adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution of Electron Acceleration by Corotating Interaction Region Shocks at 1 au
Authors: Xinnian Guo, 新年 郭, Linghua Wang, 玲华 王, Wenyan Li, 文妍 李, Qianyi Ma, 千一 马, Liu Yang, 柳 杨, Robert F. Wimmer-Schweingruber, Stuart D. Bale
Figure caption: The upstream (blue) and downstream/shocked (red) electrons measured by Wind (squares) and MMS1 (triangles) near the CIR #1 forward and reverse shock. ((a)–(b)) Omnidirectional electron flux vs. energy spectra for the forward shock and reverse shock. The dotted lines show the thermal Maxwellian distribution that is estimated from the observed solar wind electron density and temperature. The solid lines represent the best fit from the (extended) pan-spectrum fitting. (c) The omnidirectional ﹩{J}_{\mathrm{dn}}/{J}_{\mathrm{up}}﹩ ratio vs. the downstream electron energy ﹩{\varepsilon }_{\mathrm{dn}}﹩. (d) The ﹩{j}_{\mathrm{dn}}/{j}_{\mathrm{up}}﹩ ratio vs. PA at 165 eV by Wind (at 133 eV by MMS1). (e) The estimated L drift vs. ﹩{\varepsilon }_{\mathrm{dn}}﹩. In panels ((c)–(e)), the purple (black) color indicates the forward (reverse) shock. (f) The temporal profile of IMF magnitude measured by Wind. The green curve shows the best fit for the tanh function. The green vertical lines show the time at which ﹩\dot{\tilde{B}}(t)﹩ equals ﹩\dot{\tilde{B}}({t}_{0})/10﹩. And time between the two vertical lines is the duration time Δt of the ramp.
Paper: Evolution of Electron Acceleration by Corotating Interaction Region Shocks at 1 au
Authors: Xinnian Guo, 新年 郭, Linghua Wang, 玲华 王, Wenyan Li, 文妍 李, Qianyi Ma, 千一 马, Liu Yang, 柳 杨, Robert F. Wimmer-Schweingruber, Stuart D. Bale
Figure caption: The CIR # 1 measured by the Wind ((a)–(c)) and MMS1 ((d)–(h)) spacecraft from 2018 January 8 to 9. Wind measurements: (a) omnidirectional electron fluxes at 18 eV–66 keV; (b) electron PA distributions at 427 eV, normalized by the PA-average flux for each time bin; (c) IMF magnitude (black) and solar wind speed V SW (blue). The vertical orange line indicates the SI that is determined by a sudden decrease in solar wind density N SW and increase in V SW (Wimmer-Schweingruber 1997; Jian et al. 2006; Tao et al. 2021). MMS1 measurements: (d) omnidirectional electron fluxes at 12 eV–439 eV; (e) N SW; (f) V SW; (g) electron PA distributions at 312 eV, normalized by the PA-average flux for each time bin; (h) IMF magnitude. In panels ((a)–(c)) ((d)–(h)), the vertical solid and dashed black lines indicate the arrivals of forward and reverse shock at Wind (MMS1), respectively. (i) The positions of Wind and MMS1 in GSE coordinates at the arrival of CIR shocks. The circle marks the Earth’s location, while the gray surface indicates the best single-surface fitting bow-shock model (Jerab et al. 2004). The purple (black) plane represents the surface of the forward (reverse) shock with an arrow indicating the fitted-shock normal ﹩\hat{n}﹩.
Paper: Evolution of Electron Acceleration by Corotating Interaction Region Shocks at 1 au
Authors: Xinnian Guo, 新年 郭, Linghua Wang, 玲华 王, Wenyan Li, 文妍 李, Qianyi Ma, 千一 马, Liu Yang, 柳 杨, Robert F. Wimmer-Schweingruber, Stuart D. Bale
Figure caption: The upstream (blue) and downstream/shocked (red) electrons measured by Wind (squares) and MMS1 (triangles) near the CIR #2 reverse shock. ((a)–(c)) Same legend as panels ((b)–(d)) of Figure 2. (d) The temporal profile of IMF magnitude measured by MMS1. The green curve shows the best fit for the tanh function.
Paper: Evolution of Electron Acceleration by Corotating Interaction Region Shocks at 1 au
Authors: Xinnian Guo, 新年 郭, Linghua Wang, 玲华 王, Wenyan Li, 文妍 李, Qianyi Ma, 千一 马, Liu Yang, 柳 杨, Robert F. Wimmer-Schweingruber, Stuart D. Bale
Figure caption: The CIR #2 measured by the Wind ((a)–(c)) and MMS1 ((d)–(h)) spacecraft from 2020 February 6 to 7. Same legend as Figure 1.
Paper: Detection of Rydberg Lines from the Atmosphere of Betelgeuse
Authors: W. R. F. Dent, G. M. Harper, A. M. S. Richards, P. Kervella, L. D. Matthews
Figure caption: Azimuthally averaged projected radial distributions. Left panel shows the RTLs (blue and magenta) and the 1.3 mm continuum (green). Solid lines are the observations, and dashed lines represent the model convolved with the azimuthally averaged ALMA beam (size shown lower right). Right panel illustrates the adopted semiempirical model structure, including the radial profile of the gas (electron) temperature T  e  and neutral H density n  H  above the photosphere. Also shown are the inner edge of the MOLsphere and the τ = 1 continuum radius at the observing frequency. The electron density (not shown) is dominated by the photoionization of abundant low FIP elements, Mg, Si, and Fe, with contributions from C and S.
Paper: Detection of Rydberg Lines from the Atmosphere of Betelgeuse
Authors: W. R. F. Dent, G. M. Harper, A. M. S. Richards, P. Kervella, L. D. Matthews
Figure caption: Spectrum of 30α Rydberg lines from Betelgeuse. Left panel shows emission after continuum subtraction, integrated over a 130 mas aperture (blue) and from only the central 22 mas (scaled by ×4, magenta). The frequencies of H30α, He30α, and the group of O, Mg, S, and Fe (in order of increasing Rydberg frequency and marked X30α) are indicated by the vertical dashed lines. Also shown by short dotted lines are the line frequencies of TiO2. Right panel shows the spectrum after binning by two channels, on velocity scales based on the calculated H30α and X30α rest frequencies in Table 1. Voigt profiles (magenta lines) provide good fits to the line core and wings, while Gaussian profiles (green) underpredict the line wings. Residuals for the two types of profiles are shown offset below. Details of the fits are given in Table 1. Axes in both cases are adjusted to the rest frame with respect to V ⋆.
Paper: Detection of Rydberg Lines from the Atmosphere of Betelgeuse
Authors: W. R. F. Dent, G. M. Harper, A. M. S. Richards, P. Kervella, L. D. Matthews
Figure caption: Maps of the continuum-subtracted integrated emission of H30α (231.82–231.97 GHz, left) and X30α (231.97–232.08 GHz, right) in the vicinity of Betelgeuse. The size of the IR photosphere is shown by the dashed circle, and the 214–233 GHz continuum is shown by the contours. Contours start at 1 mJy beam−1, with an interval of 8 mJy beam−1, and the color scales of line intensity are in Jy beam−1  km s−1. The beam size is shown lower left.
Paper: Detection of Rydberg Lines from the Atmosphere of Betelgeuse
Authors: W. R. F. Dent, G. M. Harper, A. M. S. Richards, P. Kervella, L. D. Matthews
Figure caption: Simulations of the RTLs computed with and without enhanced C and H ionization. Left: X30α (232.023 GHz). Mg, Si, and Fe computed with the Saha–Boltzmann-level populations producing ∼1/4 of the observed flux (shown by the red line). In the second simulation (blue) the C is singly ionized, and this improves the match of the total fluxes but shifts the combined profile redward by ∼5 km s−1, farther away from the observed peak. Right: H30α (231.901 GHz). In the first simulation no emission is predicted (see Section 4 for details). We artificially increased the ionization fraction of H to 1 × 10−4, which now leads to H30α emission. Inclusion of non-LTE level populations will likely alter the predicted line fluxes. The observed lines, especially H30α, show excess flux in the line wings.
Paper: Calcium Chemistry in Carbon-rich Circumstellar Environments: The Laboratory and Astronomical Discovery of Calcium Dicarbide, CaC2 
Authors: H. Gupta, P. B. Changala, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Rotational transitions of 40CaC2 toward IRC+10216 in the 7–22 mm wavelength region. The bottom two spectra were observed with the 100 m GBT, and the top three were observed with the Yebes 40 m telescope. The Yebes 40 m lines are overlaid with the profile of J = 16 − 15 line of HC5N (magenta trace) to show the close similarity between emission from molecules residing in the molecular shell of IRC+10216. The 101 − 000 and 202 − 101 lines were detected after 13.5 and 3.8 hr of observation; the 303 − 202, 322 − 221, and 321 − 220 lines were detected after 696 hr of observation. The 101 − 000 and 202 − 101 lines have been smoothed to 2.8 km s−1 and 1.4 km s−1, and the 303 − 202, 322 − 221, and 321 − 220 lines have been smoothed to 1.7 km s−1.
Paper: Calcium Chemistry in Carbon-rich Circumstellar Environments: The Laboratory and Astronomical Discovery of Calcium Dicarbide, CaC2 
Authors: H. Gupta, P. B. Changala, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Rotational temperature diagram of 40CaC2 in IRC+10216, fitted with the two-temperature model described in Changala et al. (2022). The slope of the parallel lines through each K ladder gives the rotational temperature (T rot), and that of the line through points across the K ladders gives the kinetic temperature (T kin). The flux of the K = 4 transitions is assumed to be one-half the total flux of the unresolved doublets listed in Table 2. The error bar on each data point is twice the error shown in Table 2. Error bars on the parameters are twice the standard error of the fit.
Paper: Calcium Chemistry in Carbon-rich Circumstellar Environments: The Laboratory and Astronomical Discovery of Calcium Dicarbide, CaC2 
Authors: H. Gupta, P. B. Changala, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Rotational transitions of 40CaC2 toward IRC+10216 in the 3 mm wavelength region observed with the IRAM 30 m telescope. Fitted profiles are plotted in red, and unidentified lines are indicated with a “U.”
Paper: Calcium Chemistry in Carbon-rich Circumstellar Environments: The Laboratory and Astronomical Discovery of Calcium Dicarbide, CaC2 
Authors: H. Gupta, P. B. Changala, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Lower rotational energy levels of CaC2. Red dumbbells indicate the observed laboratory transitions, and blue arrows indicate the astronomical transitions. The inset shows the semi-experimental equilibrium structure.
Paper: Generation of Low-inclination, Neptune-crossing Trans-Neptunian Objects by Planet Nine
Authors: Konstantin Batygin, Alessandro Morbidelli, Michael E. Brown, David Nesvorný
Figure caption: Census of well-characterized TNOs with a > 100  au, i < 40°, and q < 30  au. Among the 29 objects within the Minor Planet Center database that meet these orbital criteria, our analysis is restricted to 17 objects whose orbits have been quantified through multi-opposition observations. The left panel shows a top-down view of the orbits. The right panel depicts a plot of perihelion distance against semimajor axis; the numbers adjacent to the points indicate each object’s orbital inclination in degrees. Notably, the spread of perihelion distances forms a relatively flat distribution between ∼16 au and Neptune’s orbit.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
Authors: Simon Petrus, Niall Whiteford, Polychronis Patapis, Beth A. Biller, Andrew Skemer, Sasha Hinkley, Genaro Suárez, Paulina Palma-Bifani, Caroline V. Morley, Pascal Tremblin, Benjamin Charnay, Johanna M. Vos, Jason J. Wang, Jordan M. Stone, Mickaël Bonnefoy, Gaël Chauvin, Brittany E. Miles, Aarynn L. Carter, Anna Lueber, Christiane Helling, Ben J. Sutlieff, Markus Janson, Eileen C. Gonzales, Kielan K. W. Hoch, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Thomas Henning, Dean C. Hines, Callie E. Hood, Alex R. Howe, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Minjae Kim, Daniel Kitzmann, Adam L. Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Jarron M. Leisenring, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Mathilde Mâlin, Elena Manjavacas, Sebastián Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Maxwell A. Millar-Blanchaer, Paul Mollière, Sarah E. Moran, Sagnick Mukherjee, Eric Pantin, Marshall D. Perrin, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Shrishmoy Ray, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Steph Sallum, Matthias Samland, Benjamin Sargent, Joshua E. Schlieder, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Kimberly Ward-Duong, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Alice Zurlo, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou
Figure caption: Same figure as Figure 2 but with the exploration of the interstellar extinction A  V . The estimate of the other parameters, obtained with each model, are given in each panel, respectively.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
Authors: Simon Petrus, Niall Whiteford, Polychronis Patapis, Beth A. Biller, Andrew Skemer, Sasha Hinkley, Genaro Suárez, Paulina Palma-Bifani, Caroline V. Morley, Pascal Tremblin, Benjamin Charnay, Johanna M. Vos, Jason J. Wang, Jordan M. Stone, Mickaël Bonnefoy, Gaël Chauvin, Brittany E. Miles, Aarynn L. Carter, Anna Lueber, Christiane Helling, Ben J. Sutlieff, Markus Janson, Eileen C. Gonzales, Kielan K. W. Hoch, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Thomas Henning, Dean C. Hines, Callie E. Hood, Alex R. Howe, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Minjae Kim, Daniel Kitzmann, Adam L. Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Jarron M. Leisenring, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Mathilde Mâlin, Elena Manjavacas, Sebastián Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Maxwell A. Millar-Blanchaer, Paul Mollière, Sarah E. Moran, Sagnick Mukherjee, Eric Pantin, Marshall D. Perrin, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Shrishmoy Ray, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Steph Sallum, Matthias Samland, Benjamin Sargent, Joshua E. Schlieder, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Kimberly Ward-Duong, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Alice Zurlo, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou
Figure caption: Same as Figure 12 but with the zoom chosen to represent the data acquired with MIRI between 4.90 and 17.98 μm.
Paper: Generation of Low-inclination, Neptune-crossing Trans-Neptunian Objects by Planet Nine
Authors: Konstantin Batygin, Alessandro Morbidelli, Michael E. Brown, David Nesvorný
Figure caption: Statistical comparison between the observed perihelion distribution of trans-Neptunian objects (TNOs) and simulations with and without P9. The top panel illustrates the distribution of the variable ξ, which represents the cumulative distribution function values of the perihelia for the known objects, derived from the numerical models, accounting for observational bias. A uniform distribution of ξ between 0 and 1 indicates a strong agreement between the observational data and the simulation. The P9 model shows a more uniform distribution of ξ (p = 0.41) as opposed to the P9-free model (p = 0.0034), suggesting a better match with the observational data. The bottom panel displays the probability distribution function of the logarithmic statistic, ζ, which quantifies the uniformity of the ξ distribution across the observed objects, adjusted for observational bias. The vertical lines represent the values of ζ corresponding to the P9 model (at −7.9) and the P9-free model (at −16.5), with the mean of the expected ζ distribution marked at −7.2. The spread of the distribution, denoted by σ (standard deviation), is 1.8. The proximity of the P9 model statistic to the overall mean compared to the P9-free model—lying more than 5σ away—reflects a statistically significant preference for the P9 hypothesis.
Paper: Generation of Low-inclination, Neptune-crossing Trans-Neptunian Objects by Planet Nine
Authors: Konstantin Batygin, Alessandro Morbidelli, Michael E. Brown, David Nesvorný
Figure caption: A comparison of the orbital distributions from P9-inclusive (left) and P9-free (right) N-body simulations. Both panels depict the perihelion distance against the semimajor axis of orbital footprints of simulated TNOs with i < 40°. The overlaying contour lines represent density distributions, with brighter colors indicating higher concentrations of objects. While the panels themselves show raw simulation data, the histograms along the axes show a biased frequency distribution for the perihelion distances (vertical) and semimajor axes (horizontal), assuming a limiting magnitude of ﹩{V}_{\mathrm{lim}}=24﹩.
Paper: Generation of Low-inclination, Neptune-crossing Trans-Neptunian Objects by Planet Nine
Authors: Konstantin Batygin, Alessandro Morbidelli, Michael E. Brown, David Nesvorný
Figure caption: Evolution of selected particles within our calculations that attain nearly planar (i < 40°) Neptune-crossing orbits, within the final 500  Myr of the integration. The top, middle, and bottom panels depict the time series of semimajor axis, perihelion distance, and inclination, respectively. Some particles experience large perihelion oscillations while remaining on prograde orbits for the duration of the simulation. Others exhibit coupled eccentricity–inclination dynamics that the drive orbital flips. Although the orbital evolution is always stochastic, the rate of chaotic diffusion greatly increases when particles attain Neptune-crossing trajectories.
Paper: Generation of Low-inclination, Neptune-crossing Trans-Neptunian Objects by Planet Nine
Authors: Konstantin Batygin, Alessandro Morbidelli, Michael E. Brown, David Nesvorný
Figure caption: Inclination distribution generated in presence and absence of P9. The smooth curves represent the probability density function fitted to the histogram data for each simulation. The P9 simulation shows a more pronounced peak and a distribution that extend toward higher inclinations, whereas the P9-free simulation exhibits a broader distribution with a gentler slope, peaking at lower inclinations.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
Authors: Simon Petrus, Niall Whiteford, Polychronis Patapis, Beth A. Biller, Andrew Skemer, Sasha Hinkley, Genaro Suárez, Paulina Palma-Bifani, Caroline V. Morley, Pascal Tremblin, Benjamin Charnay, Johanna M. Vos, Jason J. Wang, Jordan M. Stone, Mickaël Bonnefoy, Gaël Chauvin, Brittany E. Miles, Aarynn L. Carter, Anna Lueber, Christiane Helling, Ben J. Sutlieff, Markus Janson, Eileen C. Gonzales, Kielan K. W. Hoch, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Thomas Henning, Dean C. Hines, Callie E. Hood, Alex R. Howe, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Minjae Kim, Daniel Kitzmann, Adam L. Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Jarron M. Leisenring, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Mathilde Mâlin, Elena Manjavacas, Sebastián Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Maxwell A. Millar-Blanchaer, Paul Mollière, Sarah E. Moran, Sagnick Mukherjee, Eric Pantin, Marshall D. Perrin, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Shrishmoy Ray, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Steph Sallum, Matthias Samland, Benjamin Sargent, Joshua E. Schlieder, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Kimberly Ward-Duong, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Alice Zurlo, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou
Figure caption: Same as Figure 3 but for the bolometric luminosity L bol (left panel) and the mass M (right panel). These parameters are estimated from the Stefan–Boltzmann law and the gravitational law, respectively.