adsabs/AstroCLIMB huggingface dataset:
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: SPH simulation of a BdHN I: model “30m1p1eb” of Table 2 in Becerra et al. (2019). The binary progenitor comprises a CO star of ≈9M ⊙ (produced by a ZAMS star of 30M ⊙) and a 2M ⊙ NS companion. The orbital period is ﹩\approx 6\,\min ﹩. From left to right, each snapshot corresponds to selected increasing times where t = 0 s refers to the SN shock breakout. The upper and lower panel shows the mass density on the equatorial plane and the plane orthogonal to the latter. The reference system is rotated and translated to align the x-axis with the line joining the binary components. The origin of the reference system is located at the NS companion position. In the first snapshot at t = 40 s, particles in the NS gravitational capture region form a tail behind the NS companion. These particles then circularize around the NS, forming a thick disk visible in the second snapshot at t = 80 s. Part of the ejecta produces a fallback accretion process onto the νNS visible in the third snapshot at t = 171 s. At t = 337 s (about one orbital period), a disk structure is visible around the νNS and the NS companion. This figure has been produced with the SNsplash visualization program (Price 2011). The figure highlights that the νNS is coeval with the SN explosion and remains at the SN center while the ejecta expands. It also shows that the timescale of the physical phenomena leading to the transient activity of the GRB (e.g., the hypercritical accretion and its consequences) is shorter than the timescale of changes in the orbital properties, e.g., an orbital widening or eventual binary disruption owing to mass loss (Blaauw 1961; van den Heuvel & Heise 1972; Fryer et al. 2015).
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: Perturbation functions of a population fit to GWTC-3 when using LVK-released posterior samples for each event (orange), and when using posterior samples simulated by GWMockCat (blue and green). Shaded bands correspond to 90% credible intervals, and solid lines are the medians. The two sets of figures correspond to two selection criteria, one which is analogous to the one used for mock catalogs in this work (S/N >8, top two panels), and one which is identical to that used for the LVK analysis (FAR<1yr−1, bottom two panels). The main difference between the selection criteria is that they result in catalog sizes that are different by nearly a factor of 2, and therefore, the statistical error on the perturbation function is noticeably different between them. Using the same number of events in the simulated catalog as the LVK-released catalog results in a perturbation function that is similar in amplitude to the LVK-released population analysis. We conclude that the prescriptions used in GWMockCat are sufficient for the purposes of population analyses. We use the green curves in the bottom two panels for the analysis presented in the body of this paper, and the orange curves in the bottom two panels for the analysis presented in this appendix.
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: Isotropic-equivalent energy (E  γ,iso) of GRB vs. the peak time of luminosity of the bolometric light curve of the associated SN (﹩{t}_{{\rm{P}},\mathrm{SN}}﹩). The plot shows the lack of correlation: the SN peaking times (in the rest frame) stay within an order of magnitude spread, while the GRB energy spans ∼6 orders of magnitude.
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: GRB redshifts (z) vs. the values of peak luminosity of the bolometric light curve of the associated SN (﹩{L}_{{\rm{P}},\mathrm{SN}}﹩). The plot shows the spread in data points and the lack of correlation between these two quantities.
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: Isotropic-equivalent energy (E  γ,iso) of GRB vs. the peak luminosity of the bolometric light curve of the associated SN (﹩{L}_{{\rm{P}},\mathrm{SN}}﹩). The plot shows the lack of correlation: the SN luminosities stay within an order of magnitude spread, while the GRB energy spans ∼6 orders of magnitude.
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: GRB redshifts (z) vs. the peak time of luminosity of the bolometric light curve of the associated SN (﹩{t}_{{\rm{P}},\mathrm{SN}}﹩). The plot shows the lack of correlation between these two quantities.
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: Mock posteriors simulated with GWMockCat (red) compared to posteriors made with full parameter estimation as released by the LVK (blue) for the event GW191215_223052. The two sets of posterior samples appear consistent to the level needed for a population analysis.
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: A corner plot of the inferred hyperposterior from a fit to a mock catalog with 345 events. The injected values are shown in orange. The recovered hyperposterior is consistent with the injected population.
Paper: An Updated Reference Frame for the Galactic Inner Parsec
Authors: Jeremy Darling, Jennie Paine, Mark J. Reid, Karl M. Menten, Shoko Sakai, Andrea Ghez
Figure caption:                         Locations in epoch 2022.227 and proper motions of the stellar SiO masers used for the Galactic center astrometric reference frame (Table 2 and Figure 3). The color indicates the sign of the stellar radial velocities (red is positive; blue is negative). The gray circle marks Sgr A* (not to scale). Projected distances assume a Galactic center distance of 8.2 kpc, and the R.A. offset is corrected for decl.
Paper: An Updated Reference Frame for the Galactic Inner Parsec
Authors: Jeremy Darling, Jennie Paine, Mark J. Reid, Karl M. Menten, Shoko Sakai, Andrea Ghez
Figure caption: Composite spatially integrated SiO v = 1, J = 1 − 0 maser spectra from the 2022.227 epoch image cubes. The colors indicate the projected distance from Sgr A*, assuming a Galactic center distance of 8.2 kpc.
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: The UV emission-line ratios measured in Pox 186 (blue star), literature SF galaxies (circles, various colors with limits indicated by black dots with arrows of the same color), and photoionization models from BOND (lightly colored squares) and nonequilibrium models (gray triangles). The photoionization models are selected to have metallicity and log(U) similar to that of Pox 186. Panel (a): log(C IV/O III]) vs. log(C IV/C III]); panel (b): log(O III]/He II) vs. log(C III]/He II). Panel (b) can distinguish between stellar ionizing sources (ratios in the area noted by blue arrows) and AGNs (noted by green arrows). Two SF galaxies discussed in Section 4.2.2 are highlighted with cyan borders.
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: SPS results for Pox 186. Top row: full spectrum after correction for Galactic and Pox 186 Lyα absorption. The spectrum is normalized between 1256 and 1268 Å, the regions used for fitting are highlighted in green, and the best-fit model continuum is provided in cyan. Middle row: two stellar wind features, N V (left) and O V (right), are highlighted. These are sensitive to the age of the stellar population. Bottom row: the fraction of each model in the best-fit continuum, where model ages are plotted on the x-axis and model metallicities are provided in different colors. The best-fit age, metallicity, and E(B−V) are given in this panel.
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: The Pox 186 [O III]λ5007 (left) and He II λ4686 (right) spatial distributions obtained from the GMOS IFU data. The magenta extraction profile matches the 2.″5 diameter of the COS beam, while the cyan profile mirrors the narrower, un-vignetted 1.″25 diameter beam. The [O III]λ5007 emission fills the narrow beam and extends into the full 2.″5 aperture while the He II emission is compact.
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: The optical line ratios log(He II λ4686/Hβ) vs. log([O III]λ5007/Hβ). For Pox 186, the black and pink star represent the Guseva et al. (2004) MMT and 3.6 m ESO spectra, respectively, while the blue star indicates the ratios measured from the GMOS IFU spectrum. The optical ratios from literature SF galaxies appear as colored circles and limits. Top panel: the same BOND photoionization models used in Figure 7, excluding the 5 and 6 Myr models. Bottom panel: the metallicity range of the photoionization models is increased and no limits are placed on log(U).
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: log(O III]/He II) vs. log(C III]/He II) with the same data as panel (b) of Figure 7, except the BOND photoionization model line ratios are color-coded by SED age. The model line ratios cover age ranges from 1–3 Myr (left panel) and 4–6 Myr (right panel).
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: Portions of the G130M spectrum containing the Galactic, geocoronal, and Pox 186 Lyα profiles. Top: spectrum (black), the Galactic Lyα absorption profile determined from Galactic extinction (blue), and the Pox 186 Lyα profile (green) determined from the areas of the spectrum free from other spectral features (red). The combination of Galactic and Pox 186 Lyα absorption is shown in orange. Geocoronal Lyα is grayed out. Bottom: the spectrum with the composite Lyα profile removed.
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: Low-ionization state absorption features present in Pox 186. Top: Si II 1260 Å (green). The flux is normalized based on the continuum neighboring the absorption line. The fit to the absorption profile is provided in orange. Bottom: the C II 1334 Å absorption profile and fit.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: Initial magnetic fields for the cartesian simulations (left) and the axisymmetric simulations (right), with magnetic field lines in black. These are PFSS fields with the lower radial boundary conditions as in Equations (15) and (16). In the axisymmetric simulations, the computational domain only covers one hemisphere, and the other is only plotted here for illustrative purposes.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Top panel: snapshots of the radial distribution of particle number density of bound disk material (solid curves) and the outflowing photoevaporation wind (dashed curves; see Equation (53)) for our fiducial model. For the disk material, we show a spherically averaged density defined according to ﹩\overline{\rho }\equiv {\rm{\Sigma }}\,\pi {r}^{2}/(4\pi {r}^{3}/3)﹩, where ﹩n\equiv \overline{\rho }/{m}_{p}﹩ and m  p  is the proton mass. The density profile obtained by modeling the radio/millimeter emission of AT2018cow (Margutti et al. 2019) is shown with green stars. Bottom panel: snapshots of the optical depth (Equation (54)) to UV/optical wavelengths external to a given radius r due to scattering off of spherical dust grains of size a ≈ 1 μm and assumed opacity κ UV = 200 cm2 g−1. Shown for comparison with vertical dashed lines are the photoevaporation radius R  g  (Equation (29); black) and the dust sublimation radius (Equation (55); magenta). Dust grains are formed roughly exterior to R  s , so the optical depth profiles begin at r = R  s .
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Effect of varying parameters of the model about their fiducial values on the cumulative change of the binary separation Δa bin (solid lines; left axes) and cumulative wind mass loss M w (dashed lines; right axes). For comparison, we show the thermal time (Equation (13); vertical dashed line) and an approximate range of nuclear times (gray shaded region) of the core.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Top panel: fractional change in binary semimajor axis a bin,0 at t ≈ 105 yr due to accretion-driven binary migration during the CBD phase. Results are shown for the fiducial model (Table 1), varying f m (hence the initial disk mass M d,0) and the binary–CBD torque coupling efficiency χ. We terminate our simulations when a bin = 2.5 R ⊙ is achieved, which is roughly the RLOF radius for a He core of radius R  c  ≈ R ⊙ and q = 1. The models with f m = 1 and χ = −3 and χ = −2 reach this final orbital separation by t ≈ 105 Bottom panel: corresponding change in the effective value of the CE efficiency parameter λ α CE (Equation (49)) compared to the value λ α CE,0 at the immediate post-CE phase (black, dotted line).
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Comparison of timescales relevant to the mass-transfer evolution of the post-CE binary as a function of elapsed time since CBD formation (blue line) for our fiducial model. A green line shows the timescale for gravitational-wave-driven inspiral, while ﹩{t}_{\dot{a},\mathrm{CBD}}\equiv {a}_{\mathrm{bin}}/{\dot{a}}_{\mathrm{bin}}﹩ shows the rate of binary shrinkage due to interaction with the CBD. If the He core begins mass transfer onto the BH/NS companion at early times when ﹩{t}_{\dot{a},\mathrm{CBD}}\lt {t}_{\mathrm{KH}},{t}_{\mathrm{nuc}}﹩, angular momentum loss to the CBD could substantially accelerate the mass-transfer rate of the binary relative to the CBD-free case, potentially affecting its dynamical stability and leading to tidal disruption of the He core.
Paper: Constraining Thermal Emission of Pluto’s Haze from Infrared Rotational Lightcurves
Authors: Linfeng Wan, 霖丰 万, Xi Zhang, Jason D. Hofgartner
Figure caption: Rotational emission lightcurves of Pluto and Charon from our best-fit models (lines) and observations (dots) at Spitzer 24 and 70 μm (first two columns), Herschel 70 μm (third column). Contributions from Pluto’s different components are separately plotted for the “free retrieval” scenario with haze (upper panel) and “surface only” scenario (lower panel).
Paper: Constraining Thermal Emission of Pluto’s Haze from Infrared Rotational Lightcurves
Authors: Linfeng Wan, 霖丰 万, Xi Zhang, Jason D. Hofgartner
Figure caption: Surface maps of Pluto and Charon derived from New Horizons observations. Part of the southern hemispheres was in winter darkness (polar night) during the flyby, and thus the albedo distributions are not well determined south of ∼ −33°. (a) Map of Pluto’s bolometric hemispherical albedo from Hofgartner et al. (2023). (b) Histogram of Pluto’s albedo distribution, where local minima of 0.36 and 0.82 are adopted as unit boundaries. (c) The distribution of different albedo units on Pluto’s surface. (d) Map of Charon’s albedo from Buratti et al. (2017). Note that, Charon rotates synchronously with Pluto and their lit hemispheres exhibit a 180° difference in longitude.
Paper: Constraining Thermal Emission of Pluto’s Haze from Infrared Rotational Lightcurves
Authors: Linfeng Wan, 霖丰 万, Xi Zhang, Jason D. Hofgartner
Figure caption: Rotational emission lightcurves of Pluto and Charon simulated for the JWST observations at 18, 21, and 25.5 μm. Results of the “free retrieval” scenario with haze (upper panel) and the “surface only” scenario without haze (lower panel) are plotted with contributions from different geologic units and haze on Pluto and the surface of Charon. The haze emission fluxes at multiple wavelengths are calculated using the atmospheric model from Zhang et al. (2017) assuming Titan-like tholins.
Paper: Constraining Thermal Emission of Pluto’s Haze from Infrared Rotational Lightcurves
Authors: Linfeng Wan, 霖丰 万, Xi Zhang, Jason D. Hofgartner
Figure caption: The posterior distribution of retrieved parameters for the “free retrieval” scenario with haze (red) and “surface only” scenario without haze (cyan), including 24 μm haze flux F haze (mJy), CH4 ice emissivity ϵ, thermal inertia Γ (MKS) for both Pluto and Charon. Vertical dashed lines in the diagonal panels denote the 2.5%, 50%, and 97.5% quantiles of the distributions. Off-diagonal panels show the two-dimensional parameter covariance plots, indicating a strong negative correlation between the haze flux and Charon’s thermal inertia (lower-left panel).
Paper: Constraining Thermal Emission of Pluto’s Haze from Infrared Rotational Lightcurves
Authors: Linfeng Wan, 霖丰 万, Xi Zhang, Jason D. Hofgartner
Figure caption: Variation of rotational emission lightcurves (in units of microjansky) simulated for JWST’s observations at 18, 21, and 25.5 μm. Results of the “free retrieval” scenario with haze (upper panel) and the “surface only” scenario without haze (lower panel) are plotted. Dashed lines indicate the 10σ faint-source detection limits in a 104 s integration for corresponding channels of the JWST/MIRI.
Paper: Constraining Thermal Emission of Pluto’s Haze from Infrared Rotational Lightcurves
Authors: Linfeng Wan, 霖丰 万, Xi Zhang, Jason D. Hofgartner
Figure caption: Comparison of Pluto’s rotational lightcurves from the orbit-rotating model (blue) and self-rotating model (orange) at 24 μm. Their difference (green) is less than 5% of the total emission flux in 2003 and smaller than 1% in 2017 and 2031.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Top panel: MW (green circles) and SE SN (blue diamonds) reddenings against their respective Na I D EWs measured from SE SN spectra. The blue solid line is the E  B−V  vs. EWNaID relation for SE SNe, while dashed lines are the ﹩\pm 1\,\hat{\sigma }﹩ limits. Bottom panel: similar to the top panel but for SNe II instead of SE SNe. The red line and the gray region are the relation between MW reddening and EWNaID reported by Poznanski et al. (2012) and its ﹩\pm 1\,\hat{\sigma }﹩ region, respectively. Orange squares are the MW reddenings and EWNaID values for the QSO sample of Poznanski et al. (2012). Error bars are 1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Left: ﹩\hat{\sigma }﹩ values of the ﹩\mathrm{log}{M}_{\mathrm{Ni}}^{\mathrm{tail}}﹩ estimates calculated with ﹩{f}_{\mathrm{dep}}^{{\rm{S}}\&{\rm{K}}}﹩ against those computed with ﹩{f}_{\mathrm{dep}}^{{\rm{C}}\&{\rm{W}}}﹩ for 39 SNe with n > 1. The solid line is a one-to-one correspondence. Right: ratios of the 56Ni masses estimated with ﹩{f}_{\mathrm{dep}}^{{\rm{S}}\&{\rm{K}}}﹩ to those computed with ﹩{f}_{\mathrm{dep}}^{{\rm{C}}\&{\rm{W}}}﹩ against n. The solid line is the median value and dotted lines are ﹩\pm 1\hat{\sigma }﹩ limits. The dashed line is ﹩{f}_{\mathrm{dep}}^{{\rm{C}}\&{\rm{W}}}/{f}_{\mathrm{dep}}^{{\rm{S}}\&{\rm{K}}}﹩ with t esc/t = 1.37 for ﹩{f}_{\mathrm{dep}}^{{\rm{C}}\&{\rm{W}}}﹩ and t esc/t = 1.22 for ﹩{f}_{\mathrm{dep}}^{{\rm{S}}\&{\rm{K}}}﹩.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Ratios of the 56Ni masses estimated with different methods in the literature to our recalibrated ﹩{M}_{\mathrm{Ni}}^{\mathrm{tail}}﹩ values against peak time. Solid lines are median values, dashed lines are ﹩\pm 1\,\hat{\sigma }﹩ limits, and error bars are 1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption:                       ﹩{A}_{V}^{{\rm{h}}}/{E}_{B-V}﹩ (top panels), ﹩{K}_{V}^{s}/z﹩ (middle panels), and ﹩{A}_{V}^{\mathrm{MW}}/{E}_{B-V}^{\mathrm{MW}}﹩ (bottom panels) as a function of (B − V)0 for SNe IIb (left panels), Ib (middle panels), and Ic (right panels) at times before (blue circles) and after (red squares) the maximum of the B − V color. Solid lines are straight line fits, while dashed lines are the ﹩1\,\hat{\sigma }﹩ limits around the fits.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Continuum normalized spectra of SN 2004gq around the host galaxy Na I D line (thin colored lines) and the corresponding weighted-average spectrum (thick line). The thick red line indicates the line region, and vertical error bars are 1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption:  56Ni mass distribution for each SN subtype. Dashed and dotted lines indicate mean and median 56Ni mass values, respectively. The four SN Ic events with 56Ni masses between 0.45 and 0.70 M ⊙ are not shown for clarity. For comparison, we include the distribution for the SN II sample of Rodríguez et al. (2021).
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Top and middle rows: shapes of the magnitude transformation between Sloan and ZTF systems for SNe IIb (blue circles), Ib (green squares), and Ic (red diamonds). Solid lines are the best fits to the data, while dashed lines are the ﹩1\hat{\sigma }﹩ limits around the fits. Bottom panels: cumulative distributions for the zero-points of the g − g ZTF (left panel) and r − r ZTF (right panel) calibrations.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Cumulative distributions for the ﹩{M}_{r}^{\mathrm{peak}}﹩ values in the volume-limited (solid lines) and NVL (dotted lines) samples.