adsabs/AstroCLIMB huggingface dataset:
Paper: Emergence of the Galaxy Morphology–Star Formation Activity–Clustercentric Radius Relations in Galaxy Clusters
Authors: Sungwook E. Hong, Changbom Park, Preetish K. Mishra, Juhan Kim, Brad K. Gibson, Yonghwi Kim, C. Gareth Few, Christophe Pichon, Jihye Shin, Jaehyun Lee
Figure caption: Time evolution of Sérsic index (top) and sSFR (bottom) with stellar mass for top-20% massive HR5 central galaxies (d(z f) < 0.1R 200;  solid) and outskirts galaxies (0.3 < d(z f)/R 200 < 1;  dashed) from z = 3.6 (red) to 0.625 (purple). Thick lines and thin crossbars correspond to the median and 68% percentiles at the given time, respectively.
Paper: Emergence of the Galaxy Morphology–Star Formation Activity–Clustercentric Radius Relations in Galaxy Clusters
Authors: Sungwook E. Hong, Changbom Park, Preetish K. Mishra, Juhan Kim, Brad K. Gibson, Yonghwi Kim, C. Gareth Few, Christophe Pichon, Jihye Shin, Jaehyun Lee
Figure caption: Similar to Figure 3, showing the detailed evolution of various parameter–parameter relations for the first (left), second (middle), and fifth (right) most massive HR5 cluster galaxies from z = 6 (red) to 0.625 (purple). The Sérsic parameter with null values at snapshots with A > 0.4 is shown as dashed lines.
Paper: Emergence of the Galaxy Morphology–Star Formation Activity–Clustercentric Radius Relations in Galaxy Clusters
Authors: Sungwook E. Hong, Changbom Park, Preetish K. Mishra, Juhan Kim, Brad K. Gibson, Yonghwi Kim, C. Gareth Few, Christophe Pichon, Jihye Shin, Jaehyun Lee
Figure caption: Similar to Figure 7, showing the three selected HR5 cluster galaxies with M * < 1011 M ⊙ and d/R 200 > 0.3 at z = 0.625.
Paper: Emergence of the Galaxy Morphology–Star Formation Activity–Clustercentric Radius Relations in Galaxy Clusters
Authors: Sungwook E. Hong, Changbom Park, Preetish K. Mishra, Juhan Kim, Brad K. Gibson, Yonghwi Kim, C. Gareth Few, Christophe Pichon, Jihye Shin, Jaehyun Lee
Figure caption: Evolution of clustercentric radial profiles of galaxy morphology (left) and type (right) fractions from z = 1 to 0.625 (top to bottom). Error bars: Poisson error estimated from each radial bin.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: Posterior densities for the mass of GW230529 under different binary evolution assumptions. We also include the distributions of the log-likelihood and log-prior of the posterior samples. The dotted lines in the first two rows denote the maximum-likelihood estimates of m BH and m NS, respectively.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: KN light curves in the i band corresponding to the different population models for the H4 EOS. The dotted line shows the light curve associated with the maximum-likelihood parameter estimates for each model.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: The probability density function (PDF) for the total ejecta mass for different EOSs and corresponding to the various population models. No ejecta was obtained for the APR4 EOS.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: Posterior densities for the remnant BH mass and spin under different binary evolution assumptions. These quantities are computed from NR fits of BHNS binaries using the posteriors from Section 3.2 and the EOS information coming from multimessenger analyses of GW170817 and AT2017gfo. For most of the scenarios considered, we find ﹩{M}_{f}={5.3}_{-0.1}^{+0.1}\,{M}_{\odot }﹩ and ﹩{a}_{f}={0.53}_{-0.01}^{+0.01}﹩.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: Predicted component mass distributions for BHNS (top panel) and NSBH systems (bottom panel) across varying subsolar metallicities, as outlined in D. Chattopadhyay et al. (2021). As can be observed, NSBH systems tend to produce binaries with lighter BHs across different metallicities.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: Posterior densities for the mass of GW230529 as inferred using the population-inspired BHNS (top panel) and NSBH (bottom panel) priors described in Section 3.1. In the right-hand column, we include the log-likelihood ratio distribution.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: Predicted BHNS component mass distributions. Each row shows the 15 different population-synthesis variations used by F. S. Broekgaarden et al. (2021).
Paper: Global Simulation of the Solar Wind: A Comparison with Parker Solar Probe Observations during 2018–2022
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Y. M. Wang
Figure caption: A sequence of synoptic maps at 2.5 R ⊙ for 2018–2022 derived from the Wilcox Solar Observatory (WSO) photospheric measurements using the PFSS model. The Carrington rotation numbers are provided on the top of the figure. The x-axis represents the time/year of maps, and the y-axis represents the solar latitude (in degrees). The color bar, which provides the scale of the radial magnetic field (B  r ), is given at the bottom of the figure. The minimum (=−0.41 Gauss) and maximum (=0.43 Gauss) values of B  r  are listed near the bottom left corner.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: Match ﹩{ \mathcal F }﹩ and sky-maximized match ﹩{{ \mathcal F }}_{\mathrm{SM}}﹩ between polarizations constructed using the dominant quadrupolar (top) and subdominant (bottom) modes of TEOBResumS-GIOTTO and IMRPhenomNSBH. We consider posterior samples from the fiducial PE and compute ﹩{ \mathcal F }﹩ between 20 and 1796 Hz. Depending on whether higher modes are employed or not, we find median mismatches of about ∼1.4% (0.8%) and maximum mismatches of ∼3% (∼2%), corresponding to systems with large tidal parameters Λ2 > 3000. Overlaid, we also plot the tidal parameters obtained with a few selected EOSs, assuming a fixed BH source-frame mass of 4.2 M ⊙.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: The mass–radius curves for the EOSs chosen in this study. We also show the BSK24 EOS, which was used by LVK.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: The posterior distribution of the primary and secondary source masses for two different waveform models—TEOBResumS-GIOTTO and IMRPhenomNSBH. Each contour shows the 90% credible intervals. We find that the resulting parameter estimates are robust to possible waveform systematics, with good agreement between the two waveform models.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: The distribution of the peak luminosity in the g and r bands for the DD2 EOS corresponding to samples from the “fiducial” population model. The black dotted line shows the peak luminosity corresponding to the maximum-likelihood binary parameters.
Paper: On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Koustav Chandra, Ish Gupta, Rossella Gamba, Rahul Kashyap, Debatri Chattopadhyay, Alejandra Gonzalez, Sebastiano Bernuzzi, B. S. Sathyaprakash
Figure caption: KN light curves in the i band corresponding to the different population models for the DD2 EOS. The dotted line shows the light curve associated with the maximum-likelihood parameter estimates for each model.
Paper: Global Simulation of the Solar Wind: A Comparison with Parker Solar Probe Observations during 2018–2022
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Y. M. Wang
Figure caption: Comparison of PSP in situ solar wind plasma and magnetic field data vs. G3DMHD simulation results during 2018–2022. Panels from top to bottom panels are temperature (units in K), magnetic field (B in nT), velocity in the radial (r) direction (V  r  in km s–1), number density (N  p  in  no. cm−3), and the location of the Parker Solar Probe (PSP) spacecraft (black, blue, and orange lines are the distance from the center of the Sun to the PSP, latitude, and longitude location of the PSP, respectively.
Paper: Global Simulation of the Solar Wind: A Comparison with Parker Solar Probe Observations during 2018–2022
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Y. M. Wang
Figure caption: Same format as Figure 3. The input of the magnetic field intensity at inner boundary has a scaling factor as SB = 4.63–0.767 × (f yr − 2018), where f yr is the fractional year of the PFSS result.
Paper: Global Simulation of the Solar Wind: A Comparison with Parker Solar Probe Observations during 2018–2022
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Y. M. Wang
Figure caption: Selected snapshots of G3DMHD-simulated solar wind radial velocity in chronicle. Top to bottom in order from 2018 to 2022. In each row (left to right), there are four maps corresponding to March, June, September, and December at a plane defined by θ = 2.°5N.
Paper: Global Simulation of the Solar Wind: A Comparison with Parker Solar Probe Observations during 2018–2022
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Y. M. Wang
Figure caption: Same format as Figure 3. The input of the magnetic field intensity at inner boundary employs a uniform Br  along a fixed longitude.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Hycean and mini-Neptune scenarios with two photochemical models. Top row: original simulations from N. F. Wogan et al. (2024), showing the mixing ratio of molecules against atmospheric pressure in bar. Bottom row: VULCAN simulations of the same scenarios with equivalent assumptions (see main text). The scenarios are: an uninhabited Hycean (left column), an inhabited Hycean (middle column), and a mini-Neptune case (right column). The given molecular constraints are from the “one offset” case (N. Madhusudhan et al. 2023b) because this case gives the best fit to the observed data. 1σ error bars are given for detected molecules (CH4 in orange; CO2 in green), and 2σ upper limits are given for CO (purple), H2O (blue), and NH3 (gray), which were not detected by N. Madhusudhan et al. (2023b). The photosphere—the region in the atmosphere that impacts the transmission spectrum observed—is given in a light gray shade between 10−2 and 10−4 bar. A variety of simulations were run with both the W24 setup (see Table A1) and VULCAN (see Table A2). All of the simulations shown in this figure use the GJ 176 spectrum. Only the inhabited Hycean scenarios in both models are consistent with the retrieved abundances.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Mini-Neptune scenario for K2-18 b using the W24 setup (PICASO and Photochem). The predicted mixing ratios for different metallicities (200 ×, 100 ×, 50 ×, 30 × solar metallicity, denoted by M/H) are shown by the shaded regions, indicating the maximum deviations between the different simulations. The various simulations used different cross-section sources and resolutions in the first and third rows, assuming the host star is represented by GJ 176, and the internal temperature (T int) is 60 K. The second and fourth rows show the same, but this time including all the same simulations but with GJ 176, GJ 849, and GJ 436 as the host stars. The photosphere is marked in light gray. 1σ constraints are given for detected molecules (CH4 and CO2) using the values from N. Madhusudhan et al. (2023b), while 2σ upper limits are given by the arrows for NH3, H2O, and CO. The colors used for the constraints are the same as those used in Figure 3, with SO2 and H2S also shown in light blue and pink, respectively. The thick lines in each panel show the results when GJ 176 is used with Photochem cross sections.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Mini-Neptune scenario with different Bond albedos. These simulations used the W24 setup for the mini-Neptune scenario for K2-18 b, showing the standard 100 × solar metallicity scenario with no albedo (solid lines) and the 0.4 top-of-atmosphere albedo case (dashed lines). The photosphere is marked in light gray. 1σ constraints are given for detected molecules (CH4 and CO2) using the “one offset” values from N. Madhusudhan et al. (2023b), while 2σ upper limits are given by the arrows for NH3, H2O, and CO. In the 0.4 albedo case, H2O is on the border of the upper limit, with CO2 still lower than its 1σ limit, and CO and NH3 remain too high.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption:  P– T profiles for Hycean and mini-Neptune scenarios. The two pressure–temperature profiles that are used in W24 are for the Hycean (red) and mini-Neptune (black) atmospheric simulations at pressures less than 1 bar. At pressures less than 3 × 10−3 bar, the temperature is 215 K in both models. Two further mini-Neptune models that we simulated show the mini-Neptune temperature profiles when 30% (magenta) and 40% (light blue) of radiation is reflected off the top of the atmosphere, represented by A = 0.3 and A = 0.4 in the figure, respectively.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Photochemical modeling of an uninhabited Hycean scenario for K2-18 b using VULCAN with a surface pressure of (a) 25 bar and (b) 50 bar. The GJ 436 spectrum with a varied UV albedo is implemented in the model. The P–T profile is PT3 from N. Madhusudhan et al. (2023a). Different initial metallicities of between 100 and 200 times solar metallicity are used. In the uninhabited Hycean scenario, the inclusion of sulfur (labeled S in the legend) in the photochemical network affects the abundance of CO. The uninhabited simulations have no imposed flux for CH4 at the planetary surface. CO2 has a fixed mixing ratio of 1 × 10−3 (25 bar cases) and 2 × 10−3 (50 bar cases). The mixing ratios of CH4, CO2, CO, H2O, and NH3 are plotted against atmospheric pressure. The constraints and colors are the same as in Figure 1. Depending on the assumed physical conditions and the chemical network used, the uninhabited Hycean scenario can be shown to be consistent with the retrieved abundance constraints from JWST observations (N. Madhusudhan et al. 2023b) for all five molecules.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Photodissociation cross sections for 12 molecules are compared across three models. Cross sections (σ  λ ) in terms of cm2 molecule−1 are shown for H2O, CH4, H2, CO, CO2, and NH3 in the left column on a log scale vs. wavelength in nanometers, and the right column shows the cross sections for HO2, HCN, CS2, H2S, C2H6, and OCS vs. wavelength in nanometers. Available cross sections in Atmos and Photochem are shown in red and light blue, respectively. VULCAN has cross sections given in terms of absorption (gray) and dissociation (black). The vertical magenta dotted line shows where the Photochem photolysis grid starts at 92.5 nm.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Inhabited Hycean scenario for K2-18 b using VULCAN. The GJ 176 spectrum with a top-of-atmosphere albedo of 0.3 is used, as in W24, with the same P–T and K zz profile as W24. The inhabited Hycean scenario imposes a flux for CH4 at the planetary surface of 8 × 109 molecules cm−2 s-1 and starts with a CH4 volume mixing ratio of 10−10. CO2 has a fixed mixing ratio at the surface of 8 × 10−3. The mixing ratios of CH4, CO2, CO, H2O, and NH3 are plotted against atmospheric pressure. The constraints and colors are the same as in Figure 1. This inhabited Hycean scenario is consistent with the retrieved abundance constraints from JWST observations (N. Madhusudhan et al. 2023b) for all five molecules, similar to the W24 inhabited Hycean scenario.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Hycean scenarios for K2-18 b using the W24 setup. The photochemical modeling uses Photochem in the W24 setup for an uninhabited Hycean case (left column) and an inhabited Hycean case (right column). The first, second, and third rows use Photochem, VULCAN, and Atmos cross sections, respectively (see Appendix B). The solid lines, dashed lines, and long-dashed lines are with native cross sections using the GJ 176, GJ 436, and GJ 849 spectra, respectively. The dashed–double-dotted lines, dotted lines, and dashed–dotted lines are with binned cross sections using the GJ 176, GJ 436, and the GJ 849 spectra, respectively. The final row shows shaded regions that display the range of results for all perturbations in the top three rows. The thick lines in the final row also show the original W24 results. The “observable” portion of the atmosphere and the molecular constraints are marked as in Figure 1.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Branching ratios for four molecules compared between three models. Photolysis channels and their respective branching ratios are shown for H2O, NH3, CO2, and CH4 vs. wavelength in nanometers. The data are taken from VULCAN, Atmos, and Photochem, and are shown in black, red, and light blue, respectively. H2O branching ratio data from Photochem and VULCAN match, but they differ for Atmos. The data for the three other molecules do not match. Additionally, not all three models consider the same photolysis channels.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Mini-Neptune scenario for K2-18 b using VULCAN. The mini-Neptune simulations use the same P–T and K zz profiles as were used in W24 from 10−8 to 500 bar. The colors and constraints are the same as in Figure 1. The solid line is a 100 × solar metallicity case, the dashed line is a 50 × solar metallicity case, and the dotted line is a 200 × solar metallicity case. None of the cases are consistent with all five retrieved abundances. The predicted abundances are comparable to those produced when using the W24 setup.
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: Stellar spectra for four M dwarf stars. The flux density of MUSCLES stars vs. wavelength in nanometers is plotted for the following stars: GJ 163 (gray), GJ 176 (black), GJ 436 (light blue), and GJ 849 (magenta). The spectra are normalized to the irradiance K2-18 b receives, which is 1368 W m−2. These stars are all reported to be between M2.5V and M3.5V, with associated errors in observations (see main text, Figure C2, and Table C1).
Paper: Considerations for Photochemical Modeling of Possible Hycean Worlds
Authors: G. J. Cooke, N. Madhusudhan
Figure caption: The uncertainty in the stellar spectra for four stars at UV/VIS wavelengths. The fractional error in flux density of MUSCLES stars vs. wavelength in nanometers is plotted for the following stars: GJ 163 (gray), GJ 176 (black), GJ 436 (light blue), and GJ 849 (magenta). The black dotted line shows where the reported error in flux is equal to the flux.
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: Empirical XLFs for galaxy subsamples with (a) metallicity in the range of ≈ 0.6–1.6 Z ⊙ and groupings based on sSFR, and (b) ﹩\mathrm{log}﹩ sSFR ≥ −10 in groupings based on metallicity (see annotations). These empirical XLFs have been corrected for completeness and estimates of CXB contributions have been subtracted. They provide proxies for how the XRB XLFs vary with stellar population age (a) and metallicity (b). We find that with increasing stellar age, the XLF normalization per M ⋆ declines, and the shape of the XLF transitions to becoming flatter at L ≲ 1037.5 erg s−1 and steeper at L > 1037.5 erg s−1 (a). With increasing metallicity, we find that the high-sSFR XRB population XLFs become steeper and contain fewer L > 1038 erg s−1 sources (b). These observed trends motivate the construction of our age- and metallicity-dependent XLF modeling (see Section 5.2 for details).
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: Galaxy-integrated intrinsic 0.5–8 keV luminosity per SFR, L X/SFR, vs. sSFR, for the full sample of 88 galaxies. Each symbol is color-coded by gas-phase metallicity (see color bar) and our best-fit model for the dependence of L X on SFR and M ⋆ (see Equation (11)) is shown as a solid-black curve. For comparison, we have overlaid the best fit from the L19 gray curve and two relations from K. Kouroumpatzakis et al. (2020) appropriate for regions of size 4 × 4 kpc2 (gold-dashed curve) and 1 × 1 kpc2 (gold-dotted curve).