink ellipse corresponds to the dwarf galaxy NGC 205 in this map. The positions of the AGB stars and their region labels are available as 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.)
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: Star formation density rate for the past 8 Gyr in the six regions, which are labeled in Figure 9. The star formation density rates and their uncertainties of each region are available as 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.)
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: CMD of our UKIRT data outside of a deprojected distance of 20 kpc. Color indicates the number of data points in each place in the CMD. The gray box shows our selection criteria for the AGB stars, where the lower limit was determined by the 50% completeness limit of the most crowded regions in the stellar halo. Isochrones of 100 Myr, 1 Gyr, and 8 Gyr with a metallicity of [M/H] = 0.0 dex are overlaid with the AGB evolutionary phase highlighted in red.
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: Star formation rate density as a function of position for six different epochs.
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: Photometric uncertainty as a function of J- and K-band magnitudes. Quality cuts are shown in red, with the sources passing the given restriction in black and the sources not passing the restriction in gray.
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: Cumulative stellar mass formed for the past 8 Gyr in the six regions, which are labeled in Figure 9.
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: Same plots as Figure 7 now with all model sets from W17.
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: (Left) total star formation rate versus age for the entire halo footprint. (Right) The cumulative stellar mass formed as a function of time.
Paper: Measuring Star Formation Histories from Asymptotic Giant Branch Stars. I. A Demonstration in M31
Authors: Abigail J. Lee, Daniel R. Weisz, Yi Ren, Alessandro Savino, Andrew E. Dolphin
Figure caption: Time at which 90% of the stellar mass formed in each region of the inner stellar halo. The median uncertainty for t90 across all regions was measured to be ∼0.5 Gyr.
Paper: Probing Proton versus Electron Heating and Energization during Magnetic Reconnection
Authors: Zhiyu Yin, 志宇 尹, J. F. Drake, M. Swisdak
Figure caption: The temporal evolution of particle electron (left) and proton (right) temperatures in the x–y plane for Bg/B0 = 0.25. Six time steps are shown: t/τA = 0, 2, 3, 7, 13,  and 21. In each panel, magnetic field lines are overlaid in black.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: Set of trajectories of the spin axis for a freely precessing star, represented by the contours of λ0, norm = const. The numbers that label the curves are values of λ0, norm. Four different values of the ratio ε3/ε1 are shown. In each case the spin vector Ω follows one of the contour lines (the polhodes) with precession period ∼2π/εdΩ. The bold plus signs at the centers of the closed sets of contours correspond to minima of λ0. The maxima occur at the polar angles θ = 0 and 180°. The crosses depict the positions of the saddle points (X-points). Case (a) with ε3 = 0 represents a prolate biaxial deformation along the e1 axis. In case (b), both deformations have the same amplitude: ε1 = −ε3. The other two cases, ε3/ε1 = −10 and ε3/ε1 = −0.1, correspond to deformations predominantly along e3 and e1, respectively.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: Precession trajectories (contours of λnorm) for a triaxial star with ε1 = −ε3 and nonzero radiative torque nμ with ratios εμ/εd = −0.1, −1, −3 and −10. In all plots, the north magnetic pole has the coordinates φm = 250°, θm = 50°. For different orientations of the magnetic axis, the configurations are qualitatively the same. The north (N) and south (S) magnetic poles are represented by blue and red stars, respectively. The dotted red line depicts the magnetic equator, while other lines and marks have the same meaning as in Figure 3.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: Trajectories of the spin axis for an oblate biaxial star, modeled over several hundred million years, for εμ = −ε3 = −​​​​​​10−12 (a), and εμ = −0.1ε3 = −10−13 (b). The gray lines in the upper panels are contours of λnorm. In both panels, the initial period is P0 = 0.02 s, and the constant magnetic moment is μ = 2.25 × 1030 G cm3. The magnetic axis is tilted relative to the deformation axis e3 by 45°. The initial orientation of the spin axis is shown by the orange circle (Ω0) in the upper panels, while the color of the trajectory represents time. In the upper-left panel, the spin axis may be seen approaching one of the precession poles, following a tightly wound spiral trajectory. This precession pole does not coincide with the magnetic pole nor with any of the principal axes. The corresponding evolution of the magnetic angle χ is exhibited in the bottom-left panel; it wobbles significantly and remains nonzero even after millions of years of rotational history. The evolution of χ for a spherical star with the same parameters is shown for comparison by the solid black line. In panel (b), the spin axis precesses around the symmetry axis and evolves toward the attractor, at ﹩{\lambda }_{{\rm{norm}}}^{* }\approx 0.85﹩.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: Precession-averaged ﹩\dot{\lambda }﹩ calculated for an oblate biaxial star with a magnetic moment tilted at 45° relative to the deformation axis. For ∣εμ∣ ≫ εd, λnorm = 0 at the magnetic poles and 1 at the magnetic equator, while for ∣εμ∣ ≪ εd, λnorm = 0 at the deformation equator and 1 at the deformation (symmetry) axis. White arrows show the direction of evolution of λ. As seen, in the case of strong radiative precession, the spin axis tends to align with the magnetic axis. On the other hand, when free precession dominates, it aligns with the symmetry axis instead. An attractor exists in a certain range of parameters where εd ≳ few × ∣εμ∣, and is marked by the solid black line. The black dashed line marks the locus of saddle points on the map.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: Precessional attractors of a biaxial NS, affected by the pulsar torques nχ and nμ. (a) The case of an oblate star (ε3 > 0, ε1 = 0). The plot is similar to that shown in Figure 6. The black lines depict attractors in cases when the magnetic axis is tilted at 10° to 53° relative to the symmetry axis. To the left of these lines, λ increases so that the spin axis evolves toward the symmetry axis (SA) when ∣εμ∣ ≪ εd. In the case of a strongly magnetized star (∣εμ∣ ≫ εd), λ decreases and the spin axis aligns with the magnetic one (MA). ME and DE denote the magnetic and deformation equators, respectively. (b) The case of a prolate star is qualitatively similar to that of an oblate star; however, the lines marking the attractor have slightly different shapes. The angles in this plot are between the magnetic and deformation axes.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: The classical period–period derivative diagram for known isolated radio pulsars. Levels of constant effective radiative deformation ﹩{\hat{\varepsilon }}_{\mu }﹩ are shown by solid black lines. Gray dashed lines represent constant magnetic fields, obtained from the relation ﹩{B}_{{\rm{md}}}=3.2\times 1{0}^{19}\sqrt{P\dot{P}}﹩ G, and constant age, ﹩{\tau }_{{\rm{ch}}}=P/2\dot{P}﹩. Assuming that all the NSs have comparable deformations εd, one concludes that the precession of highly magnetized stars (Bmd ∼ 1013. . 1014 G) is dominated by the radiative torque, even if εd ∼ 10−10. . 10−9. On the other hand, even a small deformation εd ∼ 10−17. . 10−16 is sufficient to make free precession dominant in a millisecond pulsar rotation.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: Principal axes of a deformed NS and associated coordinate systems. The angles θ and φ are the polar and azimuthal angles, respectively, measured in the principal frame. The magnetic axis m is represented by the red arrow. The auxiliary basis s1−3 constructed on vectors Ω and m is shown by green arrows.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: Qualitative summary for asymptotic evolutionary states of a precessing magnetized NS. Here Ω denotes the angular velocity vector and χ denotes the magnetic angle. For a biaxial star, α is the angle between the magnetic and symmetry axes.
Paper: Rotational Evolution of Deformed Magnetized Neutron Stars: Implications for Obliquity Distribution and Braking Indices Statistics
Authors: Anton Biryukov, Pavel Abolmasov, Amir Levinson
Figure caption: Representation of evolution of a triaxial NS with ε1 = −ε3. The plots are similar to those shown in Figures 8(a) and (b) and Figure 6. Shaded regions have ﹩\langle \dot{\lambda }\rangle \gt 0﹩. Each plot corresponds to a specific orientation of the magnetic axis; the values of φm and θm are given in degrees in the title of each panel. Due to symmetry with respect the planes e1 − e2 and e1 − e3, only the regime φm = 0. . 180° and θm = 0. . 90° are shown.
Paper: Discovery of a ∼208 day Quasiperiodic Oscillation in the X-Ray Emission of the TeV Blazar 1ES 1959+650
Authors: Bing-Kai Zhang, Min Jin, Peng Zong
Figure caption: The X-ray light curve of BL Lac object 1ES 1959+650 during its outburst phase (MJD 56700–59600). The solid and dashed lines represent the fits to the dataset (MJD 56700–59000) using Equations (1) and (5), respectively. The dotted and dashed–dotted lines show the two segmented light curve fits from Equation (1). The long dashed line depicts the cubic function (the pol3 component in Equation (1)), illustrating the long-term trend of the flux evolution.
Paper: Discovery of a ∼208 day Quasiperiodic Oscillation in the X-Ray Emission of the TeV Blazar 1ES 1959+650
Authors: Bing-Kai Zhang, Min Jin, Peng Zong
Figure caption: The X-ray light curve of 1ES 1959+650 during its low state (MJD 53400–56700). The solid and dashed lines show the fits to the data from MJD 54200 to 56700 using Equations (1) and (5), respectively. The fit using Equation (1), extended back to MJD 53400, is shown by the dotted line. The long dashed line represents the cubic function (the pol3 component in Equation (1)), illustrating the long-term trend of the light curve.
Paper: Discovery of a ∼208 day Quasiperiodic Oscillation in the X-Ray Emission of the TeV Blazar 1ES 1959+650
Authors: Bing-Kai Zhang, Min Jin, Peng Zong
Figure caption: The Lomb–Scargle periodogram analysis result on the detrended light curve spanning MJD 54200–56700. The long dashed line denotes the fit to the LSP itself with a power-law function. The red dashed line, the green dotted line, and the blue dashed–dotted line correspondingly denote 3σ, 4σ, and 5σ confidence levels.
Paper: Discovery of a ∼208 day Quasiperiodic Oscillation in the X-Ray Emission of the TeV Blazar 1ES 1959+650
Authors: Bing-Kai Zhang, Min Jin, Peng Zong
Figure caption: WWZ analysis of 1ES 1959+650 (MJD 54200–56700). Left panel: WWZ power spectrum; the long dashed curve marks the cone of influence. Right panel: time-averaged global wavelet power; the long dashed and dashed lines indicate the 3σ and 4σ local confidence levels, respectively. The peak at 4.89 × 10−3 days−1 (P = 204.41 days) reaches a global significance of 3.79σ.
Paper: Discovery of a ∼208 day Quasiperiodic Oscillation in the X-Ray Emission of the TeV Blazar 1ES 1959+650
Authors: Bing-Kai Zhang, Min Jin, Peng Zong
Figure caption: WWZ analysis of 1ES 1959+650 (MJD 56700–59000). Left panel: WWZ power spectrum; the long dashed curve marks the cone of influence. Right panel: time-averaged global wavelet power; the long dashed and dashed lines indicate the 3σ and 4σ local confidence levels, respectively. The dominant peak at 4.75 × 10−3 days−1 (P  = 210.33 days) reaches a global significance of 3.14σ.
Paper: Discovery of a ∼208 day Quasiperiodic Oscillation in the X-Ray Emission of the TeV Blazar 1ES 1959+650
Authors: Bing-Kai Zhang, Min Jin, Peng Zong
Figure caption: The Lomb–Scargle periodogram analysis result on the detrended light curve spanning MJD 56700–59000. The long dashed line denotes the fit to the LSP itself with a power-law function. The dashed, dotted, and dashed–dotted lines denote 3σ, 4σ, and 5σ confidence levels, respectively.
Paper: Discovery of a ∼208 day Quasiperiodic Oscillation in the X-Ray Emission of the TeV Blazar 1ES 1959+650
Authors: Bing-Kai Zhang, Min Jin, Peng Zong
Figure caption: The X-ray light curve of BL Lac object 1ES 1959+650. The measurement uncertainties are indicated by error bars, which are often comparable to or smaller than the plotted symbols.