adsabs/AstroCLIMB huggingface dataset:
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Intermediate (midway between edge- and face-on) projections of LOS velocity (vlos) weighted by the O VIII line emissivity for all galaxies in the sample sorted from lowest to highest halo mass (with ﹩\mathrm{log}(M\,[{M}_{\odot }])﹩ indicated in each bottom right corner). The vlos structure varies significantly, even between halos of similar masses, as a function of simulation and environment.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Edge-on projections of kT weighted by the broadband X-ray emissivity for all galaxies in the sample sorted from lowest to highest halo mass (with ﹩\mathrm{log}(M\,[{M}_{\odot }])﹩ indicated in each bottom right corner). The temperature structure of hot CGM in galaxies varies significantly as a function of galaxy mass, simulation, and environment.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Intermediate (midway between edge- and face-on) projections of broadband X-ray surface brightness (XSB).
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Face-on projections of kT weighted by the broadband X-ray emissivity.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Intermediate (midway between edge- and face-on) projections of LOS velocity dispersion (σv,los) weighted by the O VIII line emissivity.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Face-on projections of LOS velocity dispersion (σv,los) weighted by the O VIII line emissivity.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Intermediate (midway between edge- and face-on) projections of kT weighted by the broadband X-ray emissivity.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Edge-on projections of LOS velocity (vlos) weighted by the O VIII line emissivity.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Face-on projections of LOS velocity (vlos) weighted by the O VIII line emissivity.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Face-on projections of broadband X-ray surface brightness (XSB).
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Histogram showing the distribution of the difference in the SNR of the spectral covariance matrix, defined in Equation (20), relative to the case with ζ = −1. The SNR is computed assuming 2000 isotropically distributed pulsars with identical timing residual noise. Panels (a) and (b) correspond to red noise amplitudes Ared = 10−14 and 10−15, respectively, with a fixed spectral index γ =  −3 and white noise level σw = 10−7 s. Each histogram is generated using 300 independent Monte Carlo realizations. The dashed vertical line indicates the median value of the distribution.
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Schematic diagram summarizing our simulation technique, showing the multiscale framework linking Gpc-scale structure (MICECAT), Mpc-scale SMBH-galaxy coevolution (ROMULUS25), and subparsec binary dynamics, including environment and eccentricity, to model the nHz SGWB. The SMBHB population is generated via a Monte Carlo sampling procedure based on the MICECAT simulated galaxy catalog. For each binary, a time-domain gravitational waveform is computed using eccentric waveform modeling. These waveforms are then truncated to match the chosen observation time and are subsequently Fourier transformed. Finally, the SGWB map is constructed by summing the GW energy density contributions from all sources within each sky pixel.
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: SGWB spectrum, ΩGW(f), for three different eccentricity distributions characterized by ζ = −1, ζ = 0, and ζ = 1. The solid lines represent the median ΩGW(f) obtained from 300 Monte Carlo realizations, while the shaded regions denote the 68% credible intervals.
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Histogram showing the distribution of the difference in the combined SNR of the ΩGW(f) and C(f1, f2), defined in Equations (20) and (19), relative to the case with ζ = −1. The SNR is computed assuming 2000 isotropically distributed pulsars with identical timing residual noise. Panels (a) and (b) correspond to red noise amplitudes Ared = 10−14 and 10−15, respectively, with a fixed spectral index γ =  −3 and white noise level σw = 10−7 s. Each histogram is generated using 300 independent Monte Carlo realizations. The dashed vertical line indicates the median value of the distribution.
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Time-domain waveforms generated by InspiralESIGMAHM, along with their Fourier transforms for an eccentric binary (e = 0.5). ﹩{h}_{\ell m}^{{\mathbb{R}}}﹩ and ﹩{h}_{\ell m}^{{\mathbb{I}}}﹩ represent the real and imaginary parts of the (ℓ, m) GW mode, while ﹩| {\tilde{h}}_{\ell m}^{{\mathbb{R}}}| ﹩ and ﹩| {\tilde{h}}_{\ell m}^{{\mathbb{I}}}| ﹩ denote the absolute values of their respective Fourier transforms. The (2, 2) mode is shown along with the next three dominant modes: (2, 1), (3, 3), and (4, 4).
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Time-domain waveforms generated by InspiralESIGMAHM, along with their Fourier transforms for a circular binary (e = 0). ﹩{h}_{\ell m}^{{\mathbb{R}}}﹩ and ﹩{h}_{\ell m}^{{\mathbb{I}}}﹩ represent the real and imaginary parts of the (ℓ, m) GW mode, while ﹩| {\tilde{h}}_{\ell m}^{{\mathbb{R}}}| ﹩ and ﹩| {\tilde{h}}_{\ell m}^{{\mathbb{I}}}| ﹩ denote the absolute values of their respective Fourier transforms. The (2, 2) mode is shown along with the next three dominant modes: (2, 1), (3, 3), and (4, 4).
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Normalized spectral covariance matrix CN(f1, f2) (defined in Equation (18)) for three different eccentricity distributions characterized by ζ = −1, 0, and 1. The spectral correlations become increasingly prominent with increasing eccentricity, reflecting the broader harmonic content of GW signals from eccentric binaries.
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Eccentricity distributions of SMBHBs modeled using a power-law probability density function, P(e) ∝ eζ. Distributions are shown for three values of the power-law index: ζ = −1 (favoring nearly circular binaries), ζ = 0 (uniform distribution), and ζ = 1 (favoring highly eccentric binaries).
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Eccentricity (e) of the SMBH binary as a function of its orbital frequency (forb). The binary begins with an initial eccentricity of e = 0.6 at forb = 10−9 Hz and evolves solely under the influence of GW radiation.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. II. Hard X-Ray Spectra, Light Curves, and Spatial Distributions
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Simulated hard X-ray spatial profiles for an injected flux ﹩{{ \mathcal F }}_{o}=3\times 1{0}^{10}﹩ erg cm−2 s−1. The top row (panels (a) and (b)) shows results at t = 10 s into the simulation, while the bottom row (panels (c) and (d)) shows results at t = 20 s, the end of the electron injection phase. Each row presents results for two different flare orientations on the solar disk: panels (a) and (c) correspond to a limb event viewed at right angles to the loop axis, and panels (b) and (d) to an event at disk center, for which the line of sight passes vertically through the loop structure so that line-of-sight projection effects are important. Each set of panels shows the results for three different observed photon energies: ϵ = 10 keV (left column), 15 keV (middle column), and 20 keV (right column). Each row in a given panel shows results for four different values of the parameter α (Equation (2)): (from top to bottom) α = 0, 2, 4, and 6; within each plot, profiles are shown for values of the parameter R = 0, 1, 2, 5, and 10.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. II. Hard X-Ray Spectra, Light Curves, and Spatial Distributions
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Results for different injected electron energy fluxes ﹩{{ \mathcal F }}_{o}﹩ (Equation (1)). Top row: temperature vs. position; Bottom row: density vs. position. All cases are for α = 0 and at t = 20 s. From left to right, results are shown for ﹩{{ \mathcal F }}_{o}=3\times 1{0}^{10}﹩ erg cm﹩{}^{{}_{2}}﹩ s−1, ﹩{{ \mathcal F }}_{o}=1{0}^{11}﹩ erg cm﹩{}^{{}_{2}}﹩ s−1, and ﹩{{ \mathcal F }}_{o}=3\times 1{0}^{11}﹩ erg cm﹩{}^{{}_{2}}﹩ s−1, respectively. After A. G. Emslie et al. (2024).
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. II. Hard X-Ray Spectra, Light Curves, and Spatial Distributions
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Profiles of hard X-ray intensity (including both thermal and nonthermal contributions) at (from left to right) photon energies of 10, 15, and 20 keV, for an injected electron spectrum given by Equation (1), with ﹩{{ \mathcal F }}_{o}=3\times 1{0}^{10}﹩ erg cm−2 s−1 (top row), ﹩{{ \mathcal F }}_{o}=1{0}^{11}﹩ erg cm−2 s−1 (middle row), and ﹩{{ \mathcal F }}_{o}=3\times 1{0}^{11}﹩ erg cm−2 s−1 (bottom row). Each plot shows the spatial profile of hard X-ray emission for α = 0 and for five different values of the turbulence parameter R (Equation (2)) and for time t = 0, 10, and 20 s into the beam injection phase. For ease in presentation, the profiles for t = 10 s and t = 20 s have been scaled upwards by factors of 10 and 100, respectively.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. II. Hard X-Ray Spectra, Light Curves, and Spatial Distributions
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Loop-integrated X-ray spectra for α = 6 (top left), 4 (top right), 2 (bottom left), and 0 (bottom right), for an injected electron flux ﹩{{ \mathcal F }}_{o}=1{0}^{11}﹩ erg cm−2 s−1. In each case, spectra for various values of R, from R = 0 (collisions only) to R = 10 are shown; the black dashed–dotted spectra are for a collisions-only model obtained by setting the resistivity η to zero. Both thermal and nonthermal contributions to the hard X-ray emission are included. For ease of presentation, the spectra for t = 10 and t = 20 s are scaled upwards by factors of 10 and 100, respectively.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. II. Hard X-Ray Spectra, Light Curves, and Spatial Distributions
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Loop-integrated X-ray light curves for α = 0, photon energies ϵ = 15 keV (top row), 20 keV (middle row), 25 keV (bottom row), and injected energy fluxes ﹩{{ \mathcal F }}_{o}=3\times 1{0}^{10}﹩ erg cm−2 s−1 (left column), 1011 erg cm−2 s−1 (middle column), and 3 × 1011 erg cm−2 s−1 (right column). In each case light curves are shown for various values of R, from R = 0 (collisions only) to R = 10; the black dashed–dotted spectra (shown only for the case ﹩{{ \mathcal F }}_{o}=1{0}^{11}﹩ erg cm−2 s−1) are for a collisions-only model obtained by artificially setting the resistivity η to zero. Both thermal and nonthermal contributions to the hard X-ray emission are included (solid lines); the nonthermal component is shown as a dashed line.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. II. Hard X-Ray Spectra, Light Curves, and Spatial Distributions
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Local spectral indices ﹩\gamma =-d\,{\mathrm{log}}\,I(\epsilon )/d\,{\mathrm{log}}\epsilon ﹩ for the spectra in Figure 2.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. II. Hard X-Ray Spectra, Light Curves, and Spatial Distributions
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: As for Figure 6, but for an injected flux ﹩{{ \mathcal F }}_{o}=1{0}^{11}﹩ erg cm−2 s−1.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Theoretical limb-brightening correction curves (LBCCs) used to correct the limb brightening of AIA 193 Å intensity in this study. Left panel: LBCCs for different electron density scale heights. Right panel: the difference from the LBCC suggested by R. Caplan et al. (2016).
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: Two-dimensional distributions of Ωm vs. w assuming a flat wCDM cosmology. The dark and light-shaded regions represent the 68% and 95% credible regions for AGEL0353 alone, three DSPLs combined, and Planck CMB measurements (Planck Collaboration 2020) in red, green, and pink. The red, blue, and orange dashed contours represent the 68% credible levels for AGEL0353, AGEL1507, and J0946. The black contours represent the 68% and 95% credible levels for the combined constraints of the DSPLs and CMB measurements.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: Regions within the Ωm − w parameter space for a flat wCDM cosmology. In the left and right panels, the possible range of β12 is given for the lensing configurations of AGEL0353 and J0946, where β12 ∈ [0.911, 0.934] and β12 ∈ [0.706, 0.763], respectively. AGEL0353 and J0946 each have distinct values of β12,fid = 0.916 and β12,fid = 0.721, respectively. Red and blue regions are bounded by an uncertainty of ±0.3% on two values of β12/β12,fid. In red are the regions centered on β12/β12,fid = 1.007 and in blue are the regions centered on β12/β12,fid = 0.999. The black dashed lines represent where the median values of β12, which we measure from lens models of AGEL0353 and J0946, exist within the parameter space.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: Two-dimensional distributions of Ωm vs. w under the assumption of a flat wCDM cosmology. The dark and light-shaded regions in green, purple, yellow, pink, and cyan represent the 68% and 95% credible regions for our DSPL, DESI year 1 BAO plus SDSS (DESI Collaboration 2025a), 5 yr DES SNe (DES Collaboration 2024), Planck CMB (Planck Collaboration 2020), and all the former measurements combined, respectively. The black dashed line represents values where w = −1 following a ΛCDM cosmology.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). IV. Surface Gravity Estimation and Giant–Dwarf Separation with the DDO51 Filter
Authors: Qiqian Zhang, Zhou Fan, Gang Zhao, Ying Wu, Wei Wang, Kai Xiao, Hongrui Gu, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Ali Luo, Nan Song, Yujuan Liu, Yaqian Wu
Figure caption: Comparison of log g predictions from XGBoost models trained on SAGES and Gaia XP synthetic photometry, with and without the DDO51 filter. (a) Results using SAGES colors and E(B – V), without the DDO51 filter. (b) Results with the same features as panel (a), but additionally including the (g – DDO51) color. Large panels: 2D histograms of XGBoost predicted vs. spectroscopic log g from LAMOST. The color scale indicates stellar density (logarithmic scale). The cyan dashed line indicates the one-to-one relation. Small top panels: standard deviation of residuals (predicted-spectroscopic) log g as a function of spectroscopic log g, binned in 0.5 dex intervals. The cyan line and error bars indicate the median and standard deviation within each bin. Small bottom panels: histograms of residuals, annotated with mean (μ) and standard deviation (σ).
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). IV. Surface Gravity Estimation and Giant–Dwarf Separation with the DDO51 Filter
Authors: Qiqian Zhang, Zhou Fan, Gang Zhao, Ying Wu, Wei Wang, Kai Xiao, Hongrui Gu, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Ali Luo, Nan Song, Yujuan Liu, Yaqian Wu
Figure caption: Residual analysis of log g predictions as a function of spectroscopic parameters, with and without the DDO51 Filter. (a) Residuals (predicted log g – spectroscopic log g) plotted against spectroscopic log g. (b) Residuals vs. [Fe/H]. (c) Residuals vs. against Teff. In all panels, solid lines show the standard deviation of the residuals, and dotted lines indicate the mean of the residual within bins. Bin widths are 0.2 dex for log g, 0.2 dex for [Fe/H], and 200 K for Teff. Blue lines represent the model without DDO51, while red lines represent the model including DDO51.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). IV. Surface Gravity Estimation and Giant–Dwarf Separation with the DDO51 Filter
Authors: Qiqian Zhang, Zhou Fan, Gang Zhao, Ying Wu, Wei Wang, Kai Xiao, Hongrui Gu, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Ali Luo, Nan Song, Yujuan Liu, Yaqian Wu
Figure caption: Schematic diagram illustrating the DDO51 filter’s sensitivity to stellar surface gravity. Solid lines represent theoretical spectra of dwarf and giant stars with identical Teff = 5000 K and [M/H] = −0.5. The green dashed line indicates the DDO51 filter transmission. The spectra have been normalized and vertically shifted for clarity. The depth of the Mg I absorption features within the DDO51 passband (highlighted by the gray shaded region) increases markedly with increasing log g, demonstrating the filter’s effectiveness in distinguishing between different surface gravities.