adsabs/AstroCLIMB huggingface dataset:
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: Spectrum during the impulsive phase of the 2021 September 8 flare (17:24-17:25 UTC) fitted with two different isothermal models considering only part of the spectrum. The spectrum below 4 keV (blue shaded interval) is fitted to obtain the best-fit model shown in blue and a fit to the spectrum above 4 keV (red shaded interval) gives the best-fit model shown in red.
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: XSM light curves in different energy bands for the three C-class flares on 2020 October 16 (a), 2021 October 7 (b), and 2021 September 8 (c). GOES XRS 1–8 Å band flux is shown in gray. All light curves are at 1 minute cadence. The y-range is selected such that the points shown have at least 2σ detection. The derivative of the XSM 1–15 keV count rate is shown with a black dashed line and the vertical black dashed line denotes the peak of the impulsive phase where the derivative is maximum. The blue vertical dotted line corresponds to the peak of the 1–15 keV light curve.
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: Results of an isothermal fit to the time-resolved spectra of the three flares. Best-fit temperature and emission measure with 1σ uncertainties are shown in the top and middle panels. Lower panels show the reduced chi-squared of the spectral fits. Impulsive phase peak times are marked by the vertical dashed lines. For the two brighter events, the reduced chi-squared is seen to be higher around the impulsive peak, marked by the gray-shaded region.
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: XSM spectra of the three flares (panel a: C1.57, panel b: C5.70, panel c: C8.40) at their impulsive phase peak (marked by vertical dashed lines in Figure 1) fitted with an isothermal model. Orange lines show the best-fit models and the lower panels show the residuals.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Light curves of TXS 0506+056 showing nonsimultaneous infrared and γ-ray flares. The top panel is the infrared light curve from WISE multiepoch data, and the middle panel is the Fermi γ-ray light curve analyzed with the Fermi Science Tool. The bottom panel represents the flaring periods in infrared (blue thick lines) and γ-ray (red thick lines), as well as the simultaneous flaring stages (green lines). Black lines represent the arrival time of IceCube-170922A.
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: (a) XSM spectrum of the impulsive peak of the 2021 September 8 flare fitted with different multithermal and isothermal models. The best fit with each model is shown in different colors and the residuals are shown in the lower panels. (b) The best-fit DEM models from the spectral fit in panel a are shown with the respective colors. Lighter color lines correspond to DEMs from 100 random samples from the MCMC analysis showing the uncertainty of the derived DEM models.
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: Differential Emission Measure (DEM) evolution during the 2021 September 8 flare (a) and the 2021 October 7 flare (b) obtained from spectral fitting. The top three panels show DEM with two-temperature, Gaussian, and double Gaussian models, respectively. Color represents the EM in units of 1046cm−3MK−1. The isothermal temperature measurements (purple solid line) and 1–15 keV X-ray light curves (dashed line) are also shown for reference. The reduced chi-squared of the fit with two-temperature (green), Gaussian (red), and double Gaussian (purple) are shown in the lowermost panels. The reduced chi-squared for the isothermal fit is shown in orange for comparison. Intervals when the isothermal and multithermal models have a similar fit to the spectra are grayed out and during the remaining period in the impulsive phase, the DEM models provide a much better fit to the spectra in comparison with the isothermal model.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Examples of CFS light curves with J0739+0137. The top panel is the infrared light curve from WISE multiepoch data, and the middle panel is the γ-ray aperture light curve from Fermi-LAT. The bottom panel represents the flaring periods in infrared (blue thick lines) and γ-ray (red thick lines), as well as the simultaneous flaring stages (green lines).
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: Panel a shows the temperature and emission measure of the 2021 September 8 flare. The red line is interpolated values from the measurements at 1 minute. The spectrum for the gray-shaded interval (17:24-17:25) is shown in panel b with blue data points. Isothermal models corresponding to the interpolated temperature and EM for every 1 s within the interval are shown with light orange lines and the average model considering the variation of temperature and EM is shown by a solid orange line. Residuals of the observed spectrum with this average model (solid orange line in the upper panel) are shown in the lower panel.
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: Panel a shows the temperature response of the XSM in 1 keV energy bins from 1 to 15 keV in sequence while panel b has normalized temperature responses of selected energy channels near the Si line complex. Simulated XSM spectra near the Si and Fe line complexes at different temperatures are shown in panels c and d, respectively.
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: Measured abundances of Mg, Si, and Fe during the 2021 September 8 flare obtained from spectral fitting considering three different multithermal models: two-temperature (green), Gaussian (red), and double Gaussian (purple), are shown. Coronal abundances from Feldman (1992) and Del Zanna (2013) as well as photospheric abundances from Asplund et al. (2009) are shown with purple, gray, and yellow dashed lines, respectively. The X-ray light curve is shown in gray for reference.
Paper: Soft X-Ray Spectral Diagnostics of Multithermal Plasma in Solar Flares with Chandrayaan-2 XSM
Authors: N. P. S. Mithun, Santosh V. Vadawale, Giulio Del Zanna, Yamini K. Rao, Bhuwan Joshi, Aveek Sarkar, Biswajit Mondal, P. Janardhan, Anil Bhardwaj, Helen E. Mason
Figure caption: EM loci curves obtained from the XSM spectrum during the impulsive peak of the 2021 September 8 flare. Each line corresponds to the ratio of the observed counts in the given energy range to the counts predicted by the model for an isothermal plasma with an EM of 1 cm−3 at different temperatures. The width of the lines takes into account the 1σ uncertainties of the observed counts. The best-fit isothermal temperature and emission measure are shown by the black star.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Azimuthally averaged 450 μm rms noise for the 10 clusters vs. radius. Note that the two clusters A2744 (green curve) and MACSJ2129 (gray curve) have shallower observations than the remaining eight clusters (see Table 1).
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: 450–850 μm flux ratio vs. 850 μm flux. (Top two panels) Central sample divided by magnification: >4.2 for z = 2 (top) and <4.2 for z = 2 (middle). The uncertainties show a range from z = 1–4. (Bottom panel) Full sample outside a ﹩2\buildrel{\,\prime}\over{.} 5﹩ radius from the cluster center, where we do not apply a magnification correction. In all panels, sources with ALMA identifications are shown in red.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Magnification computed at the SCUBA-2 850 μm position for z = 2 (squares) and for a range from z = 1 to z = 4 (error bars) vs. magnification computed at the ALMA position and accurate redshift for sources from A370 and MACSJ1149 with high enough 850 μm fluxes to appear in Table 2.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Images of the (left) 850 μm and (right) 450 μm SCUBA-2 data for nine of the 10 clusters (MACSJ1149 is shown in Figure 2). In each panel, we show the central ﹩4\buildrel{\,\prime}\over{.} 5﹩ radius region of the SCUBA-2 field. In both panels, the white circles show the >4σ 850 μm selected sample, including a confusion noise of 0.33 mJy. The sources are summarized in Table 2.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Histogram of the 450–850 μm flux ratio for the outer sample (black), the central sample with moderate magnifications (red), and the central sample with high magnifications (green).
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: See the caption for Figure 23.
Paper: The Effect of Primordial Black Holes and Streaming Motions on Structure Formation
Authors: F. Atrio-Barandela
Figure caption: (a) Variance of the matter distribution times its redshift dependence. From left to right, blue, green, red, gold, and black lines correspond to f PBH = 1, 0.1, 10−2, 10−3, 0. Solid lines correspond to no advection and broken lines to advection. Dashed lines and their nearby solid lines correspond to z = 80 while the triple-dotted–dashed lines and nearby solid lines correspond to z = 20. In (b) we plot the relative difference of the variance. Solid and triple-dotted–dashed lines correspond to f PBH = 0 and f PBH = 1, respectively. From top to bottom lines correspond to z = 20 (black), z = 40 (blue), z = 60 (red), and z = 80 (green). In (c) we plot the ratio of the variance with advection to variance without advection. Lines follow the same convention than in (b). In (d) we show the effect of varying the background advection velocity. The top three solid blue lines correspond to z = 80 and the bottom green dotted–dashed ones to z = 20. At each redshift, the top, middle, and bottom lines correspond to ﹩{v}_{{bc}}^{(\mathrm{bg})}=20,30,40﹩ km s−1, respectively.
Paper: The Effect of Primordial Black Holes and Streaming Motions on Structure Formation
Authors: F. Atrio-Barandela
Figure caption: Ratio of the number density of collapsed objects per unit of total mass for models with advection to models without advection. (a) corresponds to redshift z = 80, (b) to z = 60, (c) to z = 40, and (d) to z = 20. Dashed (blue), dotted–dashed (red), triple-dotted–dashed (green), long-dashed (gold), and solid (black) lines correspond to f PBH = 1, 0.1, 10−2, 10−3, 0, respectively. The vertical gray lines correspond to the masses of halos that have reached a virial temperature T vir = 103 K (left) and T vir = 104 K (right).
Paper: The Effect of Primordial Black Holes and Streaming Motions on Structure Formation
Authors: F. Atrio-Barandela
Figure caption: Variance of the streaming velocity field between baryons and DM. The dashed (blue), dotted–dashed (red), triple-dotted–dashed (green), and long-dashed (gold) lines also include the contribution from PBHs with fractions f PBH = (1, 0.1, 0.01, 10−3), respectively. The solid black line corresponds to the concordance ΛCDM model, i.e., f PBH = 0.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Excess number of neutrinos around the position of four groups of blazars with respect to the reconstructed energy. Filled regions show the 1σ statistical errors from random trials of simulation.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Comparison between the neutrino flux upper limits from our selected TXS-like blazars and IceCube 9.5 yr astrophysical neutrino flux.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Light curves of selected TXS-like sources. The top panel is the infrared light curve from WISE multiepoch data, and the middle panel is the Fermi γ-ray light curve analyzed with the Fermi Science Tool. The bottom panel represents the flaring periods in infrared (blue thick lines) and γ-ray (red thick lines), as well as the simultaneous flaring stages (green lines). Black lines represent the arrival time of the neutrino alerts.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Pretrial p-values of the excess number of neutrino around the position of four groups of blazars with respect to the reconstructed energy.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Excess number of neutrinos around the position of three groups of blazars with respect to the reconstructed energy. Filled regions show the 1σ statistical errors from random trials of simulation.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: C+I+E continuum image (gray) overlaid with the C+I continuum dendrogram structures (light green). Also overlaid are the C+I SiO(5-4) (red–blue) and C+I integrated intensity maps of hot core molecular lines C2H5CN(271,27 − 261,26, E up = 157.73  K) (dark green), C2H3CN(250,25 − 240,24, E up = 145.54  K) (cyan), and NH2CHO(101,9 − 91,8, E up = 60.81  K) (magenta). Three concentrations were identified for C2H5CN and C2H3CN, with both coinciding at the main continuum peak. The other two concentrations are located separately in the neighborhood of the secondary continuum structure and in the northern part outside the ring-like structure. On the other hand, NH2CHO traces more the wider region around the continuum ring. The intensities of the contours for C2H5CN are [0.16, 0.24, 0.32, 0.40] Jy beam−1 km s−1;  those for C2H3CN are [0.16, 0.24] Jy beam−1 km s−1;  and those for NH2CHO are [0.16, 0.32, 0.64] Jy beam−1 km s−1.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: Summary figure of dendrogram-identified structures (leaves) of C-only (top), C+I with minvalue = 4σ (middle), and C+I with minvalue = 5σ (bottom). The boundaries of the leaves are shown by solid black lines. The corresponding rms noise levels are 1.29  mJy beam−1 for C-only and 0.358 mJy beam−1 for C+I. The color stretch of each panel extends down to 0.1σ. The dashed circle designates the ALMA primary beam.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: (a) Left panel: best-fitting SEDs of G28.20-0.05 based on Zhang & Tan (2018) model grid based on the indicated data (see text). (b) Right panel: as (a), but only showing the best model (black line) and next four best models (gray lines).
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: Constrained parameter space (M  c , Σcl and m *) of the SED analysis. The color indicates the χ 2 parameter. The black plus sign indicates the best model.
Paper: Magellan/IMACS Spectroscopy of Grus I: A Low Metallicity Ultra-faint Dwarf Galaxy 
Authors: Anirudh Chiti, Joshua D. Simon, Anna Frebel, Andrew B. Pace, Alexander P. Ji, Ting S. Li
Figure caption: Top: UFD dynamical masses as a function of UFD mean metallicity (see Appendix A for a full list of references). The Grus I properties derived in Walker et al. (2016) are shown in green. The properties derived in this study are shown in red. Our derived metallicity and dynamical mass (see Table 4) place Gru I in the expected mass–metallicity regime for UFDs. Bottom: same as above, but for the metallicity-luminosity relation. Our results place Grus I exactly on the UFD trend.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Comparison of (a) the AFT map derived from observations at 12 noon on 2015 March 20 with (b) the flux transport simulation using bipoles derived from the daily AFT maps and (c) the flux transport simulation using bipoles derived from HMI Carrington rotation maps. Panels (b) and (c) are shown on the same date and time as panel (a). In each panel, the radial field at the photosphere is shown, where white/black represent positive/negative flux, where the values saturate at ±50 G. The image in panel (a) has been smoothed with a Gaussian filter to match the resolution of the simulations. In panel (a), key bipoles are identified with the numbers 1–5. In each panel, the dashed lines denote the longitude at central meridian on the 2015 March 20 at 12 noon.
Paper: Comparison of Electron Capture Rates in the N = 50 Region using 1D Simulations of Core-collapse Supernovae
Authors: Zac Johnston, Sheldon Wasik, Rachel Titus, MacKenzie L. Warren, Evan P. O'Connor, Remco Zegers, Sean M. Couch
Figure caption: Neutrino emission at r = 500 km for the 20 M ⊙ progenitor. Top row: neutrino luminosity, L  ν . Bottom row: mean neutrino energy, 〈E  ν 〉. Left: electron-neutrino (ν  e ) emission. Right: electron antineutrino (﹩{\bar{\nu }}_{e}﹩) and heavy-lepton neutrino (ν  x ) emission. Note the different time and L  ν  ranges.
Paper: Comparison of Electron Capture Rates in the N = 50 Region using 1D Simulations of Core-collapse Supernovae
Authors: Zac Johnston, Sheldon Wasik, Rachel Titus, MacKenzie L. Warren, Evan P. O'Connor, Remco Zegers, Sean M. Couch
Figure caption: Fractional and absolute differences of LMP+N50 and IPA models relative to LMP vs. progenitor iron core mass (Section 3.2). The quantities compared, from top to bottom: time to bounce from the start of the simulation (t  b ); accretion rate through r = 500 km at bounce (﹩{\dot{M}}_{b}﹩); and maximum shock radius reached for failed-explosion models (﹩\max ({r}_{\mathrm{sh}})﹩). Note the grid resolution of the simulation limits the precision of r sh here to ≈0.5 km.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Properties of the new emerging bipoles determined from the high-cadence AFT model (left column) and low-cadence SDO/HMI Carrington rotation maps (right column). Panels (a) and (b) show the emergence latitude against longitude. Panels (c) and (d) show the flux against the bipole half separation, while panels (e) and (f) show the tilt angle versus the latitude of emergence. Finally, panels (g) and (h) show the number of bipoles emerging each day over the 210 days of the simulation.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Portions of AFT magnetograms at (a) 12:00UT on 2014 September 4 and (b) 12:00UT on 2014 September 6. In each plot, white/black denotes positive/negative flux, where the values saturate at ±50 G. (c) Graph of flux against day for the new emerging bipole (solid line). The dotted line denotes the time of panel (a), while the dashed line shows the first identification of the new emerging bipole (red dashed box) at the time of panel (b). The dashed–dotted line gives the time of maximum flux where the bipole properties are determined.
Paper: Comparison of Electron Capture Rates in the N = 50 Region using 1D Simulations of Core-collapse Supernovae
Authors: Zac Johnston, Sheldon Wasik, Rachel Titus, MacKenzie L. Warren, Evan P. O'Connor, Remco Zegers, Sean M. Couch
Figure caption: Neutrino burst signal in a DUNE-like liquid argon detector for all 200 progenitors, vs. progenitor iron core mass. Top row: total neutrino counts. Bottom row: mean detected neutrino energy. From left to right are the adiabatic flavor-mixing implementations: no flavor mixing, normal mass ordering, and inverted mass ordering. The signal is integrated over 100 ms centered on the bounce (Section 2.3), across all detection channels (Table 1), and assuming a distance of 10 kpc. The error bars show typical 1σ uncertainties due to Poisson counting statistics alone. Note the different y-axis ranges.
Paper: Comparison of Electron Capture Rates in the N = 50 Region using 1D Simulations of Core-collapse Supernovae
Authors: Zac Johnston, Sheldon Wasik, Rachel Titus, MacKenzie L. Warren, Evan P. O'Connor, Remco Zegers, Sean M. Couch
Figure caption: Absolute difference of compact remnant properties relative to LMP (Section 3.3), vs. progenitor iron core mass. Top: PNS mass at the end of the simulation (M PNS) for exploding models. Bottom: time from bounce to BH formation (t BH).