adsabs/AstroCLIMB huggingface dataset:
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: (a) Distribution of galaxies in the K–AF plane. Galaxies from ATLAS3D, xGASS, and THINGS are shown as blue symbols, gray dots, and dark red squares, respectively. The ATLAS3D symbols follow P. Serra et al. (2012): D = regularly rotating H I disks larger than the stellar disk, d = regularly rotating H I disks smaller than the stellar disk, u = H I with unsettled morphology/kinematics, and c = H I in small, scattered clouds. The vertical dashed lines mark the K values for an idealized disk and a Gaussian profile (Section 2.3), respectively. Contours enclosing 50% and 90% xGASS galaxies are shown in gray. The typical measurement uncertainty of xGASS is provided in the lower left. (b) ATLAS3D and THINGS galaxies in the K–AF plane. The unsettled H I disks are highlighted in red, including all the u-types, UGC 3960, and NGC 3077. The remaining galaxies are shown in gray. The red dashed line marks an empirical boundary separating normal (D-types and THINGS) and unsettled H I disks (Equation (3)).
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: (a) Correlation between ﹩{K}^{{\prime} }﹩ and the spatial H I concentration for 25 THINGS galaxies. The red and blue dots represent galaxies with no obvious rotation pattern (n-rot) and with counter-rotating H I disks (c-rot), respectively. The error bars and the inset panel display the change in K when artificially rotating the H I mass distribution within the disk plane (see Section 4.2 and Appendix B for details). (b) The Pearson r correlation coefficients and p-values as a function of Rin. The vertical dashed line indicates the radius where panel (a) is plotted. The shaded region at the bottom corresponds to p < 0.05. The uncertainties in r are obtained from 1000 bootstraps. The correlation is strongest at Rin ∼ 0.7Re and becomes insignificant at Rin ≳ 2.5Re.
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: (a) Normalized distribution of K. The same color scheme is used as in Figure 1. The short lines in the lower left represent the typical uncertainty in K (σK) for each sample. The vertical dashed line marks K = 0, the division of single-peaked and double-horned H I spectral shapes. The numbers (percentages) of galaxies in both categories are also provided. (b) Normalized distribution for ﹩{K}^{{\prime} }﹩ for PSBs, xGASS, and starburst galaxies in xGASS. The p-value in red is evaluated between PSBs and xGASS, while the blue one is calculated between PSBs and the starburst galaxies.
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: Variations in spectral concentration (ΔK) as a function of changes in Fourier amplitudes (﹩{\rm{\Delta }}{\mathrm{log}}\,{A}_{{\rm{m}}}﹩) for modes m = 1 to m = 6. Solid lines represent individual THINGS galaxies, color coded by the ΔK value at ﹩{\rm{\Delta }}{\mathrm{log}}\,{A}_{{\rm{m}}}=0.5﹩. Black dots with error bars denote the median values and standard deviations of ΔK for all 34 THINGS galaxies.
Paper: X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 13+1
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Herman L. Marshall
Figure caption: Schematic representation of the geometry of GX 13+1 based on our X-ray and radio polarimetry. The radio jet with a position angle of ∼ −68° is shown in green. The disk (PA = 22°), assumed to be oriented orthogonally with respect to the radio jet, is shown in red. The BL/SL with a PA of ∼ −37° representing the Comptonization region is shown in magenta. Assuming the BL/SL spreading parallel to the NS equator, we find a misalignment between the estimated NS spin and the orbital axis of GX 13+1.
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: Examples of PSB spectra obtained with FAST, ordered by increasing K and normalized by the peak flux density. Each panel displays the K value and SDSS DR7 objID in the upper left corner. The short orange bars at the top of each panel represent the velocity range of Δv = ± V85, where V85 is the half-width enclosing 85% of the total flux, as defined for K.
Paper: X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 13+1
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Herman L. Marshall
Figure caption: Image of the linear radio polarization detection of GX 13+1 at a frequency of 10 GHz. Contours plotted are equal to 3σ, 5σ, and 7σ flux density levels, where σ is the background rms value of 5.6 μJy beam−1. The synthesized beam is shown in the lower left corner.
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: Normalized distributions of sample properties for PSBs (red open) and the comparison sample from xGASS (blue filled).
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: The logarithm of Lyα flux (log(FLyα)) at the stellar surface (top row) and peak-to-trough ratio of the intrinsic Lyα profile (bottom row) vs. Teff (left column) and the logarithm of surface gravity (right column). Linear regression fits are plotted as pink dashed lines and the Sun is plotted as a yellow circle (the Sun is excluded from the fits). We find strong trends (R > 0.7, p < 0.01) between Teff and both log(FLyα) and peak-to-trough ratio. We note that the K0 star HD 64090 (5528 K) exhibits a markedly deeper self-reversal than the rest of the sample, including the Sun, and appears as an outlier in the peak-to-trough ratio plots. This pronounced reversal is likely attributable to the star’s old age and correspondingly low activity level, consistent with the behavior observed in the Sun, whose core reversal deepens during periods of low activity and becomes more filled in when activity is higher.
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: (a) Distributions of PSBs and xGASS galaxies on the K–AF plane. Contours enclosing 50% and 90% xGASS galaxies are shown in gray, as in Figure 6(a). PSBs with and without postmerger (PM) features in their optical images are overlaid using red stars and red diamonds, respectively. The error bar in the lower left represents the typical measurement uncertainty of PSBs. (b) Similar to Figure 3, except that galaxies defined by Equation (3) are separated from their parent samples.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Lyα profiles of low-mass K and M stars with high radial velocities (∣RV∣ > 84 km s−1) ordered by spectral type. HST/STIS observations are plotted in black, with associated errors shaded in gray. All stars were observed with the G140M grating, except for HD 191408, Kapteyn’s Star, GJ 411, and Barnard’s Star, which were observed with E140M. The ISM transmittance curve for each star is plotted as a gray dashed line. Intrinsic PHOENIX model profiles are plotted in yellow. The intrinsic PHOENIX model, after being multiplied by the ISM transmittance curve, is plotted in pink; this profile should match the observations. The yellow profile represents the intrinsic stellar emission before ISM absorption.
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: (a) Comparison of K measured with different surveys for 13 galaxies observed with both THINGS and FEASTS. From left to right: (i) THINGS cubes; (ii) cutouts of FEASTS cubes within the sky region of THINGS cubes; (iii) FEASTS full cubes. An example of the moment-0 maps of the three data sets is shown in the upper right panels. (b) Distribution of differences in K between (i) and (ii) (ΔK+miss). (c) Correlation between ∣ΔK+miss∣ and the mass fraction of missing H I (fmiss). The filled dots and open circles represent increased and decreased K after adding H I missed by THINGS, respectively.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Of the 12 high-RV stars with Lyα measurements, two have observations taken over multiple days and both exhibit variability on the order of 20% over the 3–4 days observing windows. Left: HST/STIS Lyα spectra of Ross 1044 (top) and Ross 451 (bottom) over multiple visits (various colors) compared to the final coadded spectrum in black. The ISM transmittance curves are plotted as gray dashed lines. Right: Lyα flux variability of Ross 1044 (top, adapted from A. C. Schneider et al. 2019) and Ross 451 (bottom), as measured over the observed spectrum from ±0.5 Å from the line center. Each set of points are normalized to the flux of the final coadded spectrum.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Measured (dashed) and modeled (solid; shifted in wavelength for visual clarity) Lyα profiles for Ross 1044 (left) and Ross 451 (right) from the multiple HST orbits that exhibited variable behavior. The modeled profiles show the stellar emission in the absence of ISM absorption. For Ross 1044, there is a 5% difference in self-reversal depth as measured via peak-to-trough ratio; there is no difference in peak-to-trough ratio for Ross 451. The ISM transmittance curve is plotted as the yellow dashed line.
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: Dependence of K (upper) and ﹩{K}^{{\prime} }﹩ (lower) on stellar mass, H I mass, optical concentration, and inclination angle. Blue dots and red stars represent xGASS galaxies and PSBs, respectively. The Pearson-r coefficient and the p-value for xGASS are shown at the top of each panel. The median trends of xGASS are plotted as solid blue lines.
Paper: Decoding the Single-peaked H I Spectra of Low Redshift Poststarburst Galaxies
Authors: Qifeng Huang, 齐丰 黄, Jing Wang, 菁 王, Sara L. Ellison, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Dong Yang, 冬 杨
Figure caption: The H I moment-0 maps of UGC 3960 (left; ATLAS3D) and NGC 3077 (right; THINGS). The background images are from the Legacy Surveys (A. Dey et al. 2019). The cyan circles in the lower left indicate the synthesized beam.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Left: nNLTE/nLTE for hydrogen in the n = 2 state vs. column mass, zoomed in to show detail in the transition region and upper chromosphere (these values go to 1 deep in the atmosphere). Initial models are shown in pink, revised models with an imposed minimum set at the boundary between these layers shown in orange. Right: Lyα profiles. HST/STIS observations are plotted in black, with associated errors shaded in gray. The ISM transmittance curve for each star is plotted as a gray dashed line. Initial intrinsic PHOENIX model profiles are plotted in pink and show deep central reversals. Revised intrinsic PHOENIX model profiles are plotted in orange. The revised intrinsic PHOENIX model, after being multiplied by the ISM transmittance curve, is plotted in blue; this profile should match the observations. Stars shown in this figure are (from top to bottom): HD 64090 (K0), HD 134439 (K1), HD 134440 (K2), and HD 191408 (K2.5). We include a comparison to the intrinsic Lyα profile computed in A. Youngblood et al. (2022) for HD 19148, plotted in green.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Reconstructed (B. E. Wood et al. 2005; J. L. Linsky et al. 2014; V. Bourrier et al. 2017a, 2017b; K. Melbourne et al. 2020; A. Sandoval et al. 2023) and directly observed (this work; A. Youngblood et al. 2022) Lyα fluxes scaled to the habitable zone, following R. K. Kopparapu et al. (2014) and assuming a 1 Earth mass planet. Error bars give the flux range between the recent Venus and early Mars limits, not the estimated uncertainties. All stars older than 1 Gyr are plotted in color, and those younger than 1 Gyr in gray. Linear regression fits to all stars >1 Gyr (red dotted line), to just the high-RV stars from this work and A. Youngblood et al. (2022; blue dashed line), and a weighted fit to the young stars (<1 Gyr; gray dotted line) are shown. We note that the Sun and the A. Sandoval et al. (2023) values (improved Lyα reconstructions from those presented in A. Youngblood et al. 2016) align more closely with the high-RV fit line.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Same as Figure 9. Stars shown in this figure are (from top to bottom): Kapteyn’s Star (M1), GJ 411 (M2), L 802-6 (M3), and Barnard’s Star (M4). We include comparisons to the intrinsic Lyα profiles computed in A. Youngblood et al. (2022) for Kapteyn’s Star, GJ 411, and Barnard’s Star, plotted in green.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: The evolution of ﹩{\mathrm{log}}\,({L}_{{\rm{Ly}}\alpha }/{L}_{{\rm{bol}}})﹩ as a function of stellar age for M dwarf stars. Solid lines show the parameterized empirical trends for M0–M2 and M2.5–M6.5 spectral types from S. G. Engle (2024), with shaded regions representing 1σ uncertainties on the fits. Overplotted are our sample stars, color-coded by spectral type: M0–M2 (purple) and M3–M4 (orange). The three M0–M2 stars lie within or exceed the upper bound of the extrapolated uncertainty envelope at older ages. In contrast, the M3–M4 stars fall significantly below the empirical track, suggesting either lower intrinsic activity or potential limitations of the model extrapolation at late ages for mid-M dwarfs.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Minimum values for nNLTE/nLTE in the n = 2 state of H I at the transition region–chromosphere boundary (left column) and the ratio of that value to the corresponding maximum nNLTE/nLTE in the chromosphere (right column) vs. Teff (left column) and the logarithm of surface gravity (right column). Linear regression fits are plotted as pink dashed lines. We find a strong trend (R = 0.75, p = 0.01) between Teff and the ratio of the minimum nNLTE/nLTE at the transition region–chromosphere boundary to the corresponding maximum value in the chromosphere.
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Same as Figure 9. Stars shown in this figure are (from top to bottom): Ross 825 (K3), HIP 117795 (K8), Ross 451 (M0), and Ross 1044 (M0).
Paper: Lyα Emission from K and M Dwarfs: Intrinsic Profiles, Variability, and Flux in the Habitable Zone
Authors: Sarah Peacock, Travis S. Barman, R. O. Parke Loyd, Adam C. Schneider, Allison Youngblood, Kenneth G. Carpenter, Evgenya L. Shkolnik
Figure caption: Temperature–column mass structures for the models of each star. We shade the approximate temperature ranges over which the core and wings of Lyα forms in purple (≈8000–25,000 K for the core, and ≈4000–7500 K for the wings); the actual range of temperatures varies by star and is determined by where the optical depth, τ(λ), is equal to 1.
Paper: On the Stability Analysis of Astrophysical Cooling Functions
Authors: Amanda Stricklan, Tim Waters, James Klimchuk
Figure caption: TI zones plotted on phase diagrams for the KI cooling function. Top panels:T–p and T–n phase diagrams, displaying a color map of the net cooling rate, Lnet, where red indicates heating (Lnet < 0) and blue cooling (Lnet > 0). The solid, dotted, and dashed lines are the equilibrium curve (Lnet = 0), the isobaric Balbus contour (﹩{N}_{p}^{\prime} =0﹩), and the isochoric Balbus contour (﹩{N}_{\rho }^{\prime} =0﹩), respectively. Bottom panels: color maps of ﹩{N}_{p}^{\prime} ﹩ and ﹩{N}_{\rho }^{\prime} ﹩, which are the dimensionless isobaric and isochoric growth rates (orange colors) and damping rates (purple colors). In T–p phase diagrams, positively sloped regions of an equilibrium curve are isobarically unstable, while in T–n phase diagrams, positively sloped regions are isochorically unstable. Note that while the slopes of the equilibrium curves are entirely negative in the right panels, there is nevertheless a prominent region of isochoric instability above the equilibrium curve (the orange region in the lower-right panel, which defines an isochoric TI zone).
Paper: On the Stability Analysis of Astrophysical Cooling Functions
Authors: Amanda Stricklan, Tim Waters, James Klimchuk
Figure caption: Λc-based nonequilibrium analysis of the KI cooling function. Left panel: an equivalent T–n phase diagram to the top-right panel of Figure 2, this time also showing two nonequilibrium evolutionary paths: (i) an isobaric path from an unstable state to a stable state (diagonal arrow); and (ii) an isochoric path from a hot state back to an equilibrium state. Right panels: the Λ(T) vs. T curve from Figure 1 is reproduced here as the solid black lines. The dotted portions of these lines correspond to the temperatures spanned by the isobaric and isochoric paths from the left panel. We arrive at the highlighted portions by first plotting the blue and orange lines, which represent the isobaric and isochoric Λc values (Equation (25) and Equation (26), respectively). Gray (red) highlights when Λ(T) > Λc for the isobaric value (both values) of Λc. Comparing the highlighted regions with the purple paths in the left panel, notice how the isobaric path avoids passing through the isochoric TI zone; hence, it is only shaded gray, while the isochoric path starts off in the isochoric TI zone and exits this zone when the highlighting changes color from red to gray. From there, it changes from isobarically unstable to stable (unshaded) upon exiting the isobaric TI zone.
Paper: On the Stability Analysis of Astrophysical Cooling Functions
Authors: Amanda Stricklan, Tim Waters, James Klimchuk
Figure caption: Analysis of the stabilizing effect of thermal conduction on isobaric TI zones for the KI and SPEX cooling functions. Top panels: T–n phase diagrams showing equilibrium curves (solid black lines) and the isobaric contours Λ(T) = Λc(5λF), Λc(λF), and Λc(0.5λF) (blue, orange, and green lines, respectively). Notice how the isobaric TI zone grows smaller with increasing thermal conduction (the green contour in the KI phase diagram falls off of the plot completely). The purple arrow shows the same isobaric paths from Figures 4 and 5. TI zones for SPEX are no longer horizontal lines and in fact resemble the isochoric TI zones in Figure 5 because λF introduces density dependence. Bottom panels: cooling-curve plots comparing Λ(T) and isobaric Λc for each value of λ used to evaluate the TI zones in the top panel. The strength of thermal conduction increases from top to bottom, illustrating stabilization for λ ≲ λF. Gray highlights have the same meaning as in Figure 4.
Paper: On the Stability Analysis of Astrophysical Cooling Functions
Authors: Amanda Stricklan, Tim Waters, James Klimchuk
Figure caption: Stability analysis of a stable coronal loop simulation from KL19. Top panel: “tracks” of the steady-state solution (Loop 1) are plotted as gray points on a T–n phase diagram; the apex and the coronal edge position are marked with blue and red dots. The blue and red lines correspond to equilibrium curves computed at the blue and red dots (which are also marked in the lower panels). The gray band illustrates the range of equilibrium curves at each intermediate location between these points. Lower panels: the cooling rate, Λ(T), and the critical isobaric cooling rate as functions of the loop position for λ = 1.5λF, λF, and 0.35λF.
Paper: On the Stability Analysis of Astrophysical Cooling Functions
Authors: Amanda Stricklan, Tim Waters, James Klimchuk
Figure caption: Same as Figure 2 but for the SPEX cooling function. Unlike in Figure 2, the equilibrium curve has positive sloping regions in the T–n phase diagram, indicating that both the isobaric and isochoric instability criteria are satisfied. Such a slope-based analysis tells one nothing about the stability of regions off the equilibrium curve. By plotting TI zones, we recover the sloped-based results but also see where there is instability in nonequilibrium parameter space.
Paper: On the Stability Analysis of Astrophysical Cooling Functions
Authors: Amanda Stricklan, Tim Waters, James Klimchuk
Figure caption: Comparison of three different radiative loss functions, Λ(T): a commonly used one for the ISM computed by H. Koyama & S.-i. Inutsuka (2002), one used to model the solar corona based on collisional ionization equilibrium from K. M. Schure et al. (2009), and a simplified curve used for coronal loop modeling by J. A. Klimchuk & M. Luna (2019).
Paper: On the Stability Analysis of Astrophysical Cooling Functions
Authors: Amanda Stricklan, Tim Waters, James Klimchuk
Figure caption: Same as Figure 4, showing the SPEX cooling function. For simplicity, here we omit the blue and orange curves in the top-right panel. Again, red highlights indicate TI zones where Λ(T) > Λc for both the isobaric and isochoric values of Λc.
Paper: Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae
Authors: Wanqing Liu, Mohit Bhardwaj, Ben Margalit
Figure caption: Probability Pcc that at least one unrelated CCSN lies within an FRB 90% localization region, for z ≤ 0.043. The color scale shows ﹩{{\mathrm{log}}_{10}}{P}_{{\rm{cc}}}﹩ and white curves mark the 10%, 1%, 3σ, and 5σ thresholds, which can be separated by different line styles.