adsabs/AstroCLIMB huggingface dataset:
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Temperature as a function of Si X 1.43 μm/S XI 1.92 μm line ratio and distance from Sun center.
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: The H2O and SiO maser spectra of VX Sgr in SiO v = 1, 2, J = 1–0; v = 1, J = 2–1, J = 3–2 (43.1, 42.8, 86.2, 129.3 GHz); and H2O 61,6–52,3 (22.2 GHz) transitions. The intensity is given in units of antenna temperature ﹩{T}_{A}^{* }﹩ (K), and the abscissa is V LSR (km s−1). The red dotted line represents the stellar velocity of 5.3 km s−1 (Chapman & Cohen 1986).                 1 of 5 images
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: Variations of the H2O 61,6–52,3 maser spectra according to observation epochs. The red dotted line in the middle represents the stellar velocity of 5.3 km s−1. The y-axis is the antenna temperature, and the spectra are arranged according to observational dates (epochs). The observational dates and epochs are marked on the right side of the vertical axis.
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: Optical magnitude variation of VX Sgr from AAVSO. The red dashed lines denote the optical maxima. The blue and red triangles correspond to the single-dish and VLBI observations, respectively. The numbers around the triangles indicate the order of observational epochs in the single-dish and VLBI observations.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Electron densities obtained from a selection of EIS line ratios on the west and east regions. The dashed line indicates the expected radial density profile for the QS, from Del Zanna et al. (2018).
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: Peak and integrated antenna temperature variations of the H2O and SiO masers according to observational dates (Julian dates). The first row is the optical magnitude variation of VX Sgr from the AAVSO. Blue and red triangles correspond to the single-dish and VLBI observations, respectively. The red dashed lines indicate the optical brightness maxima according to the optical phases.
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: The VLBI observations of the H2O maser on 2016 January 26 (ϕ = 1.53). (a) Moment zero map, (b) position–velocity spot map, and (c) recovered spectrum from the velocity-dependent maser spots superposed on the single-dish spectrum on 2016 February 15 (ϕ = 1.56) in Figure 10. The red dotted line in panel (c) represents the stellar velocity (V * = 5.3 km s−1). The strongest features in the −6 to 3 km s−1 velocity range are mostly located in the red dotted square in panels (a) and (b). The color of the spots indicates the local standard of rest velocity in panels (b) and (c), and the size of the spot is a logarithmic scale of the intensity in panel (b). The red asterisk denotes the position of VX Sgr determined by the ring fitting of the SiO masers (Yoon et al. 2018).
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: Velocity and intensity variations of the H2O maser components from (a) to (k) over time. The upper and lower panels represent the peak antenna temperature and velocity difference of each component with respect to the stellar velocity (V * = 5.3 km s−1), respectively. The horizontal red dotted line represents a set of similar peak velocities within our velocity resolution. The lower right panel displays the magnitude variation in AAVSO.
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: The H2O maser spectrum on 2016 February 15 (ϕ = 1.56) obtained with the KVN single-dish telescope. The upper panel indicates the enlarged vertical axis, displaying a weak spectrum. In the lower panel, the short black lines represent the positions of spectra from (a) to (k). The vertical red dotted line indicates the stellar velocity (V * = 5.3 km s−1).
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: Variations of the SiO v = 1, 2, J = 1–0; v = 1, J = 2–1, J = 3–2 (43.1, 42.8, 86.2, 129.3 GHz) maser spectra according to the observational epochs. The red dotted line in the middle represents the stellar velocity of 5.3 km s−1. Other indices are the same as in Figure 3.
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: Blue- and red-edge velocity variations of each maser line with respect to the stellar velocity. As indicated in the upper box, the black circles, red triangles, blue squares, green pentagons, and yellow hexagons indicate the H2O (22.2 GHz) and SiO (43.1, 42.8, 86.2, and 129.3 GHz) masers, respectively. The black dotted line on the horizontal axis represents the stellar velocity, which demarcates the blue- and redshifted spectral boundaries. The x- and y-axes represent the modified Julian date and local standard of rest (LSR) velocity, respectively.
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: Peak antenna temperature ratios of the H2O and SiO masers according to the observational dates. The other indices are the same as those in Figure 5.
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: Peak and mean velocity variations of each maser spectrum according to the observational dates. The reference of the blue dotted line on the abscissa is the stellar velocity V * of VX Sgr (V * = 5.3 km s−1). The other indices are the same as in Figure 5.
Paper: Simultaneous Time-monitoring Observations of H2O and SiO Masers toward the Supergiant VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Haneul Yang, Youngjoo Yun, Jaeheon Kim
Figure caption: The FWZPs according to the observational dates. The other indices are the same as in Figure 5.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: The proper motion distribution of two samples. The blue and green dots refer to stars with different distant slicing. The red dashed circles represent an OC where the members assembled.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: Spatial (l, b), proper motion (﹩{\mu }_{\alpha }^{* }﹩, μ  δ ), magnitude–parallax (G, ϖ), and CMDs (G BP − G RP, G) of the eight separated cluster candidates using HDBSCAN. The colors and symbols represent member stars of different cluster candidates.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: Position and proper-motion distributions of one block sample. The gray dots refer to stars with membership probabilities less than 0.1, while the colored dots are stars with membership probabilities greater than 0.1. The color bar represents the probabilities of the member stars.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: Three examples of target and reference clusters. The left panels present the spatial distributions of the members’ isodensity contours. The middle panels present the proper motion distribution of the members’ isodensity contours. The right panels present the G-parallax distribution with parallax histograms on the right edge.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: Example of the results of our searching procedure for two clusters. For each cluster, the three scatter plots (from left to right) represent the Galactic coordinate distribution, proper motion distribution, and CMD. The blue dots refer to the members identified in this work. The orange, green, pink, and red circles represent the members of CWNU_375 and CWNU_510 from He22a, UPK_101 from Sim19, and NGC_7058 from CG20, respectively. CWNU_375 and UPK_101 have four common members and CWNU_510 and UPK_101 have three common members in previous results.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: An example of binary cluster in our samples, OCSN_98 in blue and OCSN_100 in orange. Left panel: the spatial distributions of the two OCs, and the black arrows refer to their projected moving direction. Middle panel: histograms of the RVs of their members. Right panel: absolute CMDs for the two OCs, and the black line refers to an isochrone with a solar metallicity of Z ⊙ = 0.0152 (Caffau et al. 2009, 2011) and a logarithm of age of log t = 6.85.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: Comparison of the mean OC RVs between Gaia DR3 and APOGEE/LAMOST-MRS. The error bars of the blue points/triangles are the 1σ of the Gaussian fitting or standard deviations for OC RVs. The black dashed lines are 1:1 scale lines. The red dashed lines are the mean values of the differences between Gaia DR3 RVs and APOGEE RVs or LAMOST-MRS RVs, and the gray-filled regions are the corresponding 1σ regions.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: A comparison of the distributions of member numbers, r h, and age parameters between the reported clusters from ref_OCs and the OCs obtained in this work. The blue dots refer to the OCs with “OC_flag” = 3 and the orange circles refer to the OCs with “OC_flag” = 2. The black dashed lines both show the relation of y = x.
Paper: Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc
Authors: Songmei Qin, 松梅 秦, Jing Zhong, 靖 钟, Tong Tang, 通 唐, Li Chen, 力 陈
Figure caption: Distribution of the OC population in Galactic coordinates. The black points represent the reported OCs found in this study, and the red squares represent the OCs newly identified in this work using Gaia DR3. The blue circles refer to the r h values given in this work.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Flowchart of the hybrid identification approach. The process of this approach consists of three stages. Stage 1 deals with rough FoF clustering within Gaia EDR3. Then, each OC’s membership is identified in stage 2. After refining the star member, we implement recognition of OCs, including a submodule of modeling for identifying OCs, isochrone fitting, and visual inspection in stage 3.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Preliminary data check for our 801 OCs. ID 3093, 3066, 3096, and 3595 are listed, respectively. Leftmost plots: position of the OC in (α, δ). Inner left plots: (ϖ , ﹩{\mu }_{{a}^{* }}﹩ ) distribution. Inner right plots: (﹩{\mu }_{{a}^{* }}﹩, μ  δ  ) distribution. Rightmost plots: CMD of the OC. The data for all 801 OCs are available in machine-readable format.(The data used to create this figure are available.)
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Distributions of the matched and new OCs in the Galactic X−Y plane in relation to the spiral arms. The image is viewed from the north pole of the Galaxy, around which it rotates clockwise. We adopted the Reid et al. (2019) recommended values of R ⊙ = 8.15 kpc and Z ⊙ = 5.5 pc. The red point represents the position of the Sun.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: The CMDs of members identified for the cluster OC0033 compared with Hao22 and the FoF method.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: The CMDs of members identified for the cluster UBC1029 compared with CG22.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Same as Figure 4, but with an edge-on view.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: The CMDs of members identified for the cluster M67 compared with CG20.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Histograms of Z and age for the 46 OCs.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: The confusion matrix.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: The spatial distribution of M67 cluster members compared to VV21 and the FoF method. It should be noted that VV21 appears to have a more comprehensive census. This is because VV21 uses the UVIT on ASTROSAT and Gaia EDR3 to determine a combination of astrometric, photometric, and systematic parameters of the M67 cluster members (Jadhav et al. 2021), while our work only used the astrometric and photometric data from Gaia EDR3. A Venn diagram of members is shown in the rightmost subplot. VV21 and ours have 460 identical member stars (over 61%), while FoF and VV21 only have 355 identical members (47.5%). Our approach resulted in a 14.5% increase in joint membership, suggesting that our method is valuable.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Schematic diagram of the four OCs identified in the study. From left to right, five panels illustrate the position of the OC in the (α, δ), (ϖ, ﹩{\mu }_{{a}^{* }}﹩) distribution, parallax distribution, (﹩{\mu }_{{a}^{* }}﹩, μ  δ ) distribution, and CMD of OC, respectively. Blue points represent observed stars, and the red line is for the best-fit isochrone. ID means cluster-ID.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Comparison of distribution of the OC population in (l, b) Galactic coordinates. The black circles present OCs known prior to this study, reported by CG20. Blue triangles represent the OCs found in this work matched with known OCs. Red points represent the new OCs found in this work using Gaia EDR3.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Class A, B, and C for the new OCs. Blue points show observed stars, and the red ones are for the best-fit isochrone. The name of each cluster in the catolog is given in the figure.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Blue points represent cluster members. The red dotted curve is the best-fitting isochrone.
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Total observed proper-motion dispersion using Gaia EDR3 vs. parallax. The x-axis is in log scale for known OCs from the homogeneous OC catalog of CG20 (black dots) compared with the new candidates in this study (red dots).
Paper: Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method
Authors: Huanbin Chi, 焕斌 迟, Shoulin Wei, 守林 卫, Feng Wang, 锋 王, Zhongmu Li, 忠木 李
Figure caption: Histogram of parallaxes for the OCs. Black represent the OCs reported by CG20. Blue represent the 46 new OCs found in this work using Gaia EDR3.
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: Schematic of the deep sets–inspired architecture employed in this work to support arbitrary image stacks. The CCD features are the summary properties of each CCD (10 in total). The depth corresponds to the 16 NSIDE = 2048 subpixels (some of which are removed by the mask, if they do not fall within the valid region) contributing to each NSIDE = 512 pixel, which are to be aggregated by a permutation-invariant operator (e.g., the sum). The height corresponds to one CCD, which may not cover all the subpixels. Sky-level systematics (the extinction, stellar counts, etc., as given in Table 7) are appended, before a final prediction is calculated for an NSIDE = 512 pixel. φ and ρ are parameterized with neural networks.
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: Illustrations of the diversity of the properties for single-epoch exposures, as well as their variable lengths. Subsets of properties are shown for the exposures covering three NSIDE = 2048 subpixels (IDs 21975319, 27803830, and 791280). We develop a method to predict the contamination of galaxy catalogs from the permutation-invariant and variable-length stacks of the exposure properties, rather than from the summary statistics (e.g., mean over exposures) that are employed by conventional methods.
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: Comparisons of the angular power spectra of the uncorrected and corrected galaxy overdensity maps obtained with the different cleaning methods. The bottom panels show the fractional changes, i.e the corrected spectra minus the uncorrected one, divided by the Gaussian uncertainties defined in Section 3.5. While the changes on large scales are the most pronounced, the cleaning results in a reduction of power on almost all scales, as well as the removal of sharp contamination features (e.g., ℓ ∼ 300).
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: Original uncorrected galaxy catalogs (number counts in HEALPIX pixels NSIDE = 512) constructed from DLS DR9. Suspicious features on a variety of scales are present and most likely noncosmological.
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: Correlations found by the neural network model between the original number-count maps of Figure 4 and the maps of potential contaminants (which only include the mean seeing, airmass, and CCD noise over the exposure stacks).
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: Additional spurious correlations found (on top of those shown in Figure 6) in the number-count maps by the new deep sets model from the full-exposure stacks.
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: Number-count maps obtained after correcting for correlations with potential contaminants using the new deep sets–based technique. Residual fluctuations are nearly isotropic and uniform across the sky.
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: The sky coverage of the three regions used in this work (distinguished by color). Additional sky cuts (indicated in light blue) are performed according to the coverage of the survey as well as the statistics of the various potential contaminants (e.g., pixels with extreme values were cut).
Paper: Spurious Correlations between Galaxies and Multiepoch Image Stacks in the DESI Legacy Surveys
Authors: Edgar Eggert, Boris Leistedt
Figure caption: Residual contamination as measured in the cross-power spectra between the cleaned galaxy overdensity maps and the contaminant maps. The reduced chi-squared values are calculated by comparing the cross-spectra (up to ﹩{{\ell }}_{\max }=1024﹩) with the zero-power spectrum, as a hypothesis, using the procedure detailed in Section 3.5.
Paper: Application of Deep Reinforcement Learning to Major Solar Flare Forecasting
Authors: Kangwoo Yi, Yong-Jae Moon, Hyun-Jin Jeong
Figure caption: CNN architecture from Yi et al. (2021). K is kernel size. D is the number of feature dimensions and is displayed in the case that it is changed in the layer.
Paper: Application of Deep Reinforcement Learning to Major Solar Flare Forecasting
Authors: Kangwoo Yi, Yong-Jae Moon, Hyun-Jin Jeong
Figure caption: A flow chart of the DQN algorithm for flare forecasting. The model’s experiences are stored in the replay memory. Randomly selected experiences in the replay memory are used for the DQN model training.