adsabs/AstroCLIMB huggingface dataset:
Paper: An Ultrafast Image Simulation Technique with Spatially Variable Point-spread Functions
Authors: Zeyu Bai, Peng Jia, Jiameng Lv, Xiang Zhang, Wennan Xiang, Lin Nie
Figure caption: Comparison of simulated and actual celestial object characteristics. Panel (a) shows the histogram of the ellipticity differences between simulated images and actual celestial object images. This plot demonstrates that the simulated images have an ellipticity distribution similar to the actual images, though some differences exist due to the telescope's wide field of view and white light mode. Panels (b) and (c) display the FWHM distribution along the row and column directions, respectively, comparing simulated data (in light orange) with sample data (in light blue). The x-axis represents the FWHM, while the y-axis represents the percentage. These histograms highlight the differences in the peak positions and spread between the simulated and actual data. These results indicate that the simulation method produces images with characteristics close to real observations.
Paper: An Ultrafast Image Simulation Technique with Spatially Variable Point-spread Functions
Authors: Zeyu Bai, Peng Jia, Jiameng Lv, Xiang Zhang, Wennan Xiang, Lin Nie
Figure caption: The method proposed in this study is delineated in this figure, which illustrates a two-stage procedure for image simulation. The first stage involves coefficient matrix generation, wherein PSF basis is derived from empirical PSF data. The second stage encompasses the convolution and addition step, where the previously obtained PSF basis is convolved with the original image to generate image basis. These image basis is weighted by the coefficients in each pixel and added together to produce the final blurred image.
Paper: An Ultrafast Image Simulation Technique with Spatially Variable Point-spread Functions
Authors: Zeyu Bai, Peng Jia, Jiameng Lv, Xiang Zhang, Wennan Xiang, Lin Nie
Figure caption: This figure shows the distribution of 1458 sampling points from astronomical images, where duplicate coordinates have been removed and the remaining points were randomly selected. The X-axis and Y-axis represent the image's horizontal and vertical coordinates, respectively. The blue dots represent the positions of the sampled points.
Paper: An Ultrafast Image Simulation Technique with Spatially Variable Point-spread Functions
Authors: Zeyu Bai, Peng Jia, Jiameng Lv, Xiang Zhang, Wennan Xiang, Lin Nie
Figure caption: Spatial comparison of mean squared error (MSE) and ellipticity component differences between simulated and true data. Panel (a) presents the MSE distribution across a two-dimensional grid, highlighting error variations across different areas. Panel (b) shows the spatial differences in ellipticity components e1 (left) and e2 (right), with both subplots using a unified color scale to represent the magnitude of these differences. The left subplot displays the distribution of differences in the e1 component, while the right subplot displays the distribution of differences in the e2 component. Together, these visualizations provide insights into the spatial accuracy and ellipticity consistency of the simulation compared to actual data.
Paper: An Ultrafast Image Simulation Technique with Spatially Variable Point-spread Functions
Authors: Zeyu Bai, Peng Jia, Jiameng Lv, Xiang Zhang, Wennan Xiang, Lin Nie
Figure caption: Comparison of two key metrics between simulated and true PSFs. Panel (a) displays the distribution of ellipticity differences, with the x-axis representing the ellipticity difference and the y-axis indicating the percentage of occurrence for each value. A red dashed line marks the 90% cutoff point at approximately 0.0901, identifying the range where most ellipticity differences are concentrated. Panel (b) illustrates the distribution of mean absolute error (MAE) values across 2916 positions, with the x-axis showing the MAE values and the y-axis representing the percentage of occurrence for each value. Together, these plots provide insights into the variation and concentration of differences between simulated and true PSFs.
Paper: An Ultrafast Image Simulation Technique with Spatially Variable Point-spread Functions
Authors: Zeyu Bai, Peng Jia, Jiameng Lv, Xiang Zhang, Wennan Xiang, Lin Nie
Figure caption: The original and blurred image obtained by our method. We can find that there are no boundaries in the blurred image, which could often be seen in images generated by other methods.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: Each set of three vertical panels shows 0.9 m V-band rotation results for a single component in a twin system. The top panel is a relative light curve in the same general format as Figure 5, the middle panel is a Lomb–Scargle Periodogram of the same data, and the bottom panel is a phase-folded light curve of the same data based on the measured period. The Julian time of 2455197.5 corresponds to the 2010.0 epoch, a convenient reference time preceding all new observations in this paper. Note the different vertical scales between light curves. The periodogram shows horizontal green lines at the 10% (dotted)/1% (dashed)/0.1% (solid) Baluev false-alarm probability (FAP) values, the selected maximum power period peak with a vertical solid red line, vertical dashed orange lines at the 2/3/4 harmonic multiples, and vertical solid purple lines at the integer n = [ −3,…, 3] 1 day−1 sampling aliases. Phase-folding begins at the epoch of the first point, with a red sine wave corresponding to the selected Lomb–Scargle model result. Values in red are given for the rotation period, FAP, and peak-to-peak amplitude (Δ) in mmag. The number of filled data points (N) and the observation filter (V for all of these stars) are given in the top left of the phase-folded subplot—open points correspond to incomplete visits that only obtained one frame. The un-phased light-curve data are available as Data behind the Figure (DbF) products.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption:                         Blended light curves for the NLTT 44989 AB system. (Left)—TESS 2 minutes cadence PDCSAP pipeline data from sector 39, shown in the same general format as Figures 6 and 7. The ∼6.55 day rotation period from the B component is plainly evident, while the A component’s longer signal is absent due to the default TESS pipeline processing. (Right)—Alternative TESS-unpopular light curves from sectors 12 (top) and 39 (bottom), with the MADs given in the top left and numbers of data points (N) in the bottom left. The shorter periodic rotation pattern of ∼6.55 days from the B component is weakly visible intermixed with the more obvious long-term rotation signal of the A component. Red curves overlay the 38.27 days Lomb–Scargle sine wave result from the 0.9 m data (Figure 6) but extended in time to compare the phase alignment with the signal in each TESS-unpopular sector; the small shift in phase in sector 39 is likely explained by a small offset between the adopted and true period, or possibly differential rotation. See Section 4.2 for further discussion.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: CHIRON spectra of the Hα line region—shifted to zero RV and blaze corrected—stacked for multiple epochs to visually compare the A and B components in each system. We only include nonflaring epochs with both stars successfully observed back-to-back; the legends indicate the final number of epochs shown and the time span of those spectra. Work by E. K. Pass et al. (2024) indicates the emission seen in the blended spectra for KX Com BC is primarily from the B star while C is flat (see Section 6.2).
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: One-to-one equivalency plots comparing (a) L X and (b) VEM between components in each of the four systems for each observation ID. The cases with three exposures from Chandra—KX Com A-BC and GJ 1183 AB—have results from their individual epochs numbered after the associated system letter label following the designations in Table 3. Gray diagonal one-to-one lines are shown along with leftward arrows for the upper limits on NLTT 44989 A. Open symbols indicate the non-twin triple KX Com A-BC. In panel (a), the pink shaded region shows a factor of 4 both above and below the one-to-one line (see Section 4.4 for discussion). In panel (b), a green point indicates the hotter component in the 2T model result for 2MA 0201+0117 B.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: Radial velocity time series from CHIRON for four resolved targets. The weighted average RV value for each case is shown with a black dashed line and given in black in the top left (except KX Com BC listing the MAD instead), with the average single-point uncertainty spanning above and below in gray and given in the top right. Error bars are always shown, but appear smaller than the points for KX Com BC owing to the different scale. (Top)—NLTT 44989 A and B show all 15 epochs across roughly 1.5 yr, with neither star showing RV variations beyond the noise. (Bottom)—KX Com A also appears nonvarying within the noise for the eight available epochs. In contrast, KX Com “B” shows the only case we find with RV variations, which we ascribe to orbital motion with an unresolved third component “C.” We only show 23 of the 30 total epochs available for KX Com BC so as to highlight the orbital arc captured from our sequential visits throughout 2023 April.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption:                         Format details are largely the same as for Figure 6, now showing example results using archival data from ZTF (top left and top right), ASAS-SN (bottom left), and TESS-unpopular (bottom right). The phased light curves show data folded every two phases in time instead of one phase for visual clarity. TESS is also space-based without 1 day sampling, so does not show the corresponding alias lines. ZTF spatially resolves 2MA 0201+0117 A and B, while the other two examples have the A-B(C) components blended.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: An example speckle detection limit curve from the 880 nm channel of QWSSI on LDT for 2MA 0201+0117 A is shown. No new unresolved companions were found for this star, to limiting magnitude differences (Δm) of 1.82 mag at 0.″1, 3.08 mag at 0.″2, and 4 mag or more beyond ∼0.″3. A 0.″1 separation corresponds to 4.93 au at the stellar distance of 49.3 pc.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: A one-to-one equivalency plot comparing Hα EWs between components in each system. Individual epochal measurements are black circles while the means of these are red squares. Open symbols indicate the non-twin triple KX Com A-BC. Absorption and emission regions are indicated with blue lines and labels. We only include nonflaring epochs with both stars successfully observed back-to-back.
Paper: Disequilibrium Chemistry, Diabatic Thermal Structure, and Clouds in the Atmosphere of COCONUTS-2b
Authors: Zhoujian Zhang, 周健 张, Sagnick Mukherjee, Michael C. Liu, Jonathan J. Fortney, Emily Mader, William M. J. Best, Trent J. Dupuy, Sandy K. Leggett, Theodora Karalidi, Michael R. Line, Mark S. Marley, Caroline V. Morley, Mark W. Phillips, Robert J. Siverd, Joseph A. Zalesky
Figure caption: Forward-modeling analysis results with the Y-band Gemini/F2 spectrum fully masked. The format is the same as Figure 4.
Paper: Disequilibrium Chemistry, Diabatic Thermal Structure, and Clouds in the Atmosphere of COCONUTS-2b
Authors: Zhoujian Zhang, 周健 张, Sagnick Mukherjee, Michael C. Liu, Jonathan J. Fortney, Emily Mader, William M. J. Best, Trent J. Dupuy, Sandy K. Leggett, Theodora Karalidi, Michael R. Line, Mark S. Marley, Caroline V. Morley, Mark W. Phillips, Robert J. Siverd, Joseph A. Zalesky
Figure caption: Forward-modeling analysis results with the W3 photometry included. The format is the same as Figure 4.
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Evolution of the main orbital parameters of the 200 realizations of Eris in barycentric coordinates; see text for details. In the top three panels, we present the evolution of a/a 0, e, and i, respectively; in the fourth panel, we present q in blue and Q in red. The green component highlights a single realization.
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Due to the rapid oscillations of e and i, we zoom in to three selected shorter time intervals within Figure 6; see text for details.
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Similar to Figure 2 but for Pluto’s angular elements and the Kozai constant, as well as the resonant argument of the 3:2 MMR, ϕ 3:2, presented in the first row of panels. Due to the rapid oscillations and circulations of these variables, we only show the three time intervals presented in Figure 7 for better comparison.
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Same as Figure 1, but for the evolution of the orbital parameters of Pluto. The dashed yellow line in the top panel represents the nominal location of the 3:2 MMR.
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Evolution of the angular elements of the 200 realizations of Eris in barycentric coordinates; see text for details. In the top three panels, we present the evolution of ω, Ω, and ϖ, respectively; in the fourth panel, we present the evolution of ﹩H=\sqrt{1-{e}^{2}}\cos (i)﹩, i.e., the Kozai constant. As in Figure 1, the green component highlights a single realization.
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Eris’s orbital density, represented by a heat map based on the 200 realizations shown in Figure 1. The white star indicates the initial condition. The color scale shows the number of points that falls into each bin across all simulations. All the regular orbits populate the dark area; the orange area contains seven nonregular orbits; and two unstable realizations populate the yellow cloud at low q. The vertical blue lines are the location of Neptune’s perihelion (solid) and the distance of three Hill radii away from Neptune’s perihelion (dashed).
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Same as Figure 1, but for the evolution of the orbital parameters of 2015 KH162.
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Same as Figure 3 but for Pluto's orbital density.
Paper: Long-term Dynamical Stability in the Outer Solar System. II. Detailed Secular Evolution of Four Large Regular and Resonant Trans-Neptunian Objects
Authors: Marco A. Muñoz-Gutiérrez, Antonio Peimbert, Angeles Pérez-Villegas
Figure caption: Same as Figure 3 but for the orbital density of 2015 KH162.
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: Sensitivity map for our injection-recovery tests on the HD 119130 RV data using RVSearch. Points represent individual P and K combinations that were injected into the RV residuals. Blue points correspond to signals that were successfully recovered after removing the orbit of HD 119130 b and the candidate signal at P ≈ 200 days, while red points correspond to signals that were not recovered. Signals were considered “recovered” if their corresponding peak in a periodogram of the residuals rose above the 0.1% FAP threshold, as determined following the methods of A. W. Howard & B. J. Fulton (2016). The results of the individual injections and recovery searches were used to compute the contours, which correspond to detection probability (see color bar). The solid black line corresponds to a detection efficiency of 50%. The white star represents HD 119130 b, and the gray circle represents the outer candidate, signal c.
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: For the different scenarios listed in Table 4, we show the distributions of the known planet’s recovered RV semiamplitude, K fit, relative to the baseline value, K baseline, in units of the uncertainty on the baseline value, ﹩{\sigma }_{{K}_{\mathrm{baseline}}}﹩. The distributions have been smoothed using a Gaussian kernel with a bandwidth of 0.25 ﹩{\sigma }_{{K}_{\mathrm{baseline}}}﹩. Blue and purple lines correspond to known planets with P = 3 days and P = 31 days, respectively. For each orbital period, the lines for the cases of M p = 2 and 20 M ⊕ generally fall on top of one another, save for the scenario with added red noise.
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as Figure 10, but now the realization of a GP has been added to the synthetic RV time series to mimic correlated noise due to stellar activity. Results for the P = 31 days and M p = 2 M ⊕ scenario are not shown due to numerical errors during the RV fitting routine.
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: The HD 119130 RVs. Top: the RV time series (data points with error bars), MAP model (solid black line), and residuals about the MAP solution (lower panel). Note the broken x-axis. Middle: the RVs folded to the orbital period of HD 119130 b. RVs binned in units of 0.125 orbital phase are shown as the blue data points. Black lines represent 25 random realizations of the model posterior. Error bars shown represent point-wise measurement errors added in quadrature with the associated instrument-specific jitter value that was fit to the data. Bottom: the same as above but for signal c.
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: GLS periodograms of the HD 119130 RVs (minus instrumental offsets), RV residuals, and RV window function. The solid (dashed) blue (orange) vertical line corresponds to the period of planet b (signal c). The dotted, dashed, and solid red horizontal lines correspond to the 0.1%, 1%, and 10% FAP thresholds, respectively, for each periodogram, as computed following R. V. Baluev (2008).
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: GLS periodograms of the HARPS activity indices and window function. The HARPS data comprise 31 spectra obtained over a baseline of 98 days. The solid blue vertical line corresponds to the orbital period of planet b. The dotted, dashed, and solid red horizontal lines correspond to the 0.1%, 1%, and 10% FAP thresholds, respectively, for each periodogram, as computed following R. V. Baluev (2008).
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: The HARPS and HARPS-N data (with instrumental offsets applied) compared to 25 random realizations of HD 119130 b’s orbit, generated using the P, T conj, and K values from L19. The new data are inconsistent with the L19 solution.
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as Figure 8 but now σ RV,inst = 0.4 m s−1 (i.e., the “KPF” case for internal RV precision) and σ RV,astro = 1.2 m s−1 (i.e., the “active” case for stellar jitter).