adsabs/AstroCLIMB huggingface dataset:
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Posterior distributions (smoothed by GetDist KDEs) of radius, compactness, and mass. The data sets were generated and analyzed adopting the ST+PST model. In the left panel, we present results obtained using data sets produced with three different noise realizations, labeled from 1 to 3 in the legend. For all of these runs, we adopted the X-PSI low-resolution setting (LR), SE 0.3 and ET 0.1. For noise realization 2 and 3, we use LP 6 × 103 and MM off, for noise realization 1 LP 104 and MM on (the right panel demonstrates that these two settings lead to similar results). This plot shows that, given these settings, model, and observing properties, our recovered posterior distribution is sensitive to the noise realization adopted to generate the analyzed data sets. In the right panel, we show the corner plots corresponding to different runs analyzing the data set generated with noise realization 1 and different X-PSI and MULTINEST settings as shown in the legend. The three curves with broader posteriors represent the runs with ≥5 × 103 LP (the first two and the last one in the legend). This corner plot demonstrates the need for a large number of live points to sensibly estimate the width of the marginalized posteriors. All of these inference runs are described in Sections 3.3.2 and 2.4, and their details are reported in Table 3. In both plots, credible intervals and colored areas refer to the inference run adopting SE 0.3, ET 0.1, LP 104, MM on and LR as MULTINEST and X-PSI settings (represented with dashed black lines), and applied to the data set generated with noise realization 1. See caption of Figure 5, for further details.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Posterior distributions (smoothed by GetDist KDEs) of radius, compactness, and mass. Results are obtained using data sets produced with seven different noise realizations, labeled from 1 to 7 in the legend. The data sets were generated and analyzed with the ST-U model. Credible intervals and colored areas refer to the inference run labeled as noise realization 1 (also represented with dashed black lines). See the caption of Figure 5 for further details on the plot. These inference runs were performed with the X-PSI and MULTINEST settings described in the Sections 3.3.1 and 2.4 and reported in Table 2. As expected, the different noise realizations introduce some scatter in the marginalized posteriors. The outlier (see, in particular, the mass plot) is the run corresponding to noise realization 5, and the presence of this outlier may be simply due to random fluctuations arising in the sampling process (see also the presence of outliers in Figure 5). The purple line delineating broad radius and compactness posteriors represents results from noise realization 2.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Posterior distributions (smoothed by GetDist KDEs) of radius, compactness, and mass. The data set was generated adopting the ST+PST model (noise realization label 1) and analyzed assuming the ST-U model. Credible intervals and colored areas refer to the inference run enabling the mode-separation modality (also represented with dashed black lines). See caption of Figure 5, for further details on the plot. The inference runs shown in this plot were performed with the MULTINEST settings reported in the legend (see Section 2.4 for definitions) and in Table 2. For all inferences, the injected parameter values are in the bulk of the marginalized posteriors even though the model adopted for inferences does not allow for the complex configuration used to generate the data set. The obtained distributions also well resemble those obtained when the correct model is used (see Figure 9). The outlier corresponds to the run with MULTINEST settings: SE 0.8, ET 0.1, LP 103, MM off, and again it may simply be due to statistical fluctuations, possibly reflecting the need of more stringent sampling parameters.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Schematic representation of the geometric configurations, as seen from Earth, of the NS hot spots adopted to create the data analyzed in this work. The parameter values corresponding to the ST-U and ST+PST models, respectively, shown in the left and right panels, are reported in Table 1. The configurations show, with solid lines, the hot spot section visible to us at phase ϕ = ϕ  p  = 0.0 cycle (the reference phase of the primary hot spot); in transparency we show the component parts on the hemisphere, which, at this rotation phase, is opposite to the observer. With a second point on the equator, we also display how the NS rotates. The blue/red line is used to mark the hottest/coldest component. We also remind the reader that for the ST-U configuration, the primary hot spot is defined as the component with lower colatitude, while for the ST+PST it is set by the hot spot description as a single spherical cap with uniform temperature.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Posterior distributions (smoothed by GetDist KDEs) of radius, compactness, and mass. We report posterior distributions for data analyzed and generated with the ST+PST model. With these inference analyses, we explore the effect of external constraints on our analysis (see Section 3.3.2 for more details). MULTINEST and X-PSI settings, as well as the model parameters a priori constrained (M stands for mass, D for distance, and I for inclination), are shown in the legend. For this plot, we used the data generated with noise realization 1. Credible intervals and colored areas refer to the inference run obtained with constraints on mass, distance, and inclination and using 104 live points (also represented with dashed black lines). For clarity, here we also show the 1D marginalized prior distributions on radius, mass, and compactness with dashed–dotted lines. Including the inclination constraints (which is otherwise not well recovered) shifts the inferred marginalized posterior distributions away from the injected values of radius and compactness, highlighting the multimodal structure and complexity of our posterior surfaces. See caption of Figure 5 for further details.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Posterior distributions (smoothed by GetDist KDEs) of radius, compactness, and mass. We present results from two ST+PST inference runs analyzing the data set generated with the ST-U model defined by noise realization 1; MULTINEST settings are reported in the legend. “LR” stands for the X-PSI low-resolution setting. Credible intervals and colored areas refer to the mode-separation inference run (also represented with dashed black lines). The injected parameter values are well within the bulk of the obtained marginalized posteriors. These distributions are also similar to those found when the ST-U model was used to analyze this data set. Increasing the number of live points used in the sampling procedure to 104 slightly shifts the obtained posterior distributions, highlighting that 103 live points are probably not enough to adequately explore the parameter space. See the caption of Figure 5 for further details.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption:  P–P plot for the seven noise realizations produced and analyzed with the ST-U model. It represents (for mass, radius, and compactness) the cumulative fraction recovered within a credible interval (i.e., the cumulative of the left-side p-value at which the injection is found) as a function of the credible intervals. The legend values in parentheses are the p-values from the Kolmogorov–Smirnov test against the theoretical uniform expectations (the injected value should appear p% of the times within the p% credible interval). The gray areas represent the 1σ, 2σ, and 3σ confidence intervals on the theoretical expectations, calculated according to Cameron (2011).
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Schematic representation of the hot spot configurations, as seen from Earth, for the three modes found by the X-PSI inference run when using the ST-U model to analyze a data set generated with ST+PST. The specific configurations correspond to the maximum likelihood sample associated with each mode (for other details, see the caption of Figure 3).
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: Left panel: temperature anisotropies in the CMB calculated for various viscous DM. The bottom part of the panel displays the relative temperature differences between the models and the CDM model. Physical processes that provide dominant contributions on different scales are quoted (Sugiyama 2014). Right panel: nonlinear matter power spectrum in z = 0 for various viscous DM and CDM models and the fractional difference between them. As can be seen, all viscous DM cases suppress P(k) at large scales. We use the best-fit values of various free and derived parameters that have been shown in Table 1 for the total data.
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: Left panel: theoretically predicted Hubble parameters and their relative differences as a function of redshift compared to the observational data from CCs (Marra & Sapone 2018). Right panel: the redshift evolution of the deceleration parameter q(z) and their differences as a function of redshift. For both panels, the values of the parameters obtained from Table 1 with the total data have been used for the proposed viscous DM scenarios and the CDM model.
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: 68% and 95% CL constraint contours on the matter density parameter Ω m , the Hubble parameter, H 0, and S 8. It is obtained by considering the Planck+BAO+CC+SN Ia+LSS data
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: The linear growth rate, f (the scalar perturbations) for mode k = 10−4 (the galaxy cluster scale) and 1 Mpc−1 (the dwarf galaxy scale).
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: Planck 2018 EE (left panel) and TE (right panel)power spectra using the best-fit values of various parameters have been obtained in Table 1 for the total data.
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: The evolution of the effective equation of state of viscous DM as a function of factor scale using the best-fit values from Table 1 for the total data.
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: The evolution of the fractional energy density of viscous DM in terms of scale factor. We use the best-fit values from Table 1 for the total data.
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: The preferred ranges of the parameters ﹩{S}_{8}\equiv {\sigma }_{8}{({{\rm{\Omega }}}_{m}/0.3)}^{0.5}﹩ and H 0 for all the models reviewed using the total data. For reference, the measurements of S 8 = 0.759 ± 0.02 by KiDS-1000 are also shown.
Paper: Kinetic Simulations of Nonrelativistic High-mach-number Perpendicular Shocks Propagating in a Turbulent Medium
Authors: Karol Fulat, Artem Bohdan, Gabriel Torralba Paz, Martin Pohl
Figure caption: The power spectrum of the electric field parallel to the wavevector,  E ∥ k , for all runs, in the region where Buneman waves are the strongest during the latest reformation cycle. The power spectrum is shown in units of ﹩{({\omega }_{{pe}}{m}_{e}c/e)}^{2}﹩.
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: 68% and 95% constraint contours on the matter density parameter Ω m , the lowest neutrino mass m 0, the Hubble parameter, H 0 and S 8. This is obtained by considering the Planck+BAO+CC+SN Ia+LSS data
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: The growth rate of matter fluctuations for our baseline viscous DM models compared to the ΛCDM model. The observational constraints are taken from Planck Collaboration et al. (2020).
Paper: Kinetic Simulations of Nonrelativistic High-mach-number Perpendicular Shocks Propagating in a Turbulent Medium
Authors: Karol Fulat, Artem Bohdan, Gabriel Torralba Paz, Martin Pohl
Figure caption: Maps of the electron number density (top panel) and the x-components of the magnetic (middle panel) and the electric fields (bottom panel) at a shock with preexisting upstream density fluctuations (run T2). The scaling of the fields is logarithmic and sign preserving, e.g., for B  x /B 0 it is ﹩\mathrm{sgn}({B}_{x})\cdot [2+\mathrm{log}\{\max ({10}^{-2},| {B}_{x}| /{B}_{0})\}]﹩.
Paper: Kinetic Simulations of Nonrelativistic High-mach-number Perpendicular Shocks Propagating in a Turbulent Medium
Authors: Karol Fulat, Artem Bohdan, Gabriel Torralba Paz, Martin Pohl
Figure caption: The evolution of the ion number density averaged over the y-direction for run T2. Dark blue stripes represent upstream density fluctuations, which are advected to the shock front. For visualization purposes, the presentation is truncated 20λ si ahead of the shock.
Paper: Dark Matter Cosmology with Varying Viscosity: A Possible Resolution to the S 8 Tension
Authors: Amjad Ashoorioon, Zahra Davari
Figure caption: Comparison between the absolute magnitude, M  B , for all models considered in this study.
Paper: Kinetic Simulations of Nonrelativistic High-mach-number Perpendicular Shocks Propagating in a Turbulent Medium
Authors: Karol Fulat, Artem Bohdan, Gabriel Torralba Paz, Martin Pohl
Figure caption: The ion number density profile averaged over the y-direction (top panel), as well as the ratio of the magnetic field strength to the density (bottom panel).
Paper: Observational Evidence of a Centi-parsec Supermassive Black Hole Binary Existing in the Nearby Galaxy M81
Authors: Wu Jiang, Zhiqiang Shen, Ivan Martí-Vidal, Zhen Yan, Lei Huang, Roman Gold, Ya-Ping Li, Fuguo Xie, Noriyuki Kawaguchi
Figure caption: Radio and X-ray variations of M81* from 1980–2022. (A) Jet PAs observed at multifrequencies and assembled at 8.4 GHz. The solid curves represent the Bayesian fitting to the SMBHB model and the results of the evolution of PA (red) and viewing angle (blue). (B) Radio light curve formed assembled at 8.4 GHz (gray: original; blue: Doppler beaming corrected). (C) X-ray (2–10 keV) light curve (gray: original; dark: Doppler beaming corrected). (D) Six epoch VLBI images at 8.4 GHz from 2005–2022, all the uniform-weighted interferometry beams shown in the bottom left corner are restored to a normal beam size (0.5 × 0.5 mas), which is the intercontinental interferometry, including VLBA and EF or SH at 8.4 GHz. The contour levels are 0.3 ×(−1, 5, 10, 20, 40, 80,160, 240) mJy beam−1. The lowest level is about three times the rms of the noise in the image. The red line indicates the projection on the sky of the rotation axis of the M81 galaxy at 62° (Bartel et al. 1982); the green-dashed lines indicate the PAs of the jet in the center region from the results of model fitting.
Paper: Observational Evidence of a Centi-parsec Supermassive Black Hole Binary Existing in the Nearby Galaxy M81
Authors: Wu Jiang, Zhiqiang Shen, Ivan Martí-Vidal, Zhen Yan, Lei Huang, Roman Gold, Ya-Ping Li, Fuguo Xie, Noriyuki Kawaguchi
Figure caption: Schematic representation of the black hole binary model in M81*. The secondary is orbiting around the primary black hole with an angular velocity of ω  o  and a separation of a. The orbital plane is misaligned θ  p  to the disk plane of the primary black hole. ξ 0 and ϕ  o  are the projections of the orbital axis  z  orb in the sky and its inclined angle to the LOS, respectively. The disk jet of the primary black hole undergoes short-term (2π/ω  b ) nodding and wobbling (smaller purple ellipse), superimposing a long-term (2π/Ω p ) precession (blue ellipse).
Paper: Observational Evidence of a Centi-parsec Supermassive Black Hole Binary Existing in the Nearby Galaxy M81
Authors: Wu Jiang, Zhiqiang Shen, Ivan Martí-Vidal, Zhen Yan, Lei Huang, Roman Gold, Ya-Ping Li, Fuguo Xie, Noriyuki Kawaguchi
Figure caption: Corner plot of the MCMC fitting to a binary black hole model in M81*. The six parameters in the binary black hole model are Ω p , θ  p , ω  b , η  p , ξ 0, and ϕ  o  is the precession rate, the inclined angle of the orbit plane to the disk plane, the wobbling and nodding rate, the initial projection angle of jet on the orbital plane at t 0, the projection of the orbital axis in the sky and its inclined angle to the LOS, respectively.
Paper: Observational Evidence of a Centi-parsec Supermassive Black Hole Binary Existing in the Nearby Galaxy M81
Authors: Wu Jiang, Zhiqiang Shen, Ivan Martí-Vidal, Zhen Yan, Lei Huang, Roman Gold, Ya-Ping Li, Fuguo Xie, Noriyuki Kawaguchi
Figure caption: LSP of the time series of X-ray (upper panel), radio fluxes (middle panel), and PAs (lower panel) for M81*. A peak at ∼15.2 yr can be detected in the LSP of the PAs and the X-ray light curve, respectively. There are two comparable peaks at 27.6 and 12.5 yr in the radio LSP. All these time series measurements suggest a periodic mechanism in the central region.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Comparison of the 56Ni mass and the ejecta mass based on the Arnett fit for our sample and usual stripped-envelope Type IIb SNe from Taddia et al. (2018) and USSNe from De et al. (2018) and Yao et al. (2020). We find that the SSSNe in our sample are a transient class between the USSNe and the usual SESNe (rough boundaries indicated by the vertical dashed lines). We also note that there is a region in the parameter space that is unoccupied by the SESN population.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Nebular spectra showing the [Ca II] λ λ7291, 7324 and [O I] λ λ6300, 6364 lines. The phase of the spectra is measured as the number of rest-frame days since the second peak. The spectra with the full wavelength range are shown in Appendix A.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Comparison of the light curves of the Ca-rich Type IIb SNe in our sample (in filled shapes of different types) with canonical Type IIb SN light curves from Taddia et al. (2018; in blue circles). The y-axis shows the absolute magnitude (mag), with galactic extinction correction. The x-axis shows the number of rest-frame days since the second peak.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Light curves for our sample of nine Ca-rich Type IIb SNe. This has forced-photometry from ZTF, ATLAS, and follow-up observations from various instruments. See Section 2.2 for further description on the photometry. The left y-axis shows the apparent magnitude (mag), and the right y-axis shows the absolute magnitude (mag), without host extinction correction. The x-axis shows the number of rest-frame days since the second peak.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Collage of a few spectra for the SNe in our sample showing H and He emission lines. The phase of the spectra is measured as the number of rest-frame days since the second peak.