adsabs/AstroCLIMB huggingface dataset:
Paper: Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Shu-Qing Zhong, Long Li, Biao Zhang, Zi-Gao Dai
Figure caption: Phase-averaged spectra and polarization properties within the model of the emission from a trapped fireball modified by RCS. Top left: one good fitting for the spectrum of the FXRB associated with FRB 20200428. Middle left: polarization degrees (Π) as a function of energy (ε) in different values of magnetic colatitude (θ  k ), in which θ  k  = 40° is the value that corresponds to the good fitting for the FXRB spectrum. Bottom left: polarization angles (χ p) as a function of energy in different magnetic colatitudes. Right panels: same as left panels, but with contour plots.
Paper: Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Shu-Qing Zhong, Long Li, Biao Zhang, Zi-Gao Dai
Figure caption: Pulse profiles (top panels), phase-resolved PDs (Π; middle panels), and phase-resolved PAs (χ p; bottom panels) in different energy intervals ε and angles χ and ς, which the spin axis makes with the LOS and the magnetic axis, respectively.
Paper: Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Shu-Qing Zhong, Long Li, Biao Zhang, Zi-Gao Dai
Figure caption: Pulse profiles (F  ν ; top panels), phase-resolved PDs (Π ν ; middle panels), and phase-resolved PAs (χ p;  bottom panels) in different energies ε and angles χ and ς, which the spin axis makes with the LOS and magnetic axis, respectively.
Paper: Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Shu-Qing Zhong, Long Li, Biao Zhang, Zi-Gao Dai
Figure caption: The best fit for the spectrum of the FXRB associated with FRB 20200428 within the trapped-expanding fireball model. The dashed blue and dotted orange lines represent E-mode and O-mode photospheric radiation, respectively, while the solid red line represents the total radiation.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption:  Redback modeling results for SN 2020wgz, for the magnetar- and nickel-powered model.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption:  Redback modeling results for SN 2020adow, with the arnett + tophat model above and the Radio SSA model below.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Systematic biases of LyCAN predictions on DESI Y5 mock spectra. The top panels show the FFE as functions of SNR and z, while the bottom panels show the AFFE (see Equation (3)) as functions of SNR and z. The solid line indicates the median (A)FFE, and the shaded regions show the 1 and 2σ regions. LyCAN tends to perform best on higher SNR, low-z spectra, and is more likely to overpredict the true continuum at higher z. This is a small effect (∼2% at highest z).
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: AFFE scores for candidate CNN architectures. Filled symbols indicate that a kernel size of three was used for the convolutional layers, while open symbols indicate a kernel size of six. The colors and symbols of the points vary depending on the number of convolutional layers in the network. Our chosen architecture is marked with a large circle in the lower left-hand corner and minimizes both the median AFFE score (﹩{\left|\delta {F}\right|}_{{\rm{m}}-\mathrm{score}};﹩ Equation (4)) and the 1σ range AFFE score (﹩{\left|\delta {F}\right|}_{{\rm{p}}-\mathrm{score}};﹩ Equation (5)).
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Distribution of AFFEs in the forest region for LyCAN, PCA, and NMF models on the DESI mock testing set. We also show the distribution of AFFEs for LyCAN predictions on our COS-based synthetic testing spectra. The dashed vertical lines indicate the median AFFE for each sample.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Top panel: effective optical depth measurements for the DESI Y5 mock data set based on truth continua (gray points) or LyCAN continuum predictions (red crosses). These are raw measurements and are not corrected for metals or optically thick absorbers. The error bars represent the statistical uncertainties. Bottom panel: the residual between the true and predicted measurements with statistical error bars.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Correlation matrices for optical depth measurements in DESI Y1 with LyCAN continuum predictions, Y5 mock spectra with LyCAN predictions, and the same sample of Y5 mock spectra with their true continua. These matrices do not include corrections for uncertainties due to continuum bias, metals, or optically thick absorbers.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Illustration of the diversity of the spectra. From left to right: DESI Y5 mock spectra included in our input data, COS-based synthetic spectra with DESI Y1-like noise, the combination of Y5 mock spectra and COS-based synthetic spectra with COS-like and DESI Y1-like noise, and the real DESI Y1 data. The shaded areas indicate the 1 and 2σ regions. The third panel is representative of our training set.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: The dispersions of continuum predictions for DESI Y1 quasars. The top panels show three ranges of SNR, while the bottom panels show three ranges of redshift. The solid line in each panel corresponds to the median prediction for that SNR or redshift range, and the shaded regions indicate the 1 and 2σ regions.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: LyCAN continuum predictions for DESI Y1 and DESI Y5 mock quasars. The panels on the left-hand side show predictions for real DESI Y1 quasars at increasing redshifts from top to bottom, and the right-hand panels show predictions on DESI Y5 mock spectra. The panels with mock spectra also include their true continua and the AFFE values in the forest region.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Examples of PCA, NMF, and LyCAN continuum predictions for four different classes of spectra, i.e., a real DESI Y1 spectrum, a DESI Y5 mock spectrum, a COS-based synthetic spectrum, and a real COS spectrum. None of these spectra appear in our training set.
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: The relation between kT  e  and τ. The green dots are the constrained values of the parameters, and the red dots denote the lower and upper limits of kT  e  and τ, respectively. The yellow dashed line and the yellow shaded region are the linear fits to the constrained values of kT  e  and τ, and the errors in the slope and the intercept of the linear fit (Method I). The beige-filled diamond points represent the median values of kT  e  in each bin of τ obtained from the survival analysis using the KMPL approach. The black dashed line and the black shaded region are the linear fit and the errors in the fit parameters to the median values of kT  e  (Method II). The green dashed line and the green shaded region represent the linear fit and the errors in the slope and the intercept for the fit between two parameters considering both uncensored (including the corresponding asymmetric errors in kT  e ) and censored (upper bound of kT  e  = 150 keV) values of two parameters (Method III).
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: Plot of the estimated E cut values from this work and those obtained from the literature. The green dots indicate the constrained E cut values obtained from both this study and prior research. The red dots signify the lower limits of E cut values derived from both this study and the existing literature. The black dots denote the constrained E cut values from this study and the lower limits of E cut from the literature. The blue dots represent the constrained E cut values from the literature and the lower limits of E cut values from this study. The 1:1 line is also shown (the black dotted line) for reference.
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: Confidence contours between E cut and Γ obtained from Model 1 for six sources. The color codes for the contours are as follows: red, green, and blue for 68% (Δχ 2 = 2.30), 90% (Δχ 2 = 4.61), and 99% (Δχ 2 = 11.8) confidence levels, respectively. In each panel, the best-fit location is marked by the black plus sign.
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: The relation between Γ–λ Edd (left panel) and E cut–Γ (right panel). The descriptions of the lines and the shaded regions are the same as those in Figure 7.
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: The relation between Γ and E cut with the black hole mass. The descriptions of the lines and the shaded regions are the same as the descriptions given in Figure 7.
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: The relation between R–Γ (left panel) and E cut–R (right panel). The descriptions of the lines and the shaded regions are the same as those in Figure 7.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Synthesized nei spectra of a solar-abundance plasma in the 0.6–1.05 keV band for varying τ and abundances. The blue solid lines show the synthesized spectrum predicted by our model with V sh = 1000 km s−1, β = 0.01, and τ = 1011 cm−3 s. The orange dashed lines show the synthesized spectrum predicted by our model with an electron temperature of 0.91 keV and varying τ values. The τ values for the nei model are 1.0 × 1011 cm−3 s for (a) and (d), 0.7 × 1011 cm−3 s for (b) and (e) and 0.4 × 1011 cm−3 s for (c) and (f). The abundances for the nei model are solar abundances for (a), (b), and (c), and optimized by the least squares method for (d), (e), and (f). The ratios between the two models are shown at the bottom of each panel. Each spectrum is convolved with the instrumental response matrices of XRISM Resolve.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Thermal broadening width in FWHM of oxygen Lyα (red line), silicon Lyα (green line), and iron Lα (blue line) in the solar-abundance plasma shock heated with V sh = 1000 km s−1 and β = m  e /μ m p as a function of τ.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Temperature and ionization equilibration processes in a pure-iron plasma shock-heated with V sh = 1000 km s−1 and β = 0.01: (a) Electron and iron temperatures as a function of τ. (b) Total internal energy density (solid lines) and contribution from each species (dashed lines) as a function of τ, with the total scaled to unity at τ = 0. (c) Ion fraction of iron for our model (solid lines) and nei model (dashed lines) and (d) their ratio as a function of τ. The ratios are plotted only when the ion fractions are greater than 10−2.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Temperature equilibration processes in a solar-abundance plasma for varying initial conditions. The simulations used V sh = 500 km s−1, 1000 km s−1, and 3000 km s−1, and β = 0.01, 0.1, and 1.0, resulting in a 3 × 3 array of subplots. The dashed line in each subplot shows the case with the same shock velocity but β = m  e /μ m p for reference.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: The Chandra ACIS-S source spectra of N132D and the best-fit models. The red, green, and blue lines show the thermal emission of the IONTENP model, detector background, and sky background, respectively.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Chandra ACIS-S background spectrum of N132D (black crosses). The best-fit models for sky and detector background components are shown in blue and green lines, respectively.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: A three-color ACIS flux image of N132D. Red, blue, and green correspond to 0.5–1.2 keV, 1.2–2.0, and 2.0–7.0 keV, respectively.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: The best-fit pairs of the electron temperature and τ determined with the IONTENP (filled circles) and nei (crosses) in each source region.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Same as Figure 3 but for a pure-iron plasma.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: To demonstrate the difference between models with different physical choices, we show the evolution tracks of 3 M ⊕ planets, based on the GSS18 analytical model with their original initial conditions. The model with the original physics is shown in red, with the GSS18 energy-limited wind without the energy-loss term ﹩{\dot{E}}_{\mathrm{adv}}﹩ (see Equation (32)). A decoupled isothermal Parker wind without ﹩{\dot{E}}_{\mathrm{adv}}﹩ is shown by the dashed black line. Including the energy-loss term ﹩{\dot{E}}_{\mathrm{adv}}﹩ is shown by the solid black line. This black model represents what we believe is a more appropriate combination of physics, which is more consistent with the behavior from our numerical model. In gray is an improved GSS18 energy-limited wind, now with ﹩{\dot{E}}_{\mathrm{adv}}﹩. See Sections 4.1 and 4.2 for discussion.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We demonstrate the behavior of the decoupled Parker wind that different initial mass fractions for planets with a given initial entropy, core mass (8.5 M ⊕), and stellar bolometric flux (300 F ⊕) converge to a common final mass fraction value by the end of boil-off. We vary the initial mass fraction from our 10% default (gray curve, with post-boil-off mass fractions shown in Table 2) to the scaling function developed in GSS18 (black curve). The mass fraction right after boil-off at 1 Myr is nearly identical to that after 3 Gyr of evolution under the long-lived Parker wind, implying the insignificance of the post-boil-off Parker wind. As a comparison, we include an evolution track for the model under the GSS18 coupled escape, with all other conditions the same as the black model, which never converges in a few gigayears, due to the coupling effect with the thermal evolution. More examples are shown in Figure 11.