adsabs/AstroCLIMB huggingface dataset:
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: The probability distribution function of compression, ∇ ·  v , is averaged within 5 ≤ t/τ  A  ≤ 10 across the entire domain. The results are shown for CASE1 (red), CASE2 (green), and CASE3 (blue). A is the area corresponding to each compression bin, and A 0 is the total domain size.
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: (Left) L1 error dependency on the number of particles per cell. The red and blue dots indicate particles in the nonrelativistic and relativistic regimes, respectively. The black dashed line indicates the inverse proportionality to the square root of the total number of particles. (Right) L1 error dependency on grid resolution. The color code is the same as in the left panel. The green solid line indicates the L1 error of pure MHD simulation.
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: The magentohydrodynamic shock tube with relativistic nonthermal fluid simulation results for (a) density of the plasma (red dot) and nonthermal fluid (green dot), (b) total pressure (red dot), thermal plasma pressure (purple dot), and nonthermal fluid pressure (green dot), (c) v  x , and (d) nonthermal fluid pressure at t = 0.08.
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: The hydrodynamic shock tube with nonrelativistic nonthermal fluid simulation results for (a) density of the plasma (blue dot) and nonthermal fluid (cyan dot), (b) v  x , (c) thermal plasma pressure (red dot) and total pressure (black dot), and (d) nonthermal fluid pressure at t = 0.1. Solid black lines indicate the analytic Riemann solution.
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: The Advection of the Pressure Balance Mode test at t = 2 with (left) second, (middle) fourth, and (right) sixth order differencing methods (Equation (A1)). Red dot indicates the plasma pressure profile, blue dot indicates the nonthermal fluid pressure, and black dot indicates the total pressure.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: Moment maps and spectra from  3D  BAROLO for sources C1–C7. The first, second, and third columns are the moment-0, moment-1, and moment-2 maps, respectively. These moment maps are generated from data cubes that are not corrected for beam smearing. For each source, the synthesized beam is shown in the bottom-left of the moment-0 map. Column (1): the black ellipse is the outermost ring used in fitting with  3D  BAROLO. The black and blue crosses are the kinematic and flux-weighted centers of the [C II] emission, respectively. The black and blue dashed lines are the kinematic and morphological major axes, respectively. The red contour is at 0.2[C II]peak. Column (2): the filled white circles mark the kinematic major axis of the galaxy, respectively. Column (4): spectrum of the source obtained from a data cube masked according to the SEARCH task. The dashed vertical line is the systemic velocity of the source.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: Results from  3D  BAROLO for sources C1–C7. Columns (1) and (2) show the velocity and dispersion profiles, where the errors were obtained from an MCMC sampling of the parameter space surrounding the best-fit values. Column (3) shows the V rot/σ disp profile for each source. Column (4) shows the Toomre parameter profile for each source (see Section 5.2). The vertical dashed lines denote the beam extent (≈1.6 kpc). The horizontal dashed line in column (3) marks the demarcation line between rotation- and pressure-supported systems. The horizontal dashed line in column (4) marks the Q = 1 stability criteria.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: Comparison of the rotation-to-dispersion ratios of the galaxies within SPT2349−56 and samples of simulated and observed galaxies. The V/σ ratio for our sample is obtained using V flat and σ ext, both computed beyond ≈1.55 kpc. The solid and faded black error bars are the uncertainty of the mean and standard deviation of the sample, respectively. The gray-shaded region includes the theoretical predictions made by A. Dekel & A. Burkert (2014), C. C. Hayward & P. F. Hopkins (2017), A. Pillepich et al. (2019), and A. Zolotov et al. (2015). The dashed line at V/σ = 3 marks the A. Burkert et al. (2010) criteria we use for kinematic classification. Details of the comparison samples are presented in Table 3. The colored dot and cross markers represent MS and starburst galaxies, respectively.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: SNR presentation of the continuum-subtracted and primary-beam corrected integrated [C II] intensity (moment-0) distribution of the core region in SPT2349−56. The sources are named according to R. Hill et al. (2020), and the green boxes indicate the cutout boundaries for each source. The white contour indicates where the primary beam response falls to 80%. The black areas are at SNR < 0. See Section 2 for a description of how the map was prepared.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption:  p–v plots for sources C1–C7 obtained from  3D  BAROLO. Each slice is derived from unmasked cubes. In each 1 × 2 subfigure, the left and right panels are the p–v slices along the major and minor axes, respectively. ϕ and i are the derived position and inclination angle, respectively, for each source. The blue and red contours are at n σ C II (n = 2, 5) for the data and model, respectively. The gray contours are at −n σ C II. The derived rotation curve is overplotted with black-filled circles.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: The Toomre parameter plotted against the V/σ ratio. The dashed line at Q T = 1 marks the stability criteria, while the dashed line at V/σ = 3 marks the rotation-to-dispersion transition. Note that the markers for sources C2 and C6 overlap.
Paper: Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Authors: Claude Cournoyer-Cloutier, Alison Sills, William E. Harris, Brooke Polak, Steven Rieder, Eric P. Andersson, Sabrina M. Appel, Mordecai-Mark Mac Low, Stephen McMillan, Simon Portegies Zwart
Figure caption: Binary fraction as a function of time in units of initial GMC freefall time. Binaries with close (≤100  au) and wide (>100 au) companions are shown as faint solid and dotted curves. For comparison, a fully sampled binary population with the prescription used in this work has a binary fraction of 21%, with 12% of the stars having a close companion and 9% of the stars having a companion with an orbital separation above 100 au.
Paper: Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Authors: Claude Cournoyer-Cloutier, Alison Sills, William E. Harris, Brooke Polak, Steven Rieder, Eric P. Andersson, Sabrina M. Appel, Mordecai-Mark Mac Low, Stephen McMillan, Simon Portegies Zwart
Figure caption: Left: binary fraction as a function of stellar mass after 2.5 t ff. The vertical lines correspond to the Poisson error, and the different runs are offset along the mass axis for readability. The mass bins used are the same ones as in Table 2, with the center of the mass bin at the midpoint between the M1 and M2 data points.
Paper: Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Authors: Claude Cournoyer-Cloutier, Alison Sills, William E. Harris, Brooke Polak, Steven Rieder, Eric P. Andersson, Sabrina M. Appel, Mordecai-Mark Mac Low, Stephen McMillan, Simon Portegies Zwart
Figure caption: Top left: PDF of semimajor axes for M3, color coded as a function of time in units of freefall times of the initial cloud. The black line denotes the primordial distribution. Top right: the same, but normalized to the primordial distribution. Bottom left: PDF of primary masses, normalized to the primordial distribution (in black). Bottom right: PDF of mass ratios, normalized to the primordial distribution (in black).
Paper: Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Authors: Claude Cournoyer-Cloutier, Alison Sills, William E. Harris, Brooke Polak, Steven Rieder, Eric P. Andersson, Sabrina M. Appel, Mordecai-Mark Mac Low, Stephen McMillan, Simon Portegies Zwart
Figure caption: Star formation rate as a function of time in units of initial GMC freefall time. Note that all lines are slightly truncated at the end due to the Gaussian smoothing.
Paper: Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Authors: Claude Cournoyer-Cloutier, Alison Sills, William E. Harris, Brooke Polak, Steven Rieder, Eric P. Andersson, Sabrina M. Appel, Mordecai-Mark Mac Low, Stephen McMillan, Simon Portegies Zwart
Figure caption: Left: probability that the semimajor axes are smaller than in the primordial distribution as a function of time. M1, M2, and M3 consistently show a difference relative to the primordial distribution after 2.37, 1.98, and 1.66 t ff (2.51, 1.05, and 0.44 Myr). Right: KS statistic measuring the amount of change from the primordial distribution as a function of time.
Paper: Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Authors: Claude Cournoyer-Cloutier, Alison Sills, William E. Harris, Brooke Polak, Steven Rieder, Eric P. Andersson, Sabrina M. Appel, Mordecai-Mark Mac Low, Stephen McMillan, Simon Portegies Zwart
Figure caption: Gas column density, with stars overplotted as small white circles. The columns correspond to the different simulations, while the rows show the distribution of stars and gas at approximately 1.0, 1.5, 2.0, and 2.5 freefall times of the initial GMC.
Paper: Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Authors: Claude Cournoyer-Cloutier, Alison Sills, William E. Harris, Brooke Polak, Steven Rieder, Eric P. Andersson, Sabrina M. Appel, Mordecai-Mark Mac Low, Stephen McMillan, Simon Portegies Zwart
Figure caption: Left: semimajor of primordial binaries, all binaries present in cluster after 2.5 t ff, and dynamically formed binaries for M3. Right: the same, but for binaries with O-star primaries only.
Paper: Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Authors: Claude Cournoyer-Cloutier, Alison Sills, William E. Harris, Brooke Polak, Steven Rieder, Eric P. Andersson, Sabrina M. Appel, Mordecai-Mark Mac Low, Stephen McMillan, Simon Portegies Zwart
Figure caption: Median and 90th percentile local stellar density as a function of time in units of initial GMC freefall time.
Paper: Turbulent Transport Characteristics of the Particles within Pulsar Wind Nebulae 3C58 and G54.1+0.3
Authors: Fang-Wu Lu, Bo-Tao Zhu, Wen Hu, Li Zhang
Figure caption: Top panels: the current spectral distributions of the turbulent waves (left) and electrons (right) of 3C58 calculated in the framework of KO and KR models, respectively. Bottom panels: the current timescales of the turbulent waves (left) and electrons (right) of 3C58. The spectra and timescales for the turbulent waves with wavenumber k are plotted at the resonant energy of ﹩{E}_{\mathrm{res}}(k)={eB}/k﹩ for the convenience of discussions.
Paper: Turbulent Transport Characteristics of the Particles within Pulsar Wind Nebulae 3C58 and G54.1+0.3
Authors: Fang-Wu Lu, Bo-Tao Zhu, Wen Hu, Li Zhang
Figure caption: Left-hand panels: The current distributions of the energy (top panel) and spatial (bottom panel) diffusion coefficients obtained in the KO model for the Crab Nebula (black line), 3C58 (red line), and G54.1+0.3 (blue line). Right-hand panels: Same as the left-hand panels but for the KR model. Corresponding dashed lines shown in the top and bottom panels are the fitting results for the power-law fits with indices of 5/3 (3/2) for the energy diffusion coefficient and 1/3 (1/2) for the spatial diffusion coefficient in the Kolmogorov (Kraichnan) turbulence at E e ≥ 1 TeV.
Paper: Turbulent Transport Characteristics of the Particles within Pulsar Wind Nebulae 3C58 and G54.1+0.3
Authors: Fang-Wu Lu, Bo-Tao Zhu, Wen Hu, Li Zhang
Figure caption: Top panels: The current spectral distributions of the turbulent waves (left-hand panel) and electrons (right-hand panel) of G54.1+0.3 calculated in the framework of KO and KR models, respectively. Bottom panels: The current timescales of the turbulent waves (left-hand panel) and electrons (right-hand panel) of G54.1+0.3.
Paper: Turbulent Transport Characteristics of the Particles within Pulsar Wind Nebulae 3C58 and G54.1+0.3
Authors: Fang-Wu Lu, Bo-Tao Zhu, Wen Hu, Li Zhang
Figure caption: Fitting results of the SEDs of G54.1+0.3 in KO (black-solid line) and KR (red-dashed line) models.
Paper: Turbulent Transport Characteristics of the Particles within Pulsar Wind Nebulae 3C58 and G54.1+0.3
Authors: Fang-Wu Lu, Bo-Tao Zhu, Wen Hu, Li Zhang
Figure caption: Fitting results of the SEDs of 3C58 in KO (black-solid line) and KR (red-dashed line) models.
Paper: Turbulent Transport Characteristics of the Particles within Pulsar Wind Nebulae 3C58 and G54.1+0.3
Authors: Fang-Wu Lu, Bo-Tao Zhu, Wen Hu, Li Zhang
Figure caption: The evolution of the Alfvén speed for G54.1+0.3 in KO (black-solid line) and KR (red-dashed line) models.
Paper: Turbulent Transport Characteristics of the Particles within Pulsar Wind Nebulae 3C58 and G54.1+0.3
Authors: Fang-Wu Lu, Bo-Tao Zhu, Wen Hu, Li Zhang
Figure caption: The evolution of the Alfvén speed for 3C58 in KO (black-solid line) and KR (red-dashed line) models.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: (a) Perturbation vertical and azimuthal velocities at t/T 0 = 36.1 showing their correlation and their N-waveform. (b) Specific angular momentum j  z  ≡ u  ϕ  r at z = 2H 0. Solid black line: at t/T 0 = 36.1 for the axisymmetric run. Solid blue line: at t/T 0 = 422.10 for the 3D run (azimuthal location ϕ = 0). (c) Similar to panel (a) except evaluated at z = 0.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Perturbation vorticity for the axisymmetric run.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Perturbation velocity for the axisymmetric simulation on a 5722 mesh at t/T 0 = 36.1. (a) Vertical velocity, u  z . (b) Perturbation azimuthal velocity, δ u  ϕ . (c) The product, δ u  z  δ u  ϕ . Pure white regions represent values that are outside of the range of the color bar/legend.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Time history of the components of the volume-averaged disturbance kinetic energy (relative to the basic state) for the 3D run in the period t/T 0 ∈ [0, 300.27] during which the strength of the Padé filter was set to ϵ filter = 0.125.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Probability density function of perturbation vorticity components for the axisymmetric run at t/T 0  =  36.1. The parameter c in the Cauchy distribution (Equation (28)) was set to c = 4.35 to obtain the green dashed curve.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: (a) Deviations from the basic state of the vertical shear term T 1 on the rhs of the transport Equation (B11) for azimuthal vorticity. (b) Similarly, the deviation T 2 (baroclinic term). In panel (b), values exceeding the range of the color legend are rendered in white. The actual range of values is indicated in the headings.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Basic-state vorticity.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: Gas density distribution at t = 0, 10,000t g, 24,000t g for models D_d001 and Q_d001. Stream plots are magnetic field vectors. Vectors in panels (A-3) and (B-3) are the gas velocity vectors in the region where ﹩4\pi {r}^{2}\rho {u}^{r}\gt {\dot{M}}_{\mathrm{Edd}}﹩. Here, the color of each vector indicates the magnitude of the velocity in the poloidal direction. The gray region of r < 10km is the NS.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: Time evolution of the mass accretion rate (black), outflow rate (blue), radiative luminosity (red), and kinetic luminosity (green).
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: The ratio of the kinetic luminosity to the radiative luminosity as a function of f.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: The measured number density ρ n (top panel), initial stellar mass M ini (middle panel), and SFR (bottom panel) for NGC 6822 across the age–metallicity plane (left panel) and their projection over the age-axis (right panel). The yellow/gray shadow indicates the random/total (random and systematic) uncertainties, guided by the output of SFHNet (red solid line). A zoom-in view of SFR at the old age side (log(t) ≥ 8.0) is provided in the inset panel. The average SFR over the past 100 Myr, i.e., SFR100 is marked as a black dash line and black plus in the bottom-right panel and its inset panel, respectively.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: Same as Figure 8, but for dIrrs and dTrans.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: Same as Figure 10, but for Tucana.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: Same as Figure 10, but for Sextans A.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: Same as Figure 10, but for NGC 185.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: Same as Figure 10, but for NGC 205.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: Same as Figure 10, but for Ursa Minor.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: Same as Figure 10, but for Pegasus.
Paper: The Star Formation History of Nearby Galaxies: A Machine Learning Approach
Authors: Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng,  Hao  Tian
Figure caption: Same as Figure 10, but for Phoenix.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: Left panels: theoretical light curves in various Johnson–Cousins passbands for a CC F-mode model (bottom panel) and FO-mode model (upper panel), both located at the center of the IS. The metallicity, mass (in solar units), luminosity (in solar units), and effective temperature (in kelvin) for the selected model are labeled. Right panels: same as the left panels but for RRL models.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: Upper panels: comparison between multifilter PL relations in the Rubin-LSST i, z, and y bands for RR Lyrae stars with Z = 0.001 derived in the present work and those from M. Marconi et al. (2022). Lower panels: same as the upper panels but for RR Lyrae stars with Z = 0.02.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: The Wesenheit function, W (I, V−I) (left panels) and W (K, V−K) (right panels), plotted as a function of the logarithmic period for F-mode CCs with Z = 0.004 (upper panels) and Z = 0.02 (bottom panels).