adsabs/AstroCLIMB huggingface dataset:
Paper: Influence of Solar Wind Variations on the Shapes of Venus’ Plasma Boundaries Based on Venus Express Observations
Authors: C. Signoles, M. Persson, Y. Futaana, S. Aizawa, N. André, S. Bergman, A. Fedorov, V. Lindwall, N. Martinez, C. Mazelle, S. Rojas Mata, A. Wolff, T. L. Zhang
Figure caption: BS radius at the terminator and its dependence on upstream parameters for solar minimum and solar maximum. Dependence on (a) the solar wind dynamic pressure and (b) the IMF magnitude. The vertical error bars are obtained from the standard errors on the fitted parameters propagated to the radius at the terminator. The horizontal dotted lines are the radius at the terminator value for the solar minimum (blue) and solar maximum (orange) BS fits. (c) Dependence on the Alfvén Mach number: BS crossings (blue for solar minimum and orange for solar maximum) extrapolated to the terminator plane (see Section 2.5). The blue diamonds (solar minimum) and orange circles (solar maximum) represent the median values over the Alfvén Mach number bins, and the vertical error bars show the median absolute deviation. In each plot, the horizontal error bars indicate the bin sizes.
Paper: Influence of Solar Wind Variations on the Shapes of Venus’ Plasma Boundaries Based on Venus Express Observations
Authors: C. Signoles, M. Persson, Y. Futaana, S. Aizawa, N. André, S. Bergman, A. Fedorov, V. Lindwall, N. Martinez, C. Mazelle, S. Rojas Mata, A. Wolff, T. L. Zhang
Figure caption: ICB radius at the terminator and its dependence on upstream parameters. The blue diamonds (orange dots) represent ICB dayside crossings at solar minimum (maximum). The connected blue diamonds (solar minimum) and orange circles (solar maximum) are the median values over each (a) solar wind dynamic pressure or (b) IMF magnitude bin. The vertical error bars show the median absolute deviation, and the horizontal ones show the widths of the bins.
Paper: Improving Distances to Binary Millisecond Pulsars with Gaia
Authors: Abigail Moran, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, David N. Spergel
Figure caption: Distances to J1012+5307 and J1024–0719. All DM distances are shown for comparison only and are not used in any distance calculations. The uncertainties in DM distances assume a standard error of ±20%. In panels (a) and (b) the combined measurements to J1012+5307 include the Desvignes et al. (2016), Ding et al. (2023), and Agazie et al. (2023) parallax measurements as well as the VLBI distance found in Ding et al. (2020). The combined Gaia DR2 distance is more precise than the combined DR3 distance since the DR3 parallax is very small and therefore results in a broader distribution, even when combined with the other parallaxes. In panels (c) and (d) the combined measurements include the IPTA DR2, the NANOGrav 15 yr data (Agazie et al. 2023), and Ding et al. (2023) parallax measurements. All parallaxes correspond to distances more than double the DM distances, which may indicate that the NE2001 and YMW16 underestimate their errors.
Paper: Improving Distances to Binary Millisecond Pulsars with Gaia
Authors: Abigail Moran, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, David N. Spergel
Figure caption: The combined parallax measurements to J1843–1113 and the resulting distances. Despite being a more precise parallax measurement, the Gaia DR3 parallax corresponds to a less precise combined distance than when the Gaia DR2 value is used as a result of its inconsistency with the PTA parallax measurement. The PTA measurement is also consistent with the NE2001 (blue strip) and YMW16 (yellow strip) DM distances. This casts further doubt on the association.
Paper: Improving Distances to Binary Millisecond Pulsars with Gaia
Authors: Abigail Moran, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, David N. Spergel
Figure caption: Distances to the system of J0437–4715. The combined curves include parallax based distances from Deller et al. (2008), Reardon et al. (2016), and Agazie et al. (2023) in addition to the specified Gaia distance. The distances are not significantly impacted by the Gaia parallaxes since the curves are dominated by the ultraprecise VLBI (Deller et al. 2008) and timing (Reardon et al. 2016) parallaxes.
Paper: Improving Distances to Binary Millisecond Pulsars with Gaia
Authors: Abigail Moran, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, David N. Spergel
Figure caption: The sky position of the Gaia companion to J1012+5307 in Gaia DR2 and DR3 for comparison. The pulsar’s position in IPTA DR2 is shown in red. The Gaia R.A. error decreased by 15% from DR2 to DR3, and the decl. error by 33%.
Paper: NuSTAR Observations of Four Mid-IR–Selected Dual AGN Candidates in Galaxy Mergers
Authors: Ryan W. Pfeifle, Kimberly Weaver, Shobita Satyapal, Claudio Ricci, Nathan J. Secrest, Mario Gliozzi, Laura Blecha, Barry Rothberg
Figure caption: Example of one of our SED fits, SDSS J084905.51+111447.2. The two dashed–dotted gray subcomponents are the star-forming templates, while the red subcomponent is the reddened AGN. The LOS best-fit extinction of the AGN component is E(B − V) = 16 mag, indicating that this object is likely Compton-thick with N H ∼ 1.6 × 1024 cm−2. This is within ∼3% of the value found in Pfeifle et al. (2019b) using X-ray data from Chandra and NuSTAR. The wavelength scale is rest-frame.
Paper: NuSTAR Observations of Four Mid-IR–Selected Dual AGN Candidates in Galaxy Mergers
Authors: Ryan W. Pfeifle, Kimberly Weaver, Shobita Satyapal, Claudio Ricci, Nathan J. Secrest, Mario Gliozzi, Laura Blecha, Barry Rothberg
Figure caption: Best-fitting models for J0841+0101. Top: borus model. Bottom: PEXRAV model. Each of these best-fitting models include two soft thermal components in the 0.1–1 keV band, components for reflection and scattered emission, and an absorbed power-law component that accounts for photoelectric absorption and Compton scattering.
Paper: SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Authors: Ronan Kerr, Adam L. Kraus, Aaron C. Rizzuto
Figure caption: (a) Distribution of groups we identify in galactic coordinates, shown here in XY space, with all groups labeled. Stars shown are limited to young founding members. This panel shows the 15 groups with eight or more O and B stars included in the founding population, which we use to indicate the most heavily populated groups. (b) The remaining 101 groups we identify, are shown in XY galactic space. The labeled groups in the first panel are shown in the background in gray so that locations relative to these larger groups can be assessed without the larger groups obscuring the smaller ones. An interactive version in XYZ 3D galactic coordinates is available in the online-only version of this figure, which includes age data (see Section 6.2), as well as buttons to restrict the sample to interesting subsets of groups.
Paper: Universal Upper End of the Stellar Initial Mass Function in the Young and Compact LEGUS Clusters
Authors: Dooseok Escher Jung, Daniela Calzetti, Matteo Messa, Mark Heyer, Mattia Sirressi, Sean T. Linden, Angela Adamo, Rupali Chandar, Michele Cignoni, David O. Cook, Clare L. Dobbs, Bruce G. Elmegreen, Aaron S. Evans, Michele Fumagalli, John S. Gallagher, Deidre A. Hunter, Kelsey E. Johnson, Robert C. Kennicutt, Mark R. Krumholz, Daniel Schaerer, Elena Sabbi, Linda J. Smith, Monica Tosi, Aida Wofford
Figure caption: Left: the location of 〈L Hα /M cl〉 (=Σ L Hα /Σ M cl) with their standard deviations (Table 3) as a function of the mean of the sample’s mass in each bin. Different colors and shapes identify different galaxies. The dark-gray squares are the 〈L Hα /M cl〉 ratios of all galaxies combined, as a function of binned mass. The horizontal bar associated with each symbol shows the size of each mass bin. The horizontal dotted lines show the evolution of model 〈L Hα /M cl〉 as a function of age (1–6 Myr) with fixed ﹩{m}_{\max }=120\ {M}_{\odot }﹩ from SB99. Right: the same data points as in the left panel shown with a range of model upper mass values ﹩{m}_{\max }﹩ averaged within the 1–4 Myr age produced by SB99 from 20 M ⊙ to 120 M ⊙ in 10 M ⊙ intervals (horizontal dotted lines).
Paper: Universal Upper End of the Stellar Initial Mass Function in the Young and Compact LEGUS Clusters
Authors: Dooseok Escher Jung, Daniela Calzetti, Matteo Messa, Mark Heyer, Mattia Sirressi, Sean T. Linden, Angela Adamo, Rupali Chandar, Michele Cignoni, David O. Cook, Clare L. Dobbs, Bruce G. Elmegreen, Aaron S. Evans, Michele Fumagalli, John S. Gallagher, Deidre A. Hunter, Kelsey E. Johnson, Robert C. Kennicutt, Mark R. Krumholz, Daniel Schaerer, Elena Sabbi, Linda J. Smith, Monica Tosi, Aida Wofford
Figure caption: Left: the ratio L Hα /M cl of all the selected clusters as a function of stellar mass, as listed in the LEGUS catalogs. Star markers are the clusters with Hα emission, and dots are those without Hα emission. For the latter, the indicated values of L Hα  are upper limits. Dashed horizontal lines are the average of L Hα /M cl for the sources detected in Hα (〈L Hα /M cl〉★) and those undetected in the line (〈L Hα /M cl〉•), respectively. Right: the same plot as the left panel, but including the error bars of each cluster. Here the upper limits are clearly marked.
Paper: Universal Upper End of the Stellar Initial Mass Function in the Young and Compact LEGUS Clusters
Authors: Dooseok Escher Jung, Daniela Calzetti, Matteo Messa, Mark Heyer, Mattia Sirressi, Sean T. Linden, Angela Adamo, Rupali Chandar, Michele Cignoni, David O. Cook, Clare L. Dobbs, Bruce G. Elmegreen, Aaron S. Evans, Michele Fumagalli, John S. Gallagher, Deidre A. Hunter, Kelsey E. Johnson, Robert C. Kennicutt, Mark R. Krumholz, Daniel Schaerer, Elena Sabbi, Linda J. Smith, Monica Tosi, Aida Wofford
Figure caption: The distribution of L Hα /M cl values for each galaxy and for all samples combined. The blue bars are Hα-emission-detected sources and the red bars are undetected ones, for which the indicated values are upper limits. For the sources detected in Hα, the typical two-sided 1σ uncertainties are about 1/2 bin in size. The SFR of each galaxy is given under the name of the galaxies.
Paper: Universal Upper End of the Stellar Initial Mass Function in the Young and Compact LEGUS Clusters
Authors: Dooseok Escher Jung, Daniela Calzetti, Matteo Messa, Mark Heyer, Mattia Sirressi, Sean T. Linden, Angela Adamo, Rupali Chandar, Michele Cignoni, David O. Cook, Clare L. Dobbs, Bruce G. Elmegreen, Aaron S. Evans, Michele Fumagalli, John S. Gallagher, Deidre A. Hunter, Kelsey E. Johnson, Robert C. Kennicutt, Mark R. Krumholz, Daniel Schaerer, Elena Sabbi, Linda J. Smith, Monica Tosi, Aida Wofford
Figure caption: The ratio L Hα /L I of the cluster samples in this study as a function of L I. This figure has the same structure as Figure 4 but for L I instead of M cl.
Paper: Universal Upper End of the Stellar Initial Mass Function in the Young and Compact LEGUS Clusters
Authors: Dooseok Escher Jung, Daniela Calzetti, Matteo Messa, Mark Heyer, Mattia Sirressi, Sean T. Linden, Angela Adamo, Rupali Chandar, Michele Cignoni, David O. Cook, Clare L. Dobbs, Bruce G. Elmegreen, Aaron S. Evans, Michele Fumagalli, John S. Gallagher, Deidre A. Hunter, Kelsey E. Johnson, Robert C. Kennicutt, Mark R. Krumholz, Daniel Schaerer, Elena Sabbi, Linda J. Smith, Monica Tosi, Aida Wofford
Figure caption: The spatial distribution of the star clusters in NGC 4449 selected for this study, and showing the presence/absence of Hα (left), their masses (middle), and their ages (right). The values of the masses (102–105 M ⊙) and the ages (1–4 Myr) are shown by the color bars in the middle and right panels, respectively. The gray dots are all star clusters in NGC 4449 from the LEGUS catalogs.
Paper: Universal Upper End of the Stellar Initial Mass Function in the Young and Compact LEGUS Clusters
Authors: Dooseok Escher Jung, Daniela Calzetti, Matteo Messa, Mark Heyer, Mattia Sirressi, Sean T. Linden, Angela Adamo, Rupali Chandar, Michele Cignoni, David O. Cook, Clare L. Dobbs, Bruce G. Elmegreen, Aaron S. Evans, Michele Fumagalli, John S. Gallagher, Deidre A. Hunter, Kelsey E. Johnson, Robert C. Kennicutt, Mark R. Krumholz, Daniel Schaerer, Elena Sabbi, Linda J. Smith, Monica Tosi, Aida Wofford
Figure caption: Left: the locations of the selected LEGUS clusters by class (class 1 as red, class 2 as green, and class 3 as blue circles) with ages within 1–4 Myr in NGC 4449 are shown in the F555W image. Right: a zoomed-in image of the selected area (the black solid square) in the left panel. Candidates identified as class 4 are excluded here and the morphology-based cluster classification is explained in Section 2.1.
Paper: Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations
Authors: Benjamin Vermette, Ciro Salcedo, Kaya Mori, Julian Gerber, Kyung Duk Yoon, Gabriel Bridges, Charles J. Hailey, Frank Haberl, Jaesub Hong, Jonathan Grindlay, Gabriele Ponti, Gavin Ramsay
Figure caption: Pulse profiles at the peak frequency and its harmonics for 0870990201 MOS (top), 0870990201 PN (middle), and 0870990201 joint (bottom). The red horizontal lines indicate the mean counts per phase bin and 1σ error bars are included at ϕ = 0 − 1.
Paper: Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations
Authors: Benjamin Vermette, Ciro Salcedo, Kaya Mori, Julian Gerber, Kyung Duk Yoon, Gabriel Bridges, Charles J. Hailey, Frank Haberl, Jaesub Hong, Jonathan Grindlay, Gabriele Ponti, Gavin Ramsay
Figure caption: The blue box indicates the step related to X-ray timing analysis. We derived variables from the known or fit parameters in the steps colored in green. Magenta boxes indicate the steps involved in spectral fittings.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Mixed-mode parameters for the 1068 Kepler red giants from the Gehan et al. (2018) study. (a) ΔΠ1–Δν relation as previously investigated by Mosser et al. (2014) and Vrard et al. (2016). (b) Δν –q relation, previously demonstrated by Mosser et al. (2017). (c) ϵ  g –Δν relation (Mosser et al. 2018). (d) Observed mixed-mode rotationally frequency splitting, δ ν rot, as a function of the mixed-mode density ﹩{ \mathcal N }={\rm{\Delta }}\nu /({\rm{\Delta }}{{\rm{\Pi }}}_{1}\cdot {\nu }_{\max }^{2})﹩ (Mosser et al. 2012a; Gehan et al. 2018).
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Δν−q relation for red giants across different metallicity ([M/H]) bins. The top panel shows all 684 targets with abundances from APOGEE DR17. The highlighted points are stars below the ΔΠ1–Δν degenerate sequence in Figure 6(a). The bottom panels show the Δν−q relation for stars within specific metallicity bins. A linear relation is fit to the targets in each bin using a hierarchical linear model (see Section 3.3), where the intervals indicate 95% highest-density regions from the posterior predictive distribution of the fit.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Bayesian optimization for the fitting of KIC 3973247. (Left) Samples of the optimizer in the joint (ΔΠ1, q, ϵ  g , δ ν rot) space, shown in three separate 2D slices. Darker points correspond to better fits (lower loss). Highlighted points indicate solutions whose fits are shown in the right panel. (Right) Example fits identified from four minima identified by the optimizer from the the joint (ΔΠ1, q, ϵ  g , δ ν rot) space, of which one is the global minimum or best fit. In each subpanel, the blue points correspond to observed mixed-dipole-mode frequencies, while the other underlying points correspond to simulated mode frequencies.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Optimization for the power spectrum of the stretched-period spectrum for KIC 2568912. (a) Background-corrected oscillation spectrum of the star, with the l = 0,2 modes shown in light gray. The residual spectrum is obtained by dividing the full spectrum with a template that models only the l = 0,2 modes as described in the text. (b) Power spectrum of the τ spectrum (PS × PS) for different combinations of (ΔΠ1, q). The ideal combination is that which maximizes the PS × PS power at that value of ΔΠ1 itself. Here, the best solution is at ΔΠ1 = 86.2 s because the PS × PS generated using a candidate ΔΠ1 of 86.2 s peaks at that exact same value, as traced by the vertical line. In contrast, the PS × PS generated using a candidate ΔΠ1 of 66.0 s (green) has no power at ΔΠ1 = 66.0 s, which makes this solution suboptimal. (c) Output from BayesOpt on the PS × PS, where the optimum is located at (ΔΠ1, q) = (86.2 s, 0.2). The contour represents likelihoods from the Gaussian process of the optimizer, with lighter colors indicating better (ΔΠ1, q) solutions.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Flowchart detailing the estimation of the mixed-mode parameters in this work. Bayesian optimization (BayesOpt) is used in the two procedures shown in blue. The first optimization step iteratively determines estimates of the asymptotic dipole mode period spacing, ΔΠ1,PS × PS, from the power spectrum of the stretched-period (τ) spectrum (PS × PS) method. Next, ΔΠ1,init initializes the search range for the second optimization step that estimates the four-parameter solution (ΔΠ1, q, ϵ  g , δ ν rot) from matching both τ and ν between the model and peak-bagged modes.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: ΔΠ1–Δν relation for 684 stars with atmospheric parameters from the Sloan Digital Sky Survey APOGEE DR17 across a range of stellar mass bins. Highlighted stars are those that with a large vertical distance (>6 s) from the “degenerate sequence” (Deheuvels et al. 2022). The target marked with a star symbol is KIC 4350501, a known young α-rich star (Martig et al. 2015).
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Estimating the uncertainties for the fitting of KIC 3973247. (Left) Samples from the optimization, similar to that shown in Figure 3. The highlighted point indicates the best fit (global optimum). The various colors indicate clusters of low-loss samples that are identified by DBSCAN. (Right) Joint distribution of the cluster containing the best fit. The lines in each parameter’s 1D histogram are the distribution median and the 67% highest-density interval (HDI). We report the HDI as 1σ uncertainties for each fit in this work.
Paper: JWST/NIRSpec Balmer-line Measurements of Star Formation and Dust Attenuation at z ∼ 3–6
Authors: Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Gabriel B. Brammer
Figure caption: Composite spectra for each of the three redshift bins, where, from bottom to top, we show spectra, respectively, for the 2.7 ≤ z < 4.0, 4.0 ≤ z < 5.0, and 5.0 ≤ z < 6.5 samples. In each row, the left set of panels represents the “low-mass bin,” while the right side indicates the “high-mass bin,” where each redshift sample is divided at the median stellar mass. Each composite spectrum is zoomed in on the regions covering Hβ and [O III]λ λ4959, 5007, as well as Hα, [N II]λ λ6548, 6583, and [S II]λ λ6717, 6731. These features are marked and labeled.
Paper: JWST/NIRSpec Balmer-line Measurements of Star Formation and Dust Attenuation at z ∼ 3–6
Authors: Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Gabriel B. Brammer
Figure caption: Attenuation vs. M * based on the Balmer-line ratio, Hα/Hβ. In each panel, the background grayscale histogram corresponds to the distribution of local SDSS galaxies. The running median Hα/Hβ ratio for z ∼ 2.3 star-forming galaxies in the MOSDEF survey is shown in red (Shapley et al. 2022). In the left panel, we show individual CEERS galaxies color-coded by redshift as in previous plots. On the right, plotted Hα/Hβ ratios are measured from composite spectra in two bins of stellar mass for each redshift range, as shown in Figure 3.
Paper: JWST/NIRSpec Balmer-line Measurements of Star Formation and Dust Attenuation at z ∼ 3–6
Authors: Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Gabriel B. Brammer
Figure caption: Left: redshift distribution of all 113 CEERS galaxies at 2.7 ≤ z ≤ 6.5, from which the sample of star-forming galaxies we analyze is drawn. The three redshift bins we delineate are indicated in green (2.7 ≤ z < 4.0), blue (4.0 ≤ z < 5.0), and magenta (5.0 ≤ z < 6.5). Right: stellar-mass distributions for the three redshift samples indicated in the left-hand panel, using the same color coding. For each redshift distribution, the median stellar mass is marked with a vertical dotted line. These median stellar-mass values are ﹩\mathrm{log}({M}_{* }/{M}_{\odot })﹩ = 9.59, 9.38, and 8.38, respectively, for the 2.7 ≤ z < 4.0, 4.0 ≤ z < 5.0, and 5.0 ≤ z < 6.5 redshift samples.
Paper: JWST/NIRSpec Balmer-line Measurements of Star Formation and Dust Attenuation at z ∼ 3–6
Authors: Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Gabriel B. Brammer
Figure caption: SFR(Hα) vs. M *. Green, blue, and magenta symbols are used, respectively, for the 2.7 ≤ z < 4.0, 4.0 ≤ z < 5.0, and 5.0 ≤ z < 6.5 samples, and galaxies with Hβ upper limits are indicated as SFR(Hα) lower limits (i.e., due to the lower limit on the Balmer decrement). The median error bar for each sample is shown in the lower right corner of the plot in its designated color. Along with CEERS data points, we plot the best-fit relation from Speagle et al. (2014; their Equation (28)) at the median redshift of each sample (z = 3.30, 4.60, and 5.65, respectively, for the 2.7 ≤ z < 4.0, 4.0 ≤ z < 5.0, and 5.0 ≤ z < 6.5 samples) and offset by −0.34 dex in the y-axis to account for different assumptions regarding the conversion between observables and SFR.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Radial profiles for (a) density (full lines) and temperature (dashed) from the MESA reference states, and for (b) the BVF squared N 2 used in our three models: ZAMS (magenta), midMS (cyan), and TAMS (orange). The color-coded vertical lines used in (a) mark the extent of the respective simulation domains, while the dashed portions of the N 2 profiles in (b) indicate convectively unstable regions.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Kinetic energy frequency spectra for all three stellar ages just below (a) and above (b) the CB. For each radial location, the Fourier transform of the kinetic energy (from Equation (12)) presented in the top panel (i) is multiplied by the frequency f in the bottom panel (ii) to compensate for the integration over ﹩d\mathrm{log}f﹩. The color-coded vertical lines represent estimates for the turnover frequencies of the models.