adsabs/AstroCLIMB huggingface dataset:
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Hubble residuals from the DES sample (top row) and external low-z SN samples (bottom row) as a function of (from left to right) the SALT3 stretch x 1, SALT3 color c, host galaxy stellar mass, and host galaxy rest-frame u − r color. Note that the residuals shown include bias corrections and the “mass step correction” following Equation (1).
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Comparison between observed (black symbols) and simulated (solid lines) distributions of host galaxy stellar mass (left) and host r-band brightness (right) for different redshift bins. We present the results for DES shallow and deep fields separately (upper and lower panels, respectively).
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Bias corrections on μ for the DES sample (squares for deep fields, hexagon for shallow fields) and external low-z SN samples (triangles). Depending on the depth of the survey, corrections for selection effects start increasing at different redshifts.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: Distributions, weighted by SFR, of ISM pressure and expected weight as measured in TNG50 at z = 0 (top) and z = 2 (bottom). For each panel, we show ﹩{\mathrm{SFR}}_{\mathrm{tot}}^{-1}d\,\mathrm{SFR}/d{\mathrm{log}}_{10}{\rm{}}x﹩, where x represents the property on the x-axis. Left: contribution of various pressure components (thermal P th, turbulent P turb, magnetic Πmag) to the total pressure P tot as measured at the midplane in TNG50 for the stellar mass range M ⋆ = 107−11 M ⊙. Middle: Contribution of different weight components (gas ﹩{{ \mathcal W }}_{{\rm{g}}}﹩, star ﹩{{ \mathcal W }}_{* }﹩, dark matter ﹩{{ \mathcal W }}_{{\rm{d}}}﹩) to the total expected weight ﹩{ \mathcal W }﹩ in TNG50 for M ⋆ = 107−11. The contribution to expected weight from stellar gravity slightly exceeds the other contributions, particularly at high-z (bottom). Right: Distribution of the ratio between the total pressure at the midplane, P tot, and the total expected weight, ﹩{ \mathcal W }﹩ in TNG50 for the whole stellar mass range (solid), and for the stellar mass range M ⋆ = 109.5−10.5 M ⊙ (dashed). Here, we also compare to results from TNG100 for the high end of the mass range (dotted). P th and P turb are the dominant contributors to P tot at z = 0 and z = 2, respectively. The distribution of the ratio P tot/﹩{ \mathcal W }﹩ is close to unity (dashed vertical lines) for TNG50 galaxies, indicating that they are generally consistent with vertical equilibrium; the mean and variance are ﹩{\mathrm{log}}_{10}({P}_{\mathrm{tot}}/{ \mathcal W })=-0.08\pm 0.34﹩ and −0.01 ± 0.36 for z = 0 and z = 2, respectively. Unlike TNG50, the distribution of the ratio in TGN100 (dotted) is shifted toward lower values (﹩{P}_{\mathrm{tot}}\lt { \mathcal W }﹩), resulting in ﹩{\mathrm{log}}_{10}({P}_{\mathrm{tot}}/{ \mathcal W })=-0.31\pm 0.31﹩ and −0.20 ± 0.34 for z = 0 and z = 2, respectively, due to the low resolution.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: The effective velocity dispersion σ eff in TNG50 galaxies as a function of the total pressure P tot at z = 0 (left) and z = 2 (right). The top row shows the mass-weighted vertical average σ eff,avg, while the bottom row shows the midplane value σ eff,mid. For each panel, the two-dimensional distribution is weighted by the fractional contribution to the total SFR at given redshift from each 1 kpc patch in TNG50 galaxies. The TIGRESS fits of the mass-weighted average (Equation (33)) and the midplane value (Equation (34)) of σ eff are shown by the dashed and dotted lines, respectively. The distribution of σ eff in TNG50 broadly follows a similar slope and normalization to the results from TIGRESS (especially consistent with σ eff,avg), albeit with scatter that extends to larger σ eff.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: The depletion time t dep vs. dynamical time t dyn comparison between the SH03 model adopted in TNG50 (right) and the PRFM model using the calibrations from OK22 (left). Both z = 0 (top) and z = 2 (bottom) are shown. The color scale represents the fraction of the total SFR. For reference, t dep/t dyn = 100, 10, and 1 are shown with dashed lines. The SH03 model follows close to constant t dyn/t dep since the model has been calibrated to a constant star formation efficiency per freefall time. In the PRFM model, from Equation (29), t dep/t dyn = ϒtot/σ eff; with less efficient feedback (smaller ϒtot) and higher velocity dispersion (larger σ eff) in higher-pressure environments where t dyn is smaller, a reduction in t dep/t dyn is expected. Thus, PRFM predicts a steeper than unity slope for t dep vs. t dyn.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: Left: Comparison between the measured scale height H g (measured) in TNG50 (black), and the predicted equilibrium scale height using different choices for the effective velocity dispersion. For all predictions, we use Equation (20). The different choices of velocity dispersion are: σ eff = 15 km s−1 (blue), the TIGRESS fit ﹩{\sigma }_{\mathrm{eff}}\propto {{ \mathcal W }}^{0.22}﹩ (i.e., Equation (33) with ﹩{P}_{\mathrm{tot}}={ \mathcal W };﹩ red) for ﹩{ \mathcal W }﹩ the ISM weight, and the TNG50 measured value ﹩{\sigma }_{\mathrm{eff}}=\sqrt{{P}_{\mathrm{tot}}/\rho }﹩ (green). Right: Ratio of the measured to the predicted equilibrium scale height for each case. The vertical dashed line shows the identity (perfect agreement). The top row shows z = 0, and the bottom row shows z = 2. For the theoretical prediction given the measured σ eff in TNG50 (green line), ﹩{\mathrm{log}}_{10}({H}_{{\rm{g}}}({measured})/{H}_{{\rm{g}}}({equil}.))=0.08\pm 0.34﹩ and −0.01 ± 0.36 at z = 0 and z = 2, respectively.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: A flowchart displaying a step-by-step summary of the equations used to implement the PRFM prescription for postprocessing the TNG50 simulation outputs. The first step, above the first dotted horizontal line, describes determination of properties from the simulation. The second step is simultaneous determination of scale height H g, effective velocity dispersion σ eff, and total pressure P tot assuming vertical equilibrium and a calibrated eEoS. The third step, below the second horizontal dotted line, is determination of the SFR from PRFM theory and calibrated feedback yield. For testing how well vertical equilibrium is satisfied within TNG, only the first and third rows of the flowchart are needed, adopting σ eff measured from the TNG simulation.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: The depletion time (t dep) vs. the equilibrium gas density ρ g(equil. ) ≡ Σg/(2H g), for H g in equilibrium obtained using Equation (20). On the right, we show the SH03 value for t dep, while on the left we show the PRFM prediction based on the TIGRESS calibrations in OK22. Both z = 0 (top) and z = 2 (bottom) results are shown, with the color scale representing the fraction of the total SFR. Results from TIGRESS runs are also shown with blue stars. Similar to Figure 9, the PRFM model with the TIGRESS calibration predicts a steeper t dep slope than the SH03 model, leading to much shorter depletion times (by nearly an order of magnitude) at high densities.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: Comparison between Kennicutt–Schmidt relations for the PRFM model (left) and the SH03 model (right) at z = 0 (top) and z = 2 (bottom). The color scale represents contribution to the total SFR. Also shown are results from TIGRESS simulations depicted by blue star symbols, and shaded gray bands showing empirical global KS relations with constant Milky Way (labeled MW) and variable (labeled Bolatto + 2013) α CO (R. C. Kennicutt & M. A. C. De Los Reyes 2021); the width of the band represents ±2σ about the reported best-fit power law. The SH03 model follows the constant–α CO empirical global relation, an earlier version of which was used in the original calibration of the model. At high densities, the PRFM model predicts more efficient star formation and hence a steeper slope.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: Comparison of the SFR-weighted distributions of the depletion time (t dep) in TNG50 (solid) vs. PRFM predictions (dashed) within 1 kpc patches of all galaxies in TNG50 at z = 0 (left) and z = 2 (right). While relatively similar at z = 0, PRFM tends to predict much shorter depletion times at high z, meaning much more efficient star formation.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: Comparison between the eEoS adopted in TNG50 based on SH03 (two-dimensional histogram distribution) and the eEoS fit from the TIGRESS simulations analyzed in OK22 (Equation (36), dotted lines; and Equation (35), dashed lines). Both z = 0 (left) and z = 2 (right) are shown. The slopes are quite similar, but P tot is shifted upward in TNG50 compared to the TIGRESS fits.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: Comparison between models and observations of the relation between the star formation rate surface density ΣSFR and the equilibrium total pressure ﹩{P}_{\mathrm{tot}}({equil}.)={ \mathcal W }﹩. The color scale shows the contribution to the total SFR from kiloparsec-scale patches in TNG50 galaxies based on the native SH03 star formation prescription, at z = 0 (top) and z = 2 (bottom). Also shown are results from different TIGRESS simulations for local galactic disk models (OK22; blue star symbols) and semiglobal galactic center models with (S. Moon et al. 2023; blue circle symbols labeled “TIGRESS-GC-MHD) and without magnetic fields (S. Moon et al. 2021; blue square symbols labeled “TIGRESS-GC-HD). A power-law fit from OK22 is shown as blue line. These models are compared to observations of kiloparsec-scale patches in nearby galaxy surveys PHANGS (J. Sun et al. 2023, green bands) and EDGE (J. K. Barrera-Ballesteros et al. 2021, gray bands), adopting both constant (solid, shown to left) and variable (dashed, shown to right) α CO. The width of the band represents ±2σ about the reported best-fit power law.
Paper: Photonuclear Reaction Rates of 157,159Ho and 163,165Tm and Their Impact in the γ-process
Authors: Hao Cheng, Bao-Hua Sun, Li-Hua Zhu, Motohiko Kusakabe, Yudong Luo, Toshitaka Kajino, Chang-Jian Wang, Xing-Qun Yao, Chuang-Ye He, Fu-Long Liu, Bing Guo
Figure caption: Results of the TALYS calculation compared with experimental data (black dots), for (a) 160Dy(p, γ)161Ho using default parameters (green line), one set of sampling models (colored areas), and the optimized one (red line) that best reproduces the experimental data on both 160Dy(p, γ)161Ho and 162Er(p, γ)163Tm reactions; (b) 162Er(p, γ)163Tm using default parameters (green line), sampling models (blue filled area) and the optimized one (red line).
Paper: Photonuclear Reaction Rates of 157,159Ho and 163,165Tm and Their Impact in the γ-process
Authors: Hao Cheng, Bao-Hua Sun, Li-Hua Zhu, Motohiko Kusakabe, Yudong Luo, Toshitaka Kajino, Chang-Jian Wang, Xing-Qun Yao, Chuang-Ye He, Fu-Long Liu, Bing Guo
Figure caption: Sensitivity s of the 160Dy(p, γ)161Ho (a) and 162Er(p, γ)163Tm (b) cross sections, when the p, n, α, and γ widths are varied by a factor of two, as a function of center-of-mass energy. The data are from T. Rauscher (2012). The shaded area denotes the Gamow window. Within the Gamow windows, the cross sections are predominantly sensitive to the p width.
Paper: Photonuclear Reaction Rates of 157,159Ho and 163,165Tm and Their Impact in the γ-process
Authors: Hao Cheng, Bao-Hua Sun, Li-Hua Zhu, Motohiko Kusakabe, Yudong Luo, Toshitaka Kajino, Chang-Jian Wang, Xing-Qun Yao, Chuang-Ye He, Fu-Long Liu, Bing Guo
Figure caption: Final abundances (upper panel) and their fractional changes from the case of JINA rates (lower panel) in nuclear mole fractions as a function of the peak temperature T 9p for five p-nuclei. The values are taken at a longer simulation time, i.e., 1 yr after the peak temperature. Thick lines correspond to the best-fit rates in this paper, and thin lines correspond to upper and lower limits on the ranges of 20% χ 2.
Paper: Photonuclear Reaction Rates of 157,159Ho and 163,165Tm and Their Impact in the γ-process
Authors: Hao Cheng, Bao-Hua Sun, Li-Hua Zhu, Motohiko Kusakabe, Yudong Luo, Toshitaka Kajino, Chang-Jian Wang, Xing-Qun Yao, Chuang-Ye He, Fu-Long Liu, Bing Guo
Figure caption: Abundances of nuclei around 156,158Dy (upper panel) in the case with the “optimized” fit rates in this paper and their fractional changes from the case of JINA rates, i.e., (Y  i  − Y  iJINA)/Y  iJINA (lower panel) for the profile of T 9p = 2.5.
Paper: Photonuclear Reaction Rates of 157,159Ho and 163,165Tm and Their Impact in the γ-process
Authors: Hao Cheng, Bao-Hua Sun, Li-Hua Zhu, Motohiko Kusakabe, Yudong Luo, Toshitaka Kajino, Chang-Jian Wang, Xing-Qun Yao, Chuang-Ye He, Fu-Long Liu, Bing Guo
Figure caption: (a) Ratios of 157Ho(γ, p)156Dy and 159Ho(γ, p)158Dy stellar rates deduced from the “TALYS_optimized” and JINA (solid lines). The associated uncertainties are shown as the colored bands. (b) The same as (a) but for the 163Tm(γ, p)162Er and 165Tm(γ, p)164Er reactions.
Paper: Photonuclear Reaction Rates of 157,159Ho and 163,165Tm and Their Impact in the γ-process
Authors: Hao Cheng, Bao-Hua Sun, Li-Hua Zhu, Motohiko Kusakabe, Yudong Luo, Toshitaka Kajino, Chang-Jian Wang, Xing-Qun Yao, Chuang-Ye He, Fu-Long Liu, Bing Guo
Figure caption: The same as in Figure 4 but for nuclei around 162,164Er.
Paper: Photonuclear Reaction Rates of 157,159Ho and 163,165Tm and Their Impact in the γ-process
Authors: Hao Cheng, Bao-Hua Sun, Li-Hua Zhu, Motohiko Kusakabe, Yudong Luo, Toshitaka Kajino, Chang-Jian Wang, Xing-Qun Yao, Chuang-Ye He, Fu-Long Liu, Bing Guo
Figure caption: Average overproduction factors calculated by our rates (open circles) compared with JINA (triangles) and M. Kusakabe et al. (2011; diamonds). The horizontal solid and dashed lines correspond to 〈F〉/F 0 equal to 1 and (3, 1/3), respectively.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Quantities averaged over the steady-state period Δt steady for the eight combinations of relative field orientation and stellar magnetic moment. From top: stellar accretion rate; open and disk-connected stellar magnetic flux; EM jet power; stellar torque; magnetospheric radius in units of the corotation radius; and flux-opening efficiency parameter (ζ jet and ζ  ψ ). Vertical bars represent the standard deviation over the averaging period.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: The same as Figure 3, but for the results inferred (i) using data excluding GW190519, (ii) using χ eff, and (iii) using a 1, respectively (from left to right).
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: Two gravitational waveforms for two 30–30M ⊙ BBHs with χ N = 0.15 but having different spin projections. The results are generated using the “IMRPhenomXPHM” model in PYCBC (C. M. Biwer et al. 2019).
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: The same as the right panel of Figure 2, but for the results inferred using data excluding GW190519, using χ eff, and using a 1.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: Posterior predictive check for the TWO_COM model on the χ N distribution (left) and redshift distribution (right). The lighter regions are the model-predicted cumulative distributions (90% credibility), and the darker regions are the observed distributions.