adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Mass–Dispersion Measure Correlations Constrain Baryonic Feedback in Fast Radio Burst Host Galaxies
Authors: Calvin Leung, Sunil Simha, Isabel Medlock, Daisuke Nagai, Kiyoshi W. Masui, Lordrick A. Kahinga, Adam E. Lanman, Shion Andrew, Kevin Bandura, Alice P. Curtin, B. M. Gaensler, Nina Gusinskaia, Ronniy C. Joseph, Mattias Lazda, Lluis Mas-Ribas, Bradley W. Meyers, Kenzie Nimmo, Aaron B. Pearlman, J. Xavier Prochaska, Mawson W. Sammons, Kaitlyn Shin, Kendrick Smith, Haochen Wang
Figure caption: Measurements of ﹩{{\rm{DM}}}_{{\rm{host}}}^{{\rm{Macquart}}}﹩ as a function of r-band host galaxy luminosity for FRBs at z < 0.2 in the literature. The stellar mass implied by the S. Mahajan et al. (2018) conversion from r-band light to M* (S. Mahajan et al. 2018) is shown on the top y-axis to provide a rough sense of scale. For each source, we plot 1σ error bars according to Equation (4). Labels identify systems cut from our sample according to one or more criteria in Section 2. We find that high ﹩{{\rm{DM}}}_{{\rm{host}}}^{{\rm{Macquart}}}﹩ outliers can often be explained astrophysically by high scattering timescales, cluster membership of the host galaxy, or edge-on host galaxies. Low ﹩{{\rm{DM}}}_{{\rm{host}}}^{{\rm{Macquart}}}﹩ outliers are often close to the Galactic plane. “Low-DM” FRBs, which have downwardly biased DM values, are shown with gray crosses.
Paper: Stellar Mass–Dispersion Measure Correlations Constrain Baryonic Feedback in Fast Radio Burst Host Galaxies
Authors: Calvin Leung, Sunil Simha, Isabel Medlock, Daisuke Nagai, Kiyoshi W. Masui, Lordrick A. Kahinga, Adam E. Lanman, Shion Andrew, Kevin Bandura, Alice P. Curtin, B. M. Gaensler, Nina Gusinskaia, Ronniy C. Joseph, Mattias Lazda, Lluis Mas-Ribas, Bradley W. Meyers, Kenzie Nimmo, Aaron B. Pearlman, J. Xavier Prochaska, Mawson W. Sammons, Kaitlyn Shin, Kendrick Smith, Haochen Wang
Figure caption: Posterior distributions of the model parameters in our fiducial analysis using all 20 bursts. We fit the M*–DMhost relation for a slope (m), an intercept (b) referenced to M* = 1010 M⊙, a quadratic curvature parameter (a), and the scatter on the relation (σ) (see Equations (5) and (6)). We fit both the observed sight lines (gray) and the sight lines simulated through CAMELS snapshots (blue, orange, and green). The best-fit parameter estimates are shown as solid lines and quoted in Table 2. Comparing the data to the Astrid fits, we find that the slope parameter m is significantly discrepant between observations and simulations and that measured values of the intercept parameter b are difficult to reconcile with the existence of the host ISM.
Paper: Stellar Mass–Dispersion Measure Correlations Constrain Baryonic Feedback in Fast Radio Burst Host Galaxies
Authors: Calvin Leung, Sunil Simha, Isabel Medlock, Daisuke Nagai, Kiyoshi W. Masui, Lordrick A. Kahinga, Adam E. Lanman, Shion Andrew, Kevin Bandura, Alice P. Curtin, B. M. Gaensler, Nina Gusinskaia, Ronniy C. Joseph, Mattias Lazda, Lluis Mas-Ribas, Bradley W. Meyers, Kenzie Nimmo, Aaron B. Pearlman, J. Xavier Prochaska, Mawson W. Sammons, Kaitlyn Shin, Kendrick Smith, Haochen Wang
Figure caption: Left: the M*–DMhost relation for the FRB host galaxies in Table 1 (red and purple downward triangles), to which we fit the model in Equation (6) (gray). Right: the M*–DMh,CGM prediction for halos in the CAMELS-ASTRID, CAMELS-IllustrisTNG, and CAMELS-SIMBA simulations (blue, orange, and green points). For the fits to observational data and simulations, the model prediction best fitting the data is visualized as three lines to show the relation as its scatter ±1σ. In addition, model evaluations randomly sampled from the posterior probability distributions are plotted translucently in those same colors.
Paper: 3D Simulations of Convective Entrainment in Gas Giants: Rotation and Decreasing Luminosity as Barriers to Mixing
Authors: Shu Zhang, 舒 张, J. R. Fuentes, Andrew Cumming
Figure caption: 3D snapshots of the z-component of the vorticity ω = ∇ × u for the nonrotating case (panel (a)) and rotating case (panel (b)), both cooling with a decreasing flux from the top boundary. For both cases, the snapshots are shown at the same time, when the heat flux that drives convection has decreased to 10% of its initial value. The Rossby number of the convective flow in the rotating case is Ro ≈ 0.01, computed using the averaged flow velocity in the convection zone and the thickness of the convection zone. At t = 8 × 10−2, the convection zone depth in units of the box size H is h = 0.37 for the rotating case and h = 0.56 in the nonrotating case.
Paper: Stellar Mass–Dispersion Measure Correlations Constrain Baryonic Feedback in Fast Radio Burst Host Galaxies
Authors: Calvin Leung, Sunil Simha, Isabel Medlock, Daisuke Nagai, Kiyoshi W. Masui, Lordrick A. Kahinga, Adam E. Lanman, Shion Andrew, Kevin Bandura, Alice P. Curtin, B. M. Gaensler, Nina Gusinskaia, Ronniy C. Joseph, Mattias Lazda, Lluis Mas-Ribas, Bradley W. Meyers, Kenzie Nimmo, Aaron B. Pearlman, J. Xavier Prochaska, Mawson W. Sammons, Kaitlyn Shin, Kendrick Smith, Haochen Wang
Figure caption: One-dimensional parameter estimates for a, b, m, and σ for our fiducial observational data (open gray histogram), several variants thereof, and our simulation data (filled blue, orange, and green histograms). Parameter estimates are quoted in Table 2.
Paper: Stellar Mass–Dispersion Measure Correlations Constrain Baryonic Feedback in Fast Radio Burst Host Galaxies
Authors: Calvin Leung, Sunil Simha, Isabel Medlock, Daisuke Nagai, Kiyoshi W. Masui, Lordrick A. Kahinga, Adam E. Lanman, Shion Andrew, Kevin Bandura, Alice P. Curtin, B. M. Gaensler, Nina Gusinskaia, Ronniy C. Joseph, Mattias Lazda, Lluis Mas-Ribas, Bradley W. Meyers, Kenzie Nimmo, Aaron B. Pearlman, J. Xavier Prochaska, Mawson W. Sammons, Kaitlyn Shin, Kendrick Smith, Haochen Wang
Figure caption: The level of suppression of the matter power spectrum on small scales due to baryonic feedback as predictions from ASTRID, IllustrisTNG, and SIMBA, as well as the official DES Y3 and HSC analyses (A. Chen et al. 2023; R. Terasawa et al. 2025). The Astrid model, which corresponds to weak feedback, is difficult to reconcile with observations, implying an upper limit on S(k, z).
Paper: 3D Simulations of Convective Entrainment in Gas Giants: Rotation and Decreasing Luminosity as Barriers to Mixing
Authors: Shu Zhang, 舒 张, J. R. Fuentes, Andrew Cumming
Figure caption: Color maps showing the evolution of the horizontally averaged composition over time. In each case, the red dashed line shows the measured location of the convection zone boundary.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Main results of the WASP-107 b uniform helium envelope fit. The top left panel shows the Keck/NIRSPEC light curve in red, corresponding to a ∼0.75 Å bin centered around the He triplet, together with the fitted model light curve in blue. The right panel shows the median retrieved envelope in blue, with the shaded region showing the 1σ uncertainty region. The gray line represents the star, and the purple circle illustrates the planet.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Results from fitting a simulated HAT-P-18 b light curve, assuming the envelope has no leading tail. The left panel shows the simulated light curve in red, together with the fitted model in blue. The right panel shows the posteriors of the four fitted parameters, with the injected values shown in red.
Paper: A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots
Authors: David J. Setton, Jenny E. Greene, Justin S. Spilker, Christina C. Williams, Ivo Labbé, Yilun Ma, 逸伦 马, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Joel Leja, Anna de Graaff, Stacey Alberts, Rachel Bezanson, Leindert A. Boogaard, Gabriel Brammer, Sam E. Cutler, Nikko J. Cleri, Olivia R. Cooper, Pratika Dayal, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Michaela Hirschmann, Vasily Kokorev, Michael V. Maseda, Ian McConachie, Jorryt Matthee, Tim B. Miller, Rohan P. Naidu, Pascal A. Oesch, Richard Pan, Sedona H. Price, Katherine A. Suess, John R. Weaver, Mengyuan Xiao, Yunchong Zhang, Adi Zitrin
Figure caption: 6″ x 6″ cutouts of A2744-45924 (top) and RUBIES-BLAGN-1 (bottom), showcasing the F444W imaging (A2744-45924: R. Bezanson et al. 2024; J. R. Weaver et al. 2024; RUBIES-BLAGN-1: JWST-GO-1837; PI: Dunlop), as well as MIRI imaging (this program for A2744-45924, PRIMER for BRD-BLAGN-1) and new FIR continuum imaging and spectroscopy obtained with ALMA. On the ALMA images, −2σ and 2σ contours are indicated as pink and gray, respectively, and the beam is indicated with a blue ellipse. Both sources are detected in the mid-IR but not in the FIR. Additionally, neither source is significantly detected in [C II].
Paper: A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots
Authors: David J. Setton, Jenny E. Greene, Justin S. Spilker, Christina C. Williams, Ivo Labbé, Yilun Ma, 逸伦 马, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Joel Leja, Anna de Graaff, Stacey Alberts, Rachel Bezanson, Leindert A. Boogaard, Gabriel Brammer, Sam E. Cutler, Nikko J. Cleri, Olivia R. Cooper, Pratika Dayal, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Michaela Hirschmann, Vasily Kokorev, Michael V. Maseda, Ian McConachie, Jorryt Matthee, Tim B. Miller, Rohan P. Naidu, Pascal A. Oesch, Richard Pan, Sedona H. Price, Katherine A. Suess, John R. Weaver, Mengyuan Xiao, Yunchong Zhang, Adi Zitrin
Figure caption: A demonstration of the fundamental assumption that goes into the vast majority of LRD models, using the composite model from I. Labbe et al. (2024) for A2744-45924. In blue, we show the intrinsic, unattenuated galaxy+AGN model, which, via a combination of reddening and scattering, is observed in the rest-optical as the NIRSpec/PRISM spectrum (orange). The total attenuated luminosities for both the galaxy and AGN components are listed in the bottom right. Assuming energy balance, this model, and models like it, predict significant FIR output where the dust is being heated by the intrinsically blue engine of the LRD, regardless of whether that engine is primarily driven by a starburst or an AGN.
Paper: A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots
Authors: David J. Setton, Jenny E. Greene, Justin S. Spilker, Christina C. Williams, Ivo Labbé, Yilun Ma, 逸伦 马, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Joel Leja, Anna de Graaff, Stacey Alberts, Rachel Bezanson, Leindert A. Boogaard, Gabriel Brammer, Sam E. Cutler, Nikko J. Cleri, Olivia R. Cooper, Pratika Dayal, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Michaela Hirschmann, Vasily Kokorev, Michael V. Maseda, Ian McConachie, Jorryt Matthee, Tim B. Miller, Rohan P. Naidu, Pascal A. Oesch, Richard Pan, Sedona H. Price, Katherine A. Suess, John R. Weaver, Mengyuan Xiao, Yunchong Zhang, Adi Zitrin
Figure caption: The full SEDs for A2744-45924 (top) and RUBIES-BLAGN-1 (bottom) containing all existing optical-FIR data, with existing NIRCAM photometry shown as circles and NIRCam spectra shown in black. Herschel PACS and SPIRE upper limits are shown as triangles. New MIRI and ALMA limits are shown as hexagons. The colored curves indicate the maximum contribution of single-temperature modified Tdust = 20, 30, 50, 130, 200, 320, 510, and 800 K blackbodies to the 3σ upper limit FIR SED. The nondetection of any rising dust at rest-frame 4 μm essentially rules out any significant luminosity contribution from hot (T > 500 K) dust. Similarly, the ALMA nondetections rule out any significant contribution from cold (T < 75 K) dust. Herschel nondetections place a ceiling of ∼1012 L⊙ in a warm component at T ∼ 200 K. Also shown is the stacked maximal LRD SED from H. B. Akins et al. (2024; gray), scaled to the λrest = 0.6 μm luminosity of our sources, illustrating that our observations allow for a much narrower range of LIR/Loptical than their limits.
Paper: A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots
Authors: David J. Setton, Jenny E. Greene, Justin S. Spilker, Christina C. Williams, Ivo Labbé, Yilun Ma, 逸伦 马, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Joel Leja, Anna de Graaff, Stacey Alberts, Rachel Bezanson, Leindert A. Boogaard, Gabriel Brammer, Sam E. Cutler, Nikko J. Cleri, Olivia R. Cooper, Pratika Dayal, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Michaela Hirschmann, Vasily Kokorev, Michael V. Maseda, Ian McConachie, Jorryt Matthee, Tim B. Miller, Rohan P. Naidu, Pascal A. Oesch, Richard Pan, Sedona H. Price, Katherine A. Suess, John R. Weaver, Mengyuan Xiao, Yunchong Zhang, Adi Zitrin
Figure caption: The IR SEDs of A2744-45924 (top) and RUBIES-BLAGN-1 (bottom). Herschel PACS and SPIRE upper limits are shown as triangles, and the Spitzer/MIPS 24 μm for RUBIES-BLAGN-1 is shown as a square. New MIRI and ALMA limits are shown as hexagons. Existing ALMA Band 6 data, in the case of A2744-45924, are shown as circles. In the first row, we show the predictions for the IR SED using the galaxy-only fits from I. Labbe et al. (2024) and B. Wang et al. (2024a), assuming the dust emits as a 〈Tdust〉 = 45 K (B. T. Draine et al. 2007) template scaled to the attenuated luminosity (blue). On the right, we show the composite models from the same work, with the attenuated luminosity of the galaxy component emitted in the same B. T. Draine et al. (2007) template and the attenuated AGN emitted with the coldest SKIRTOR model (M. Stalevski et al. 2012, 2016; pink). In all cases, the total model is shown in black and is inconsistent with our new constraints.
Paper: A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots
Authors: David J. Setton, Jenny E. Greene, Justin S. Spilker, Christina C. Williams, Ivo Labbé, Yilun Ma, 逸伦 马, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Joel Leja, Anna de Graaff, Stacey Alberts, Rachel Bezanson, Leindert A. Boogaard, Gabriel Brammer, Sam E. Cutler, Nikko J. Cleri, Olivia R. Cooper, Pratika Dayal, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Michaela Hirschmann, Vasily Kokorev, Michael V. Maseda, Ian McConachie, Jorryt Matthee, Tim B. Miller, Rohan P. Naidu, Pascal A. Oesch, Richard Pan, Sedona H. Price, Katherine A. Suess, John R. Weaver, Mengyuan Xiao, Yunchong Zhang, Adi Zitrin
Figure caption: (Top) The 3σ upper limits of the maximum single-temperature modified blackbody luminosity that can be consistent with our new IR constraints for these sources as a function of the dust temperature (see Section 3.2). The widths of the horizontal error bars denote the temperature range where 68% of the power of a given blackbody is emitted. (Bottom) The posteriors for the maximum IR luminosity constrained in our fitting. We also show as dashed lines the attenuated luminosity predictions for galaxy-only (blue) and galaxy+AGN composite (black) models from I. Labbe et al. (2024) and B. Wang et al. (2024a). The AGN-only energy balance prediction for A2744-45924 is also shown in pink. In both cases, the models predict IR luminosities that either exceed or are right at the edge of what is allowable by our panchromatic dust SED fitting.
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: The high-redshift gas-phase MZR in FIRE-2 for z = 5–12 from A. Marszewski et al. (2024; black solid line) and in observations from z = 3 to 11. All observational data (fits, binned means, and individual galaxies) are colored by redshift. Observational best fits are shown at z ∼ 3.3 from R. L. Sanders et al. (2021; blue solid line) and at z ∼ 7 from I. Chemerynska et al. (2024; diagonal hatching representing uncertainty in the best linear fit) and L. E. Rowland et al. (2025; orthogonal hatching representing the typical scatter of galaxies about the best fit). Shapes with black borders show stellar mass and redshift-binned means from A. Sarkar et al. (2025; hexagons), K. Nakajima et al. (2023; diamonds), and M. Curti et al. (2024; squares). The sizes (areas) of these shapes are proportional to the number of galaxies within these bins. Shapes without black borders are measurements of individual galaxies from I. Chemerynska et al. (2024; crosses), L. E. Rowland et al. (2025; circles), T. Morishita et al. (2024; pentagons), M. Curti et al. (2023; triangles), T. Y.-Y. Hsiao et al. (2024; MACS0647-JD; diamond), and A. J. Bunker et al. (2023; GN-z11; star). The slope and normalization of the FIRE-2 MZR are in good agreement with high-redshift observations. Moreover, the prediction of a weakly evolving MZR at high redshift is broadly consistent with JWST results that show little evidence for evolution from z ∼ 3 to 8. Some preliminary evidence for a decreased normalization in the MZR is measured at z ≳ 8; however, the galaxy samples in these high-redshift bins remain small and potentially have a stronger selection bias toward galaxies with higher recent SFRs and therefore lower gas-phase metallicities given the existence of an FMR.
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: MZR of FIRE-2 galaxies predicted by the full gas-regulator model (left; Equation (2)) and the reduced burst model (right; Equation (6)) at z ∼ 5.5 (blue), 6.5 (orange), 8.0 (green), and 10.5 (red). Smaller, transparent points represent predicted metallicities of individual galaxies. Open squares represent stellar-mass-binned median-predicted metallicities. Black boxes show the MZR of FIRE-2 galaxies measured by A. Marszewski et al. (2024) at z = 7. Error bars represent the 16th and 84th percentiles. The black line shows the best-fit MZR reported by A. Marszewski et al. (2024) for z = 5–12 (no significant redshift evolution is predicted over this redshift interval). Median metallicities predicted by both analytic models are in general agreement with the values measured directly from the simulations and match the prediction of a weakly evolving MZR at these redshifts. The simplification between the full gas-regulator model and the reduced burst model has a negligible impact on the predicted MZR, motivating analysis of the reduced model to explain the form and evolution of the MZR for z = 5–12.
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: SFR (upper) and stellar/gas/metal mass (lower) time series for an example high-redshift FIRE-2 galaxy with a stellar mass of M⋆ = 1.8 × 108 M⊙ at z = 5. The SFR (black) is characterized by strong bursts. The stellar mass (blue) grows over time via these bursts. Intense stellar feedback following the starbursts drives strong outflows, decimating the gas mass (orange) and gas-phase metal mass (green) within the galaxy. We analyze individual burst cycles denoted here by highlighted regions separated by darker yellow lines.
Paper: The Detection of Teraelectronvolt Radiation from a Flat-spectrum Radio Quasar
Authors: Vaidehi S. Paliya, M. Böttcher, Kiran Wani, P. N. Naseef Mohammed, C. S. Stalin, S. Sahayanathan, D. J. Saikia, S. Muneer
Figure caption: Top left: the γ-ray spectrum of S5 1027+74. The power law and broken power-law model parameters are quoted. Top right: the broadband SED along with the fitted polynomial function (dashed line). Middle: the γ-ray light curves generated using different binning are shown in this panel. The arrival times of VHE photons are highlighted by vertical dashed lines. Flux upper limits are at an estimated 95% confidence level. Bottom: the V- and g-bands light curve using ASAS-SN observations.
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: Channels by which galaxies can gain and lose metals and gas in the full gas-regulator model (left; Equation (2)) and the reduced burst model (right; Equation (6)). The full gas-regulator model includes all possible channels (i.e., inflows, outflows, star formation, and stellar mass return). The reduced burst model includes only the channels relevant for explaining the form and evolution of the MZR in the scenario where galaxies have their ISM reset by bursty feedback.
Paper: The Detection of Teraelectronvolt Radiation from a Flat-spectrum Radio Quasar
Authors: Vaidehi S. Paliya, M. Böttcher, Kiran Wani, P. N. Naseef Mohammed, C. S. Stalin, S. Sahayanathan, D. J. Saikia, S. Muneer
Figure caption: The 10–2000 GeV Fermi-LAT counts map (scale = 0﹩\mathop{.}\limits^{^\circ }﹩05 pixel−1) centered at the radio position of S5 1027+74. The dotted circle refers to 68% Fermi-LAT PSF containment radius above 100 GeV for front-converting events (∼0﹩\mathop{.}\limits^{^\circ }﹩1). The positions of >100 GeV events estimated by the gtsrcprob tool are highlighted with different markers as labeled.
Paper: The Detection of Teraelectronvolt Radiation from a Flat-spectrum Radio Quasar
Authors: Vaidehi S. Paliya, M. Böttcher, Kiran Wani, P. N. Naseef Mohammed, C. S. Stalin, S. Sahayanathan, D. J. Saikia, S. Muneer
Figure caption: Optical depth due to γγ pair production on BLR photons as a function of the γ-ray photon frequency for different locations of the γ-ray emission region along the jet axis.
Paper: The Detection of Teraelectronvolt Radiation from a Flat-spectrum Radio Quasar
Authors: Vaidehi S. Paliya, M. Böttcher, Kiran Wani, P. N. Naseef Mohammed, C. S. Stalin, S. Sahayanathan, D. J. Saikia, S. Muneer
Figure caption: Optical spectrum of S5 1027+74 taken on 2025 April 17 with the Himalayan Chandra Telescope.
Paper: Neutron-quark Stars: Discerning Viable Alternatives for the Higher-density Part of the Equation of State of Compact Stars
Authors: Sudipta Hensh, Yong-Jia Huang, Toru Kojo, Luca Baiotti, Kentaro Takami, Shigehiro Nagataki, Hajime Sotani
Figure caption: Scatter plot of f2,mean and dimensionless tidal deformability. Hadronic EOSs include our Togashi and ChEFTex EOSs and the SLy, APR4, and LS220 EOSs from L. Rezzolla & K. Takami (2016). Data for the QHC19 models are from Y.-J. Huang et al. (2022). The dashed line shows the best-fit curve considering the hadronic models only. The shaded area shows the maximum residual of the fitting. The error bars indicate the fitting error in f2,mean for the NQS models. Inset: scatter plot of the relation between the dimensionless tidal deformability and compactness for various EOSs. The dashed curve is the best fit considering the fitting relation, ﹩{\rm{\Lambda }}=\gamma +\frac{\delta }{{(M/R)}^{5}}\,﹩, where the parameters from the fit are γ = −59.23 ± 24.29 and δ = 0.071 ± 0.003. The shaded area shows the maximum residual of fitting hadronic models.
Paper: Neutron-quark Stars: Discerning Viable Alternatives for the Higher-density Part of the Equation of State of Compact Stars
Authors: Sudipta Hensh, Yong-Jia Huang, Toru Kojo, Luca Baiotti, Kentaro Takami, Shigehiro Nagataki, Hajime Sotani
Figure caption: Scatter plot of GW energy released in the postmerger EGW,post and instantaneous frequency fGW,post. EGW,post is calculated as the difference between the total energy emitted in GWs at the end of the simulation (when further emission is negligible; see Figure 5) and that emitted until the time of the merger from the l = m = 2 mode (emission in other modes is negligible). fGW,post is the average GW frequency in an interval when the emission has become negligible, in practice, the last 5 ms of the simulation. The dashed line shows the best-fit curve.