adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: The four morphological parameters, C, A, G, and M 20, vary with λ rf in the three redshift bins, shown in red, green, and blue. The lines and dots represent the mean value of all galaxies in each bin. The shaded areas indicate their 32% and 68% (1σ) quantiles. The thick solid lines represent the values that have been matched to the F444W PSF. The thin dashed lines represent the values that have been matched to the F200W PSF, while the thin solid lines represent values without any PSF matching. The arrows at the LW ends are the rough corrections of the underestimated A in F444W.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: Left panel: the relationship between the mass and orbital inclination of the third body. Middle panel: the relationship between the orbital semimajor axis and the orbital inclination of the third body. Right panel: the relationship between the percentage of the third light contributions in the wavelength range of SDSS spectrum and the orbital inclination of the third body. The star symbols represent the mass, orbital semimajor axis, and orbital inclination of the third body when the third light contribution is consistent with the result of the SDSS spectrum. The triangle symbol represents these values when the third body is coplanar with the central binary.
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: Distribution of the M F444W and M * of our galaxies with redshift. The blue dots represent sources with high 〈S/N〉s and valid morphological parameters (2068). The gray dots represent other sources removed due to not meeting the conditions above (826). The horizontal dashed black line represents our cut of M *. The three colored rectangular regions divided by vertical dashed black lines represent our three redshift bins, in which the numbers represent the number of galaxies.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: The RV curves of NY Boo. Circles and triangles represent components with velocities V1 and V2, respectively. The filled symbols represent data from LAMOST spectra and open symbols represent data from SDSS spectra.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: The relationship between τ th/τ P and temperature T1. The star symbol represents NY Boo.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: W-D theoretical light curves and geometric configurations for seven different stages (TJD = BJD-2,457,000; TJD 1739–1741, TJD 1746–1749, TJD 1761–1763, TJD 1928–1931, TJD 2637–2640, TJD 2665–2667, and TJD 2689–2691). The red area is the location where the dark spot is located.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: The CCF profiles of SDSS infrared spectra. The red part represents the third component, which is considered to be caused by additional body.
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: The four morphological parameters, C, A, G, and M 20, evolve with redshift at four matched λ rf for the two stellar mass bins, 9 < log M * < 10 and log M * ≥ 10, shown in blue and red, respectively. The lines and dots represent the mean value in each bin. The shaded areas indicate their 32% and 68% (1σ) quantiles. The first column represents the values that have been matched to the F200W PSF, and the other columns represent the values that have been matched to the F444W PSF. The arrows at the longest-wavelength diagrams are the rough corrections of the underestimated A in F444W.
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: Movements of the mean value of galaxy morphological parameters on the G–M 20 diagram with the increase of λ rf. Different colors represent different redshift bins, and black dots represent the overall sample.
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: Comparison of the results of five main morphological parameters between statmorph_csst and the original statmorph. The σ at the upper left is the standard deviation.
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: Systematic error (mean of Δ) of C, A, G, and M 20 of the F115W images of galaxies in the low-redshift bin. The error bars are the random error (standard deviation of Δ). Detailed data are given in Table 3.
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: Distribution of the optimized multipliers, which is the ratio of the time consumed by the original version (statmorph) to the time consumed by the optimized version (statmorph_csst).
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: Same as Figure 2, but the cutoff of 〈S/N〉 increases to 5.
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: H/He line ratios involving O, Ne, Mg, and Si, as indicated, against source effective temperature. The left-hand side shows all stars in our sample and the right-hand side shows only the normal stars. The upper panel displays ratios with flux measurement uncertainties. The lower panel displays linear regressions to the respective ratio data sets. The different lengths of line fits indicate the domain of temperature for which there are data. Line fluxes were corrected for the nominal interstellar absorption values given in Table 2.
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: Error-weighted mean line centroid offsets vs. line wavelength (top panel, (A)), and error-weighted-mean line widths vs line wavelength (bottom panel, (B)). Classes of objects were defined from the velocity-offset histogram group (see Figure 2) and are denoted as squares (gray) for zero offset, circles (orange) for intermediate offset and triangles (blue) for large negative offsets.
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: For each star with good measurements of the line width, we show their error-weighted-mean FWHM over Ne X 12 Å, Fe XVII 15, and 17 Å. Colors are as in Figure 3. The dashed-diagonal line is the 1: 1 dependence.
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: The correlation of centroid offset vs. line width for the groupings defined by centroid offset vs. wavelength shown in Figures 2 and 3 for lines in the 7.1–15.3 Å range. Symbols and colors are as in Figure 3.
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: The H- to He-like photon flux ratios (y-axis) for several elements as labeled, for power-law emission measure distributions vs. the high-temperature cutoff (x-axis) for three values of the exponent on temperature, β (solid lines: 2.5, dashed: 2.0, and dotted: 1.5, with larger values meaning steeper, or relatively less high-temperature plasma).
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: The luminosity density for stars from each of the three velocity-offset selected groups, plus the very different γ Cas. Colors are as in Figure 3; γ Cas is shown in gray. Spectra have been corrected for absorption using the nominal interstellar values from Table 2.
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: The frequency histogram of line centroid velocity offsets. Two distinct groups are present, centered near 0 and −400 km s−1, with a long tail to large negative velocities.
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: The black histogram shows the flux spectrum for ζ Oph. The light-colored curve overlaying it (cyan) is a plasma model including line plus continuum emission. Below that (red) is the continuum contribution only, which is used as the baseline for Gaussian line fitting.
Paper: Survey of X-Rays from Massive Stars Observed at High Spectral Resolution with Chandra
Authors: Pragati Pradhan, David P. Huenemoerder, Richard Ignace, Joy S. Nichols, A. M. T. Pollock
Figure caption: The Fe XVII 15 Å velocity profile for stars from each of the three velocity-offset selected groups. Colors are as in Figure 3.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: We rank order the galaxy properties for Astrid, such that the variables contributing the most to the model accuracy are on the right, while the features contributing the least are on the left (see the text for details of the procedure used). The vertical bars indicate the accuracy (in terms of RMSE) achieved by the considered variables, cumulatively from left to right, and the black numbers on top of them show the loss in accuracy with respect to a model trained using all variables. For instance, a model that only uses M * achieves an RMSE of ∼0.1 and performs 176.3% worse than the model trained on all 14 properties (with an RMSE of ∼0.04). We emphasize that this ordering was derived when training gradient boosting tree models to perform regression to the value of Ωm.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: We have trained a neural network to perform likelihood-free inference on the values of the cosmological (Ωm and σ 8) and astrophysical (﹩{A}_{\mathrm{SN}1}﹩, ﹩{A}_{\mathrm{SN}2}﹩, A AGN1, and A AGN2) parameters using as input 14 properties of individual galaxies from the Astrid simulations at z = 0. Once the network is trained, we test it using individual galaxies from the test set. The different panels show the posterior means (points) and standard deviations (error bars) predicted by the network versus the true values. Every point with its error bar represents a single galaxy chosen randomly from each simulation of the test set. We find that our model is able to infer the value of Ωm from the properties of individual galaxies with a ∼10% precision.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: Robustness test. We test models trained on individual galaxies from IllustrisTNG (left column), SIMBA (middle column), and Astrid (right column) on galaxies from the IllustrisTNG (first row), SIMBA (second row), Astrid (third row), and Magneticum (fourth row) suites. Each point represents the average result of all the galaxies in that simulation (see Equation (9)). We find that none of the models are robust. On the other hand, the model trained on the Astrid galaxies performs relatively well when tested on the IllustrisTNG and SIMBA galaxies.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: We have trained three different models using IllustrisTNG (top), SIMBA (middle), and Astrid (bottom) galaxies at z = 0. We test each model on galaxies from the IllustrisTNG, SIMBA, Astrid, and Magneticum simulations. For each galaxy i, we compute ﹩{\chi }_{i}^{2}={({\theta }_{i}-{\mu }_{i})}^{2}/{\sigma }_{i}^{2}﹩. The different lines show the distribution of χ 2 in the different setups. As can be seen, the χ 2 distribution changes if the simulation is tested on galaxies from a different code than the one used for training. On the other hand, most of the galaxies have low χ 2 values. The numbers in the subpanels indicate the fractions of galaxies with values of χ 2 smaller than the indicated threshold.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: Redshift dependence: we have trained neural networks to infer the value of Ωm using the properties of individual galaxies at different redshifts, for galaxies of the Astrid simulations. For each galaxy of each simulation of the test set, we compute the posterior mean and standard deviation for Ωm. Next, we compute the means of those two numbers (Equation (9)) and plot them in the figure for the 50 different simulations in the test set. We show the results at redshifts 1, 2, and 3. As can be seen, our networks can infer the value of Ωm from individual galaxies at redshifts higher than z = 0 with an accuracy similar to the one achieved by the models at z = 0.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: The same as Figure 4, but removing all galaxies whose individual χ 2 values are higher than 7. As can be seen, the models trained on the Astrid and IllustrisTNG galaxies are very robust (with the exception of the Magneticum galaxies with Ωm ≳ 0.3), while the model trained on the SIMBA galaxies is not.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: We have tested the model trained on Astrid galaxies on Magneticum galaxies after removing galaxies with ﹩{\chi }_{i}^{2}\geqslant 3﹩ (left), ﹩{\chi }_{i}^{2}\geqslant 5﹩ (middle), and ﹩{\chi }_{i}^{2}\geqslant 7﹩ (right). As expected, the more aggressive we are in removing outliers, the better the model works.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Left panel: the averages of the frequency shifts for 2017 December 22 for windows w0–w8 relative to w4 for the six scans in Figure 5. Right panel: the corresponding frequency shifts for 2018 February 26 averaged over all scans, the two polarizations, and the two telescopes. Uncertainties are standard errors.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Comparison of ART and GBT time-averaged LCP spectra for leading (S 0) and trailing (S 8) windows, each with the spectrum for the off-pulse subtracted. Upper panels show spectra before correction and lower panels after correction. The spectra correspond to scan 1 of 1160 s duration on 2017 December 22. The spectra were normalized so that the frequency-averaged power spectral density ﹩\bar{S}=1﹩.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Frequency shifts of dynamic spectra in w0–w8 relative to spectrum in w4. Panels (a)–(g) present results for the six scans obtained in LCP at ART (blue lines) and GBT (green lines) on 2017 December 22. For scan 6 the GBT data were not usable and are omitted. Each scan is 840 pulse periods long. Dashed lines correspond to original, uncorrected frequency shifts. Solid lines correspond to remaining relatively small frequency shifts after correction for distortion discussed in Section 4.1. Uncertainties are 1σ statistical standard errors determined from the fit of Equation (4).
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Maximum frequency difference observed in ART LCP dynamic spectra in w8 relative to w0 as a function of decorrelation bandwidth, Δf 1/e , taken from Table 2. The shift is to lower frequencies for the dynamic spectra from the leading part of the pulse profile in w8 to the trailing part in w0. The data from 2018 February 26 are shown in the lower left corner.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Examples of frequency sections of the two-dimensional CCF(Δf, Δt) functions for Δt = 0 of dynamic spectra as a function of frequency lag, Δf. Panels (a) and (b) correspond to ART and GBT, respectively. The CCFs are computed for two pairs of dynamic spectra, one corresponding to the leading and the middle window (w0–w4, solid curves) and the other to the trailing and the middle window (w8–w4, dashed curves). The CCFs were normalized to have equal values at zero lag. LCP data were used from scan 1 at epoch 2017 December 22.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Average profile of PSR B1237+25 for the original data obtained at ART for scan 1 on 2017 December 22 (copied from Figure 1) and the profile after correction. Note the intensity dips on both sides of the profile have disappeared.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Top panel: average profile of PSR B1133+16 at LCP obtained at ART for scan 1 on 2018 December 17. Bottom panel: phase rates as the derivatives of the ART-GBT VLBI visibility phases with respect to delay as a function of pulse longitude for the same observing scan. Plots are based on original, uncorrected data. For more information, compare with Figure 1.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Bandpasses for ART and GBT from average spectra of off-pulse longitude windows, w9–w 11, from scan 1 on 2017 December 22.
Paper: Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. II. Toward a Self-consistent Model
Authors: Antranik A. Sefilian, Roman R. Rafikov, Mark C. Wyatt
Figure caption: The evolution of the planetary eccentricity e  p  (panel A) and longitude of pericenter ϖ  p  (panel B) in the nominal N-ring simulation of the fiducial planet–disk model, i.e., Model A, as an example of the general behavior observed in all other planet–disk systems simulated (Table B1). Results obtained within the simplified, “Paper I–like” N-ring simulation of the same planet–disk system are shown in red dashed lines in each panel. One can see that in the nominal simulation, the planetary eccentricity does not remain constant at its initial value of e  p (0) = 0.05 (as in Paper I), but rather decays exponentially with time, accompanied by small-amplitude oscillations; see the inset in panel (A). The dashed yellow line in panel (A) shows a numerical fit using an exponential model ﹩{e}_{p}(t)={e}_{p}(0)\,\exp (-{Dt}/2)﹩ (see also Equation (23)), with e  p (0) = 0.05 and D ≈ 7.7 × 10−3Myr−1. Looking at panel (B), it is also evident that the planet precesses at a slower rate in the nominal simulation compared to the simplified one: indeed, ﹩{\tau }_{\sec }=2\pi /{\dot{\varpi }}_{p}\approx 57\,\mathrm{Myr}﹩ in the nominal simulation, while ﹩{\tau }_{\sec }\approx 33\,\mathrm{Myr}﹩ in the simplified one. See the text (Section 4.1.1) for more details.