adsabs/AstroCLIMB huggingface dataset:
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: On the left, the metallicities of outflowing (red) and inflowing (blue) FOGGIE absorbers are binned vs. their distance from their host central galaxies, colored by the average radial velocity for that bin. On the right, the gas in all 18 FOGGIE snapshots is shown in the same configuration. The mean metallicity (﹩\mathrm{log}\langle Z/{Z}_{\odot }\rangle ﹩) is marked with a black line. The dashed line indicates the solar metallicity level. Probability densities are shown at the top and sides of each panel.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: The [C/α] ratio against the metallicity of the absorbers from the KODIAQ-Z (2.2 ≲ z ≲ 3.6), HD-LLS (2.2 ≲ z ≲ 3.6), and CCC (z ≲ 1) surveys. The median values of the [C/α] and [X/H] posterior pdf’s are adopted with 68% CI. Note that [C/α] values with [C/α] < − 0.6 are most likely predominantly caused by ionization corrections rather than nucleosynthesis effects (see text for more details).
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Posterior pdf’s of the total H column density (left), H density (middle), and path length (right) for SLLSs, LLSs, pLLSs, and SLFSs for the entire sample from the KODIAQ-Z survey and HD-LLSs.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Comparison of the metallicity CDFs for the different categories of absorbers in the KODIAQ-Z+HD-LLS+R12 observations and FOGGIE simulations at 2 ≤ z ≤ 3 (the sample of pLLSs in this redshift interval for the observation sample is too small to produce a reliable CDF and therefore is not shown here).
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Number of right-hand side evaluations for sdc_subch2_cfl0.2, showing the L1 norm/average (solid), L2 norm (dashed), and L-inf/maximum (dotted) for two iterations of the simplified-SDC integration.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Number of right-hand side evaluations for strang_subch2_cfl0.2, showing the L1 norm/average (solid), L2 norm (dashed), and L-inf/maximum (dotted) for both halves of the Strang integration.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Reaction network for the double-detonation problem.
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) EoS (left) and TOV solution (right) for strange stars with X  V  = 1.0 (top) and X  V  = 0.4 (bottom). Solid lines indicate the minimum bag value for the stability window and dotted lines indicate the maximum bag value for the stability window.
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) Top: EoS for the different values of parameter α. Bottom: mass–radius relation for pure nucleonic and hyperonic stars. The yellowish hatched area refers to the uncertainty of the lower mass compact object present in the GW190814 event, while the bluish hatched area denotes the uncertainty about the radius of the 1.4  M ⊙ star. Both constraints are taken from Abbott et al. (2020). The radius of all canonical stars is 13.38 km.
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) EoS (left) and TOV solution (right) hybrid stars with X  V  = 1.0 (top) and X  V  = 0.4 (bottom) at the extreme values of G  V . Solid lines indicate a hadronic phase with only nucleons (NN) and dotted lines indicate a hadronic phase with nucleons and hyperons (NH).
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) Hybrid branch stability window for X  V  = 1.0 (top) and X  V  = 0.4 (bottom) with a pure nucleonic EoS (NN) and an EoS with nucleons and hyperons (NH).
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) Dimensionless tidal parameter for pure nucleonic stars, as well for two values of α. The hatched area refers to the uncertainty of the tidal deformability parameter deduced from the GW190814 event (Abbott et al. 2020).
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) Stability window for X  V  = 1.0 and 0.4.
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) Dimensionless tidal parameter Λ for strange stars with X  V  = 1.0 (top) and X  V  = 0.4 (bottom). Solid lines indicate the minimum bag value for the stability window and dotted lines indicate the maximum bag value for the stability window.
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) The square of the speed of sound with X  V  = 1.0 (top) and X  V  = 0.4 (bottom).
Paper: On the Nature of the Mass-gap Object in the GW190814 Event
Authors: Luiz L. Lopes, Debora P. Menezes
Figure caption: (Color online) Square of the speed of sound for pure nucleonic and hyperonic matter for different values of α. The horizontal line is the conformal limit predicted by pQCD.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: WISPR-I/WISPR-O composites highlighting the coronal activity during 2021 November 20–21 (see Section 3.3). The (LW-processed) images have been projected onto the HPC grid to show the physical FOVs of both detectors together. The Milky Way crosses the FOV of the WISPR telescopes during the development of the events. The inner telescope clearly shows the striated nature of the outflows in the HPS after the passage of the big CME event.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: WISPR-I/WISPR-O composite snapshots from 2021 November 22–23 (LW-processed) projected onto the HPC coordinate system showing the development of (1) a triple front between 0 at 10° latitude (top panels) and (2) three consecutive CME events toward southern latitudes that appear to start merging before reaching the end of the WISPR-I FOV (see Section 3.4).
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: LW-processed snapshot showing the dust trail associated with 3200/Phaethon in the FOV of WISPR-O. The brightness signature of the trail shows up as a diffuse band that extends from the upper right part of the image to the lower left part. The star field has been removed from the scene with a σ-filter (as implemented in IDL Solarsoft).
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: WISPR-I/WISPR-O composites of three time instances of a big CME event that developed during 2021 November 25–26. Note that the bright frontal arc is only about 180° rather than completely around the central core of the event, indicating that the view is not edge-on.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: STEREO-A COR2 snapshots of the November 20 event observed by WISPR (see Figure 8).
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Representative EVDF observed in the near-Sun fast solar wind (r ∼ 18.5 R  S , v  p  ∼ 525 km s−1). The top panel shows SPAN-Electron measurements binned by energy and pitch angle in the solar wind frame, accumulated over a 20 minute interval (colored diamonds). Positive velocity values represent pitch angles from 0° to 90° (sunward-going electrons, given the sunward magnetic field at this time), and negative values represent pitch angles from 90° to 180° (anti-sunward), as indicated. Colored curves in the top panel show the corresponding values for a drifting bi-Maxwellian fit to the core of the distribution and a Maxwellian fit to the suprathermal portion of the most anti-field aligned bin (which contains the strahl), with the corresponding parallel core and strahl temperatures (T  C∣∣ and T  S∣∣) indicated. The bottom panel shows the observed EVDF normalized by the core fit values. Vertical dashed lines in both panels delineate the low-energy portion of the EVDF contaminated by secondary electrons, and dashed curves in the top panel show the approximate instrumental background level. The vertical dotted line in both panels indicates the sunward cutoff in the EVDF, with the corresponding electric potential (ϕ  c ) indicated.
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Radial evolution of the local core parallel electron temperature (T  C∣∣) measured by SPAN-Electron, binned by asymptotic solar wind speed (v ASY) in nine ranges, as indicated. Colored lines represent median values for each radius–speed bin, and error bars represent upper and lower quartiles. The two dashed curves show approximate power law extrapolations for low and high asymptotic speeds, with diamonds indicating the intersections of these curves with the corresponding strahl parallel temperature (T  S∣∣) values.
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Radial evolution of the sum of the electric potential (same as Figure 6) and the gravitational potential per charge for protons, with respect to infinity, binned by asymptotic solar wind speed (v ASY, same ranges as Figure 6). Colored lines represent median values for each radius–speed bin, and error bars represent upper and lower quartiles. The two dashed curves show the same power law extrapolations as Figure 6, with the addition of the gravitational potential, with diamonds indicating the maxima in the total potential.
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Joint occurrence of the asymptotic solar wind speed (v ASY) and strahl parallel temperature (T  S∣∣), determined as described in the text from PSP measurements from encounters 3 to 11 over heliocentric distances of 13.3–50 R  S . The orange line shows the average value of the strahl parallel temperature for each speed bin.
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Radial evolution of the local electric potential with respect to infinity (ϕ  c ), as determined from SPAN-Electron measurements of the sunward cutoff in the EVDF, binned by asymptotic solar wind speed (v ASY) in nine ranges, as indicated. Colored lines represent median values for each radius–speed bin, and error bars represent upper and lower quartiles. The two dashed curves show approximate power law extrapolations for low and high asymptotic speeds.
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Radial evolution of the local solar wind proton speed (v  p ) measured by SPAN-Ion (same as Figure 4), with curves showing the predicted speed profiles corresponding to the total potential curves from Figure 7, with initial values estimated from the strahl parallel temperatures using ﹩{v}_{0}=\sqrt{2{{kT}}_{S| | }/{m}_{p}}﹩.
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Representative EVDF observed in the near-Sun slow solar wind (r ∼ 18 R  S , v  p  ∼ 210 km s−1), in the same format as Figure 1.
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Radial evolution of the local bulk solar wind proton speed (v  p ) measured by SPAN-Ion, binned by asymptotic solar wind speed (v ASY) in nine ranges, as indicated. Colored lines represent median values for each radius–speed bin, and error bars represent upper and lower quartiles.
Paper: On the Impact of Relativistic Gravity on the Rate of Tidal Disruption Events
Authors: Eric R. Coughlin, C. J. Nixon
Figure caption: Left: Direct capture curves for the SMBH spins shown in the legend; for a given a, the region of direct capture is bounded by the relevant (colored) curve and the black, dashed curve, which gives ℓ = ± ∣J∣ and yields the maximum and minimum values that ℓ can have for any J 2. When the spin is zero, the curve is a vertical line at J 2 = 16, while prograde (positive-ℓ) orbits can reach smaller J 2 without being directly captured when the SMBH is spinning (and retrograde orbits are captured at even larger values of J 2). Right: Curves of constant r p in the ℓ−J 2 space, with r p shown in the legend, for an SMBH with a = 0.9. For sufficiently small r p the contours intersect the direct capture curve.
Paper: On the Impact of Relativistic Gravity on the Rate of Tidal Disruption Events
Authors: Eric R. Coughlin, C. J. Nixon
Figure caption: Distribution function of r p (left) and β (right) for a tidal radius of r t = r t,⊙ ≃ 47 for the SMBH spins in the legend. The black, dashed curve in the left-hand panel is the analytic solution for a Schwarzschild SMBH calculated in Section 3 and is effectively a check on the analysis. In the right panel, the dashed curve gives f  β  = β −2, which is the result in the Newtonian limit, while the dotted–dashed curve shows f  β  ∝ β −10/3. The locations at which the distribution function goes to zero demarcate the smallest possible value of r p on the direct capture curve, which approaches 1 in the limit that a → 1.
Paper: Dependence of the Radio Emission on the Eddington Ratio of Radio-quiet Quasars
Authors: Abdulla Alhosani, Joseph D. Gelfand, Ingyin Zaw, Ari Laor, Ehud Behar, Sina Chen, Ramon Wrzosek
Figure caption: 40 mas × 40 mas VLBA images of the 1.4 GHz (left) and 4.8 GHz (right) emission of PG 0050+124. The white contours in both images indicate 1.4 GHz flux density 3σ, 5σ, 7σ, 10σ, 15σ, and 20σ of the 1.4 GHz image. In the left panel the cross-hatched ellipse represents the beam; in the right panel the larger ellipse is the size of the 1.4 GHz beam, while the cross-hatched ellipse is the size of the 4.8 GHz beam.
Paper: On the Impact of Relativistic Gravity on the Rate of Tidal Disruption Events
Authors: Eric R. Coughlin, C. J. Nixon
Figure caption: Number of TDEs relative to the total number of stars scattered into the loss cone as a function of the tidal radius (in units of gravitational radii) for the SMBH spins shown in the legend. It is clear that the SMBH spin only matters as it concerns the rate of TDEs if the SMBH is rapidly rotating, with a ≳ 0.75. The black hole mass (top axis) is derived from the standard definition for the tidal radius given a solar-like star.
Paper: Dependence of the Radio Emission on the Eddington Ratio of Radio-quiet Quasars
Authors: Abdulla Alhosani, Joseph D. Gelfand, Ingyin Zaw, Ari Laor, Ehud Behar, Sina Chen, Ramon Wrzosek
Figure caption: VLBA images of the observed PG RQQs (Table 1). For all targets, the first row is the observed VLBA emission at 1.4 GHz, and the second row is the observed VLBA emission at 4.8 GHz. In each image, the origin (0, 0) of the coordinate system is the optical center of the galaxy as given in the NASA/IPAC Extragalactic Database (NED), the size and orientation of the synthesized beam is shown in the lower left corner, the Eddington ratio r Edd is indicated in the upper left corner of the image, a physical size scale is indicated in the lower right corner, the gray scale indicates the intensity (in Jy beam−1) ranging from −5σ to 15σ (where the image σ is given in Table 2), and the white contours indicate 3σ, 5σ, 7σ, 10σ, 15σ, and 20σ intensity emission for detections. The smaller region of the 4.8 GHz image is indicated by the black square in the 1.4 GHz image. The low Eddington RQQs are detected at a higher rate and with higher significance than the high Eddington RQQs, especially at 4.8 GHz.
Paper: On the Impact of Relativistic Gravity on the Rate of Tidal Disruption Events
Authors: Eric R. Coughlin, C. J. Nixon
Figure caption: Difference in the number of TDEs, relative to the total number of stars scattered into the loss cone, between an SMBH with spin given in the legend and a Schwarzschild SMBH. This shows that a rapid SMBH spin can generate at most a ∼ 10% difference in the fraction of TDEs, with the maximum difference occurring at an SMBH mass of ∼ 3.2 × 107 M ⊙.
Paper: On the Impact of Relativistic Gravity on the Rate of Tidal Disruption Events
Authors: Eric R. Coughlin, C. J. Nixon
Figure caption: TDE rate as a function of the SMBH mass for the combinations of the SMBH spin and stellar type shown in the legend. The points on each curve show where the rate falls by an order of magnitude relative to the rate at which stars are scattered into the loss cone, where the latter is shown by the black, dotted–dashed curve.
Paper: On the Impact of Relativistic Gravity on the Rate of Tidal Disruption Events
Authors: Eric R. Coughlin, C. J. Nixon
Figure caption: Regions in the ℓ–J 2 space that delimit observable TDEs, i.e., have a pericenter distance less than a given r p but are not directly captured. In the left panel the curve of constant r p = 4 is shown by the blue line connecting the two blue points, while the right panel has r p = 9 on the curve connecting the two red points. For r p = 4, the region of observable TDEs is bounded by the two blue points and the topmost black point (which is the minimum possible J 2 and smallest pericenter; see Equation (B3)), while that for r p = 9 is bounded by the two red points and the two black points.
Paper: A Systematic Study of the Short-term X-Ray Variability of Seyfert Galaxies. I. Diversity of the X-Ray rms Spectra
Authors: Jingwei Hu, Chichuan Jin, Huaqing Cheng, Weimin Yuan
Figure caption: Some examples of the time-averaged spectra (black), LF rms spectra (red), and HF rms spectra (blue) around the Fe Kα band. The 1σ and 2σ confidence intervals of the Fe line in the time-averaged spectra are marked as dark and light shaded areas, respectively. The first row shows some examples when a narrow or relatively symmetric Fe line is present, in which case no additional variability is observed. The second row shows some examples when a broad and redshifted Fe line is present in the time-averaged spectra, which is accompanied by additional LF and HF variability.
Paper: A Systematic Study of the Short-term X-Ray Variability of Seyfert Galaxies. I. Diversity of the X-Ray rms Spectra
Authors: Jingwei Hu, Chichuan Jin, Huaqing Cheng, Weimin Yuan
Figure caption: Typical example of the results of the connection of the rms spectra with the time-averaged spectra for the case of Mrk 766. Similar plots for other sources in Table 1 can be found in the appendix. The left panel shows the unfolded time-averaged spectra of three separate observations. The middle panel shows the fractional rms of each individual observation in the low frequency (LF; < 10−4 Hz). The right panel shows the fractional rms in the high frequency (HF; 10−4–10−3 Hz).
Paper: NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario
Authors: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, D. Stern
Figure caption: The 0.3–10 keV XMM-Newton spectrum of PG 1001 fitted with the Section 4.2 model plus an additional power-law component. The spectrum is grouped for display purposes only. The bottom panel displays the ratios of the data to the best-fit model. The additional power-law component describes well the soft-excess emission with a large photon index of ≈5.0. The soft excess is probably the leaked portion of the warm corona emission through the same dust-free absorber that obscures the >1 keV main component.
Paper: A Systematic Study of the Short-term X-Ray Variability of Seyfert Galaxies. I. Diversity of the X-Ray rms Spectra
Authors: Jingwei Hu, Chichuan Jin, Huaqing Cheng, Weimin Yuan
Figure caption: Type of the spectral shape of the time-averaged spectra and the fractional rms spectra. The time-averaged spectra, plotted in E 2 N(E), can be classified as: (spec1) increasing with energy; (spec2) concave-up; (spec3) decreasing with energy; (spec4) flat. The LF and HF rms spectral shapes can be classified as: (rms1) increasing with energy; (rms2) concave-down; (rms3) decreasing with energy; (rms4) flat; (rms5) concave-up.