adsabs/AstroCLIMB huggingface dataset:
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Pantheon+ sample Hubble diagram residuals (teal) to the best-fit cosmology (μ − μ model) for the baseline analysis as a function of SALT2 c, SALT2 x 1, and host-galaxy stellar mass M ⋆. Distances (μ) follow Equation (1) and include α, β, δ bias, and δ host corrections. Binned data are shown for reference (black). No significant residual correlations are seen.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Visualizing the impact of a number of the top systematic uncertainties in this analysis. The μ residuals are described by Equation (6). Each of these systematics is explained in Section 3, and they are combined to form the covariance matrix shown in Figure 6. Fragilistic provides nine systematic sets of trained SALT2 models, zero-point solutions, and filter central wavelengths. Here we show the impact on distance of just the first three.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Sixty-eight percent and 95% confidence contours for flat wCDM for cosmological parameters Ω M , H 0, and w. The contours from the Pantheon+ (red), Pantheon+ and SH0ES combined data set (teal), Planck Collaboration et al. (2020) TTTEEE-lowE constraints (gray) are shown. The combination of Planck and Pantheon+ (blue) is also shown, which is consistent with a cosmological constant. Planck constraints are bounded by 0.2 < Ω M  < 0.4 for computational speed. The histograms depict marginalized relative probabilities between probes.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Confidence contours at the 68% and 95% levels for the Ω M  and ΩΛ cosmological parameters for the ΛCDM from the Pantheon+ data set, as well as from the Planck and combined BAO data sets. The constraints from including both the statistical and systematic uncertainties (shaded red) are shown as well as when only statistical uncertainties are propagated (unfilled dashed). We include two lines for reference: one for a flat universe, where Ω M  + ΩΛ = 1 and the other that indicates an accelerating universe.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: The systematic covariance matrix as defined in Equation (7). To show the inherent structure, the data set is sorted by survey and within each survey (colored boxes), by redshift. “CALIB” are the set of 81 SN light curves in the SH0ES Cepheid-calibrator galaxies. The shading corresponds to the size of the covariance in magnitudes.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Constraints for flat w 0 w  a CDM from the Pantheon+ data set in combination with SH0ES, Planck TTTEEE-lowE.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Constraints for flat w 0 w  a CDM from the Pantheon+ data set in combination with Planck and galaxy BAO or Planck and all BAO.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Constraints for flat w 0CDM from the Pantheon+ data set in combination with Planck and galaxy BAO or Planck and all BAO.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Healpix (NSIDE = 16) Hubble residual sky maps (the color bar is residual magnitudes) with 20° 2D-Gaussian kernel smoothing, and Hubble residuals for two selected apertures. z > 0.01 is applied. Dots show the locations of the SNe in the Pantheon+ sample, with white dots showing the nearby SNe (z < 0.15) and black dots showing the distant SNe (z > 0.15). Top left: Hubble diagram corresponding to the baseline analysis utilizing both z CMB dipole corrections and 2M++ peculiar-velocity corrections. The circled regions designate the 20° regions centered on the negative CMB dipole (red) and CMB cold-spot directions (blue). The small circle in the top right (and “x” in bottom left) of each panel represents the direction (and opposite direction) of the motion causing the CMB dipole. Top right: same as top left, but instead using 2MRS peculiar-velocity corrections. Middle left) same as top left, but instead not applying any peculiar-velocity corrections. Middle right: same as top left, but instead applying neither peculiar-velocity corrections nor the CMB dipole correction. Bottom left: 20° region aligned with the (opposite) CMB dipole velocity depicting Hubble diagram residuals as a function of redshift. Bottom right: same as bottom left, but with aperture centered at the CMB cold spot (l = 209°, b = 57°), and over a higher redshift range.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Largest differences in analysis compared to Betoule et al. (2014) and Scolnic et al. (2018b). Top: updating the extinction curve used in the light-curve fitting from CCM to F99. Middle: updating the SALT2 model, as discussed in Brout et al. (2022). Bottom: changing the baseline assumption for the intrinsic scatter to the P21, G10, and C11 models.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: The impact on recovery of H 0, as explained in Section 2, of the systematic uncertainties described in Table 4. The units of these measurements are km s−1 Mpc−1. The dashed lines are given at a ΔH 0 of 0.7, which is the entire contribution of the uncertainty in R22 from SN measurements.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Constraints on Ω M  in flat ΛCDM when the bounds of the redshift range of the sample are changed. In the top panel, the minimum redshift is varied. The nominal minimum redshift is 0.01 for Pantheon+ cosmology fits without SH0ES. In the bottom panel, the maximum redshift is varied. The nominal maximum redshift is 2.4 for all fits.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: Left: spherically symmetric, hydrostatic analytical profile made with initial conditions for a central density and composition, and closed with the Helmholtz equation of state. Right: magnified line-out of the initial profile above the WD surface in Flash-X with the heated bubble added to ignite the detonation.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: Silicon and nickel compositions around the core at the time of peak energy release for both cases. Left: a large amount of low-density material is burned to silicon at coarser resolutions due to the secondary detonation starting at the edge of the white dwarf. Right: burning to nickel in coarser resolutions is localized to the front climbing the density gradient of the core, while for higher resolutions (case 1), the off-center detonation starts at a higher density resulting in more complete burning over the lower hemisphere of the core. Subsequently, both cases evolve similarly over the rest of the domain.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: A magnified view of the antipodal point for two different maximum resolutions. As in the previous figure, the white contour marks the WD extent while the green contour demarcates a temperature of 1 GK. Left: the 4km resolution case is driven not by a core ignition but rather an antipodal detonation. In this case, shell burning continuously mixes and progressively burns some mixed core material. Right: the 2 km case driven by off-center compression. This case burns the core after a distinct pause in shell burning, and separates the two detonations spatially and therefore also in terms of density.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: Outer shell-burning remnants: equatorial slice of mass fraction of silicon-28 at the WD limb after shell burning traverses the whole cutout. At 16 km resolution (left), the thickness of the expanding band is four times larger than in the highest resolution case (0.5 km, right). Additionally, mixing is far more complex and evolved even at scales that do not represent the actual length scales of burning.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: Left: peak positive energy release within the domain, split into values for the “core” and “shell” based on radial distance from the domain center (split radius). Right: total energy added to the domain via burning. Two families of solutions emerge based on the dynamics of the event: a direct shell to core burning at resolutions over 4 km, and a case with clearly separated shell and core burning stages at finer maximum resolutions.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: Ejecta composition by mass fractions sliced by angle of view. Top, middle, and bottom enclose 30° wide slices in the domain centered at noted angles (θ , further description in Section 3.3). Left: described slices for the 4 km case. Right: described slices for the 2 km case.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: Final yields from all simulations.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: Relative yields for simulations compared to the 4 km case.
Paper: The Impact of Resolution on Double-detonation Models for Type Ia Supernovae
Authors: Fernando Rivas, J. Austin Harris, W. Raphael Hix, O. E. Bronson Messer
Figure caption: Silicon burning front thickness for all cases, measured at 20° from the antipode.
Paper: Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra
Authors: Nickolay Y. Gnedin
Figure caption: Left: evolution of the volume-weighted (solid lines) and mass-weighted (dashed lines) fractions of neutral hydrogen for three different realizations of the 120 cMpc simulation volume used in this paper. The data points are from Fan et al. (2006) and were used as the calibration data for the simulations. Right: distributions of mean opacities in 50h −1cMpc skewers for the two realizations DC = 0 and DC = −1. Gray lines and bands show the observational data from Becker et al. (2015) and Bosman et al. (2018). The mean density model DC = 0 (red lines) marginally matches the distribution of opacities (at least at z > 5.5), while the DC = −1 model (blue lines) overpredicts opacities substantially. The DC = +1 model (not shown) underpredicts the opacity by about the same amount.
Paper: Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra
Authors: Nickolay Y. Gnedin
Figure caption: Probability distribution function for gaps of different lengths per unit redshift for gaps whose central redshifts fall in the specified redshift bins ([5.7, 5.9] and [5.9, 6.1]). Black squares are observational data from Zhu et al. (2021) with error bars computed by bootstrapping. Blue and red lines show the DC = −1 and DC = 0 CROC simulations, respectively, as well as the gap distribution from a set of four smaller boxes, as a test of numerical convergence with respect to the simulation box size.
Paper: Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra
Authors: Nickolay Y. Gnedin
Figure caption: Fraction of lines of sight exhibiting long (L > 30h −1cMpc) dark gaps as a function of redshift. The orange solid line with bands is the observational data from Zhu et al. (2021) with 68th and 95th percentile ranges. The other two lines are the same quantity estimated from the two CROC simulations as shown in the legend. The distribution of dark gaps is well sampled in the simulated data, so it is not necessary to bootstrap the synthetic spectra.
Paper: Bethe–Heitler Signature in Proton Synchrotron Models for Gamma-Ray Bursts
Authors: D. Bégué, F. Samuelsson, A. Pe'er
Figure caption: Comparison of cooling rate between the BeHe and synchrotron processes at γ p,m. From top to bottom, the emitted luminosity is 1054, 1053, and 1052 erg s−1, while, from left to right, the observed spectral peak frequency is 100 keV, 300 keV, and 1 MeV. The purple, red, and black thick lines correspond to t BeHe = t synch, t BeHe = 0.1t synch, and t BeHe = 10t synch respectively. The thin black lines show the variability time expected from the Lorentz factor and radius t var ∼ r/(Γ2 c) for selected variability time 10−2, 10−1, 1, and 10 s. The figure is made with p = 2.5. A value of p = 3.5 slightly increases the valid parameter space for proton synchrotron models by increasing the timescale ratio t BeHe/t synch at small radii.
Paper: Bethe–Heitler Signature in Proton Synchrotron Models for Gamma-Ray Bursts
Authors: D. Bégué, F. Samuelsson, A. Pe'er
Figure caption: Photon spectrum in marginally dominant synchrotron cooling regime with t synch ∼ t BeHe. Parameters are r 14 = 1, Γ2 = 1, ν MeV = 1, L 52 = 10, ξ = 1, and p = 2.5 (left) or p = 3.5 (right). Blue: proton synchrotron component. Green: BeHe synchrotron component. Red: total. It is clear that the emission from the secondary BeHe pairs greatly affects the overall shape of the spectrum at low (≲30 keV) and high (≳10 MeV) energies . The frequency of the second peak is independent on the power-law index. Above the photon peak at ∼100  MeV, the photon spectrum is not specified by our analysis as it depends on the details of the pair injection spectrum, and as such on the exact shape of the proton distribution function above γ p,m. This is represented by a dashed line.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Relations between the asymmetry parameter A, i-band concentration parameter, Sérsic index ﹩{n}_{{\rm{S}}\acute{{\rm{e}}}\mathrm{rsic}}﹩, ratio of rotational velocity to velocity dispersion V rot/σ, and stellar mass M ⋆ of galaxies identified at z = 7. The short blue line in the top-left panel marks the asymmetry parameter cut of A = 0.4 dividing symmetric and asymmetric galaxies. The short red lines in the bottom panels denote the Sérsic index cut demarcating disk-type and spheroid-type galaxies. The cyan curve in the bottom-right panel shows the median V rot/σ at a given ﹩{n}_{{\rm{S}}\acute{{\rm{e}}}\mathrm{rsic}}﹩, and the error bars are the uncertainty limits of the medians.