adsabs/AstroCLIMB huggingface dataset:
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: The ratio of asteroseismic to Gaia radii for our sample. Rows denote results using different methods: the Garstec+Mosser (top), Garstec+White (middle), and Sharma+White (bottom) models and weights. RGB stars are shown on the left and RC on the right. Data points are 50 star bins, defined in a rank-ordered list in ﹩{\nu }_{{\rm{\max }}}﹩. Silver sample bins are open points, and Gold sample bins are closed points. The ﹩{\nu }_{{\rm{\max }}}﹩ dependent fits to the RGB data are shown with the lines in the left panel.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: In the upper panels, we show the solar [Fe/H] sample in the mass–radius plane. The RC in the ﹩{\rm{log}}g﹩–Teff plane for three metallicity domains (−0.3, blue; 0, black; and +0.3, red; with a range of ±0.05 dex for each) is shown in the bottom panel. In all cases, we choose stars from the α-poor sample.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Fractional difference in age between AGB and RGB stars (top) and the total mass loss on the RGB (bottom) as a function of the current mass of the star. Low-mass stars experience much more mass loss.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Stellar properties at fixed mass and variable metallicity. APOKASC-3 stars classified as α-poor, with masses between 1.1 and 1.2 M⊙, shown in the asteroseismic ﹩{\rm{log}}g﹩–spectroscopic Teff plane. Filled symbols are Gold sample RGB, open symbols are Gold sample RC, and crosses are Silver sample stars. Symbol types and colors reflect metallicity; stars shown are in the range −0.5 < [Fe/H] < +0.3.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Difference between our main (GARSTEC) and alternative (YREC) ages for both RGB stars (red) and clump stars (blue), in the sense GARSTEC-YREC. Mass loss becomes important in low-mass stars, while differences in convective overshoot treatment are significant for higher masses. Systematics are at the 10 % level for the majority of the RGB stars, and somewhat larger for more-massive RC stars. The sharp edge in the clump offsets comes from the assumptions about mass loss in the alternative (YREC) ages.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: APOKASC-3 and Yu masses compared for Gold sample stars in the RC (top), lower RGB (middle), and upper RGB (bottom). Errors in each panel are the standard deviation and the median absolute deviation (MAD) converted to σ (in brackets).
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: The first dredge-up at solar metallicity. APOKASC-3 stars classified as α-poor, with  −0.05 < [Fe/H] < +0.05, are shown in the [C/N]–mass plane. Red symbols are Gold sample RGB stars, and blue symbols are Gold sample RC stars. Higher-mass stars are preferentially seen in the RC due to lifetime effects.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: A corner plot showing the distribution of different order schemes. Blue represents ordering by SNR and uniform mean priors, while orange represents ordering by means and uniform SNRs. We reconstruct the distribution in green by re-sorting the samples from the distribution in orange by descending SNR. Note that the blue almost completely overlaps the green, as we expect.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Posteriors of Gaussian pulses using different order schemes when N is fixed at 3. Blue represents using SNR-ordered priors, while orange represents using mean-ordered priors. We reconstruct the distribution in green by re-sorting the samples from the distribution in blue by ascending mean.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Example of the failure when the sampler is not able to identify the number of wavelets correctly. Blue and orange represent the two separate sine-Gaussians in the simulated data. Green represents the combination of these two.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Example of the reconstructed waveform when the sampler is not able to identify the number of wavelets correctly. Blue represents the injected signal and red represents the fitting result.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Sky map showing the 90% credible intervals for GW150914 recovered by a CBC template fit (blue) and a transdimensional sine-Gaussian wavelet fit (orange).
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Top: the real part of the gravitational-wave strain in the (2, 2) mode, normalized by extraction radius and gravitational mass. We compare our LR, SR, and HR AthenaK runs to a comparable run in GR-Athena++. Vertical lines show merger time as estimated by the peak amplitude of ﹩{h}_{22}^{+}﹩. Bottom: phase convergence of the three AthenaK runs. The difference between ϕLR and ϕHR is rescaled by a factor Q2 assuming second-order convergence.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Contour plots for ρ azimuthally and temporally averaged over the range ϕ ∈ [0, 2π], t ∈ [5000M, 10,000M]. The 643 HARM-like data is on the left, and the 643 Valencia data is on the right. There are six logarithmically spaced bins (i.e., seven contours) in the range [10−7, 1] in units of M−2. The blue contour marks β−1 = 1, and the red contour indicates σ = 1.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Same as Figure 11 but for the 1283 data.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Mass-weighted histograms of the specific angular momentum uϕut for the 643 (top), 963 (middle), and 1283 (bottom) tests. Each distribution is temporally averaged over t ∈ [5000M, 10,000M]. The distributions are then normalized against the initial mass at t = 0 and therefore do not add up to unity.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Top: instantaneous frequency of the (2, 2) mode, ω22, for GR-Athena++ and the AthenaK runs. Bottom: plot of the reduced binding energy Eb and reduced angular momentum j. In both plots, vertical lines indicate merger times for each model.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Weak-scaling results of a single neutron star (blue) and a turbulence setup (red) on OLCF Frontier. The top plot displays raw performance (solid lines) in terms of zone-cycles per second relative to ideal scaling (dashed lines). The bottom plot shows parallel efficiency relative to a single node as a function of GPU count.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Same as Figure 18, but for strong scaling instead, and with efficiency measured against zones per GPU rather than total GPU count.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Mass conservation of AthenaK BNS runs compared to GR-Athena++.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Same as Figure 11 but for the 963 data.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: The rest-mass density ρ, pressure P, x-velocity ux = Wvx, and y-component of the magnetic field By for the shock tube tests at t = 0.5.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Oscillations of the central density of the TOV star as a function of time (top) and the power spectrum of central density oscillations (bottom). The “norm,” “fofc,” and “dmp” labels refer to runs without FOFC, with FOFC, and with FOFC+DMP, respectively. To reduce spectral leakage, the oscillations were filtered with a Tukey window of α = 0.203 prior to computing the Fourier transform. The black vertical lines mark the fundamental frequency and its first harmonic as predicted by perturbation theory.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Same as Figure 7, but for a TOV star with the Z4c solver enabled. The “norm,” “fofc,” and “dmp” labels refer to runs without FOFC, with FOFC, and with FOFC+DMP, respectively. Labels without the “-hr” suffix refer to the 1923 runs and to those with the 3843 solutions.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Diagnostic fluxes for the 643, 963, and 1283 cases plotted against some of the 963, 1283, and 1923 EHT data (respectively). From top to bottom, in each set of plots we show the rates for mass accretion, normalized energy accretion, normalized angular momentum accretion, and normalized magnetic flux.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Same as Figure 3, but for a strongly magnetized blast wave (Bx = 1.0).
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Top: the Bx component of the magnetic field during the loop advection test. Bottom: the violation of the divergence-free constraint relative to the maximum magnetic field strength. In both plots, the left half shows the initial data and the right half shows the evolved data after a single period (t = 2.4).
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: The average of the diagnostic fluxes over t ∈ [5000M, 10,000M] for each resolution, normalized by the average of all the codes considered. The error bars span a single standard deviation.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Shock tube convergence as measured by the L2 error between the numerical and exact solutions for ρ at t = 0.5. Markers indicate numerical solutions and solid lines measure first-order convergence.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: The pressure of a weakly magnetized blast wave (Bx = 0.01) at t = 4 for the FOFC (top) and FOFC+DMP (bottom) methods.
Paper: Performance-portable Binary Neutron Star Mergers with AthenaK
Authors: Jacob Fields, Hengrui Zhu, David Radice, James M. Stone, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Same as Figure 3, but for a moderately magnetized blast wave (Bx = 0.1).
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Natural log posterior odds obtained with different sampling techniques (see Equation (13)). The odds are measured relative to the favored N = 3 model. The uncertainties are 1σ. The orange and green points are the transdimensional sampling results using dynesty and ptemcee. The navy blue points labeled “N fixed” show where we calculate the evidence for each value of N with dedicated dynesty runs providing the ground truth.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: The reconstructed signal from GW150914. The red trace shows the whitened signal reconstructed using a transdimensional sine-Gaussian wavelet fit. The blue trace shows the maximum-likelihood template obtained with the IMRPHENOMXPHM approximant. The whitened data are shown in peach. The top panel is for the H1 observatory in Hanford, WA, while the bottom panel is for the L1 observatory in Livingston, LA.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Posterior distribution for the SNRs and means of N = 3 Gaussian pulses with descending SNR priors. The different shades show 1σ, 2σ, and 3σ credible intervals. The ground truth, obtained with a fixed-N dynesty run, is shown in blue. In orange, we plot the results obtained using a transdimensional implementation of dyensty, while the green shows a transdimensional implementation of ptemcee.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Corner plot of posterior samples of N = 3 Gaussian pulses re-sorted by ascending means. The different shades show 1σ, 2σ, and 3σ credible intervals. The ground truth, obtained with a fixed-N dynesty run, is shown in blue. In orange, we plot the results obtained using a transdimensional implementation of dyensty, while the green shows a transdimensional implementation of ptemcee.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Posteriors for the frequencies of the different sine-Gaussian wavelets fit to GW150914. The blue results are obtained with fixed N = 4. The orange shows the posteriors of samples with N = 4 from a transdimensional fit, which allows for any value of N.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: The model selection result for the GW150914 wavelet fit. The ratio of the number of samples at different N represents the Bayes factor of different models.
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: An example of descending SNR priors. Note here the variables are the relative SNR ρi defined in Equation (11).
Paper: Transdimensional Inference for Gravitational-wave Astronomy with Bilby
Authors: Hui Tong, Nir Guttman, Teagan A. Clarke, Paul D. Lasky, Eric Thrane, Ethan Payne, Rowina Nathan, Ben Farr, Maya Fishbach, Gregory Ashton, Valentina Di Marco
Figure caption: Simulated data (blue) for our Gaussian pulse model described in Section 3.1. The signal (orange) consists of three Gaussian pulses.
Paper: A New X-Ray and Radio Burst Activity from the Magnetar SGR 1935+2154
Authors: Noor S. Rehan, Alaa I. Ibrahim
Figure caption: The correlation between the BB emission area (﹩{R}_{\mathrm{BBh}}^{2}﹩, ﹩{R}_{\mathrm{BBs}}^{2}﹩) and temperature (kTBBh, kTBBs) of the 2BB model for the bursts from SGR 1935+2154 during the 2022-10 activity and those since 2020 April, together with their 2D kernel density and power-law (PL) fit. The 2022-10 hard BB component (blue) fits a PL with an index of −3.92 ± 0.40, and the soft component (red) fits a PL with an index of −1.19 ± 0.33. The combined fit of the hard and soft components (black line) fits a PL with an index of −3.33 ± 0.20. The other activities since 2020-04 are also presented for comparison (using data from L. Lin et al. 2020b; N. u. S. Rehan & A. I. Ibrahim 2024, 2023). The soft (orange) and hard (pink) BB components of the X-ray counterpart burst (XFRB1) of FRB 200428 (FRB1) are also shown in all panels (based on INTEGRAL, S. Mereghetti et al. 2020) for comparison with the bursts of each activity. See Sections 4.4 and 4.5. See also Sections 4.4 and 4.5.