adsabs/AstroCLIMB huggingface dataset:
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Like Figure 12, but for impulsive deepening of the underlying potential, showing the density profile (top panel) and anisotropy (bottom panel) of an initially mono-energetic stellar tracer with rh0/rmx0 = 1/64, embedded deeply in the density cusp of a dark matter halo. The stellar tracer retains centrally isotropic kinematics, but is heavily radially biased in the outskirts. The same systematics are observed for stellar tracers embedded in a cored dark matter halo (not shown).
Paper: Does DESI DR2 Challenge ΛCDM Paradigm?
Authors: Himanshu Chaudhary, Salvatore Capozziello, Vipin Kumar Sharma, Ghulam Mustafa
Figure caption: The figure shows the posterior distributions of different tracers corresponding to different zeff from the DESI DR2 data set within the ΛCDM model. These are presented at 68% (1σ) and 95% (2σ) confidence levels in the Ωm−hrd contour plane. The blue band represents the Planck ΛCDM prediction for Ωm.
Paper: Does DESI DR2 Challenge ΛCDM Paradigm?
Authors: Himanshu Chaudhary, Salvatore Capozziello, Vipin Kumar Sharma, Ghulam Mustafa
Figure caption: The figure shows the confidence contours at the 68% (1σ) and 95% (2σ) levels for the ω0ωaCDM model, using no LRG1, no LRG2, no LRG1 and LRG2, and the full DESI DR2 sample.
Paper: Does DESI DR2 Challenge ΛCDM Paradigm?
Authors: Himanshu Chaudhary, Salvatore Capozziello, Vipin Kumar Sharma, Ghulam Mustafa
Figure caption: The figure shows the posterior distributions at 68% (1σ) and 95% (2σ) in the Ωm−hrd plane using different redshift bins from the DESI DR2 compilation. The blue band represents the Planck ΛCDM prediction for Ωm.
Paper: Does DESI DR2 Challenge ΛCDM Paradigm?
Authors: Himanshu Chaudhary, Salvatore Capozziello, Vipin Kumar Sharma, Ghulam Mustafa
Figure caption: The figure shows the normalized probability distribution of Ωm for different tracers at various effective redshifts zeff, independent of the hrd dependence
Paper: Does DESI DR2 Challenge ΛCDM Paradigm?
Authors: Himanshu Chaudhary, Salvatore Capozziello, Vipin Kumar Sharma, Ghulam Mustafa
Figure caption: The figure shows the prior sensitivity of the ω0ωaCDM constraints from DESI DR2.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Spectra encompassing well-known DR21 (∼–3 km s−1) and W75N (∼+9 km s−1) regions in Cyg X North, the region in our footprint for which spectrally resolved [C II] 158 μm data have been taken. Spectra of H I, 12CO, 13CO, and [C II] have been normalized to the peak of C273α.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Illustration of a model cloud showing the parameters defined in the M. G. Wolfire et al. (2010) framework. RCO is the radius of the CO core. ﹩{R}_{{{\rm{H}}}_{2}}﹩ is the radius where ﹩2{n}_{{{\rm{H}}}_{2}}={n}_{{\rm{H}}\,{\rm{I}}}﹩ with equal mass density in H atoms and H2 molecules. RT is the total cloud radius. Within R < RCO, gas is mainly CO and H2. Within the range ﹩{R}_{{\rm{CO}}}\lt R\lt {R}_{{{\rm{H}}}_{2}}﹩, gas is mainly H2, whereas the gas-phase carbon is mainly C and C+. The CRRLs arise from a C+ layer that is mainly H2. Within ﹩{R}_{{{\rm{H}}}_{2}}\lt R\lt {R}_{T}﹩ gas is mainly H I and gas-phase carbon is mainly C+. ﹩{A}_{V}({R}_{{{\rm{H}}}_{2}})﹩ is the magnitude of extinction measured from the outer radius to ﹩{R}_{{{\rm{H}}}_{2}}﹩, and AV(RCO) is the magnitude of extinction measured from the outer radius to RCO.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Emission in the region of the SNR γ Cygni and cluster NGC 6910 (blue star; right column). The 1.4 GHz continuum emission is the background image. Maps integrated over 2 km s−1 show C273α contours (left column), 13CO contours (middle column), and with both C273α (purple) and 13CO (green) contours overlaid in the right column.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: The top and middle panels show the noise along the spatial (top) and spectral (middle) coordinates. Gray contours in the top panel show the 50th and 90th percentiles of the noise values, and the mean, 1.91 × 10−4, is indicated by a white line in the color bar. The noise profile along the spectral axis (middle panel) is extracted from the center of the map. The bottom panel shows the pdf of the S/N within the cube. The blue parabola shows the pdf of a normal distribution with a mean of 0 and variance of 1. A normal distribution is an excellent description of the S/N values, except for the strong positive tail of values arising from signal in the cube.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: A comparison of the point-by-point velocity-integrated C273α and the 8 μm emissions, revealing a correlation. The top axis shows the corresponding FUV radiation G0 estimated from the 8 μm intensity. The gray shaded region indicates where C273α has 3 ≤ S/N < 5, and the data points are colored by ﹩\int {I}_{{}^{13}{\rm{CO}}}\,dv﹩. The red solid line shows the best-fit power law with slope a = 1.3 ± 0.2.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Overlays of the 13CO, 8 μm, and 314 MHz continuum contours over the C273α emission at matched spatial resolution. The 13CO contours are drawn at [1, 2, 3,...12] K km s−1. The 8 μm contours are drawn at [0.50, 0.75, 1.0, ...4.25] × 10−3 erg s−1 cm−1 sr−1). The 314 MHz continuum contours are drawn at [60, 120, 180, ...1020] K.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Point-by-point comparison of the 8 μm intensity and velocity-integrated 13CO emission (left) and a comparison of the C273α with the continuum emission (right). The colors of the data points are the same as in Figure 12.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: The 2D color map (left) of C273α with S/N ≥ 5 (big data points) and 3 ≤ S/N < 5 (small data points) is used to discern whether/how the spatial location in the region maps to the intensity comparisons of 13CO (middle) and 8 μm (right). Black numbers indicate the DR region ID, as in Figure 1. Cospatial regions tend to group together in the 13CO plot but not in 8 μm emission.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: PAH emission at 8.3 μm with C273α integrated from –4 to 2 km s−1 overlaid, showing what may be parts of a bubble powered by the cluster NGC 6913.
Paper: The Global Structure of the Heliosphere
Authors: Nikolai V. Pogorelov, Federico Fraternale, Gary P. Zank, Ming Zhang
Figure caption: Details of the LISM flow reacceleration region in the B–V plane with a focus on a “displacement layer” occupied by a stream of compressed LISM plasma. Panels (a) and (b) show the plasma density and speed, respectively. Panel (c) shows a 3D view of the HP along the line of sight perpendicular to the B–V plane. It illustrates the HP instability, five quasi-parallel magnetic field lines with respect to the BS normal, of white color draping around the HP, and a number of LISM streamlines, shown with green color, most of which are deflected into the displacement layer. These lines represent a 3D plot, not their projections on the plane of the figure.
Paper: The Global Structure of the Heliosphere
Authors: Nikolai V. Pogorelov, Federico Fraternale, Gary P. Zank, Ming Zhang
Figure caption: (Top panel) The distributions of proton density, the tangential component of the magnetic field vector, the normal component of the velocity vector, and plasma pressure are shown with black, green, blue, and green lines, respectively, along a selected direction normal to the slow-mode BS as indicated by the blue arrow in Figure 2(a). (Bottom panel) The distributions of the normal Alfvénic and slow-mode Mach numbers, and plasma beta, demonstrate that the shock type is trans-slow magnetosonic and sub-Alfvénic. The vertical gray line indicates the location, while the black vertical lines show the upstream and downstream points as derived from a best fit of the shock properties with the analytic Rankine–Hugoniot solution.
Paper: The Global Structure of the Heliosphere
Authors: Nikolai V. Pogorelov, Federico Fraternale, Gary P. Zank, Ming Zhang
Figure caption: Panels (a) and (b) show the relative intensity anisotropy of 4 TeV GCRs from our simulation and the Tibet air shower experiment, respectively. Note that the measurements are performed only in the northern hemisphere, so the numerical results are presented in the same region. R.A. and decl. are provided in the J2000 celestial coordinate system. The markers are used to show the upwind direction, associated with the measured velocity of the primary He atoms, the direction of the deflected H atom flow, as determined by R. Lallement et al. (2005), the direction of BLISM, and the downwind direction, and the direction toward Vela.
Paper: The Global Structure of the Heliosphere
Authors: Nikolai V. Pogorelov, Federico Fraternale, Gary P. Zank, Ming Zhang
Figure caption: Proton density (left panels) and azimuthal component of magnetic field (right panels) in the B–V plane (top panels) and in the meridional plane (middle panels). The bottom panels show zoomed views of the quantities shown in the middle panels. The black lines outline the HP surface.
Paper: The Global Structure of the Heliosphere
Authors: Nikolai V. Pogorelov, Federico Fraternale, Gary P. Zank, Ming Zhang
Figure caption: Distributions of proton density (panel (a)), magnetic field magnitude (panel (b)), plasma pressure (panel (c)), and plasma temperature (panel (d)) in the B–V plane.
Paper: The Global Structure of the Heliosphere
Authors: Nikolai V. Pogorelov, Federico Fraternale, Gary P. Zank, Ming Zhang
Figure caption: Distributions of the proton density through various cross sections of the heliotail (y–z planes) at different distances from the Sun (x = 0, −500, −1000, −2000, −4000, −8000).
Paper: On the Eddington Capture Surface around Spherically Symmetric Compact Objects with Separable Luminosity Distributions
Authors: Noah Monk, Adam Rogers
Figure caption: Coordinate systems used for integral calculations and their relationship to observers. A particle is shown above the stellar pole (left-hand side) and above the equator (right-hand side). In both cases, the surface brightness is defined in terms of a coordinate system (R, Θ, Φ) fixed on the star. The visible part of the surface is shown using a coordinate grid, with the polar angle defined by the ray with vanishing impact parameter b = 0 (dashed lines). An observer at point (rp, θ1, ϕ1), located over the north pole of the pulsar (left panel), measures a distinct value for the stress–energy tensor elements compared to an observer at the equator (rp, θ2, ϕ2; right panel). Thus, the stress–energy tensor depends on the position of the observer for a neutron star with a nonuniform surface temperature.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: The schematic of a typical halo pair, as observed on the sky. The two blue ellipses represent the paired halos, which are central galaxies selected from the SDSS sample and separated by a distance of dsep. Galaxies with projected separation dsat < 0.5dsep from their nearest host are identified as “satellites” and are plotted as green ellipticals. The position angle of the satellites, θ, is measured between the line connecting it to its host central galaxy and the line connecting the two centrals. A satellite is located “inside” the halo pair if 0° ≤ θ ≤ 90°, or “outside” the halo pair if θ > 90°.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Angular distribution of satellites around halo pairs from SDSS, P(θ), as measured for pairs of varying separation, primary halo mass, and secondary-to-primary halo mass ratio, as indicated.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Like Figure 11, but with energies expressed with respect to the evolved potential minimum. The evolved energy distributions are shown for impulsive reductions of the (dark matter) mass that sources the potential (top three panels), the initial conditions (central panel), and for impulsive deepening of the underlying potential (bottom three panels; see Appendix A for a discussion of the equilibrium structural parameters for this scenario). For both the cases of impulsive (dark matter) mass increase and decrease, the stellar binding energy distributions widen with respect to the initial conditions, and may overlap, mixing the initially energetically separated populations.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Number density profiles ﹩{r}^{2}{\nu }_{\star }(r| {{ \mathcal E }}_{\star })﹩ for mono-energetic stellar tracers with purely radial orbits (Equation (B2)), embedded in a cuspy (solid curve, Equation (4)) and a cored (dashed curve, Equation (21)) dark matter halo. Profiles are shown for four different values of the stellar truncation radius rt/rmx = 1/10, 1, 10, 100. The profiles asymptotically behave like ν⋆ ∝ r−2 for r → 0, and have a caustic at the radius rt caused by the pileup of stars at the apocenter rt.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: Comparison of focc (left) and p(λ) (right). Black curves represent the original results. Blue curves correspond to the sample excluding all sources within 1′ of the observational centers with the Chandra proposal subject category “active galaxies and quasars;” red curves indicate the sample further excluding sources based on both the “active galaxies and quasars” and “normal galaxies” categories. In the left panel, solid curves show the medians of the posterior distributions, while the shaded regions and dashed curves indicate the 2σ ranges. In the right panel, curves represent the medians, with dashed segments showing extrapolations beyond the data range (as in Figure 7), and shaded regions correspond to the 2σ ranges.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: The recovered focc (left) and p(λ) (right) from mock data generated based on the p(λ) shown as the black curve in the right panel. Our inputs are focc(M⋆ ≥ 109.5 M⊙) = 1 and focc(M⋆ < 109.5 M⊙) = 0 (blue) or 1 (red). The blue and red solid curves represent the medians of the fitted posteriors, and the shaded regions indicate the 2σ levels. The vertical dashed line in the left panel marks M⋆ = 109.5 M⊙. The fitted results are largely consistent with the inputs.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: focc results when applying our methodology to the M15 data. The solid and dashed curves, along with their corresponding shaded regions, represent the 1σ and 2σ ranges, respectively. The original 1σ measurements from M15 are shown as the orange region for comparison. In agreement with M15, our results show no evidence of decreasing focc at low M⋆.
Paper: Scintillation Properties of PSR B1133+16 Measured with Very Long Baseline Interferometry
Authors: Ashley M. Stock, Fardin Syed, Marten H. van Kerkwijk, Rebecca Lin, Franz Kirsten, Ue-Li Pen
Figure caption: Visibility secondary cross-spectra. Top: phases and intensities for all baselines involving Arecibo (binned by a factor of 4 in fD and 8 in τ). Parabolae for each arc for the best-fit arc curvature are overdrawn, with colors following the panels below. Bottom: phase along the arc, determined by averaging the complex values along delay within a parabolic region around each arc of width 0.58 mHz. Gray points indicate all measured values, while black ones indicate the ones used for fitting gradients. The best fit is shown with colored lines, with the uncertainties represented by the surrounding shaded regions.
Paper: Scintillation Properties of PSR B1133+16 Measured with Very Long Baseline Interferometry
Authors: Ashley M. Stock, Fardin Syed, Marten H. van Kerkwijk, Rebecca Lin, Franz Kirsten, Ue-Li Pen
Figure caption: Baselines and scintillation screen orientations, in the u–v plane. The blue, purple, gray, and black points represent the Arecibo-VLA, Arecibo-Jodrell Bank, Arecibo-Effelsberg, and Arecibo-Westerbork baselines over the duration of the observation. The line from the origin to the mean location of each baseline represents the value we used in calculating the screen parameters. The lines surrounded by shaded regions represent the orientations of the lines of images and their uncertainties for each of the three screens, as inferred from the time delays. As the pulsar moves behind the screens in the direction indicated with the black arrow, the scintillation pattern for each screen moves across the sky, with a velocity vector opposite to that of the projection of the pulsar velocity on the screen.
Paper: Scintillation Properties of PSR B1133+16 Measured with Very Long Baseline Interferometry
Authors: Ashley M. Stock, Fardin Syed, Marten H. van Kerkwijk, Rebecca Lin, Franz Kirsten, Ue-Li Pen
Figure caption: PSR B1133+16 dynamic and secondary spectra, based on the Arecibo observation. Left: dynamic spectrum. Middle: secondary spectrum, the Fourier transform of the dynamic spectrum. Right: secondary spectrum with parabolae for the three visible arcs overlaid, with best-fit value and estimated uncertainty indicated by the solid line and shading, respectively. The excess power visible along the delay axis is due to remaining radio frequency interference (narrow in frequency and roughly constant in time), while that along the Doppler axis is due to pulse-to-pulse variations (narrow in time but roughly achromatic).
Paper: Scintillation Properties of PSR B1133+16 Measured with Very Long Baseline Interferometry
Authors: Ashley M. Stock, Fardin Syed, Marten H. van Kerkwijk, Rebecca Lin, Franz Kirsten, Ue-Li Pen
Figure caption: The differential dust extinction as a function of distance on the line of sight toward PSR B1133+16, based on the dust map of G. Edenhofer et al. (2024). The distances of the screens associated with the outer arc, middle arc, and inner arc are shown with green dashed–dotted, orange dashed, and blue dashed–dotted lines with shaded regions to indicate error. The region between the inner and outer walls of the Local Bubble modeled by T. J. O’Neill et al. (2024) is indicated by the gray hatched region.
Paper: Scintillation Properties of PSR B1133+16 Measured with Very Long Baseline Interferometry
Authors: Ashley M. Stock, Fardin Syed, Marten H. van Kerkwijk, Rebecca Lin, Franz Kirsten, Ue-Li Pen
Figure caption: Intensity secondary cross-spectra. Arrangement is as for Figure 2.
Paper: Scintillation Properties of PSR B1133+16 Measured with Very Long Baseline Interferometry
Authors: Ashley M. Stock, Fardin Syed, Marten H. van Kerkwijk, Rebecca Lin, Franz Kirsten, Ue-Li Pen
Figure caption: The mean power along parabolae of different curvatures of the Arecibo secondary spectrum (gray lines) using a range of bounds in Doppler and delay. The vertical lines and shaded regions indicate the best fits and errors for the curvatures for the outer (green), middle (orange), and inner (blue) arcs.