adsabs/AstroCLIMB huggingface dataset:
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: CMDs of likely member stars and NMSs (as determined with the Bayesian probabilities computed in Section 3.1) alongside the subset of sources with both this photometry-based Bayesian membership determination and astrometric information. Left: likely member stars. Right: likely NMSs. In both panels, crosses show sources with DAOPHOT photometry that have proper motions inconsistent with that of Boo I, and open green circles indicate sources for which the measured proper motion is consistent with Boo I (within generous 5σ error bounds). Sources without proper-motion measurements are shown as small points. Dashed lines show magnitude limits of the final catalog used to constrain the IMF.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: The normalized Hess diagram of the final Boo I catalog (left), binned identically to the procedure adopted in the ABC MCMC algorithm. To the right is the luminosity function (LF) of these data, and above is the distribution in color. Overlaid on the Hess diagram as a red dashed line is an [M/H] = −2.5 isochrone, with star-shaped points indicating the colors and magnitudes corresponding to the stellar masses given to the left of the isochrone.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: The results of the broken power-law fit to the Boo I member catalog, in which the break mass was held fixed at ﹩0.5{{ \mathcal M }}_{\odot }﹩. The dashed lines on, and text above, the one-dimensional histograms indicate the best-fit values. The text to the right of the plot denotes, for context, the Kroupa (2001) values for the low-mass, single-star IMF of stellar populations of the Milky Way.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: The results of the single power-law fit to the Boo I member catalog. The dashed lines on, and text above, the one-dimensional histograms indicate the best-fit values, defined as the median value of the marginalized posterior distribution. For context, the Salpeter single power-law slope is α = − 2.35.
Paper: The Impact of Binaries on the Dynamical Mass Estimate of Dwarf Galaxies
Authors: Camilla Pianta, Roberto Capuzzo-Dolcetta, Giovanni Carraro
Figure caption: Dependence of the ratio σ tot/σ 0 on the mean mass density of the system obtained by varying the scale radius R from 25 to 250 pc with steps of 25 at fixed total mass M = 5 × 104 M ⊙. The values of f  b  label each curve going bottom-up, according to the legend, and differ depending on whether RLOF is taken into account (lower panel) or not (upper panel) in the calculation of σ tot.
Paper: The Impact of Binaries on the Dynamical Mass Estimate of Dwarf Galaxies
Authors: Camilla Pianta, Roberto Capuzzo-Dolcetta, Giovanni Carraro
Figure caption: For the simulated dSph: the upper panels illustrate the dependence of the velocity dispersion σ tot (top-left panel) and of the luminosity averaged velocity dispersion σ tot,lum (top-right panel) on the variation of the lower boundary a min of the binary semimajor axis distribution for the reference model. Lower panels show the corresponding relative mass difference ΔM/M. Each curve refers to a different value of f  b  going bottom-up from 0.05 to 0.4 in steps of 0.05.
Paper: The Impact of Binaries on the Dynamical Mass Estimate of Dwarf Galaxies
Authors: Camilla Pianta, Roberto Capuzzo-Dolcetta, Giovanni Carraro
Figure caption: As in Figure 5, but accounting for both RLOF and the luminosity cutoff.
Paper: The Impact of Binaries on the Dynamical Mass Estimate of Dwarf Galaxies
Authors: Camilla Pianta, Roberto Capuzzo-Dolcetta, Giovanni Carraro
Figure caption: For the simulated UFD: the upper panels illustrate the dependence of the velocity dispersion σ tot (top-left panel) and of the luminosity averaged velocity dispersion σ tot,lum (top-right panel) on the variation of the upper boundary a max of the binary semimajor axis distribution for the reference model. Lower panels show the corresponding relative mass difference ΔM/M. Each curve corresponds to a different value of f  b  going bottom-up from 0.05 to 0.4 in steps of 0.05.
Paper: The Impact of Binaries on the Dynamical Mass Estimate of Dwarf Galaxies
Authors: Camilla Pianta, Roberto Capuzzo-Dolcetta, Giovanni Carraro
Figure caption: As in Figure 2, but accounting for RLOF.
Paper: The Impact of Binaries on the Dynamical Mass Estimate of Dwarf Galaxies
Authors: Camilla Pianta, Roberto Capuzzo-Dolcetta, Giovanni Carraro
Figure caption: As in Figure 1, but for the variation of a min at a fixed value of ﹩{a}_{\max }=100\,\mathrm{au}﹩.
Paper: The Impact of Binaries on the Dynamical Mass Estimate of Dwarf Galaxies
Authors: Camilla Pianta, Roberto Capuzzo-Dolcetta, Giovanni Carraro
Figure caption: As in Figure 1, but accounting for RLOF.
Paper: Empirical Dust Attenuation Model Leads to More Realistic UVJ Diagram for TNG100 Galaxies
Authors: Gautam Nagaraj, John C. Forbes, Joel Leja, Dan Foreman-Mackey, Christopher C. Hayward
Figure caption: Dust-free UVJ diagram for TNG100 vs. 3D-HST. The distribution of dust-free colors from TNG100 at z = 1—calculated for each galaxy by summing the fluxes from every star particle within 2r 1/2 to mimic the setup in Donnari et al. (2019)—is shown in red. The distribution of dust-free colors of 3D-HST galaxies (whose inference is described in Section 3.3) is shown in blue. The 68% (darker) and 95% (lighter) contours are shaded. See Section 3.2 for more details on the procedure to calculate colors. The boundaries between quiescent and star-forming are taken from Whitaker et al. (2011), with modifications at the upper right corner inspired by Belli et al. (2019), while the boundary between dusty and unobscured is from Fumagalli et al. (2014). The TNG100 and 3D-HST distributions are quite similar, both showing concentrations of galaxies representing the star-forming main-sequence and quiescent galaxies. However, the observed galaxies tend to have slightly bluer colors than the simulated galaxies, especially V − J.
Paper: Empirical Dust Attenuation Model Leads to More Realistic UVJ Diagram for TNG100 Galaxies
Authors: Gautam Nagaraj, John C. Forbes, Joel Leja, Dan Foreman-Mackey, Christopher C. Hayward
Figure caption: Galaxy-by-galaxy differences between dust-attenuated UVJ colors for TNG100 galaxies derived in this work and Donnari et al. (2019) as a function of stellar mass (top left), sSFR (top right), metallicity (bottom left), and average age of stellar populations (bottom right). Very minor differences between the dust-free UVJ colors are removed to create a fair baseline for the comparisons. We see that the UVJ differences are systematically negative for high stellar mass, low-sSFR, high-metallicity, and/or older galaxies. In other words, Donnari et al. (2019) predict bluer galaxies in that part of parameter space. If the effective attenuation curve obtained by Nelson et al. (2018) based on the simulation particle data were replaced by an effective dust screen, the predicted attenuation curve would either have a lower optical depth or be flatter than our empirical curve for such galaxies.
Paper: Empirical Dust Attenuation Model Leads to More Realistic UVJ Diagram for TNG100 Galaxies
Authors: Gautam Nagaraj, John C. Forbes, Joel Leja, Dan Foreman-Mackey, Christopher C. Hayward
Figure caption: Distributions of average stellar population age (left) and stellar metallicity (right) for TNG100 simulated galaxies at z = 1 (blue) vs. 3D-HST galaxies at 0.8 ≤ z ≤ 1.2 (red). The wider distributions of observed galaxies for age and metallicity may contribute to their larger distribution of UVJ colors. In addition, we notice that, on average, TNG100 galaxies have younger stars (29%) and higher metallicities (0.28 dex). The combination of these two differences can help explain the bluer 3D-HST colors. Higher metallicities signify redder colors, while younger populations lead to bluer colors (opposite effect). The balance of these effects as a function of wavelength can result in the disparity we see. We offer a more detailed explanation in the text, including caveats to these results, especially metallicity, from the limitations of SED fitting.
Paper: Empirical Dust Attenuation Model Leads to More Realistic UVJ Diagram for TNG100 Galaxies
Authors: Gautam Nagaraj, John C. Forbes, Joel Leja, Dan Foreman-Mackey, Christopher C. Hayward
Figure caption: Variation in the diffuse dust attenuation curve over the stellar mass–SFR parameter space from our empirical model DustE. The attenuation curves correspond to the model’s prediction at the location in parameter space at the center of each small plot (as highlighted by the dotted black lines). The 1σ errors on the mean attenuation curves are shaded but are too small to be visible. The faint points in the background show the mean Prospector posterior sample for stellar mass and SFR and are colored by sSFR, as are the attenuation curves themselves. For easier interpretation, in each attenuation curve plot we show the curve for the other eight locations as gray dashed lines. We can see that attenuation generally increases (larger optical depth and typically steeper attenuation slope) with stellar mass and SFR, but the detailed behavior is rather complex. See Paper I for extensive discussions of the science results of our models.
Paper: Empirical Dust Attenuation Model Leads to More Realistic UVJ Diagram for TNG100 Galaxies
Authors: Gautam Nagaraj, John C. Forbes, Joel Leja, Dan Foreman-Mackey, Christopher C. Hayward
Figure caption:  UVJ diagram for TNG100 vs. 3D-HST (including dust). The distribution of values from this work is shown in red, 3D-HST galaxies in blue, and those from Donnari et al. (2019) in orange, with 68% (darker) and 95% (lighter) contours shaded. Our dust model yields a longer quiescent strip of galaxies, as well as many more DSFGs than the resolved Nelson et al. (2018) model used by Donnari et al. (2019), thereby giving it greater resemblance to the observed UVJ distribution.
Paper: Empirical Dust Attenuation Model Leads to More Realistic UVJ Diagram for TNG100 Galaxies
Authors: Gautam Nagaraj, John C. Forbes, Joel Leja, Dan Foreman-Mackey, Christopher C. Hayward
Figure caption: Distributions of stellar mass for TNG100 simulated galaxies at z = 1 (blue) vs. 3D-HST galaxies at 0.8 ≤ z ≤ 1.2 (red). To first order, the distributions are very similar, suggesting that the populations of galaxies considered are quite comparable.
Paper: One-off and Repeating Fast Radio Bursts: A Statistical Analysis
Authors: Hao-Yan Chen, Wei-Min Gu, Mouyuan Sun, Tuan Yi
Figure caption: The distributions of DME vs. L p for one-off FRBs (red) and repeating FRBs (gray) from Catalog 1. We compare the distributions under the same upper limit of DME (or redshifts z). The top and right distributions are the marginal probability density estimations of the one-dimensional distribution of the corresponding parameters, i.e., DME and L p. Using the 2DKS test, we can infer the correlation between one-off FRBs and repeaters. There could be evidence that the 2D distributions for one-off FRBs and repeating ones are inconsistent with originating from the same underlying distribution, i.e., p 2DKS ≈ 1.18 × 10−10. For the E-statistic, the energy distance of ∼75 (p Energy ∼ 5 × 10−4) confirms the statistical differences between the 2D distributions.
Paper: One-off and Repeating Fast Radio Bursts: A Statistical Analysis
Authors: Hao-Yan Chen, Wei-Min Gu, Mouyuan Sun, Tuan Yi
Figure caption: The probability density distributions of L p (left) and intrinsic temporal widths (right) for one-off FRBs and repeating ones. In both panels, the red lines show the mean distributions of one-off control samples and the black lines represent the mean distributions of repeating mock samples. All shadow areas indicate the 2σ (95%) confidence intervals. The distributions of L p show that the peak luminosities of one-off sources are, on average, higher than the repeating ones. The distributions are inconsistent with arising from the same FRB group (i.e., p AD < 0.001, p KS ≈ 2 × 10−6). Furthermore, as shown by the distributions of temporal widths, the pulse temporal widths of repeating FRBs are, on average, longer than the one-off ones. There is evidence that two FRB populations might originate from different underlying distributions, i.e., p AD < 0.001 and p KS ≈ 2.5 × 10−5.
Paper: One-off and Repeating Fast Radio Bursts: A Statistical Analysis
Authors: Hao-Yan Chen, Wei-Min Gu, Mouyuan Sun, Tuan Yi
Figure caption: Top: the distributions of waiting times (WTs) of three active repeating FRBs. The WT distributions of FRB 20121102A show a bimodal structure, whereas other FRBs, i.e., FRBs 20180916B and 20201124A, have unimodal structures. Bottom: the CDFs of WTs of three FRBs. Three distribution models, i.e., the bent power law (BPL; red line), the simple power law (SPL; dashed red line), and the Weibull model (black line), are considered to fit the CDFs of WTs. The data for FRB 20121102A is taken from Li et al. (2021b); the data for FRB 20180916B are taken from Chawla et al. (2020), CHIME/FRB Collaboration et al. (2020), Marthi et al. (2020), Pastor-Marazuela et al. (2021), and Pleunis et al. (2021b); and the data for FRB 20201124A are taken from Hilmarsson et al. (2021) and Marthi et al. (2022).
Paper: One-off and Repeating Fast Radio Bursts: A Statistical Analysis
Authors: Hao-Yan Chen, Wei-Min Gu, Mouyuan Sun, Tuan Yi
Figure caption: The probability density distributions of DME (the left panel) and L p (the right panel) for a random realization of the repeating mock and the one-off control samples. For the distribution of DME, two samples should arise from the same group, i.e., p KS ≈ 0.95. For the distribution of L p, two mock samples could originate from different underlying distributions since p KS ≈ 4.16 × 10−6.
Paper: One-off and Repeating Fast Radio Bursts: A Statistical Analysis
Authors: Hao-Yan Chen, Wei-Min Gu, Mouyuan Sun, Tuan Yi
Figure caption: The joint distributions of the WTs and the luminosity differences ﹩{\rm{\Delta }}{L}_{{\rm{p}}}=\mathrm{log}({L}_{{\rm{p}},\ {\rm{i}}+1})-\mathrm{log}\ ({L}_{{\rm{p}},\ {\rm{i}}})﹩. Three active repeaters should originate from distinct groups, i.e., for FRBs 20121102A and 20180916B, the energy distance is ∼26,128 (p Energy ∼ 1 × 10−4); for FRBs 20121102A and 20201124A, the energy distance is ∼8562 (p Energy ∼ 7 × 10−4); and for FRBs 20180916B and 20201124A, the energy distance is ∼5719 (p Energy ∼ 5 × 10−4).
Paper: GRB 110213A: A Study of Afterglow Electromagnetic Cascade Radiation
Authors: Xiang-Gao Wang, Yuan-Zhuo Chen, Xiao-Li Huang, Liang-Jun Chen, WeiKang Zheng, Valerio D'Elia, Massimiliano De Pasquale, Alexei S. Pozanenko, Li-Ping Xin, Giulia Stratta, Tilan Ukwatta, Carl Akerlof, Jin-Jun Geng, Xu-Hui Han, Veli-Pekka Hentunen, E. V. Klunko, N. Paul M. Kuin, Markku Nissinen, W. Rujopakarn, V. V. Rumyantsev, E. S. Rykoff, Tuomo Salmi, B. E. Schaefer, A. A. Volnova, Xue-Feng Wu, Jian-Yan Wei, En-Wei Liang, Bing Zhang, Alexei V. Filippenko
Figure caption: X-ray and 15 optical light curves of GRB 110213A, and our empirical fit with multiple broken-power laws for the multiwavelength afterglow. The vertical dashed lines mark the phases of interest for the afterglow spectral analysis. Some data are taken from Cucchiara et al. (2011).
Paper: One-off and Repeating Fast Radio Bursts: A Statistical Analysis
Authors: Hao-Yan Chen, Wei-Min Gu, Mouyuan Sun, Tuan Yi
Figure caption: Left: the p-value of the K-S test for the DME distributions of the two mock samples in the 10,000 simulations. Right: the same as the left panel, but for L p. For all simulations, the p-value for DME is always larger than 0.05. For 90% of simulations, the p-value for L p is smaller than 0.05.
Paper: GRB 110213A: A Study of Afterglow Electromagnetic Cascade Radiation
Authors: Xiang-Gao Wang, Yuan-Zhuo Chen, Xiao-Li Huang, Liang-Jun Chen, WeiKang Zheng, Valerio D'Elia, Massimiliano De Pasquale, Alexei S. Pozanenko, Li-Ping Xin, Giulia Stratta, Tilan Ukwatta, Carl Akerlof, Jin-Jun Geng, Xu-Hui Han, Veli-Pekka Hentunen, E. V. Klunko, N. Paul M. Kuin, Markku Nissinen, W. Rujopakarn, V. V. Rumyantsev, E. S. Rykoff, Tuomo Salmi, B. E. Schaefer, A. A. Volnova, Xue-Feng Wu, Jian-Yan Wei, En-Wei Liang, Bing Zhang, Alexei V. Filippenko
Figure caption: Modeling the multiwavelength light curves with an external-shock model by cascade emission. The synchrotron + SSC and cascade emission are represented with dotted and dotted–dashed lines, respectively. The best-fitting model parameters are ﹩{E}_{{\rm{K}},\mathrm{iso}}={5.01}_{-3.43}^{+4.54}\times {10}^{53}﹩ erg, ﹩{{\rm{\Gamma }}}_{0}={120}_{-16}^{+21}﹩, ﹩{\epsilon }_{e}={0.25}_{-0.05}^{+0.04}﹩, ﹩{\epsilon }_{B}={6.5}_{-2.6}^{+8.0}\times {10}^{-4}﹩, ﹩n={0.27}_{-0.08}^{+0.19}﹩ cm−3, ﹩{\theta }_{j}={0.32}_{-0.20}^{+0.26}﹩ rad, and ﹩k={1.0}_{-0.3}^{+0.3}﹩.
Paper: GRB 110213A: A Study of Afterglow Electromagnetic Cascade Radiation
Authors: Xiang-Gao Wang, Yuan-Zhuo Chen, Xiao-Li Huang, Liang-Jun Chen, WeiKang Zheng, Valerio D'Elia, Massimiliano De Pasquale, Alexei S. Pozanenko, Li-Ping Xin, Giulia Stratta, Tilan Ukwatta, Carl Akerlof, Jin-Jun Geng, Xu-Hui Han, Veli-Pekka Hentunen, E. V. Klunko, N. Paul M. Kuin, Markku Nissinen, W. Rujopakarn, V. V. Rumyantsev, E. S. Rykoff, Tuomo Salmi, B. E. Schaefer, A. A. Volnova, Xue-Feng Wu, Jian-Yan Wei, En-Wei Liang, Bing Zhang, Alexei V. Filippenko
Figure caption: Broadband SEDs of GRB afterglows at early times (t = 100, 300, and 1000 s after the trigger) and at a late time (t = 10 hr after the trigger). Other parameter values used are E K,iso = 5.01 × 1053 erg, Γ0 = 120, ϵ  e  = 0.25, ϵ  B  = 6.5 × 10−4, n = 0.27 cm−3, θ  j  = 0.32 rad, and k = 1.0. The yellow dashed lines represent the emission from the SSC process without considering absorption in the source. The solid lines represent the sum of the emission from the synchrotron radiation (dotted lines) and the absorbed radiation of the SSC component (dashed lines).
Paper: Revisiting the Hubble Constant, Spatial Curvature, and Cosmography with Strongly Lensed Quasar and Hubble Parameter Observations
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Shuaibo Geng
Figure caption: The 1D marginalized probability distributions and 2D regions with 1σ and 2σ contours corresponding to these parameters (H 0, Ω k , q 0, j 0) in cosmography using third-order Taylor series expansion, constrained by the six time-delay measurements and cosmic chronometer data.
Paper: GRB 110213A: A Study of Afterglow Electromagnetic Cascade Radiation
Authors: Xiang-Gao Wang, Yuan-Zhuo Chen, Xiao-Li Huang, Liang-Jun Chen, WeiKang Zheng, Valerio D'Elia, Massimiliano De Pasquale, Alexei S. Pozanenko, Li-Ping Xin, Giulia Stratta, Tilan Ukwatta, Carl Akerlof, Jin-Jun Geng, Xu-Hui Han, Veli-Pekka Hentunen, E. V. Klunko, N. Paul M. Kuin, Markku Nissinen, W. Rujopakarn, V. V. Rumyantsev, E. S. Rykoff, Tuomo Salmi, B. E. Schaefer, A. A. Volnova, Xue-Feng Wu, Jian-Yan Wei, En-Wei Liang, Bing Zhang, Alexei V. Filippenko
Figure caption: Opacity of photon (afterglow phase) with energy 1 TeV in the source as a function of time. The green line represents the case of our parameters (E K,iso = 5.01 × 1053 erg, Γ0 = 120, ϵ  e  = 0.25, ϵ  B  = 6.5 × 10−4, n = 0.27 cm−3, θ  j  = 0.32 rad, and k = 1.0). The gray horizontal dashed line represents τ  γ γ  = 1.
Paper: Revisiting the Hubble Constant, Spatial Curvature, and Cosmography with Strongly Lensed Quasar and Hubble Parameter Observations
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Shuaibo Geng
Figure caption: Left: the posterior probability density function of the Hubble constant in third-order Taylor series expansion in a flat universe. Right: the posterior probability density function of the spatial curvature parameter in third-order Taylor series expansion with fixed H 0 = 73.24 km s−1 Mpc−1.
Paper: Revisiting the Hubble Constant, Spatial Curvature, and Cosmography with Strongly Lensed Quasar and Hubble Parameter Observations
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Shuaibo Geng
Figure caption: The 1D marginalized probability distributions and 2D regions with 1σ and 2σ confidence levels for the parameters (H 0, q 0, j 0) obtained with the cosmic chronometer data.
Paper: GRB 110213A: A Study of Afterglow Electromagnetic Cascade Radiation
Authors: Xiang-Gao Wang, Yuan-Zhuo Chen, Xiao-Li Huang, Liang-Jun Chen, WeiKang Zheng, Valerio D'Elia, Massimiliano De Pasquale, Alexei S. Pozanenko, Li-Ping Xin, Giulia Stratta, Tilan Ukwatta, Carl Akerlof, Jin-Jun Geng, Xu-Hui Han, Veli-Pekka Hentunen, E. V. Klunko, N. Paul M. Kuin, Markku Nissinen, W. Rujopakarn, V. V. Rumyantsev, E. S. Rykoff, Tuomo Salmi, B. E. Schaefer, A. A. Volnova, Xue-Feng Wu, Jian-Yan Wei, En-Wei Liang, Bing Zhang, Alexei V. Filippenko
Figure caption: Corner plot showing the results of our MCMC parameter estimation with an external shock and cascade emission model, and histograms on the diagonal showing the marginalized posterior densities for each parameter. A two-dimensional projection of the sample is plotted to reveal covariances. The uncertainties are computed as the 16th and 84th percentiles of the posterior samples along each axis, thus representing 1σ confidence ranges shown with black dashed vertical lines. Our best-fit parameters are also indicated with black dashed vertical lines.
Paper: GRB 110213A: A Study of Afterglow Electromagnetic Cascade Radiation
Authors: Xiang-Gao Wang, Yuan-Zhuo Chen, Xiao-Li Huang, Liang-Jun Chen, WeiKang Zheng, Valerio D'Elia, Massimiliano De Pasquale, Alexei S. Pozanenko, Li-Ping Xin, Giulia Stratta, Tilan Ukwatta, Carl Akerlof, Jin-Jun Geng, Xu-Hui Han, Veli-Pekka Hentunen, E. V. Klunko, N. Paul M. Kuin, Markku Nissinen, W. Rujopakarn, V. V. Rumyantsev, E. S. Rykoff, Tuomo Salmi, B. E. Schaefer, A. A. Volnova, Xue-Feng Wu, Jian-Yan Wei, En-Wei Liang, Bing Zhang, Alexei V. Filippenko
Figure caption: SED analysis of GRB 110213A. The dashed lines show the intrinsic power-law spectra derived from X-ray afterglow. The photon indices are also marked.
Paper: Revisiting the Hubble Constant, Spatial Curvature, and Cosmography with Strongly Lensed Quasar and Hubble Parameter Observations
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Shuaibo Geng
Figure caption: The 1D marginalized probability distributions and 2D regions with 1σ and 2σ contours corresponding to these parameters (H 0, Ω k , q 0, j 0) in the (2, 1) order Padé expansion, constrained by the six time-delay measurements and cosmic chronometer data.
Paper: Revisiting the Hubble Constant, Spatial Curvature, and Cosmography with Strongly Lensed Quasar and Hubble Parameter Observations
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Shuaibo Geng
Figure caption: Reconstructed Hubble expansion history by using third-order Taylor series and (2, 1) order Padé expansions.
Paper: Revisiting the Hubble Constant, Spatial Curvature, and Cosmography with Strongly Lensed Quasar and Hubble Parameter Observations
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Shuaibo Geng
Figure caption: The same as Figure 3, but using the (2, 1) order Padé expansion.