adsabs/AstroCLIMB huggingface dataset:
Paper: Parametric Instability of Alfvén Waves and Wave Packets in Periodic and Open Systems
Authors: Maile Marriott, Anna Tenerani
Figure caption: Growth rate γ as a function of cos(θ) for the chosen target amplitudes ﹩\tilde{\eta }﹩. The color scale of the dots shows the amplitude deviation from the target ﹩\tilde{\eta }﹩, defined as ﹩(\tilde{\eta }-{{dB}}_{z})/\tilde{\eta }\times 100﹩. In general increasing the polarization angle decreases γ. For the green and orange points, the fastest growing mode shifts from our chosen k (see Figure 2), leading to a maximum of γ. The data for these points are given in Table 1 of Appendix B.
Paper: Parametric Instability of Alfvén Waves and Wave Packets in Periodic and Open Systems
Authors: Maile Marriott, Anna Tenerani
Figure caption: Pump wave configurations for (a) a circularly polarized (Equation (20)) and (b) an arc-polarized wave packet (Equation (21)). B  y  (orange) and B  z  (blue) are defined by Equations (5) and (6). The parameters are set to η = 0.84 for (a), η = 1 for (b), and ϵ = 1, k 0 = 4, and ℓ = 10, in a box size L = 20π.
Paper: A Merger-driven Scenario for Clumpy Galaxy Formation in the Epoch of Reionization: Physical Properties of Clumps in the FirstLight Simulation
Authors: Yurina Nakazato, Daniel Ceverino, Naoki Yoshida
Figure caption: The O III λ5007 luminosity vs. SFR for our 62 simulated galaxies at z = 9 (purple), 8 (blue), 7 (green), and 6 (yellow).
Paper: Parametric Instability of Alfvén Waves and Wave Packets in Periodic and Open Systems
Authors: Maile Marriott, Anna Tenerani
Figure caption: Normalized growth rate for the periodic and open boundary cases of an arc-polarized wave for fixed ℓ = 10 values. Dashed lines represent a power law γ/ω 0 ∼ (ℓ/L) m , where m ≃ 1.
Paper: Parametric Instability of Alfvén Waves and Wave Packets in Periodic and Open Systems
Authors: Maile Marriott, Anna Tenerani
Figure caption: An approximation of a system where the pump wave is limited to a finite region of width ℓ in a box.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The K  s -band from 2005.366 observation. The K  s -band image denotes 11 regions in addition to the assumed region of IRS 1W. These 11 regions are chosen randomly in order to identify the number of sources in each one. The only criterion is the distance from Sgr A*; all regions are located at a distance of almost 6″ from Sgr A*. The radii of all circular regions are about 1.″3.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: SEDs of ADAFs associated with the putative IMBH at the geometrical center of the NW-ward flying sources. Different black lines stand for the accretion rates according to the legend. For comparison, we also show the SED of Sgr A* (gray dotted line). The red point depicts the X-ray emission upper limit.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The Chandra X-ray image from 4 to 8 keV. The north is up and east is to the left. Distinct X-ray bright sources are labeled, namely Sgr A*, IRS 13, and the pulsar wind nebula. There is no significant X-ray source at the position of the N-source association. The angular scale is indicated in the upper left corner.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: Gaussian fit of the spatial distribution of NW-flying sources.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The Chandra X-ray image from 0.5 to 8 keV. North is up and east is to the left. Distinct X-ray bright sources are labeled, namely Sgr A*, IRS 13, and the pulsar wind nebula. There is no significant X-ray source at the position of the N-source association. The angular scale is indicated in the upper left corner.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The plots show the derived positions of the N2 star as a function of time, along with the best-fitting proper motions. The left panel is along the R.A. and the right panel is along the decl. The slope of each best-fitting line is given in Table 3 (in kilometers per second).
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: Top: face-on view of the east–west (EW) stellar disk system with outer and inner radii given in the text. For the case of s1, we indicated the corresponding quantities. Bottom: the disk system is inclined by 80°. The clustering at the eastern and western tips of the disk becomes evident.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: Stellar sky surface density in arbitrary units as a function of radius in the EW direction in arcseconds. Here also, the clustering at the eastern and western tips of the disk becomes evident. The source density is almost a factor of 2 higher than in the northern and southern parts of the disk.
Paper: Digging into the Ultraviolet Luminosity Functions of Galaxies at High Redshifts: Galaxies Evolution, Reionization, and Cosmological Parameters
Authors: Yi-Ying Wang, Lei Lei, Shao-Peng Tang, Guan-Wen Yuan, Yi-Zhong Fan
Figure caption: The left panel shows the observations of UV LFs (extinction corrected) and the best-fit results in the redshift range of 4 ≤ z ≤ 10. The right panel shows the corresponding distributions of SFE. The colored regions are at the 68% credible level. The light orange region represents the range of maximum value (20%–30%) of SFE (R. H. Wechsler & J. L. Tinker 2018). Due to the redshift-dependent nature of SFE, which connects all observations at each redshift, the estimated UV LFs are tightly constrained.
Paper: Digging into the Ultraviolet Luminosity Functions of Galaxies at High Redshifts: Galaxies Evolution, Reionization, and Cosmological Parameters
Authors: Yi-Ying Wang, Lei Lei, Shao-Peng Tang, Guan-Wen Yuan, Yi-Zhong Fan
Figure caption: The evolution of the derived cosmic SFR density and UV luminosity density. The blue and red solid lines depict the best-fit values of UV LFs with M trunc = –17 and M trunc = –15, respectively. The blue and red dotted lines are the pseudo extrapolation to the low redshift range. The light blue and red shading indicate the 90% credible regions. The orange dashed line denotes the analytical form derived by P. Madau & M. Dickinson (2014). The gray region 0 ≤ z ≤ 4 implies that the galaxy evolution is in a highly nonlinear stage, which cannot be analyzed using the UV LF model. The black error bars are not considered in Bayesian analysis and are solely included for comparison with our predictions. These observations encompass the radio, near-infrared, Hα, and UV bands at the redshift range of 4 ≤ z ≤ 10.5 (P. Madau & M. Dickinson 2014; R. J. Bouwens et al. 2015; S. L. Finkelstein et al. 2015; D. J. McLeod et al. 2016; B. P. Moster et al. 2018; R. Bouwens et al. 2020; Y. Harikane et al. 2023).
Paper: Digging into the Ultraviolet Luminosity Functions of Galaxies at High Redshifts: Galaxies Evolution, Reionization, and Cosmological Parameters
Authors: Yi-Ying Wang, Lei Lei, Shao-Peng Tang, Guan-Wen Yuan, Yi-Zhong Fan
Figure caption: The evolution of the IGM neutral fraction. The black error bars and the purple bounds are the fitting data listed in Table 2. The red and blue lines correspond to the results shown in Figure 4. The light-colored regions indicate the 90% confidence level.
Paper: Digging into the Ultraviolet Luminosity Functions of Galaxies at High Redshifts: Galaxies Evolution, Reionization, and Cosmological Parameters
Authors: Yi-Ying Wang, Lei Lei, Shao-Peng Tang, Guan-Wen Yuan, Yi-Zhong Fan
Figure caption: The variation of the parameter in SFE. The red (F 1(z)) and blue (F 2(z)) colors represent the models defined by B. P. Moster et al. (2018) and N. Sabti et al. (2022b), respectively. For example, ϵ N is described by ﹩{\epsilon }_{0}+{\epsilon }_{z}(\tfrac{z}{z+1})﹩ following F 1(z) or ﹩{10}^{{\epsilon }_{i}}{\left(\tfrac{1+z}{1+{z}_{* }}\right)}^{{\epsilon }_{s}}﹩ following F 2(z). Other parameters M 1, γ, and β have the same definitions. Therefore, these two different formulae need two or three free variables and represent different variable spaces. z * represents the specific redshift value defined in Equation (12).
Paper: Digging into the Ultraviolet Luminosity Functions of Galaxies at High Redshifts: Galaxies Evolution, Reionization, and Cosmological Parameters
Authors: Yi-Ying Wang, Lei Lei, Shao-Peng Tang, Guan-Wen Yuan, Yi-Zhong Fan
Figure caption: The posterior distributions of DM halo accretion rate at z = 4, 7, and 10. The solid lines represent the best-fit values. The colored regions are at the 90% credible level and represent the value of σ MAR.
Paper: Digging into the Ultraviolet Luminosity Functions of Galaxies at High Redshifts: Galaxies Evolution, Reionization, and Cosmological Parameters
Authors: Yi-Ying Wang, Lei Lei, Shao-Peng Tang, Guan-Wen Yuan, Yi-Zhong Fan
Figure caption: The results of σ 8 in three cases. To present the σ 8 tension, the purple and light orange regions represent the estimated σ 8 from Planck Collaboration et al. (2020) and T. Tröster et al. (2020), respectively.
Paper: Digging into the Ultraviolet Luminosity Functions of Galaxies at High Redshifts: Galaxies Evolution, Reionization, and Cosmological Parameters
Authors: Yi-Ying Wang, Lei Lei, Shao-Peng Tang, Guan-Wen Yuan, Yi-Zhong Fan
Figure caption: The posterior results of H 0, σ 8, and Ω m  for Case 3. The contours indicate the 68%, 95%, and 99% credible levels. The values are at the 68% credible level.
Paper: Digging into the Ultraviolet Luminosity Functions of Galaxies at High Redshifts: Galaxies Evolution, Reionization, and Cosmological Parameters
Authors: Yi-Ying Wang, Lei Lei, Shao-Peng Tang, Guan-Wen Yuan, Yi-Zhong Fan
Figure caption: The predicted distribution of τ e. The shaded pink region represents the 68% credible uncertainty range for τ e. The light orange shading corresponds to the estimation provided by Planck Collaboration et al. (2020).
Paper: Binary Yellow Supergiants in the Magellanic Clouds. I. Photometric Candidate Identification
Authors: Anna J. G. O'Grady, Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig, Ylva Götberg, B. M. Gaensler
Figure caption:  J − K vs. K color–magnitude diagrams of the SMC (left) and LMC (right). Our YSG candidates are plotted as gray circles. The Be candidates of Mennickent et al. (2002) (SMC) and Sabogal et al. (2005) (LMC) are blue circles. Our YSG candidates that matched with Be stars are yellow diamonds, and YSG+OB candidates that matched are green squares. The census of SMC/LMC WR stars from P. Massey et al. (2014) and K. F. Neugent et al. (2018b) are plotted in dark violet, and YSG or YSG+OB candidates that match are plotted as orange diamonds and red squares, respectively. We note that WR stars that overlap the YSG region but are not in our YSG sample were either removed as possible foreground contaminants or did not have complete MCPS data.
Paper: Binary Yellow Supergiants in the Magellanic Clouds. I. Photometric Candidate Identification
Authors: Anna J. G. O'Grady, Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig, Ylva Götberg, B. M. Gaensler
Figure caption: The same as Figure 6, but showing UV classifications. Top: V − I vs. W1 − U color–color diagram. Limits are shown as triangles. Bottom: The UV classifications from the top panels, but shown in V − I vs. U – B space. The locations of the previous temperature cuts in U – B are shown with light gray lines. Stars without W1 data are show as faint gray circles.
Paper: Binary Yellow Supergiants in the Magellanic Clouds. I. Photometric Candidate Identification
Authors: Anna J. G. O'Grady, Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig, Ylva Götberg, B. M. Gaensler
Figure caption: Spectral energy distributions of four YSG candidates in our sample. Four stars are shown: two have T eff ∼ 4000 K (left panel), two have T eff ∼ 6000 K (right panel), two are likely single YSGs (yellow), and two are YSG+OB binary candidates (blue). Wavelength ranges corresponding to the SUMaC, MCPS, and 2MASS surveys are shaded violet, green, and orange, respectively.
Paper: Binary Yellow Supergiants in the Magellanic Clouds. I. Photometric Candidate Identification
Authors: Anna J. G. O'Grady, Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig, Ylva Götberg, B. M. Gaensler
Figure caption: Pickles synthetic stellar spectra for G0, G8, K0, and K8 supergiants (orange to red lines) along with the filter profiles, arbitrarily scaled, for MCPS U- and B-band (black, solid, and dashed lines, respectively).
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Left: observable cold (150 K < T ex < 400 K) and hot (T ex > 400 K) water vapor mass in each disk, calculated by integrating the best-fit exponentially tapered power-law column density profiles over each temperature range. Middle: observable H2O masses as a function of stellar mass accretion rates. The Spearman correlation coefficient and p-value for the hot water mass are indicated on the top. The dashed line indicates a power-law fit. Right: same as the middle panel, but for H2O masses vs. outer submillimeter dust disk radius. The correlation coefficient corresponds to the cold H2O mass.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: The maximum log-likelihood (circles) attained for each H2O emission model fit. The labels 2T, PL, and TPL correspond to the two-temperature, power-law, and exponentially tapered power-law models, respectively. The vertical bars show the range of ﹩\mathrm{log}{\boldsymbol{ \mathcal L }}﹩ values spanned by posterior distribution samples within the 0.025–0.975 percentiles. Note that fitting a temperature gradient always results in a statistically significant improvement, except in the case of AS 209.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Top: normalized wavelength-integrated H2O flux profiles as a function of radius, extracted from the best-fit tapered N profiles. Asterisks indicate the radii where T ex reaches 150 K in each disk. Circles show the cutoff radius at which the integrated emission drops below 5σ. Bottom: the H2O cutoff radius for each disk, and the H2O excitation temperature derived at that radius. Dashed lines indicate the average values for compact (blue) and extended (red) disks.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: The contributions to the H2O spectrum fit to the GK Tau data at each radial bin, for the exponentially tapered column density model. The excitation temperature of each component is indicated on the right side. Models in green have integrated fluxes >5σ, whereas the models in orange lie below the detection threshold. In this case, we detect H2O emission with T ex down to ∼180 K.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 5, but for the exponentially tapered column density profile fits.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: The excitation temperature profiles (blue) derived for H2O in each disk with 1σ confidence regions, compared to the expected disk surface dust temperature (magenta) for different dust size distributions (see Section 4.2).
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Gaussian process decomposition of the spectrum of HP Tau. The black line shows the MIRI-MRS continuum-subtracted spectrum, the magenta line shows the conditioned squared exponential kernel, and the blue shaded region shows the best-fit ±1σ region. The latter includes the uncertainty associated with the continuum baseline fit.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Best-fit H2O emission models to the spectrum of the compact disk of FZ Tau. The two-temperature model is shown in cyan (bottom), the power-law model in blue (middle), and the exponentially tapered power-law model in violet (top of each panel). The data are shown three times in each panel, and the models are shifted vertically for clarity.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: The full MIRI-MRS spectrum of each disk (black), and the corresponding continuum emission fit (magenta).
Paper: Reconstructing the Genealogy of LIGO-Virgo Black Holes
Authors: Parthapratim Mahapatra, Debatri Chattopadhyay, Anuradha Gupta, Fabio Antonini, Marc Favata, B. S. Sathyaprakash, K. G. Arun
Figure caption: Injection and recovery of a mock 1g+3g chain in a cluster with escape speed V esc = 400 km s−1 and metallicity Z = 0.00015. The left diagram depicts the injected 1g+3g merger chain, showing the (in principle) observed binary at the top, the parent binary below, and the grandparent binary at the bottom. Given the parameters of the grandparent binary, the mass, spin, and kick values of the later generations are consistent with the predictions of NR simulations. Gaussian noise is then added to the mass and spin parameters of the 3g (top) binary. Application of the Bayesian inference method described in Section 2 then allows recovery of the merger history, as illustrated in the right part of the diagram. There, the numbers represent the 90% credible intervals on the inferred posterior distributions.
Paper: Reconstructing the Genealogy of LIGO-Virgo Black Holes
Authors: Parthapratim Mahapatra, Debatri Chattopadhyay, Anuradha Gupta, Fabio Antonini, Marc Favata, B. S. Sathyaprakash, K. G. Arun
Figure caption: Depiction of the possible merger history of the primary components of GW190426 and GW200220 as inferred by our method. The notation and units are the same as in Figure 1.
Paper: Reconstructing the Genealogy of LIGO-Virgo Black Holes
Authors: Parthapratim Mahapatra, Debatri Chattopadhyay, Anuradha Gupta, Fabio Antonini, Marc Favata, B. S. Sathyaprakash, K. G. Arun
Figure caption: The retention probability of the primary BHs of GW190521, GW200220, and GW190426 as a function of a star cluster’s escape speed. The dotted black curve shows the prior distribution. The shaded regions show the range of escape speeds for GCs and NSCs (F. Antonini & F. A. Rasio 2016). The retention probability is computed directly from the CDF of the kick magnitude following P. Mahapatra et al. (2021).
Paper: Reconstructing the Genealogy of LIGO-Virgo Black Holes
Authors: Parthapratim Mahapatra, Debatri Chattopadhyay, Anuradha Gupta, Fabio Antonini, Marc Favata, B. S. Sathyaprakash, K. G. Arun
Figure caption: Injection and recovery of a mock merger chain that produces a GW190521-like binary. The left diagram depicts the injected merger chain, showing the properties of the GW190521-like binary at the top and the parent binary below. Given the parameters of the parent binary, the mass, spin, and kick values of the later generations are consistent with the predictions of NR simulations. Gaussian noise is then added to the GW signal produced by the GW190521-like system to generate simulated noisy GW data. A Bayesian parameter estimation technique is applied to the simulated noisy GW data to estimate the posteriors on the source-frame masses and spins of the injected GW190521-like binary. Application of the Bayesian inference method described in Section 2 then allows recovery of the merger history, as illustrated in the right part of the diagram. There, the numbers represent the 90% credible intervals on the inferred posterior distributions.
Paper: Reconstructing the Genealogy of LIGO-Virgo Black Holes
Authors: Parthapratim Mahapatra, Debatri Chattopadhyay, Anuradha Gupta, Fabio Antonini, Marc Favata, B. S. Sathyaprakash, K. G. Arun
Figure caption: The left panel shows the inferred mass parameters (at 90% and 50% credibility) for the parent BBH, whose merger produced the primary BHs of GW190521, GW200220, and GW190426. The right panel shows the corresponding inferred effective spin parameters (again at 90% and 50% credibility) for those parent binaries.
Paper: Contour Analysis Tool: An Interactive Tool for Background and Morphology Analysis
Authors: Mark A. Hutchison, Christine M. Koepferl
Figure caption: A screenshot of an interactive session in CAT. Checkboxes control contour visibilities in the plot while dropdown menus, toggle buttons, and input fields select and modify the various methods and parameters. An additional toggle button sits below the figure and prints information values for contour levels and spacing (delta_levels) as well as code to reproduce the results programmatically.