adsabs/AstroCLIMB huggingface dataset:
Paper: Radiative Cooling Changes the Dynamics of Magnetically Arrested Disks
Authors: Akshay Singh, Damien Bégué, Asaf Pe'er
Figure caption: Time evolution of the mass accretion rate ﹩\dot{M}﹩ (in normalized unit) for all our simulations with spin a = 0.94. The values are calculated at 5rg to avoid the effects of numerical floors in the highly magnetized regions close to the BH. The typical “cyclic” evolution of an MAD is clearly identifiable. The bottom-right panel shows the effective mass accretion rate (﹩{\dot{M}}_{{\rm{eff}}}﹩) as a function of the targeted mass accretion rate (﹩{\dot{M}}_{{\rm{target}}}﹩). Error bars represents the 2σ variability. It is observed that ﹩{\dot{M}}_{{\rm{eff}}}﹩ slightly deviates from ﹩{\dot{M}}_{{\rm{target}}}﹩ at large mass accretion rate. The same type of evolution is obtained for all our other simulations with other BH spins.
Paper: Radiative Cooling Changes the Dynamics of Magnetically Arrested Disks
Authors: Akshay Singh, Damien Bégué, Asaf Pe'er
Figure caption: A contour plot of density (top) and plasma β (bottom) for simulations with mass accretion rates of ﹩1{0}^{-6}{\dot{M}}_{{\rm{Edd}}}﹩ (right) and ﹩1{0}^{-7}{\dot{M}}_{{\rm{Edd}}}﹩ (left) for a BH spin parameter a = 0.94 at 20500M. The plot shows regions of high magnetic flux, which are the characteristics of the MAD state.
Paper: Radiative Cooling Changes the Dynamics of Magnetically Arrested Disks
Authors: Akshay Singh, Damien Bégué, Asaf Pe'er
Figure caption: A contour plot of the electron temperature for simulations with mass accretion rates of ﹩1{0}^{-6}{\dot{M}}_{{\rm{Edd}}}﹩ (right) and ﹩1{0}^{-7}{\dot{M}}_{{\rm{Edd}}}﹩ (left) for a BH spin parameter a = 0.94 at 29950M. Large variations in electron temperature are visible in the region above the accretion disk.
Paper: Subtle and Spectacular: Diverse White Dwarf Debris Disks Revealed by JWST
Authors: J. Farihi, K. Y. L. Su, C. Melis, S. J. Kenyon, A. Swan, S. Redfield, M. C. Wyatt, J. H. Debes
Figure caption: The four strongest silicate features observed with JWST MIRI, as compared with Spitzer IRS spectra for the previous record holder for a white dwarf debris disk (GD 362, now the weakest in the plot; M. Jura et al. 2009), and the brightest silicate emission seen toward a dusty main-sequence star (BD+20 307; I. Song et al. 2005; A. J. Weinberger et al. 2011). The data are plotted as the emissivity relative to the fitted thermal continuum at each wavelength (see Section 2 for details), where the dashed gray line represents a blackbody with an emissivity of unity everywhere. The silicate emission detected toward GD 362 in 2006 (M. Jura et al. 2007b) is roughly twice as strong as that observed around G29-38 (W. T. Reach et al. 2005), and thus the silicate features seen in the disks of J0859–3647 and J1613+5521 are six to seven times stronger than for the dusty white dwarf prototype and are among the strongest observed in any debris disk orbiting any main-sequence or white dwarf star.
Paper: Subtle and Spectacular: Diverse White Dwarf Debris Disks Revealed by JWST
Authors: J. Farihi, K. Y. L. Su, C. Melis, S. J. Kenyon, A. Swan, S. Redfield, M. C. Wyatt, J. H. Debes
Figure caption: Gallery of JWST MIRI LRS spectra for 12 targets observed in Cycle 2 Survey program 3690. These are the dust fluxes with the stellar atmosphere subtracted, plotted as data points with error bars. The processed and extracted data are shown in gray, and these are overplotted in blue for regions where features are not obscured by the scatter in flux and in green using 7 pixel boxcar smoothing for the noisiest regions. Highlights include (1) the subtle detections of disks via weak silicate features in J0547–4847 and J0720–4250, (2) the lack of any silicate emission in J0707–7438, (3) the blue-peaked solid-state features in J0719+4021, J0802+5631, and J0847+5128, which are consistent with glassy silica such as found in tektites and obsidian, and (4) the strongest silicate feature observed to date in any white dwarf; J1613+5521 is an order of magnitude stronger (see Figure 2) than the feature observed toward G29-38, the dusty white dwarf prototype (W. T. Reach et al. 2009). The narrow feature near 12 μm in J1541+6453 is almost certainly due to a cosmic ray, as it is seen in only one of the two LRS nod positions.
Paper: Subtle and Spectacular: Diverse White Dwarf Debris Disks Revealed by JWST
Authors: J. Farihi, K. Y. L. Su, C. Melis, S. J. Kenyon, A. Swan, S. Redfield, M. C. Wyatt, J. H. Debes
Figure caption: The full photometric spectral energy distributions of the 12 stars with infrared excess plotted in Figure 1. Photometric data are shown as error bars and are color-coded as follows: purple is GALEX, blue is Pan-STARRS, SDSS, or SkyMapper, green is 2MASS or VISTA, and orange is WISE. The fitting process is described briefly in Section 2. The MIRI LRS spectra are shown as gray data points with error bars and have been truncated near or just beyond 12 μm for cosmetic reasons owing to noise at these longer wavelengths.
Paper: The JWST Weather Report from the Isolated Exoplanet Analog SIMP 0136+0933: Pressure-dependent Variability Driven by Multiple Mechanisms
Authors: Allison M. McCarthy, Johanna M. Vos, Philip S. Muirhead, Beth A. Biller, Caroline V. Morley, Jacqueline Faherty, Ben Burningham, Emily Calamari, Nicolas B. Cowan, Kelle L. Cruz, Eileen Gonzales, Mary Anne Limbach, Pengyu Liu, Evert Nasedkin, Genaro Suárez, Xianyu Tan, Cian O'Toole, Channon Visscher, Niall Whiteford, Yifan Zhou
Figure caption: Panel (a) shows the nine clusters obtained from the NIRSpec light curves. The celerite fit for each light curve that comprises each cluster is shown in gray, and the average for each cluster is shown in the colored marker. The gray vertical lines in panel (a) of both Figures 5 and 6 mark the 2.4 hr rotation period of this object. Panel (b) shows the Sonora Diamondback contribution function for a clear atmosphere with Teff = 1100 K and log(g) = 4.5. The colors are the same for the same clusters across both subplots. The clusters are overlaid onto the contribution function by calculating the average pressure of maximum flux for the wavelengths that comprise each cluster. The error bars on the clusters in panel (b) are the variance for the pressure of each cluster. The green shaded region represents the pressures where forsterite clouds exist, and the pink shaded region represents the pressures where iron clouds might exist from J. M. Vos et al. (2023).
Paper: The JWST Weather Report from the Isolated Exoplanet Analog SIMP 0136+0933: Pressure-dependent Variability Driven by Multiple Mechanisms
Authors: Allison M. McCarthy, Johanna M. Vos, Philip S. Muirhead, Beth A. Biller, Caroline V. Morley, Jacqueline Faherty, Ben Burningham, Emily Calamari, Nicolas B. Cowan, Kelle L. Cruz, Eileen Gonzales, Mary Anne Limbach, Pengyu Liu, Evert Nasedkin, Genaro Suárez, Xianyu Tan, Cian O'Toole, Channon Visscher, Niall Whiteford, Yifan Zhou
Figure caption: Panel (a) shows the two clusters obtained from the MIRI light curves. The celerite fit for each light curve that comprises each cluster is shown in gray, and the average for each cluster is shown in the colored marker. The gray vertical lines in panel (a) of both Figures 5 and 6 mark the 2.4 hr rotation period of this object. Panel (b) shows the Sonora Diamondback contribution function for a clear atmosphere with Teff = 1100 K and log(g) = 4.5. The colors are the same for the same clusters across both subplots. The clusters are overlaid onto the contribution function by calculating the average pressure of maximum flux for the wavelengths that comprise each cluster. The error bars on the clusters in panel (b) are the variance for the pressure of each cluster. The green shaded region represents the pressures where forsterite clouds exist, and the pink shaded region represents the pressures where iron clouds might exist from J. M. Vos et al. (2023).
Paper: The JWST Weather Report from the Isolated Exoplanet Analog SIMP 0136+0933: Pressure-dependent Variability Driven by Multiple Mechanisms
Authors: Allison M. McCarthy, Johanna M. Vos, Philip S. Muirhead, Beth A. Biller, Caroline V. Morley, Jacqueline Faherty, Ben Burningham, Emily Calamari, Nicolas B. Cowan, Kelle L. Cruz, Eileen Gonzales, Mary Anne Limbach, Pengyu Liu, Evert Nasedkin, Genaro Suárez, Xianyu Tan, Cian O'Toole, Channon Visscher, Niall Whiteford, Yifan Zhou
Figure caption: The top panel shows the measured maximum deviation of the light curves, colored by their respective cluster. The NIRSpec data are shown as circle markers and the MIRI data as triangles. The gray spectra in the three sub panels show the deviation of our “maximum” spectrum from our median spectra. The second panel shows the comparison between a scaled model flux ratio between a clear atmosphere and a clear atmosphere with a portion covered by a hot spot (C. V. Morley et al. 2014). The third panel highlights the flux ratio between a cloudy and clear atmosphere (C. V. Morley et al. 2014). The final panel labels the locations of impact for abundant molecules in the atmosphere.
Paper: The JWST Weather Report from the Isolated Exoplanet Analog SIMP 0136+0933: Pressure-dependent Variability Driven by Multiple Mechanisms
Authors: Allison M. McCarthy, Johanna M. Vos, Philip S. Muirhead, Beth A. Biller, Caroline V. Morley, Jacqueline Faherty, Ben Burningham, Emily Calamari, Nicolas B. Cowan, Kelle L. Cruz, Eileen Gonzales, Mary Anne Limbach, Pengyu Liu, Evert Nasedkin, Genaro Suárez, Xianyu Tan, Cian O'Toole, Channon Visscher, Niall Whiteford, Yifan Zhou
Figure caption: NIRSpec and MIRI light curves in the overlapping wavelength regions (4.5–5.1 μm). The binned NIRSpec light curve (27 s cadence) is shown in blue and the MIRI light curve (19 s cadence) is shown in red. Green solid lines and purple dashed lines indicate timestamps for the “maximum” and “minimum” spectra referenced in Figure 1.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: The MIRI/MRS spectrum of WISE-0458, and our best-fit model. Panel (a) shows the full spectrum, binned to 1/10th the original spectral resolution for visual clarity. Colors represent each individual subchannel of the MRS detector (labeled 1A–3C), and we also label the locations of prominent molecular absorption features in this brown dwarf atmosphere. Panels (b), (d), and (f) show the best-fit model (black) compared to the data for each channel (at R = 1000). Our model is a free retrieval using pRT (see Section 5), including a parameterized pressure–temperature profile and seven molecular species; five molecules are confidently detected (H2O, CH4, NH3, HCN, and C2H2). Panels (c), (e), and (g) show the residuals, taking the 10b factor (see Section 5) into account.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Opacities of molecules in our best-fit model, with abundances matching the best-fit value (for H2O, CH4, NH3, HCN, and C2H2) and 2σ upper limits (for CO and CO2) from our best-fit model. Opacities in the upper panel are at R = 100 and those in the lower panel are at R = 1000 (matching the resolution used in our pRT retrievals). In the lower panel we highlight the regions where HCN and C2H2 absorb most strongly in the near- and mid-IR. For the WISE-0458 abundances, both species are only detectable in the mid-IR around 14 μm in the WISE-0458 atmosphere. With sufficiently high abundances (higher than those observed here), both species might become detectable in the near-IR, at 3 and 1.5 μm.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Comparison of the data and best-fit models with and without including the molecules HCN and C2H2. Here we show our retrieved spectra for a “basic” model with only H2O, CH4, NH3, CO, and CO2 (brown), and a model that also includes HCN and C2H2 (green), alongside the data (black, including our retrieved uncertainty inflation). The lower panel shows the residuals (data – model) for both models, and shading in the background of both panels indicates regions of high opacity for HCN (pink) and C2H2 (blue). The plot shows only the 13.4–14.6 μm region of the spectrum, where HCN and C2H2 absorption features are significant (see also Figure 3), but these species have a small continuum effect across more of the mid-IR.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Predictions of atmospheric abundance for varying assumptions about the chemistry and vertical mixing, compared with our retrieved abundances in the WISE-0458 atmosphere. Left: atmospheric profiles for a nominal model (Kzz = 1011 cm2 s−1, C/O = 1 × solar, Fe/H = 1 × solar). With strong vertical mixing, we probe only the quenched abundances of these species; HCN is underpredicted and C2H2 is drastically underpredicted in these models relative to our observations. Right: quenched atmospheric abundances, for the nominal model and three models with increased Kzz, C/O, and Fe/H, alongside the retrieval abundances. Even unphysical values for the vertical mixing, C/O or metallicity are insufficient to boost C2H2 to the observed levels; raising the C2H2 abundance by increasing C/O or Fe/H also increases CO abundance to well above our upper limit. All models are produced with VULCAN (S.-M. Tsai et al. 2017, 2021).
Paper: Bridging Scales: Coupling the Galactic Nucleus to the Larger Cosmic Environment
Authors: Kung-Yi Su, Priyamvada Natarajan, Hyerin Cho, 혜린 조, Ramesh Narayan, Philip F. Hopkins, Daniel Anglés-Alcázar, Ben S. Prather
Figure caption: Results for the Sgr A* analog runs: the BH mass; AGN wind energy flux (averaged over 100 Myr); net increase in BH mass; net stellar mass, along with the corresponding BH accretion rates and star formation rates for Runs A (red curves), B (magenta curves), C1 (purple curves), C2 (blue curves), and C3 (green curves). The gray shaded region marks the BH accretion rate estimated EHT data (Event Horizon Telescope Collaboration et al. 2022). Without AGN feedback, both Runs A and B exhibit runaway BH growth, leading to rapid growth by orders of magnitude that occurs due to the accretion of gas that would have otherwise formed stars, thereby significantly lowering the star formation rate. The higher the feedback efficiency, seen in Runs C1, C2, and C3, the lower the corresponding BH accretion rate and star formation rate. A feedback efficiency of η ∼ 1 (Run C3) or η ∼ 0.02 (Run C1), assuming missing baryons) is required to suppress the star formation rate to ≲2M⊙ yr−1 (e.g., L. Chomiuk & M. S. Povich 2011; T. C. Licquia & J. A. Newman 2015; D. Elia et al. 2022). A feedback efficiency of ∼1, combined with a low CGM mass (gray dashed line) and missing baryons, is likely necessary to maintain a BH accretion rate that is consistent with the EHT data for an extended period.
Paper: Bridging Scales: Coupling the Galactic Nucleus to the Larger Cosmic Environment
Authors: Kung-Yi Su, Priyamvada Natarajan, Hyerin Cho, 혜린 조, Ramesh Narayan, Philip F. Hopkins, Daniel Anglés-Alcázar, Ben S. Prather
Figure caption: Results for the M87* analog runs: the BH mass; AGN wind energy flux (averaged over 100 Myr); net increase in BH mass; net mass in stars formed, along with the corresponding BH accretion rates and star formation rates for Runs A (red curves), B (magenta curves), C1 (purple curves), C2 (blue curves) and C3 (green curves). The gray shaded region marks the BH accretion rate estimated from EHT data (Event Horizon Telescope Collaboration et al. 2021). Without AGN feedback, both Runs A and B exhibit runaway BH growth, even when the accretion rate is suppressed to 0.01 of the Bondi rate. As the AGN feedback efficiency is increased in Runs C1, C2, and C3, the corresponding BH accretion rates and star formation rates are lower. As seen, a feedback efficiency ranging between 0.15 and 1 (Runs C2 and C3) is required to match the EHT-inferred accretion rate. Note that Run A (red curve) has no star formation throughout the simulation, so it does not appear in the stellar mass and star formation rate panels.
Paper: Bridging Scales: Coupling the Galactic Nucleus to the Larger Cosmic Environment
Authors: Kung-Yi Su, Priyamvada Natarajan, Hyerin Cho, 혜린 조, Ramesh Narayan, Philip F. Hopkins, Daniel Anglés-Alcázar, Ben S. Prather
Figure caption: Density, temperature, and entropy profiles for the M87* and Sgr A* analog runs, averaged from 1.45 to 1.5 Gyr. The M87* analog profiles are X-ray luminosity-weighted (0.5–7 keV), while the Sgr A* analog profiles are mass weighted for gas with T > 105 K. Shaded regions in the M87* analog panels represent observed cool-core (blue) and non-cool-core (red) cluster profiles (M. McDonald et al. 2013; scaled to account for the halo mass differences), and in the Sgr A* analog panels, the Milky Way profiles (M. J. Miller & J. N. Bregman 2015; blue and red, the latter assuming no missing baryons). The M87* analog run with η ∼ 1 (Run C3) yields profiles that resemble non-cool-core clusters, while the other runs resemble cool-core clusters.
Paper: Bridging Scales: Coupling the Galactic Nucleus to the Larger Cosmic Environment
Authors: Kung-Yi Su, Priyamvada Natarajan, Hyerin Cho, 혜린 조, Ramesh Narayan, Philip F. Hopkins, Daniel Anglés-Alcázar, Ben S. Prather
Figure caption: The gas temperature (upper half) and number density (lower half) morphology in a central ∣y∣ < 2 kpc slice for the runs with feedback efficiencies of η ∼ 0.02 (C1, left column upper row) and η ∼ 1 (C3, right column lower row) at 1.5 Gyr. The blue lines represent the magnetic field lines. In the Sgr A* analog runs C3, with η ∼ 1, the AGN cocoon propagates out to 80 kpc.
Paper: Thirty-five Years of Timing of M53A with Arecibo and FAST
Authors: Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li, Lei Qian
Figure caption: Period–period derivative plot for the pulsars in the ATNF Pulsar Catalog. The blue solid lines denote the spin-up line according to F. Verbunt & P. C. C. Freire (2014; see detailed discussion in T. M. Tauris et al. 2012) and four models of the death line are marked by solid black lines from I to IV following G. W. Cruces et al. (2021). The derived period derivatives for the MSPs in 47 Tuc (shown as green stars), M53 (shown as the pink stars), M71 (shown as the cyan stars; Y. Lian et al. 2025, in preparation), and NGC 6749A (shown as the red star; P. C. C. Freire et al. 2025, in preparation) place them in the same region of the diagram where similar system in the Galactic disk occur; these clusters do not seem to have young pulsars. The young (τc < 108 yr) pulsars in denser clusters are indicated by the red dots and labels (F. Abbate et al. 2022; D. Zhou et al. 2024; Y. Wu et al. 2024).
Paper: Thirty-five Years of Timing of M53A with Arecibo and FAST
Authors: Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li, Lei Qian
Figure caption: Acceleration model for M53. The black solid lines represent the upper and lower limits for the LOS accelerations (aℓGC) caused by the cluster as a function of the total angular offset from the center of the cluster (θ⊥). The triangles pointing down represent independent upper limits for the pulsar accelerations along the line of sight, ﹩{a}_{\ell ,{\rm{P}},{\rm{\max }}}﹩ for M53A (this Letter) and the remaining pulsars in M53 (Y. Lian et al. 2023). The vertical dashed line is the core radius. The cluster model can account for the negative ﹩\dot{P}﹩ values of M53B and M53E, but can not fully explain the ﹩{a}_{\ell ,{\rm{P}},{\rm{\max }}}﹩ of M53A, C and D, this positive difference is likely due to the intrinsic spin-down of these pulsars. The red error bar shows the measurement of the LOS acceleration of M53A derived from its orbital period derivative, ﹩{\dot{P}}_{{\rm{b}}},{\rm{obs}}﹩, confirming that it has an LOS acceleration that is consistent with the cluster predictions, and confirming the large intrinsic spin-down of M53A.
Paper: Thirty-five Years of Timing of M53A with Arecibo and FAST
Authors: Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li, Lei Qian
Figure caption: Color–magnitude diagram of M53 in a combination of the F275W, F336W, and F438W filters. The red square is the position of the counterpart to M53A. The gray curve is a 13 Gyr isochrone calculated at the cluster metallicity, distance, and extinction. The colored curves are cooling tracks for CO WD taken from the BASTI database (M. Salaris et al. 2010) and He WDs from A. G. Istrate et al. (2014, 2016). The tracks are for WDs with masses of 0.9, 0.7, 0.5, 0.4, 0.3, and 0.2 M⊙, with decreasing masses from left to right, as reported in the legend. Different points are also highlighted with different markers along the tracks corresponding to different cooling ages.
Paper: Thirty-five Years of Timing of M53A with Arecibo and FAST
Authors: Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li, Lei Qian
Figure caption: Orbital orientation constraints for M53A in the full ﹩\cos i﹩-Ω plane. The orange solid line and the green-shaded region display the observed ﹩\dot{x}﹩ and its 1σ, 2σ, and 3σ error, respectively. The dashed orange line indicates the PA of the proper motion of M53A (185﹩\mathop{.}\limits^{\unicode{x000b0}}﹩71). The red-dashed lines with its red-shaded region indicate an orbital inclination of ﹩{5{1}^{^\circ }}_{-6}^{+16}﹩ (or ﹩180^\circ -{51^\circ }_{-6}^{+16}={12{9}^{^\circ }}_{-16}^{+8}﹩) derived from the mass function assuming the pulsar mass of 1.3 M⊙ and a companion mass of ﹩0.3{9}_{-0.07}^{+0.05}\,{M}_{\odot }﹩ derived from the optical photometry in Section 4.
Paper: Thirty-five Years of Timing of M53A with Arecibo and FAST
Authors: Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li, Lei Qian
Figure caption: 1D probability distributions and 2D confidence contours (at 1σ, 2σ, and 3σ levels) for the cooling age, mass, and surface temperature of M53A’s companion star. The pink solid line represents the median (50th percentile), while the black dashed lines mark the 16th and 84th percentiles, providing the best-fit estimates and associated uncertainties.