adsabs/AstroCLIMB huggingface dataset:
Paper: Ultraviolet Photometry and Habitable Zones of over 2700 Planet-hosting Stars
Authors: Xue Li, Song Wang, Henggeng Han, Jifeng Liu
Figure caption: (a) Distribution of uncertainty as a function of magnitude for the FUV band. The blue and red points represent the photometry results of AIS and MIS, respectively. The magnitudes are cut at the sensitivity limits for both AIS (=19.9 AB mag) and MIS (=22.7 AB mag). (b) Distribution of uncertainty as a function of magnitude for the NUV band. The magnitudes are cut at the sensitivity limits for both AIS (=20.7 AB mag) and MIS (=22.7 AB mag). (c) Comparison of FUV magnitudes measured from AIS and MIS. (d) Comparison of NUV magnitudes measured from AIS and MIS.
Paper: Application of Machine Learning to Background Rejection in Very-high-energy Gamma-Ray Observation
Authors: Jie Li, Hongkui Lv, Yang Liu, Jiajun Huang, Yu Wang, Wenbin Lin
Figure caption: Feature importance as given by DTC, RF, XGBoost, and CatBoost. The y-axis denotes features’ importance. The x-axis contains the list of all features. Top left: feature importance of 1012–1013 eV. Top right: feature importance of 1013–1014 eV. Lower left: feature importance of 1014–1015 eV. Lower right: feature importance of 1015–1016 eV.
Paper: Ultraviolet Photometry and Habitable Zones of over 2700 Planet-hosting Stars
Authors: Xue Li, Song Wang, Henggeng Han, Jifeng Liu
Figure caption: Left panel: growth curves for all sources in the NUV band. The magnitude differences are derived by subtracting the photometry results using a 1 pixel aperture from those at larger apertures. Colors indicate number density. The green circles represent the median magnitude differences at each aperture. Right panel: distribution of the selected apertures from the growth curves for each target.
Paper: Ultraviolet Photometry and Habitable Zones of over 2700 Planet-hosting Stars
Authors: Xue Li, Song Wang, Henggeng Han, Jifeng Liu
Figure caption: Top panel: Hertzsprung–Russell diagram of the sample stars hosting planets from NASA Exoplanet Science Institute (2023). The blue and red points represent stars with GALEX and SWIFT UVOT observations, respectively, while the gray points represent stars without UV photometry. Bottom panel: Galactic distribution of the sample stars.
Paper: Ultraviolet Photometry and Habitable Zones of over 2700 Planet-hosting Stars
Authors: Xue Li, Song Wang, Henggeng Han, Jifeng Liu
Figure caption: Examples of images for a general source (AU Mic in the left panel), an undetected source with an upper-limit magnitude estimation (TRAPPIST-1 in the middle panel), and a saturated source (HD 19994 in the right panel), respectively.
Paper: Ultraviolet Photometry and Habitable Zones of over 2700 Planet-hosting Stars
Authors: Xue Li, Song Wang, Henggeng Han, Jifeng Liu
Figure caption: Left panel: comparison of FUV magnitudes derived by this work and those from the GALEX photoobjall catalog. Right panel: comparison of NUV magnitudes derived by this work and those from the GALEX photoobjall catalog.
Paper: Application of Machine Learning to Background Rejection in Very-high-energy Gamma-Ray Observation
Authors: Jie Li, Hongkui Lv, Yang Liu, Jiajun Huang, Yu Wang, Wenbin Lin
Figure caption: Performance of models on finer energy bins for each metric. In terms of log(RecE/TeV), 1013–1014 eV and 1014–1015 eV are merged and divided into 10 bins. Overall, the performance is proportional to the energy level for the five evaluation metrics.
Paper: Improved Particle Spray Algorithm for Modeling Globular Cluster Streams
Authors: Yingtian Chen, Monica Valluri, Oleg Y. Gnedin, Neil Ash
Figure caption: Action space distributions of stream particles (left) and mass-loss histories of the progenitor cluster (right), varying the W parameter for the King model (first row), time step τ (second row), softening length ε (third row), and particle mass m (fourth row). The physical parameters are (M0, Rapo, e) = (105 M⊙, 40 kpc, 0.6), with the in-plane orbital inclination. Similarly to Figure 6, the contours in the left column enclose 50% of total particles.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: The first column of images, from top to bottom, shows the fraction of chromospheric activity spectra and the distance from the Galactic disk, the fraction of chromospherically active stars and the distance from the Galactic disk, and the fraction of flaring stars and the distance from the Galactic disk. The second column of images shows the two-dimensional distribution of the corresponding parameters in the Galaxy. The color bar indicates the ratio of the corresponding parameters.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: The top and bottom sets of images respectively show the synchronized observation results for two stars. In each set of images, the left panel displays the Hα spectral line, with the title showing the LAMOST name. The upper part of the right panel shows EWHα, and the lower part shows the corresponding TESS light curve for the same time, with the title displaying the TESS ID.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Left panel: relationship between the median ﹩{{\rm{EW}}}_{{\rm{H}}\alpha }^{{\prime} }﹩ and the median flare amplitude for each star. Right panel: relationship between the median ﹩{{\rm{R}}}_{{\rm{H}}\alpha }^{{\prime} }﹩ and the median flare amplitude for each star. In the plots, different colored dots represent stars of different spectral types. The black star line graph shows the median values of the corresponding data for each spectral type.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: These panels show the relationship between log﹩{{R}}_{{\rm{H}}\alpha }^{{\prime} }﹩ and logReff for stars of different spectral types. The red solid line in the plots represents the fitting line, the green shaded area indicates the 3σ range of the fitting error, and the color bar indicates the number density.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Six flare events in the time-domain Hα spectral lines. The colors of the spectral lines correspond to the colors of the EW scatter points.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: FORCAST 31.5 and 37.1 μm images, and HAWC+ 53, 89, 155, and 215 μm images. Each image has a differing FOV, which can be found in Table 3. The white transparent circle on the top right indicates the telescope beam size. The orange bar on the bottom left of the images is scaled to 500 pc. For all images, north is up and east is to the left.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: FORCAST 31.5 and 37.1 μm images, and HAWC+ 53, 89, 155, and 215 μm images. Note that the wavelength range for NGC 1068 starts at 19.7 μm, so its range is shifted. Each image has a differing FOV, which can be found in Table 3. For NGC 1068 FORCAST images, contours begin at 3σ and follow log(maximum) from [−2.0, 0.8] in steps of 0.2, while the HAWC+ images follow the same steps but log (max) ranges [−1.6, 0.8]. For all other images, the lowest contours are 3σ and increase in steps of 5σ. The white transparent circle on the top right indicates the telescope beam size. The orange bar on the bottom left of the images is scaled to 500 pc. For all images, north is up and east is to the left.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: FORCAST 31.5 and 37.1 μm images, and HAWC+ 53, 89, 155, and 215 μm images. Each image has a differing FOV, which can be found in Table 3. For bright objects (Centaurus A, Circinus, and Mrk 231), contours start at 3σ, then follow log(maximum) from [−1.2 to 0.8], [−1.8 to 0.8], [−1.4, 0.8] in steps of 0.2. For MCG-5-23-16 and Mrk 3, the lowest contours are 3σ and increase in steps of 5σ. The white transparent circle on the top right indicates the telescope beam size. The orange bar on the bottom left of the images is scaled to 500 pc. For all images, north is up and east is to the left.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: FORCAST 31.5 and 37.1 μm images, and HAWC+ 53, 89, 155, and 215 μm images. Each image has a differing FOV, which can be found in Table 3. The lowest contours are 3σ and increase in steps of 5σ. The white transparent circle on the top right indicates the telescope beam size. The orange bar on the bottom left of the images is scaled to 500 pc. For all images, north is up and east is to the left.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: PSF-subtracted images of host galaxy backgrounds
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: MIR to FIR SEDs of the several-arcsecond-scale nuclear fluxes in our sample of AGN. Filled pink diamonds represent SOFIA observations, while black dots represent complementary Herschel observations. The solid black lines correspond to Spitzer spectra.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: Bolometric luminosity vs. the peak wavelength of the SED for both Sy1 (filled red triangles) and Sy2 (filled purple stars).
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: Luminosity plotted against the distance of the 22 AGN in the atlas. Filled red triangles represent Sy1 and filled purple stars represent Sy2.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: Herschel PACS and SPIRE FIR images. The white circle in the top right indicates the beam size of the observation, while the pink line in the bottom left indicates a distance of 1 kpc.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: Color diagram of 21 of the 22 AGN in our sample. Sy1s are represented by filled triangles, while Sy2 are filled stars. The scale on the right shows peak wavelength by color.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: Example of the 2D Gaussian fitting routine explained in Section 4.1.
Paper: The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward
Figure caption: PSF-subtracted host galaxy images from archive Herschel data.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: (a) A section of the 100 × 100 sample of the generated 2D Gaussian random field with μ = 7 and σ = 2 with the detected minima pixels marked with cyan dots. (b) Histogram of all pixels (Parent Sample) and another histogram of detected minima pixels (Minima Sample), plotted together with the theoretical Gaussian distribution (N[7, σ = 2]), and the numerically calculated minima distribution (Minima PDF) calculated from Equation (8). (c) Relation of numerically calculated mean shift (μ − μmin) and ﹩{\sigma }_{{\rm{\min }}}﹩ with σ of the parent distribution for a Gaussian distribution plotted with their respective best-fit linear relations. (d) Relation between mean shift with the detected ﹩{\sigma }_{{\rm{\min }}}﹩ and the fit as presented in Equation (16).
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: (a) A sample Poissonian image with point sources injected as per the method described in Section 3. (b) SNR distribution of the injected sources of one of the generated images. While the mean background and standard deviation of the images change in tests, the flux of the sources is chosen such that their SNR distribution remains the same. (c) Relative absolute deviation of the recovered background from crowded fields from the source-masked images for the tests in Section 3 using Equation (18), in comparison to the SExtractor background.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: (a) Generated Poisson random variable field example, with its pixel histogram as an inset figure, and the parameter λ noted in the top-left corner. (b) Numerically calculated correction factor for the Poisson minima relation in Equation (18) with the power-law approximation which holds for μmin ≳ 0.3 (c) Recovered λ from generated Poisson random fields using Equation (18); the recovery is compared with the mean background estimations by SExtractor.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: (a) We show the least-squares-fitted linear relation between ﹩{\sigma }_{{\rm{\min }}}﹩, calculated from sampled pixels from Poisson images and ﹩\sqrt{\lambda }﹩ (Equation (23)). (b) The fitted relation between ﹩{\mu }_{{\rm{\min }}}﹩ and input λ in the Poisson images (Equation (24)).
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: A simplified flowchart showing the process of minima-based background sampling, with the detected minima in the intermediate-stage smoothed images (I2 and I3) shown by red points and the sampling boxes marked by purple in the second-to-last step. Note: the transition from I2 to I3 happens over a few iterative stages with smoothing kernels having widths in between G1 and G2.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: A simplified flowchart showing the process of maxima-based masking of regions with sources.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: (a) Pixel histograms of simulated images with texp = 3000 s (Figures 9(b) and (e)). (b) Pixel histograms of simulated images with texp = 50,000 s (Figures 9(c) and (f)). Poisson distributions of the background are shown in gray with the input mean background (﹩\widetilde{B}=1.16\times 1{0}^{-4}﹩ cps pixel–1, shown by a black line) for both exposure times. Pixel histograms of images with 500 sources + background and 4000 sources + background are shown with red and blue color, respectively. The recovered values of the mean background with the minima sampling routine and SExtractor are shown with solid and dotted–dashed lines in the same color as the histogram of the respective image.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: (a) Sigma ratio (σmin/σ) vs. sampling box size (b) with fixed FWHM of G1 = 15.3 and G2 = 3.5 pixels. (b) Calculated mean shift coefficient vs. sampling box size with fixed FWHM of G1 = 15.3 and G2 = 3.5 pixels. (c) Mean shift coefficient’s dependence on the final smoothing kernel (G2) while keeping a FWHM of G1 = 15.3 and b = 7. (d) Mean shift coefficient’s dependence on the initial smoothing kernel (G1) while keeping a FWHM of G2 = 3.5 and b = 7.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: (a) Sigma ratio (ξr) vs. sampling box size (b) with fixed FWHM of G = 16.5 pixels (cyan blue) and G = 2.35 pixels (orange). (b) Calculated mean shift coefficient vs. sampling box size with fixed FWHM of G = 16.5 pixels (cyan blue) and G = 2.35 pixels (orange). (c) Mean shift coefficient’s dependence on the smoothing kernel (G) while keeping b fixed at 7 pixels (green) and 17 (red).
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: Sample-generated UVIT-like images. (a) Background and noise-free 2.085 × 2.085 arcmin2 (300 × 300 pixels2) field with  ~500 sources (~125 per square arcminute). (b) and (c) show the same field as (a) with exposure times of 3000 and 50,000 s, respectively, at a mean background flux of 1.16 × 10−4 cps pixel−1. (d) Background and noise-free field with  ~4000 sources (~900 per square arcminute). (e) and (f) show the same field as (d) with exposure times of 3000 and 50,000 s, respectively, at the same background flux.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: Here we show a sample of generated images with sources as follows. (a) A 100 × 100 pixel (~41 × 41 arcsec2) section of the 300 × 300 pixel canvas where 500 point sources are uniformly distributed with a finite Gaussian PSF. (b) The same sources in (a) lying on a noisy background. (c) A 100 × 100 pixel (~41 × 41 arcsec2) section of the 300 × 300 pixel canvas where 4500 point sources are uniformly distributed with a finite Gaussian PSF. (d) The same sources in (c) lying on a noisy background. We can see that the source field in (a) is less crowded, and the source field in (d) is highly crowded.