adsabs/AstroCLIMB huggingface dataset:
Paper: Disk Draining in LIGO Progenitor Black Hole Binaries and Its Significance to Electromagnetic Counterparts
Authors: Xiaoshan Huang, Sierra Dodd, Sophie Lund Schrøder, Shane W. Davis, Enrico Ramirez-Ruiz
Figure caption: Disk draining in LIGO progenitors. Shown is the evolution of disk mass (spanning 0.02 < R < 0.25) with the companion present, normalized to the initial disk mass at the disk-draining phase. The red curve shows the disk mass for Am5 with αk = 10−5, and the green curve shows the disk mass for Am3 (green curve) with αk = 10−3. The measured αeff ≈ 8.9 × 10−3 ≫ 10−5 in Am5, yielding a viscous timescale tvis ≈ 55.9 that is roughly 3.6 × 103 orbital timescales. In Am3 we measure αeff ≈ 1.3 × 10−2 and tvis ≈ 32.0, which is roughly 2.1 × 103 orbital timescales. In the above plot, we scale the time to tvis ≈ 55.9, equivalent to effective viscosity αeff = 1.0−2, roughly consistent with both Am3 and Am5.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The contribution of gases and clouds in shaping the best-fit self-consistent model is shown here for the clear equilibrium chemistry scenario (top panel), cloudy equilibrium chemistry scenario (middle panel), and clear disequilibrium chemistry scenario (bottom panel). The best-fit model in each panel is shown with a solid line—green in the top panel, black in the middle panel, and red in the bottom panel. The contribution of each absorber is shown as the shaded region between the best-fit spectrum and best-fit model without that absorber.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The corner plot obtained from the grid fitting exercise from the clear equilibrium chemistry grid is shown in the left panel. The corner plots from the cloudy equilibrium chemistry grid and clear disequilibrium chemistry grid are shown in the middle and right panels, respectively. Note that the C/O shown is relative to the solar value, where the assumed solar C/O is 0.458.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The best-fit BOSZ stellar model compared with the flux-calibrated stellar spectrum from JWST for GJ 436 is shown in the top panel. The bottom panel shows the ratio between the data and the best-fit model. Deviations of this ratio from 1 indicate missing or additional opacities present in the best-fit model compared to the observed stellar spectrum.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: We integrated the JWST NIRCam bandpass over the same wavelengths as Spitzer IRAC1 and IRAC2 bands. The bandpass-integrated photometry for three different eclipses observed with NIRCam F322W2 is considerably shallower than the observed 3.6 μm Spitzer photometry (gray posteriors), likely due to uncorrected correlated noise in the Spitzer light curves. While the JWST NIRCam observations contain their own systematics, the modeled eclipses are all in agreement at a much shallower eclipse depth.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The corner plot from the clear free chemistry retrieval on the JWST data.
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: The helium abundance a function of solar wind speed. AHe has been normalized to its maximum value in each column. The helium abundance monotonically increases from 0% to 4.19% in slow wind and saturates to this AHe = 4.19% in fast solar wind for which vsw > 433 km s−1.
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: The (a) saturation speed (vs) and (b) saturation abundance (As) as a function of normalized cross helicity (∣σc∣). Marker color indicates ∣σc∣ for visual comparison with Figures 5 and 6. The pink lines and shaded regions surrounding them are the values derived for all data in Figure 3. The blue lines and shaded regions indicate the weighted mean and standard error of the mean for the indicated ranges of normalized cross helicity. Markers and error bars are colored by ∣σc∣ for visual comparison with later figures.
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: Mean alpha particle and proton number densities as a function of solar wind speed. The semitransparent regions are the standard deviations. The highlighted regions on the nHe trend indicate speeds within 1σ of the slow wind peak (vslow) in Figure 1, the fast wind peak (vfast) in Figure 1, and the saturation speed (vs) derived in Figure 3 for all data along with vn, the peak of nHe in this figure when the nα trend is recalculated across the ∣σc∣ quantiles.
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: The same PDF of vsw in Figure 1. The highlighted purple, orange, blue, and green intervals are the same as in Figure 8: the fast and slow wind peaks derived from Gaussian fits (vslow and vfast in purple), the range of saturation speeds derived across ∣σc∣ (vs in blue), the peaks of nα derived in Figure 8 across ∣σc∣ (vn in orange), and the speed at which the Gaussians used to derive vslow and vfast intersect (vi in green).
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: Three probability density functions (PDFs) of the solar wind speed observed by the Wind Faraday cups at 1 au. The PDFs indicate all the data observed (green dashed), data from solar maxima 23 and 24 (orange dashed–dotted), and solar minima 23 and 24 (solid black).
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: Fits to ﹩{A}_{{\rm{He}}}\left({v}_{{\rm{sw}}}\right)﹩ in 15 ∣σc∣ quantiles, which are given by the color bar. The green points are the fit values and uncertainties for the saturation points (vs, As). The insert zooms in on the points.
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: A cartoon illustrating the relationship between the helium abundance (AHe), cross helicity (∣σc∣), and magnetic field topology at the solar wind’s source regions. Closed magnetic loops are plotted in orange. Open magnetic field lines are plotted in red. The helium abundance is set below the sonic surface (rc) in the chromosphere and transition region. Between the sonic surface and the Alfvén surface (rA), the cross helicity is set. Above the Alfvén surface, the solar wind is magnetically disconnected from the Sun, and ∣σc∣ can only decay. The solar wind speed (blue arrows) increases during propagation through interplanetary space due to the decay of Alfvénic structures like switchbacks (S. D. Bale et al. 2023; N. E. Raouafi et al. 2023; Y. J. Rivera et al. 2024). Adapted from M. Akhavan-Tafti & S. L. Soni (2024) Figure 3.
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: The cross helicity as a function of vsw, normalized to its maximum value in each column. The blue line indicates values at 60% of the maximum in each column. The green line indicates the saturation speed (vs) as derived in Figure 3.
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: Fits to ﹩{A}_{{\rm{He}}}\left({v}_{{\rm{sw}}}\right)﹩ in 15 ∣σc∣ quantiles, which are given by the color bar, rescaled to the saturation point (vs, As). The green point indicates (1, 1), the scaled saturation point.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: Corner plot for the four-planet joint fit to MAROON-X Red channel and ESPRESSO data sets. We only plot this for the 20 planetary parameters and six GP hyperparameters.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: Phase-folded plots for planets Barnard b, c, d, and e based on joint fit between MAROON-X Red channel, Blue channel, and ESPRESSO radial velocities.
Paper: Andromeda XXXV: The Faintest Dwarf Satellite of the Andromeda Galaxy
Authors: Jose Marco Arias, Eric F. Bell, Katya Gozman, In Sung Jang, Saxon Stockton, Oleg Y. Gnedin, Richard D'Souza, Antonela Monachesi, Jeremy Bailin, David Nidever, Roelof S. de Jong
Figure caption: Left: absolute V-band magnitude (MV) vs. azimuthally averaged physical half-light radius (rh) for various stellar systems in the Local Group, including MW classical globular clusters, MW ultrafaint compact stellar systems (ambiguous objects), both MW and M31 dwarf galaxies, and other Local Volume dwarf galaxies. An inset highlights systems comparable to And XXXV in the luminosity–size plane. Data for all systems except And XXXV are sourced from the Local Volume Database (A. B. Pace 2024) and references therein. Right: metallicity–luminosity relation for Local Group dwarf galaxies, with the black solid line representing the best-fit relation from J. D. Simon (2019). The dashed lines represent a 1σ scatter of 0.16 dex around the fit. M31 dwarf galaxies are outlined in violet triangles (filled dark pink triangles, taken from M. L. M. Collins et al. 2013; filled light violet triangles, taken from A. W. McConnachie 2012 and references therein; filled light pink triangles, taken from M. L. M. Collins et al. 2022 and M. L. M. Collins et al. 2024). And XXXV is marked by a filled red star with error bars. Other measurements, including those for MW and Local Volume dwarfs, are taken from the Local Volume Database (A. B. Pace 2024) and references therein.
Paper: Andromeda XXXV: The Faintest Dwarf Satellite of the Andromeda Galaxy
Authors: Jose Marco Arias, Eric F. Bell, Katya Gozman, In Sung Jang, Saxon Stockton, Oleg Y. Gnedin, Richard D'Souza, Antonela Monachesi, Jeremy Bailin, David Nidever, Roelof S. de Jong
Figure caption: Corner plots displaying the full posterior distributions of the structural parameters of the exponential (left) and Plummer (right) models for And XXXV. The azimuthally averaged half-light radius ﹩{r}_{h}={a}_{h}\sqrt{1-\epsilon }﹩ is displayed rather than the elliptical half-light radius ah for both density profiles. The centroid of And XXXV has already been converted to its R.A. (J2000) and decl. (J2000) coordinates in degrees. The posterior distributions for both corner plots are based on over 10,000 MCMC iterations after burn-in. The red solid lines and the dashed gray lines represent the medians and the 16th and 84th percentiles of each parameter, respectively.
Paper: Andromeda XXXV: The Faintest Dwarf Satellite of the Andromeda Galaxy
Authors: Jose Marco Arias, Eric F. Bell, Katya Gozman, In Sung Jang, Saxon Stockton, Oleg Y. Gnedin, Richard D'Souza, Antonela Monachesi, Jeremy Bailin, David Nidever, Roelof S. de Jong
Figure caption: Corner plots displaying the posterior distributions of the I-band luminosity function model for the RHB feature, including the apparent magnitude of the RHB (﹩{m}_{{I}_{0}}^{\,\rm{RHB}\,}﹩), its width (﹩{\sigma }_{{I}_{0}}^{\,\rm{RHB}\,}﹩), the number of candidate RHB stars (NRHB), and the exponential slope (B). The posterior distributions are based on over 10,000 MCMC iterations after burn-in. The red solid lines and the dashed gray lines represent the medians and the 16th and 84th percentiles of each parameter, respectively.
Paper: A Large Molecular Gas Reservoir in the Protocluster SPT2349−56 at z = 4.3
Authors: Dazhi Zhou, Scott C. Chapman, Nikolaus Sulzenauer, Ryley Hill, Manuel Aravena, Pablo Araya-Araya, Jared Cathey, Daniel P. Marrone, Kedar A. Phadke, Cassie Reuter, Manuel Solimano, Justin S. Spilker, Joaquin D. Vieira, David Vizgan, George C. P. Wang, Axel Weiss
Figure caption: ACA continuum map of the protocluster SPT2349−56 with moment-0 contours of CO(4–3) in the velocity window [−1373 km s−1, 1429 km s−1] before primary-beam correction. The white solid contours are [3, 6, 9, 12, 15, 18, 21]× the rms level of the CO emission from ACA observations. The dashed contours are  −2×  the rms level. The white dotted contours indicate [0.3, 0.5, 0.7, 0.9]×  the primary-beam response from the continuum map. The cyan dashed circle represents the main beam of the APEX [C II] observations. Green circles are the locations of all cataloged galaxies from R. Hill et al. (2020). We note that the two sources in the vicinity of “N1” are “NL2” and “N3,” which are not associated with the structure at z  =  4.3 (R. Hill et al. 2022).
Paper: A Large Molecular Gas Reservoir in the Protocluster SPT2349−56 at z = 4.3
Authors: Dazhi Zhou, Scott C. Chapman, Nikolaus Sulzenauer, Ryley Hill, Manuel Aravena, Pablo Araya-Araya, Jared Cathey, Daniel P. Marrone, Kedar A. Phadke, Cassie Reuter, Manuel Solimano, Justin S. Spilker, Joaquin D. Vieira, David Vizgan, George C. P. Wang, Axel Weiss
Figure caption: [C II] spectrum from APEX/FLASH observations (blue) compared to the scaled and coadded ALMA spectra of all individually detected protocluster members within the APEX beam (red). The difference is shown in black. For the purpose of this plot, we slightly smoothed the APEX spectrum with a low-pass Savitzky–Golay filter with a polynomial order of 1 to suppress the high-frequency noise. Since we use  ±800 km s−1 for the baseline subtraction, only the excluded channels (shaded) were used for calculating the integrated line strength. The excess in [C II] line strength from the APEX observations supports our ACA result.
Paper: A Large Molecular Gas Reservoir in the Protocluster SPT2349−56 at z = 4.3
Authors: Dazhi Zhou, Scott C. Chapman, Nikolaus Sulzenauer, Ryley Hill, Manuel Aravena, Pablo Araya-Araya, Jared Cathey, Daniel P. Marrone, Kedar A. Phadke, Cassie Reuter, Manuel Solimano, Justin S. Spilker, Joaquin D. Vieira, David Vizgan, George C. P. Wang, Axel Weiss
Figure caption: ACA 7 m spectra of CO(4–3) of the southern core and “N1” (blue). The red curves are the best-fit Gaussian profiles for determining the velocity ranges of the moment-0 maps, which are also indicated as the shaded regions. The ALMA 12 m results (obtained by coadding all individually detected galaxies) are shown in red, and the differences between the two measurements are shown in black for comparison. Compared to the ALMA 12 m results, the CO(4–3) line strengths are consistently higher in ACA 7 m observations.
Paper: A Large Molecular Gas Reservoir in the Protocluster SPT2349−56 at z = 4.3
Authors: Dazhi Zhou, Scott C. Chapman, Nikolaus Sulzenauer, Ryley Hill, Manuel Aravena, Pablo Araya-Araya, Jared Cathey, Daniel P. Marrone, Kedar A. Phadke, Cassie Reuter, Manuel Solimano, Justin S. Spilker, Joaquin D. Vieira, David Vizgan, George C. P. Wang, Axel Weiss
Figure caption: Amplitudes of CO(4–3) and 3.2 mm dust continuum of the southern core from the ALMA (red) and ACA (blue) observations in the visibility plane. The MRS of the ALMA 12 m observations is shown as black dashed lines. Visibilities show a good agreement at similar uv distance, which suggests that CO(4–3) excess in ACA observations is not caused by the absolute calibration uncertainty.
Paper: A Large Molecular Gas Reservoir in the Protocluster SPT2349−56 at z = 4.3
Authors: Dazhi Zhou, Scott C. Chapman, Nikolaus Sulzenauer, Ryley Hill, Manuel Aravena, Pablo Araya-Araya, Jared Cathey, Daniel P. Marrone, Kedar A. Phadke, Cassie Reuter, Manuel Solimano, Justin S. Spilker, Joaquin D. Vieira, David Vizgan, George C. P. Wang, Axel Weiss
Figure caption: Left: uv-coverage of ACA (blue) and ALMA (red) observations. Right: ACA CO(4–3) moment-0 map overlaid with tapered ALMA CO(4–3) moment-0 contours. Details and line styles are similar to Figure 1. The synthesized beams of ACA (white) and tapered ALMA (blue) are shown in the top left and top right.
Paper: A Large Molecular Gas Reservoir in the Protocluster SPT2349−56 at z = 4.3
Authors: Dazhi Zhou, Scott C. Chapman, Nikolaus Sulzenauer, Ryley Hill, Manuel Aravena, Pablo Araya-Araya, Jared Cathey, Daniel P. Marrone, Kedar A. Phadke, Cassie Reuter, Manuel Solimano, Justin S. Spilker, Joaquin D. Vieira, David Vizgan, George C. P. Wang, Axel Weiss
Figure caption: CO(4–3) spectra of core and “N1” from the tapered ALMA (red) compared to untapered ALMA (gray) and ACA (blue) data (top panels). The extra fluxes from the low-resolution results are plotted in the bottom panels. CO(4–3) excess is also shown in tapered ALMA data cube.
Paper: Spectropolarimetry of SN 2023ixf Reveals Both Circumstellar Material and an Aspherical Helium Core
Authors: Manisha Shrestha, Sabrina DeSoto, David J. Sand, G. Grant Williams, Jennifer L. Hoffman, Paul S. Smith, Callum McCall, Justyn R. Maund, Iain A. Steele, Klaas Wiersema, Jennifer E. Andrews, Nathan Smith, Christopher Bilinski, Peter Milne, Ramya M. Anche, K. Azalee Bostroem, Griffin Hosseinzadeh, Jeniveve Pearson, Douglas C. Leonard, Brian Hsu, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, M. J. Lundquist, Darshana Mehta, Nicolás Meza Retamal, Stefano Valenti, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Simplified cross-section sketch, with relative sizes not to scale, of the evolution of the CSM and ejecta geometry of SN 2023ixf based on our imaging and spectropolarimetric data. The background pink data points show the r-band apparent magnitude, and the black data points are imaging polarimetric data from Figure 2. The shape of the scattering regions has been exaggerated for better visual representation. Left: elongated CSM (gray region) surrounding the photosphere (orange) with a scattered vector with a (red) PA of 153﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9 for the observation 2–3 days after the explosion. During this phase, there is strong evidence of CSM interaction from the spectra and the light curve. Hence, electron scattering from disk-shaped CSM during this phase produces polarization of 1.02% (Section 3.2). Middle: our first spectropolarimetry data were taken +12.40 days after the explosion, featuring high continuum polarization and inverse P Cygni line features. The continuum polarization is now due to the expanding photosphere (orange), which was constrained by the early CSM but gradually became more spherical during the plateau phase as it swept away the CSM. The inverse P Cygni features are likely due to intervening material from the remnant CSM (gray region) (Section 3.3). Right: during the fall from the plateau, there is another increase in polarization, possibly due to the revealing of an asymmetric He core (red oval) with a different elongation than any earlier structure (Section 3.2).
Paper: Spectropolarimetry of SN 2023ixf Reveals Both Circumstellar Material and an Aspherical Helium Core
Authors: Manisha Shrestha, Sabrina DeSoto, David J. Sand, G. Grant Williams, Jennifer L. Hoffman, Paul S. Smith, Callum McCall, Justyn R. Maund, Iain A. Steele, Klaas Wiersema, Jennifer E. Andrews, Nathan Smith, Christopher Bilinski, Peter Milne, Ramya M. Anche, K. Azalee Bostroem, Griffin Hosseinzadeh, Jeniveve Pearson, Douglas C. Leonard, Brian Hsu, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, M. J. Lundquist, Darshana Mehta, Nicolás Meza Retamal, Stefano Valenti, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: SPOL data from +12.40 days to +17.41 days after the explosion. For each epoch, the top panel contains relative flux (black) and %p (red) values and the bottom panel is for the PA (blue), which is binned to 20 Å. Major H and He lines at rest wavelengths are overplotted. The light gray line in the %p panel is the maximum ISP estimate as discussed in Section 3. There is a clear continuum polarization in the first two epochs and gradual evolution toward the ISP (<0.35%) with time. The PA is fairly consistent for all the epochs presented here, as shown in Table 2. Finally, clear depolarizations are observed for some lines. The observed continuum polarization above the maximum ISP suggests some level of asphericity in the initial epoch of observation.
Paper: Spectropolarimetry of SN 2023ixf Reveals Both Circumstellar Material and an Aspherical Helium Core
Authors: Manisha Shrestha, Sabrina DeSoto, David J. Sand, G. Grant Williams, Jennifer L. Hoffman, Paul S. Smith, Callum McCall, Justyn R. Maund, Iain A. Steele, Klaas Wiersema, Jennifer E. Andrews, Nathan Smith, Christopher Bilinski, Peter Milne, Ramya M. Anche, K. Azalee Bostroem, Griffin Hosseinzadeh, Jeniveve Pearson, Douglas C. Leonard, Brian Hsu, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, M. J. Lundquist, Darshana Mehta, Nicolás Meza Retamal, Stefano Valenti, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Explosion energy of SNe 2012aw, 2017gmr, 2007aa, 2006ov, and 2004dj from T. Nagao et al. (2024, red) along with SN 2023ixf (black) with respect to tpol (as defined in Section 4). For SN 2023ixf the explosion energy has been estimated to be 1–2 × 1051 erg (D. Hiramatsu et al. 2023; A. Singh et al. 2024), hence we use the center of this range as our explosion energy value and the error bar spans these two values. The calculated value of SN 2023ixf follows the relation seen for other Type II SNe in the literature.