adsabs/AstroCLIMB huggingface dataset:
Paper: Photons’ Scattering in Relativistic Plasma with Velocity Shear: Generation of High Energy Power-law Spectra
Authors: Mukesh K. Vyas, Asaf Pe'er
Figure caption: Density distribution of individual photons over the angular location at the time of escape for p = 2.5, θ j = 0.01 rad, and Γ0 = 100. The distribution marks that most photons that form a high energy tail (above ε 1/ε 0 ∼ 2.5 × 103) escape from the inner region of the jet below θ j. The photons escaped from larger angles (θ > θ j) mostly contribute to the low energy potion of the emitted spectrum.
Paper: Photons’ Scattering in Relativistic Plasma with Velocity Shear: Generation of High Energy Power-law Spectra
Authors: Mukesh K. Vyas, Asaf Pe'er
Figure caption: Geometry of scattering in lab frame in spherical coordinates r, θ, ϕ. The origin lies at the center of the star; θ is the location of a certain scattering event of the photon with electron e 1 at r radial distance; θ + θ el is the angular location of the next scattering event with electron e 2; θ s and θ 2 are the scattering angles in the lab frame for both scattering events, respectively.
Paper: Constraints on Gamma-Ray Burst Models from GRB 221009A: GeV Gamma Rays versus High-energy Neutrinos
Authors: Ruo-Yu Liu, Hai-Ming Zhang, Xiang-Yu Wang
Figure caption: Upper limits of the baryon loading factor η  p  at different r diss and Γ. The left panel shows the constraint from IceCube’s observation while the right panel shows the constraint from Fermi Large Area Telescope’s (LAT) measurement.
Paper: Constraints on Gamma-Ray Burst Models from GRB 221009A: GeV Gamma Rays versus High-energy Neutrinos
Authors: Ruo-Yu Liu, Hai-Ming Zhang, Xiang-Yu Wang
Figure caption: The background subtracted light curves in 8.0–900.0 keV extracted from the TTE data, which use a 5 ms time bin. The blue solid line represents the Bayesian block light curve and the red dashed lines represent the minimum bin size of the obtained block.
Paper: Constraints on Gamma-Ray Burst Models from GRB 221009A: GeV Gamma Rays versus High-energy Neutrinos
Authors: Ruo-Yu Liu, Hai-Ming Zhang, Xiang-Yu Wang
Figure caption: The measured spectrum of LAT for GRB 221009A in 294–400 s (black points) and 4000.0–86400.0 s (blue points). The latter is multiplied by a factor of 1000 for visibility.
Paper: Photons’ Scattering in Relativistic Plasma with Velocity Shear: Generation of High Energy Power-law Spectra
Authors: Mukesh K. Vyas, Asaf Pe'er
Figure caption: Top panel: simulated spectrum for Γ0 = 300 and θ j = 0.01 rad and p = 2.5 (black solid curve). Other parameters are the same as Figure 3. Middle panel: same as the top panel but for p = 6.0. In both the panels, the blue dotted line is the best fit to the spectra at high energy producing simulated β. In the bottom panel, we plot the theoretical values of β as a function of p for Γ0 = 100 and 300 with blue solid and black dashed curves respectively and overplot the simulated values of β by blue star (Γ0 = 100) and black filled solid (Γ0 = 300).
Paper: Inner Habitable Zone Boundary for Eccentric Exoplanets
Authors: Xuan Ji, 璇 纪, Nora Bailey, Daniel Fabrycky, Edwin S. Kite, Jonathan H. Jiang, Dorian S. Abbot
Figure caption: Stellar flux and eccentricity of observed exoplanets with masses M < 8M ⊕ (NASA Exoplanet Science Institute 2020). S  a  is the stellar flux at the semimajor axis of the orbit and S ⋆ is the stellar flux of the IHZ for a circular orbit, for which we use the moist greenhouse limit from Kopparapu et al. (2013). The thick solid black curve represents the mean stellar flux limit on the IHZ. If S  a /S ⋆ is above this curve a planet is not habitable (Not Habitable). The dashed black curve represents the maximum stellar flux limit on the IHZ. If S  a /S ⋆ is lower than this limit, a planet will not experience a moist or runaway greenhouse (Safe from IHZ). For planets in the region in between the limits (Uncertain Zone), climate calculations involving the time evolution of the surface temperature are necessary to determine planetary habitability. The horizontal bars represent the uncertainties of the observed eccentricities.
Paper: Inner Habitable Zone Boundary for Eccentric Exoplanets
Authors: Xuan Ji, 璇 纪, Nora Bailey, Daniel Fabrycky, Edwin S. Kite, Jonathan H. Jiang, Dorian S. Abbot
Figure caption: Terms contributing to the effective heat capacity (upper) and the effective heat capacity of planets with different ocean depths (lower) as a function of temperature. Upper: The inset zooms in on the small difference between dry air, land, and a 1 m mixed layer. “Land” is calculated with the modern Earth’s orbital period and “Land around M” is calculated for an equivalent planet with a smaller orbital period orbiting an M dwarf (0.09M ⊙). The black star shows the observational effective global mean heat capacity of the modern Earth considering the measurements of heat content of ocean and the surface temperature changes in decades (Schwartz 2007). Lower: The red vertical lines mark the critical temperature for a moist greenhouse from Kopparapu et al. (2013) and the boiling point on Earth. The thinner black curves denote the the effective heat capacity of planets with ocean depths of 0.01, 0.1, and 0.5 m from left to right.
Paper: Inner Habitable Zone Boundary for Eccentric Exoplanets
Authors: Xuan Ji, 璇 纪, Nora Bailey, Daniel Fabrycky, Edwin S. Kite, Jonathan H. Jiang, Dorian S. Abbot
Figure caption: The same layout as Figure 1 but with the IHZ calculated assuming different surface conditions for planets in the uncertain zone. Top left: the effective heat capacity is assumed to be constant. Top right: the effective heat capacity includes potentially variable terms from land, ocean, dry atmosphere, water vapor, and latent heat. Bottom: The same simulations as shown in the top right panel but for different types of the host stars. S ⋆ and the function of albedo are adapted according to Kopparapu et al. (2013). Assuming a planet with an Earthlike atmosphere, it is always safe to apply the mean stellar flux limit for M dwarfs and K dwarfs because of shorter orbital periods.
Paper: Inner Habitable Zone Boundary for Eccentric Exoplanets
Authors: Xuan Ji, 璇 纪, Nora Bailey, Daniel Fabrycky, Edwin S. Kite, Jonathan H. Jiang, Dorian S. Abbot
Figure caption: The function defining the transition between the mean stellar flux limit and the maximum stellar flux limit g(Π); Equation (7) based on numerical integrations of the EBM assumes a constant heat capacity (left) and a variable heat capacity evaluated at 330 K (Equation (12)) and different stellar types, which affects the orbital period (right). The functional form given in Equation (7) fits the transition well with Π0 = 0.4 and Δ = 0.6.
Paper: Inner Habitable Zone Boundary for Eccentric Exoplanets
Authors: Xuan Ji, 璇 纪, Nora Bailey, Daniel Fabrycky, Edwin S. Kite, Jonathan H. Jiang, Dorian S. Abbot
Figure caption: Comparison of the IHZ (given in terms of semimajor axis) as a function of eccentricity for a land planet and a water-rich planet. We assume that the stellar flux of the circular IHZ is 1.7 times that of the modern Earth’s for the land planet (Abe et al. 2011) and 1.015 times that of the modern Earth’s for the water-rich planet (Kopparapu et al. 2013). We assume that the land planet follows the maximum stellar flux limit and the water-rich planet follows the mean stellar flux limit.
Paper: Highly Energetic Electrons Accelerated in Strong Solar Flares as a Preferred Driver of Sunquakes
Authors: H. Wu, Y. Dai, M. D. Ding
Figure caption: WL and X-ray observations of the 2012 October 23 X1.8 flare. (a) Time profiles of the HMI continuum intensity around 6173 Å (black), RHESSI HXR count rate at 50–100 keV (red), and GOES SXR flux in 1–8 Å (blue). (b) The base-difference HMI continuum map at the continuum peak time in an inverse scale, where the dashed box encloses the main flaring region used for continuum calculation. Overplotted on the map is a simultaneous RHESSI 50–100 keV image reconstructed using the Pixon algorithm, with contour levels corresponding to 30%, 60%, and 90% of the maximum intensity, respectively. For this sunquake-active flare, the location of the sunquake epicenter is also marked out with an asterisk sign.
Paper: Highly Energetic Electrons Accelerated in Strong Solar Flares as a Preferred Driver of Sunquakes
Authors: H. Wu, Y. Dai, M. D. Ding
Figure caption: Fitting results for the RHESSI spectra taken around the HXR peak in three flares. In each panel, the event number in Table 1 is labeled in the upper left, the black and gray lines in histogram mode denote the background-subtracted photon flux and the background, respectively, while the colored curves represent different components of the modeled spectrum based on the best-fit parameters. In addition, the residual between the modeled and observed spectra is plotted in the bottom part of each panel.
Paper: Highly Energetic Electrons Accelerated in Strong Solar Flares as a Preferred Driver of Sunquakes
Authors: H. Wu, Y. Dai, M. D. Ding
Figure caption: Locations of the MIs (orange plus yellow contours), HXR source (red contours), and sunquake epicenter (green asterisk) for two flares. In each panel the background image is a corresponding HMI continuum map, with the PIL drawn in blue line. The contours for MI indicate an increase of the horizontal magnetic field at levels of 300 G and 600 G, respectively. Note that the sunquake-related MI in panel (a) is highlighted in yellow contours.
Paper: Highly Energetic Electrons Accelerated in Strong Solar Flares as a Preferred Driver of Sunquakes
Authors: H. Wu, Y. Dai, M. D. Ding
Figure caption: Histograms of the total energy of nonthermal electrons for the flare events with (upper) and without (lower) sunquakes. The left panels are for the distributions of E 50 while the right are for E 300. Note that a bin size of 0.5 dex is adopted for the histogram plotting.
Paper: Can Neutron Star Mergers Alone Explain the r-process Enrichment of the Milky Way?
Authors: Chiaki Kobayashi, Ilya Mandel, Krzysztof Belczynski, Stephane Goriely, Thomas H. Janka, Oliver Just, Ashley J. Ruiter, Dany Vanbeveren, Matthias U. Kruckow, Max M. Briel, Jan J. Eldridge, Elizabeth Stanway
Figure caption: DTDs of NSMs and SNe Ia at low (left panel) and high (right panel) metallicities, calculated with various BPS codes. Metallicity independent (black dotted lines) and dependent (gray solid lines, Z = 0.002 and 0.02) t −1 power laws are also shown (see Section 3 for more details). (Upper panels) The adopted BPS models are from: Mennekens & Vanbeveren (2014, 2016; red lines, Z = 0.002 and 0.02, Model 2); Belczynski et al. (2002, 2020; green lines, Z = 0.001 and 0.02, M30 model); Kruckow et al. (2018; cyan lines, Z = 0.0002 and 0.0088); Eldridge & Stanway (2009), Briel et al. (2022; magenta lines, Z = 0.002 and 0.02); and Mandel et al. (2021, blue lines, Z = 0.0014 and 0.014). (Lower panels) The adopted BPS models with their preferred definitions of SNe Ia are from: Mennekens et al. (2010, 2012; red lines, SD and DD with M tot ≥ 1.4M ⊙, Model 22); Ruiter et al. (2009, 2014; green lines, SD (solid line), DD with M tot ≥ 0.9M ⊙ (dashed line), and He accreted double detonations (dotted–dashed line)); for ComBinE private communication based on Kruckow et al. (2018; cyan lines, DD only, with M tot > 1.36M ⊙ (solid lines) and M tot ≥ 0.86M ⊙ (dashed lines)), but with model “CE”; Eldridge & Stanway (2009). and Briel et al. (2022; magenta lines, SD and DD).
Paper: Can Neutron Star Mergers Alone Explain the r-process Enrichment of the Milky Way?
Authors: Chiaki Kobayashi, Ilya Mandel, Krzysztof Belczynski, Stephane Goriely, Thomas H. Janka, Oliver Just, Ashley J. Ruiter, Dany Vanbeveren, Matthias U. Kruckow, Max M. Briel, Jan J. Eldridge, Elizabeth Stanway
Figure caption: Evolution of elemental abundances in the solar neighborhood, including models of DTDs of SNe Ia and NSMs in Figure 1. The GCE code includes both SD and DD for SNe Ia, and both NS–NS and BH–NS for NSMs, unless noted below. The BPS models are taken from: Mennekens et al. (2012), Mennekens & Vanbeveren (2016, red short-dashed lines); Ruiter et al. (2014, also including He double detonations), Belczynski et al. (2020, green long-dashed lines); Kruckow et al. (2018, cyan dotted–short-dashed lines, DD only); Briel et al. (2022, magenta dotted lines, NS–NS only), and Mandel et al. (2021, blue dotted–long-dashed lines). The nucleosynthesis yields are from W14, the same as in K20. See K20 for the observational data sources. The asterisk indicates the star found by Yong et al. (2021b).
Paper: Can Neutron Star Mergers Alone Explain the r-process Enrichment of the Milky Way?
Authors: Chiaki Kobayashi, Ilya Mandel, Krzysztof Belczynski, Stephane Goriely, Thomas H. Janka, Oliver Just, Ashley J. Ruiter, Dany Vanbeveren, Matthias U. Kruckow, Max M. Briel, Jan J. Eldridge, Elizabeth Stanway
Figure caption: The same as Figure 2, but with a single t −1 power law (red short-dashed lines) and metallicity-dependent (green long-dashed lines) and mass-dependent (cyan dotted–dashed lines) t −1 power laws. The blue dotted lines also assume a metallicity-dependent f spin in addition to the mass-dependent DTDs. See the main text for the assumed DTDs and for the selected subset of SNe Ia and NSMs yields from Kobayashi et al. (2020b) and Just et al. (2015), respectively.
Paper: Can Neutron Star Mergers Alone Explain the r-process Enrichment of the Milky Way?
Authors: Chiaki Kobayashi, Ilya Mandel, Krzysztof Belczynski, Stephane Goriely, Thomas H. Janka, Oliver Just, Ashley J. Ruiter, Dany Vanbeveren, Matthias U. Kruckow, Max M. Briel, Jan J. Eldridge, Elizabeth Stanway
Figure caption: The same as Figure 2, but with mass-dependent yields from Just et al. (2015), using BPS of NSMs from Belczynski et al. (2020; magenta and red lines) and Mandel et al. (2021; cyan and blue lines). The SN Ia model is the same as in K20. See the main text for additional parameters.
Paper: Discovery of a Spatially and Kinematically Resolved 55 kpc Scale Superbubble Inflated by an Intermediate-redshift Non-BAL Quasar
Authors: Qinyuan Zhao, Junfeng Wang
Figure caption: Nonparametric measurements of HE 0238−1904. The maps are (a) flux intensity of [O III] (erg s−1 cm−2 arcsec−2), (b) median velocity (km s−1), (c) line width (W 80; km s−1), and (d) asymmetry (A). The maps were obtained by selecting only those spaxels with an S/N of the [O III] λ5007 line equal to or higher than 1.5. The red cross marks the position of the quasar. The PSF (0.″8) is depicted by the open circle in the lower left corner of panel (a).
Paper: Discovery of a Spatially and Kinematically Resolved 55 kpc Scale Superbubble Inflated by an Intermediate-redshift Non-BAL Quasar
Authors: Qinyuan Zhao, Junfeng Wang
Figure caption: We select 12 spatial positions to illustrate the [O III] velocity profile therein, including central (A and B) and outer (C–L) regions as shown in Figure 1. The median and zero velocity are marked by green dotted and gray dashed lines, respectively.
Paper: Discovery of a Spatially and Kinematically Resolved 55 kpc Scale Superbubble Inflated by an Intermediate-redshift Non-BAL Quasar
Authors: Qinyuan Zhao, Junfeng Wang
Figure caption: Radial dependence of W 80. Filled squares mark the mean of W 80 in 1.5 kpc bins using the original data with an S/N of [O III] higher than 5. Gray points show the original data with an S/N of [O III] higher than 5.
Paper: Discovery of a Spatially and Kinematically Resolved 55 kpc Scale Superbubble Inflated by an Intermediate-redshift Non-BAL Quasar
Authors: Qinyuan Zhao, Junfeng Wang
Figure caption: We select four spatial positions (Figure 1) to present the [O II] λ λ3737, 3729 doublet profiles. The observed spectra and fitted lines are in black and red, respectively, while the blue dotted lines are the Gaussian components. The electron density in region II is the upper limit in 3σ.
Paper: Discovery of a Spatially and Kinematically Resolved 55 kpc Scale Superbubble Inflated by an Intermediate-redshift Non-BAL Quasar
Authors: Qinyuan Zhao, Junfeng Wang
Figure caption: Left: spectra of the Hβ and [O III] doublet at three different regions (II–IV). The red line shows the best fit, and the black line shows the stacked spectra. Right: line ratio of [O III]/Hβ in three regions. The blue dashed line marks the typical [O III]/Hβ ratio. The ratio persists at a constant level (∼10) in these three regions.
Paper: Dusty-wind-clear JWST Super-early Galaxies
Authors: Fabrizio Fiore, Andrea Ferrara, Manuela Bischetti, Chiara Feruglio, Andrea Travascio
Figure caption: Left panel: dust UV optical depth vs. Eddington ratio (lower axis) and specific SFR (upper axis) for 134 galaxies at z > 6.5 in our sample. Filled circles are JWST-detected galaxy candidates from Bradley et al. (2022), Castellano et al. (2022), Curti et al. (2022), Finkelstein et al. (2022), Furtak et al. (2022), Harikane et al. (2022), Leethochawalit et al. (2023), Naidu et al. (2022), Topping et al. (2022), Trussler et al. (2022), and Whitler et al. (2022). Filled squares identify candidates from Rodighiero et al. (2022) and filled pentagons from Barrufet et al. (2022). Starred symbols are four sources from Furtak et al. (2022) and Bradley et al. (2022) for which the authors claim a Balmer break with ﹩{ \mathcal D }(4000)\gt 2\mbox{--}3﹩. Open squares are REBELS sources from Bouwens et al. (2022), open hexagons are REBELS sources with τ 1500 estimated by Ferrara et al. (2022), and open triangles are Lyα emitters from Endsley et al. (2021). The solid line is the best-fit power law ﹩{\tau }_{1500}\propto {\lambda }_{E}^{-0.63};﹩ also shown is the adopted functional form for ﹩{\lambda }_{E}^{\mathrm{eff}}﹩ (red dashed), the range of likely values (dark green), and the outflow region (light and dark green). Right: fraction of galaxies with τ 1500 > 0.4 vs. Eddington ratio for our sample.
Paper: Dusty-wind-clear JWST Super-early Galaxies
Authors: Fabrizio Fiore, Andrea Ferrara, Manuela Bischetti, Chiara Feruglio, Andrea Travascio
Figure caption: Left panel: redshift evolution of the Eddington parameter for the galaxies in the sample. Points are the same as in Figure 2. The solid line is the best-fit power law, λ  E  ∝ (1 + z)2.1. The red dashed line marks the optically thin value of ﹩{\lambda }_{E}^{\mathrm{eff}}﹩ and the dark green region its most likely values. Right: fraction of galaxies satisfying the outflow condition ﹩{\lambda }_{E}\gt {\lambda }_{E}^{\mathrm{eff}}﹩ vs. redshift.
Paper: Dusty-wind-clear JWST Super-early Galaxies
Authors: Fabrizio Fiore, Andrea Ferrara, Manuela Bischetti, Chiara Feruglio, Andrea Travascio
Figure caption: Stellar mass, M *; Eddington ratio, λ  E ; and UV dust optical depth, τ 1500; from normalized cumulative (black curves) and differential (red points) distributions for our galaxy sample.
Paper: The Luminous Type Ia Supernova 2022ilv and Its Early Excess Emission
Authors: Shubham Srivastav, S. J. Smartt, M. E. Huber, G. Dimitriadis, K. C. Chambers, Michael D. Fulton, Thomas Moore, F. P. Callan, James H. Gillanders, K. Maguire, M. Nicholl, Luke J. Shingles, S. A. Sim, K. W. Smith, J. P. Anderson, Thomas de Boer, Ting-Wan Chen, Hua Gao, D. R. Young
Figure caption: Top panel: ATLAS o-band absolute magnitude light curve of SN 2022ilv, with the synthetic o-band Piro (2015) model for the interaction-powered early excess and a power-law fit to the radioactively driven subsequent rise. The composite model (sum of the two) is shown as a dashed line. A SNEC-based CSM model (EEx) computed by Jiang et al. (2021) to explain the short-lived early excess emission observed in SN 2020hvf is shown for comparison. Bottom panel: the Tomo-e (clear filter) light curve of SN 2020hvf from Jiang et al. (2021), along with our ATLAS photometry that enhances the sampling of the published pulse. Inset: a zoomed-in plot showing a comparison of the early excess feature in SN 2022ilv and SN 2020hvf. Since SN 2020hvf has a longer rise time, the light curve of SN 2022ilv was shifted by ≈1 day to match with SN 2020hvf.
Paper: The Luminous Type Ia Supernova 2022ilv and Its Early Excess Emission
Authors: Shubham Srivastav, S. J. Smartt, M. E. Huber, G. Dimitriadis, K. C. Chambers, Michael D. Fulton, Thomas Moore, F. P. Callan, James H. Gillanders, K. Maguire, M. Nicholl, Luke J. Shingles, S. A. Sim, K. W. Smith, J. P. Anderson, Thomas de Boer, Ting-Wan Chen, Hua Gao, D. R. Young
Figure caption: ATLAS and Pan-STARRS1 images for the field of SN 2022ilv. Top row (left to right): median-combined ATLAS input images on MJDs 59689.38, 59690.52, and 59691.26 and the reference ATLAS template used for the subtraction. Middle row: median-combined ATLAS difference images on MJDs 59689.38, 59690.52, and 59691.26 and the deep Pan-STARRS1 w-band stack with an effective exposure time of 7800 s. Bottom row: median-combined ATLAS input image on MJD 59689.38 and the Pan-STARRS1 reference stack. The SN position is marked by the cross-hairs. Two sources closest to the SN position are marked. Source 1 is a foreground star, and source 2 is a galaxy at z ≈ 0.11, and thus ruled out as a host galaxy candidate for SN 2022ilv.
Paper: Saturation of the Filamentation Instability and Dispersion Measure of Fast Radio Bursts
Authors: Emanuele Sobacchi, Yuri Lyubarsky, Andrei M. Beloborodov, Lorenzo Sironi, Masanori Iwamoto
Figure caption: Sketch of the electromagnetic vector potential a (solid) and particle number density n (dashed) in the plane perpendicular to the direction of propagation of the wave. The magnetic field of the magnetar wind is directed along x. We consider a cold plasma with β s ≪ a 0 and large wave frequencies ω 0 ≫ ω P/a 0.
Paper: The Luminous Type Ia Supernova 2022ilv and Its Early Excess Emission
Authors: Shubham Srivastav, S. J. Smartt, M. E. Huber, G. Dimitriadis, K. C. Chambers, Michael D. Fulton, Thomas Moore, F. P. Callan, James H. Gillanders, K. Maguire, M. Nicholl, Luke J. Shingles, S. A. Sim, K. W. Smith, J. P. Anderson, Thomas de Boer, Ting-Wan Chen, Hua Gao, D. R. Young
Figure caption: Our LT spectra (with SPRAT) of SN 2022ilv and SN 2020hvf (this work), plotted with the spectra of SN 2009dc (Taubenberger et al. 2011) at similar epochs for comparison. The spectra of SN 2022ilv and SN 2020hvf will be made available on the Weizmann Interactive Supernova Data Repository (WISeREP; Yaron & Gal-Yam 2012).
Paper: The Luminous Type Ia Supernova 2022ilv and Its Early Excess Emission
Authors: Shubham Srivastav, S. J. Smartt, M. E. Huber, G. Dimitriadis, K. C. Chambers, Michael D. Fulton, Thomas Moore, F. P. Callan, James H. Gillanders, K. Maguire, M. Nicholl, Luke J. Shingles, S. A. Sim, K. W. Smith, J. P. Anderson, Thomas de Boer, Ting-Wan Chen, Hua Gao, D. R. Young
Figure caption: Multiband light-curve evolution of SN 2022ilv (colored symbols), compared to SN 2020hvf (this work) and the luminous SN 2009dc (Silverman et al. 2011; Taubenberger et al. 2011). The absolute magnitudes for SN 2022ilv were computed for the assumed distance of 114 Mpc (corresponding to z = 0.026). The shaded regions represent the range of absolute magnitudes for a distance range of 91–136 Mpc. Inset for the o-band light curve (middle right panel) shows the early excess detected by ATLAS. All magnitudes are in the AB system.
Paper: The Luminous Type Ia Supernova 2022ilv and Its Early Excess Emission
Authors: Shubham Srivastav, S. J. Smartt, M. E. Huber, G. Dimitriadis, K. C. Chambers, Michael D. Fulton, Thomas Moore, F. P. Callan, James H. Gillanders, K. Maguire, M. Nicholl, Luke J. Shingles, S. A. Sim, K. W. Smith, J. P. Anderson, Thomas de Boer, Ting-Wan Chen, Hua Gao, D. R. Young
Figure caption: Bolometric light curves of SN 2022ilv (1600–23500 Å), SN 2020hvf (1600–19000 Å), and SN 2009dc (1600–23500 Å). The shaded region represents the luminosity range for SN 2022ilv given the uncertainty in the distance. Inset shows the fractional flux contribution from optical, UV, and NIR bands to the total bolometric flux of SN 2009dc. Dashed lines represent the best-fitting Arnett models for each SN.