adsabs/AstroCLIMB huggingface dataset:
Paper: The Structure and Formation Histories of Low-mass Quiescent Galaxies in the A2744 Cluster Environment
Authors: Sam E. Cutler, John R. Weaver, Katherine E. Whitaker, Jenny E. Greene, David J. Setton, Zach J. Webb, Ayesha Abdullah, Aubrey Medrano, Rachel Bezanson, Gabriel Brammer, Robert Feldmann, Lukas J. Furtak, Karl Glazebrook, Ivo Labbe, Joel Leja, Danilo Marchesini, Tim B. Miller, Ikki Mitsuhashi, Themiya Nanayakkara, Erica J. Nelson, Richard Pan, Sedona H. Price, Katherine A. Suess, Bingjie Wang, 冰洁 王
Figure caption: Low-mass quiescent galaxies in A2744 follow a similar size–mass relation to those measured from local dwarf galaxies. However, the larger intrinsic scatter relative to field studies may indicate the effect of dynamical interactions expanding and/or eroding cluster galaxies over time. In the left panel, F200W semimajor axis sizes of low-mass quiescent galaxies in our sample are indicated with gray points. Sources that have corresponding NIRSpec spectroscopy are highlighted with black stars. Open points and stars indicate sources whose sizes are measured via growth curves (due to poor GALFIT models). In the right panel, size–mass relations from the literature are shown: blue squares show the median sizes of 1 < z < 3 low-mass quiescent galaxies from S. E. Cutler et al. (2024), a dotted red line shows the fit to a combined sample of nearby dwarfs and massive ellipticals in P. Eigenthaler et al. (2018), a dashed maroon line shows the size–mass relation of local dwarf satellites in S. G. Carlsten et al. (2021), a dotted–dashed green line shows the K. V. Nedkova et al. (2021) 0.2 < z < 0.5 size–mass relation based on HFF and CANDELS, and a dotted–dashed purple line represents the PRIMER 0.25 < z < 0.75 low-mass quiescent size–mass relation from M. L. Hamadouche et al. (2025). Gray contours indicate the distribution of all A2744 cluster galaxies in our sample (both solid and open points in the left panel). In both panels, the solid black line shows the linear best-fit size–mass relation to GALFIT-modeled, ﹩{\mathrm{log}}({M}_{\star }/{M}_{\odot })\lt 9﹩ quiescent galaxies (Equation (1)), while the dashed black line shows the LOWESS fit to all galaxies in the sample. The shaded cyan region in the left panel shows the 1σ uncertainty on the linear fit. Brown contours in all panels show the distribution of 0 < z < 0.5 quiescent field galaxies from S. E. Cutler et al. (2022). The F200W PSF half-width at half-maximum is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩032, corresponding to ∼0.15 kpc at z = 0.308.
Paper: The Structure and Formation Histories of Low-mass Quiescent Galaxies in the A2744 Cluster Environment
Authors: Sam E. Cutler, John R. Weaver, Katherine E. Whitaker, Jenny E. Greene, David J. Setton, Zach J. Webb, Ayesha Abdullah, Aubrey Medrano, Rachel Bezanson, Gabriel Brammer, Robert Feldmann, Lukas J. Furtak, Karl Glazebrook, Ivo Labbe, Joel Leja, Danilo Marchesini, Tim B. Miller, Ikki Mitsuhashi, Themiya Nanayakkara, Erica J. Nelson, Richard Pan, Sedona H. Price, Katherine A. Suess, Bingjie Wang, 冰洁 王
Figure caption: The selected sample of low-mass cluster galaxies from the UNCOVER/MegaScience SW-selected catalogs. Top: the redshift distributions for all 0.238 < zphot < 0.378 galaxies and the sample of cluster galaxies selected via red-sequence fitting are shown in black and red, respectively. The purple histogram shows the distribution of all confirmed 0.238 < zspec < 0.378 spectroscopic redshifts in A2744 obtained from V. Kokorev et al. (2022). The dashed black lines highlight the redshift range used to select cluster galaxies, while dotted black lines indicate the more constrained redshift range used to select a “gold” sample of cluster members. Bottom: the positions of all sources at 0.238 < z < 0.378 in the F070W − F090W color–magnitude diagram are shown with black points and the red-sequence selection of quiescent cluster members is highlighted in red. Additional quiescent cluster members identified via UVJ selection are indicated with blue points. The green dashed line indicates the best-fit line to the red sequence, with the shaded region highlighting the 2σ scatter (roughly 0.1 ABmag). Purple stars and ×’s represent sources with corresponding NIRCam PRISM spectroscopy and other archival spectroscopic redshifts, respectively.
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: Evaluation of XGBoost log g predictions and comparison with APOGEE differences, using stars common to our test set and APOGEE DR17. (Left): XGBoost-predicted log g from our model (including DDO51) plotted against APOGEE DR17 spectroscopic log g. (Right): LAMOST DR10 spectroscopic log g plotted against APOGEE DR17 spectroscopic log g. This panel illustrates the inherent systematic differences between the LAMOST and APOGEE spectroscopic determinations for the same set of stars. The red dashed line in both panels represents the one-to-one relation. The standard deviation (σ) and systematic bias (μ) of the differences are shown.
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: Impact of input magnitude uncertainty on the precision and accuracy of stellar parameter estimation, assessed via Monte Carlo simulations. (a) Distribution of the standard deviation of predicted log g values as a function of input magnitude uncertainty. Gaussian noise with varying standard deviations (x-axis) was added to the input magnitudes, and the standard deviation of the resulting log g predictions (from 2000 simulations) is shown for each star. (b) Distribution of giant/dwarf classification accuracy as a function of input magnitude uncertainty. The fraction of simulations in which the predicted log g classification (giant if log g <  4.0, dwarf if log g >  4.0) agrees with the spectroscopic classification is shown. The 2D histogram's color scale in both panels represents the number of stars within each bin.
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: Color–color diagrams based on synthetic photometry from ATLAS9 model atmospheres, showing the behavior of DDO51, g, uSC, and vSAGES colors as a function of metallicity and surface gravity. The g − i color serves as a proxy for effective temperature. Panels (from top to bottom) show g – DDO51, uSC – DDO51, and vSAGES – DDO51 plotted against g − i. Point color indicates log g.
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: Performance of the XGBoost models from Figure 6 for log g prediction, restricted to GK-type stars with effective temperatures below 5600 K. (a) Results using SAGES colors and E(B – V) only. (b) Results including the (g – DDO51) color. The layout and symbols are the same as in Figure 6.
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: Performance of the XGBoost models on a subsample of 2323 metal-poor stars ([Fe/H] < −1.0) from the test set. (Left): predictions without the DDO51 filter. (Right): predictions including the DDO51. The color of each point represents the absolute residual between the predicted and spectroscopic values.
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: Cross-survey validation of the model’s generalization capability on an independent sample of 882 metal-poor ([Fe/H] < −1.0) stars from the APOGEE survey. The panels compare log g predicted by our LAMOST-trained model against APOGEE’s spectroscopic values. The layout and symbols are the same as in Figure 9.
Paper: Advanced Weights for IXPE Polarization Analysis
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: Polarization degrees extracted for four point sources using aperture-based methods in common use (left) and the weights considered in this work (right). Black results use Mom-reconstructed data, while red results use NN reconstruction. Uncertainties are expressed in terms of the PD uncertainty and the area of the Q–U uncertainty contour (σQσU) relative to the PCUBE area. PD results are compared in the middle column. The weights introduced in this paper together substantially reduce polarization uncertainties. For the GRB, ×s indicate 99% confidence upper PD limits since polarization is not detected.
Paper: Advanced Weights for IXPE Polarization Analysis
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: Uncertainties as a function of background flux, measured by the ratio of background counts within the 60″ PCUBE radius to source counts. The number of source counts is kept constant. Dotted lines show the true Stokes coefficients, and dashed lines show the coefficients extracted by the two fit methods. Bands reflect the estimated uncertainties. Especially for faint sources, our method delivers substantially more precise fits than PCUBE.
Paper: Diversity of Cold Worlds: Predicted Near-to-mid-infrared Spectral Signatures of a Cold Brown Dwarf with Potential Auroral Heating
Authors: Genaro Suárez, Jacqueline K. Faherty, Ben Burningham, Caroline V. Morley, Johanna M. Vos, Brianna Lacy, Melanie J. Rowland, Adam C. Schneider, Sherelyn Alejandro Merchan, Daniella C. Bardalez Gagliuffi, Thomas P. Bickle, Eileen C. Gonzales, Rocio Kiman, Austin Rothermich, Niall Whiteford
Figure caption: Observed and predicted SEDs of W1935. The observations include the NIRSpec G395H spectrum (original R ∼ 2700 resolution in light green and R ∼ 250 convolved spectrum in dark green) and NIRI, IRAC, WISE, and JWST/MIRI magnitudes (Section 2.1), as indicated in the bottom-right legend. The best retrieved spectra in J. K. Faherty et al. (2024) using either a thermal inversion (black line) or no thermal inversion (brown line) in the upper atmosphere are shown. Synthetic fluxes from both retrieved spectra for the filters with observations, along with IRAC Ch3 (5.6 μm) and Ch4 (7.6 μm), are plotted using the same color as their corresponding spectra. Additional synthetic IRAC Ch1 and Ch2 fluxes from the NIRSpec spectrum are shown in green. The main spectral features are indicated (see Figure 3), including the principal methane emission regions.
Paper: Diversity of Cold Worlds: Predicted Near-to-mid-infrared Spectral Signatures of a Cold Brown Dwarf with Potential Auroral Heating
Authors: Genaro Suárez, Jacqueline K. Faherty, Ben Burningham, Caroline V. Morley, Johanna M. Vos, Brianna Lacy, Melanie J. Rowland, Adam C. Schneider, Sherelyn Alejandro Merchan, Daniella C. Bardalez Gagliuffi, Thomas P. Bickle, Eileen C. Gonzales, Rocio Kiman, Austin Rothermich, Niall Whiteford
Figure caption: Top panel: SED for W1935 in Figure 1 along with the absorption cross sections for key molecular species at a representative temperature of 475 K and a pressure of 1 bar. Middle panel: contribution function for the retrieved spectrum with thermal inversion. The horizontal dashed line indicates the approximate maximum pressure at which the thermal inversion occurs. Bottom panel: contribution function for the retrieved spectrum without thermal inversion. The horizontal dashed line indicates is the same as in the middle panel.
Paper: Stellar Mass Segregation in Dark Matter Halos
Authors: Raphaël Errani, Jorge Peñarrubia, Matthew G. Walker
Figure caption: Several Milky Way satellites have relaxation times Trel shorter than 10 Gyr even in the presence of substantial amounts of dark matter. Those objects may exhibit stellar mass segregation driven by collisional relaxation. Shown are stellar masses M⋆ and (3D) half-light radii rh of dwarf galaxies (open circles), ambiguous stellar clusters (triangles), as well as the “microgalaxy” candidates UMa3/U1, Del1, and Eri3 (red filled circle, diamond and square, respectively). See footnote 2 for references. Curves of constant relaxation time Trel = 1 Gyr and 10 Gyr are computed assuming a dynamical-to-stellar mass ratio of ϒdyn = 10 within the half-light radius, with stellar masses sampled from a G. Chabrier (2003) present-day mass function (see text for details).
Paper: Diversity of Cold Worlds: Predicted Near-to-mid-infrared Spectral Signatures of a Cold Brown Dwarf with Potential Auroral Heating
Authors: Genaro Suárez, Jacqueline K. Faherty, Ben Burningham, Caroline V. Morley, Johanna M. Vos, Brianna Lacy, Melanie J. Rowland, Adam C. Schneider, Sherelyn Alejandro Merchan, Daniella C. Bardalez Gagliuffi, Thomas P. Bickle, Eileen C. Gonzales, Rocio Kiman, Austin Rothermich, Niall Whiteford
Figure caption: CMDs for all combinations of IRAC Ch1, Ch2, Ch3, and Ch4 magnitudes using observed data for ≥T5 dwarfs in the UltracoolSheet catalog (W. M. J. Best et al. 2024, orange points in (a) and (b) panels) and from B. M. Patten et al. (2006, brown points), as well as synthetic values for objects with NIRSpec PRISM spectra in S. A. Beiler et al. (2024, purple points). The positions of W1935 and W2220 considering synthetic values derived using the retrieved spectra in J. K. Faherty et al. (2024) are indicated with a red star (from model with inversion) and a blue star (from model without inversion) for W1935 and a green star for W2220. Labeled objects in (a) and (b) panels indicate the targets in the GO Cycle 1 2124 program.
Paper: Diversity of Cold Worlds: Predicted Near-to-mid-infrared Spectral Signatures of a Cold Brown Dwarf with Potential Auroral Heating
Authors: Genaro Suárez, Jacqueline K. Faherty, Ben Burningham, Caroline V. Morley, Johanna M. Vos, Brianna Lacy, Melanie J. Rowland, Adam C. Schneider, Sherelyn Alejandro Merchan, Daniella C. Bardalez Gagliuffi, Thomas P. Bickle, Eileen C. Gonzales, Rocio Kiman, Austin Rothermich, Niall Whiteford
Figure caption: Best retrieved spectra for W1935 with (top panel) and without (bottom panel) thermal inversion. The color axis in each panel shows the corresponding contribution function, which indicates the pressure contributing the most to the fluxes emerging at different wavelengths. The maximum pressure probed by both retrieved spectra is similar (≈60 bar). However, due to the thermal inversion, the minimum pressure probed by the retrieved spectrum with inversion (≈0.002 bar) is much lower that the one from the model without inversion (≈0.1 bar, with a few wavelength points reaching as low as 0.03 bar). The W1935 2.9–5.1 μm G395H spectrum probed pressures ≈0.002–10 bar. The main spectral features are indicated, including the principal methane emission regions.
Paper: Diversity of Cold Worlds: Predicted Near-to-mid-infrared Spectral Signatures of a Cold Brown Dwarf with Potential Auroral Heating
Authors: Genaro Suárez, Jacqueline K. Faherty, Ben Burningham, Caroline V. Morley, Johanna M. Vos, Brianna Lacy, Melanie J. Rowland, Adam C. Schneider, Sherelyn Alejandro Merchan, Daniella C. Bardalez Gagliuffi, Thomas P. Bickle, Eileen C. Gonzales, Rocio Kiman, Austin Rothermich, Niall Whiteford
Figure caption: Retrieved spectra for W1935 (with and without thermal inversion in black and brown, respectively) and W2220 (orange curve; no temperature inversion). The NIRSpec G395H spectra for W1935 and W2220 are shown in green and blue, respectively, with a light color for the original resolution (R ∼ 2700) spectra and a darker color for convolved (R ∼ 100) spectra. To facilitate comparison between the two objects, we plotted absolute fluxes, accounting for their respective distances (14.43 ± 0.79 pc and 10.47 ± 0.23 pc for W1935 and W2220, respectively; J. D. Kirkpatrick et al. 2021).
Paper: Diversity of Cold Worlds: Predicted Near-to-mid-infrared Spectral Signatures of a Cold Brown Dwarf with Potential Auroral Heating
Authors: Genaro Suárez, Jacqueline K. Faherty, Ben Burningham, Caroline V. Morley, Johanna M. Vos, Brianna Lacy, Melanie J. Rowland, Adam C. Schneider, Sherelyn Alejandro Merchan, Daniella C. Bardalez Gagliuffi, Thomas P. Bickle, Eileen C. Gonzales, Rocio Kiman, Austin Rothermich, Niall Whiteford
Figure caption: Best self-consistent atmospheric model fits to the W1935 G395H spectrum. Details are the same as Figure 1 but including the best fitting-models (dashed orange line) from Sonora Elf Owl (top panel), LB23, and ATMO 2020 (bottom panel).
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: Eccentricity (ϵ) and semimajor axis (a) distributions for 3BBF from the scattering experiments described in Appendix A.1. Note that we normalize a by R1, the radius of the interaction volume—the largest spherical volume containing all three bodies during the encounter, if those bodies were to follow straight-line trajectories. The solid lines are the raw results of the scattering experiments, while the dashed lines show the distributions as approximated by Equation (A7). Top: Eccentricity distribution for several x = a/R1 bins. As found by Y. B. Ginat & H. B. Perets (2024) and D. Atallah et al. (2024), binaries with a > R1 have ϵ distributions that become increasingly superthermal with increasing a, but are thermal when a < R1. The ϵ distribution is actually subthermal for x ∈ [10−0.75, 100.0], but this is not resolved above. Bottom: Normalized semimajor axis distribution. As predicted by D. C. Heggie (1975) and J. Goodman & P. Hut (1993), f(x) ∝ x5/2 when a ≪ R1, though the latter quoted the distribution cumulatively as C(x) ∝ x7/2.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: The results of the field distortion tests for different bands (g/r/i/z/y) and shear components (g1, g2). In each panel, the blue data points (with small error bars) represent the stacked shear signals from galaxies binned according to their field distortion shear values (﹩{g}_{1}^{f}﹩ and ﹩{g}_{2}^{f}﹩). The red lines show the best-fit results. The values of the multiplicative and additive biases are given at the bottom of each panel.
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: Assumed semi-analytic relations between cluster properties—initial mass Mcl0, half-mass radius rh, and density ρh within the half-mass radius, and age ﹩\tilde{\tau }﹩ normalized by cluster lifespan—according to our compilation of the UEE from M. Gieles et al. (2011); see Equations (A12). In the left column, the solid curves show the rh–Mcl0 relation (top) and ρh–Mcl0 relation (bottom) at several cluster ages indicated by color. The time evolution of rh, ρh, and Mcl for several specific choices of initial cluster mass Mcl0 are indicated by the dashed curves in both the left and right columns. The early truncation of the dashed yellow and light blue curves prior to ﹩\tilde{\tau }=1﹩ (cluster dissolution) reflect our choice to halt cluster evolution once there are fewer than 10 bodies, below which these semi-analytic approximations break down. All clusters shown are assumed to evolve on a circular orbit about the Milky Way center at an equivalent Galactocentric radius to the Sun (RG = 8 kpc).
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: PSF residuals as a function of position on the focal plane. The panels from left to right are respectively e1, e2, and relative area residuals. These figures are calculated using the i-band data. Other bands have similar properties.
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: The probability a binary will experience no strong encounter for the rest of a cluster’s life (Equation (A16)) vs. the radial location in the cluster at the time the binary was born. The probability curves are organized such that columns correspond to initial cluster mass, Mcl0, and rows correspond to the time since the cluster was born, ﹩\tilde{\tau }﹩, in units of the total cluster lifetime. Binaries assembled with smaller SMA, later in a cluster’s life, or in lower-mass clusters all have an elevated survival probability.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: The field distortion shear distribution recovered by astrometric calibration. Black boxes represent the CCD arrangement. The upper panels show the distributions of the two shear components of FD: ﹩{g}_{1}^{f}﹩ and ﹩{g}_{2}^{f}﹩. The lower panel shows the total shear amplitude, ﹩| {g}^{f}| =\sqrt{{({g}_{1}^{f})}^{2}+{({g}_{2}^{f})}^{2}}﹩. Green lines in each panel represent the position where gf = 0.02. This circle defines our preferred boundary of the high-quality shear catalog.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: Results of the focal plane null test for the i-band shear catalog. The left and right panels are for g1 and g2 respectively. The results of the other bands have similar properties.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: Examples of bad channels on CCD. This figure shows the images with chip IDs 0, 33, 43, and 94.