adsabs/AstroCLIMB huggingface dataset:
Paper: Polarization Reconstruction Study of Wide Field-of-view Photoelectric Polarimeter for POLAR-2/LPD
Authors: Zu-Ke Feng, 祖科 冯, Hong-Bang Liu, 宏邦 刘, Di-Fan Yi, Li-Rong Xie, Cong Dai, Huan-Bo Feng, Jian-Chao Sun, Jiang He, Yuan-Hao Wang, Rui-Ting Ma, Bin-Long Wang, Qian-Nan Mai, Jiang-Chuan Tuo, Qian Zhong, Zhen-Yu Tang, Qian Liu, Fei Xie, Shuang-Nan Zhang, En-Wei Liang
Figure caption: Statistical results of reconstructed polarization degree using the corrected modulation function and the least χ2 method by extracting 20,000 events each time from a large number of simulated samples with bootstrap. The statistical distribution of the polarization degree is fitted using a Gaussian distribution, with the mean and variance of the fit results listed in the figure. In the figure, blue, orange, and purple represent input polarization degrees of 0.2, 0.5, and 0.8, respectively. These three figures show results for three polarization angles φ0 of 0°, 45°, and 90°. The photon energy is 4 keV, and the off-axis angle is 45°.
Paper: Polarization Reconstruction Study of Wide Field-of-view Photoelectric Polarimeter for POLAR-2/LPD
Authors: Zu-Ke Feng, 祖科 冯, Hong-Bang Liu, 宏邦 刘, Di-Fan Yi, Li-Rong Xie, Cong Dai, Huan-Bo Feng, Jian-Chao Sun, Jiang He, Yuan-Hao Wang, Rui-Ting Ma, Bin-Long Wang, Qian-Nan Mai, Jiang-Chuan Tuo, Qian Zhong, Zhen-Yu Tang, Qian Liu, Fei Xie, Shuang-Nan Zhang, En-Wei Liang
Figure caption: Comparison of fitting results for simulated data after azimuthal angle reconstruction using corrected (red) and uncorrected (green) modulation functions. The three columns correspond to polarization angles of (a) φ0 = 90°, (b) φ0 = 45°, and (c) φ0 = 0°. The photon energy is 4 keV, and the off-axis angle is 45°. The fitting results show that the corrected modulation function (red) provides a better fit to the simulated data across polarization angles, with its reduced χ2 values smaller than those of the uncorrected modulation function (green).
Paper: Polarization Reconstruction Study of Wide Field-of-view Photoelectric Polarimeter for POLAR-2/LPD
Authors: Zu-Ke Feng, 祖科 冯, Hong-Bang Liu, 宏邦 刘, Di-Fan Yi, Li-Rong Xie, Cong Dai, Huan-Bo Feng, Jian-Chao Sun, Jiang He, Yuan-Hao Wang, Rui-Ting Ma, Bin-Long Wang, Qian-Nan Mai, Jiang-Chuan Tuo, Qian Zhong, Zhen-Yu Tang, Qian Liu, Fei Xie, Shuang-Nan Zhang, En-Wei Liang
Figure caption: Comparison of the fitting results of the experimental data after azimuthal angle reconstruction using corrected and uncorrected modulation functions. The left-hand panel shows the results at an energy of 4.51 keV, while the right-hand panel displays the results at 8.05 keV. The incident source is a point source at an off-axis angle of 30°, with the polarization direction in the incident plane ϒ. The fitting results indicate that the reduced χ2 value for the corrected modulation function is closer to 1, demonstrating a better match with the experimental data.
Paper: Polarization Reconstruction Study of Wide Field-of-view Photoelectric Polarimeter for POLAR-2/LPD
Authors: Zu-Ke Feng, 祖科 冯, Hong-Bang Liu, 宏邦 刘, Di-Fan Yi, Li-Rong Xie, Cong Dai, Huan-Bo Feng, Jian-Chao Sun, Jiang He, Yuan-Hao Wang, Rui-Ting Ma, Bin-Long Wang, Qian-Nan Mai, Jiang-Chuan Tuo, Qian Zhong, Zhen-Yu Tang, Qian Liu, Fei Xie, Shuang-Nan Zhang, En-Wei Liang
Figure caption: Polarization reconstruction results for a plane source following a power-law spectrum with a photon index of 1.6. The left- and right-hand figures represent input polarization degrees of 0.5 with polarization angles φ0 of 0° and 90°, respectively. The center of the red cross represents the input values of the polarization degree and polarization angle in the simulator. The black, yellow, and green rings represent the 1σ, 2σ, and 3σ confidence intervals, respectively. The off-axis angle is 45°. Each plot uses 1,500,000 events for the reconstruction. The inset in each plot is a magnified view of the confidence interval region.
Paper: Polarization Reconstruction Study of Wide Field-of-view Photoelectric Polarimeter for POLAR-2/LPD
Authors: Zu-Ke Feng, 祖科 冯, Hong-Bang Liu, 宏邦 刘, Di-Fan Yi, Li-Rong Xie, Cong Dai, Huan-Bo Feng, Jian-Chao Sun, Jiang He, Yuan-Hao Wang, Rui-Ting Ma, Bin-Long Wang, Qian-Nan Mai, Jiang-Chuan Tuo, Qian Zhong, Zhen-Yu Tang, Qian Liu, Fei Xie, Shuang-Nan Zhang, En-Wei Liang
Figure caption: Fitting results of the true value distribution of photoelectron emission azimuthal angles, extracted from the Geant4 simulation framework, using the theoretical off-axis modulation functions. The four graphs illustrate unpolarized and fully polarized light at three polarization angles φ0 with an inclination δ of 45°.
Paper: FASHI: An Untargeted Survey of the 21 cm H I Absorption Galaxies with FAST
Authors: Chuan-Peng Zhang, Ming Zhu, Peng Jiang, Cheng Cheng, Jin-Long Xu, Nai-Ping Yu, Xiao-Lan Liu, Bo Zhang
Figure caption: The histogram of velocities for the principal H I absorption components with respect to the systemic velocity estimated from optical counterparts. The derived velocity error is about σ = 100 km s−1 shown with a shaded bar.
Paper: FASHI: An Untargeted Survey of the 21 cm H I Absorption Galaxies with FAST
Authors: Chuan-Peng Zhang, Ming Zhu, Peng Jiang, Cheng Cheng, Jin-Long Xu, Nai-Ping Yu, Xiao-Lan Liu, Bo Zhang
Figure caption: Upper: two-dimensional distributions of star formation rate log(SFRSED) and stellar mass log(M ⋆). The background shows all the data in the GSWLC. The red dots indicate crossmatched and associated H I absorbers detected by FASHI. Lower: color–stellar mass diagram of the FASHI absorbers. The blue and red galaxies are separated by g − r = 0.83 (S. M. Weinmann et al. 2006; X. Yang et al. 2006).
Paper: The Impact of Host-galaxy Properties on Supernova Classification with Hierarchical Labels
Authors: V. Ashley Villar, Sebastian Gomez, Edo Berger, Alex Gagliano
Figure caption: Hierarchical graph structure used in this work. Blue text is meant as a guide to the various components of a generic tree.
Paper: FASHI: An Untargeted Survey of the 21 cm H I Absorption Galaxies with FAST
Authors: Chuan-Peng Zhang, Ming Zhu, Peng Jiang, Cheng Cheng, Jin-Long Xu, Nai-Ping Yu, Xiao-Lan Liu, Bo Zhang
Figure caption: The histograms of line width (upper) and optical depth (lower) for the 21 cm H I absorbers in FASHI and K. Geréb et al. (2015).
Paper: The Impact of Host-galaxy Properties on Supernova Classification with Hierarchical Labels
Authors: V. Ashley Villar, Sebastian Gomez, Edo Berger, Alex Gagliano
Figure caption: Scatter plot of various host-galaxy features to classify SNe in this work (see Section 2 for feature definitions). SNe are spectroscopically labeled as part of PS1-MDS, and for features where the host-galaxy features were not observed, they are inferred via K-means imputation. Even in these simple feature spaces, clear clustering is seen.
Paper: The Impact of Host-galaxy Properties on Supernova Classification with Hierarchical Labels
Authors: V. Ashley Villar, Sebastian Gomez, Edo Berger, Alex Gagliano
Figure caption: Purity (top row), completeness (middle row), and F1-score (bottom row) achieved with the various feature sets and confidence thresholds as a function of SN type (columns). Shaded regions represent 1σ uncertainties, computed using the same classifier with different random model initializations during training.
Paper: FASHI: An Untargeted Survey of the 21 cm H I Absorption Galaxies with FAST
Authors: Chuan-Peng Zhang, Ming Zhu, Peng Jiang, Cheng Cheng, Jin-Long Xu, Nai-Ping Yu, Xiao-Lan Liu, Bo Zhang
Figure caption: The relationship between the H I column density and the stellar mass in the host galaxy. The red dots indicate crossmatched and associated H I absorbers detected by FASHI.
Paper: FASHI: An Untargeted Survey of the 21 cm H I Absorption Galaxies with FAST
Authors: Chuan-Peng Zhang, Ming Zhu, Peng Jiang, Cheng Cheng, Jin-Long Xu, Nai-Ping Yu, Xiao-Lan Liu, Bo Zhang
Figure caption: The distribution between the depth of the H I absorption line (S HI) and the integrated 1.4 GHz continuum flux density (S 1.4GHz) for the detected absorbers by FASHI.
Paper: The Local Ultraviolet to Infrared Treasury. I. Survey Overview of the Broadband Imaging
Authors: Karoline M. Gilbert, Yumi Choi, Martha L. Boyer, Benjamin F. Williams, Daniel R. Weisz, Eric F. Bell, Julianne J. Dalcanton, Kristen B. W. McQuinn, Evan D. Skillman, Guglielmo Costa, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, Steven R. Goldman, Karl D. Gordon, Puragra Guhathakurta, Maude Gull, Lea Hagen, Ky Huynh, Christina W. Lindberg, Paola Marigo, Claire E. Murray, Giada Pastorelli, Petia Yanchulova Merica-Jones
Figure caption: The difference in the 50% (top panel) and 80% (bottom panel) completeness limits calculated in the lowest (Σ ≤ Σ25%) and highest (Σ > Σ75%) spatial density bins for each LUVIT pointing, for each filter (Section 5.5). The pointings are presented in order of increasing distance of the target galaxy. The lowest density bin is defined for each individual target by the source density Σ25% at which 25% of observed sources fall in a region with source density Σ ≤ Σ25%. The highest density bin threshold is defined as the source density Σ75% at which 75% of observed sources fall in a region with source density Σ ≤ Σ75%. The dotted lines in each panel indicate a ±0.2 magnitude difference between the completeness limits in the lowest and highest spatial density bins. The recovery fraction of ASTs and the bias in the recovered magnitudes as a function of recovered magnitude in four spatial density bins are shown in Figure 14 for targets which exceed the ∣Δm∣ > 0.2 threshold in any filter, for either the 50% or 80% completeness limits.
Paper: Polarization Reconstruction Study of Wide Field-of-view Photoelectric Polarimeter for POLAR-2/LPD
Authors: Zu-Ke Feng, 祖科 冯, Hong-Bang Liu, 宏邦 刘, Di-Fan Yi, Li-Rong Xie, Cong Dai, Huan-Bo Feng, Jian-Chao Sun, Jiang He, Yuan-Hao Wang, Rui-Ting Ma, Bin-Long Wang, Qian-Nan Mai, Jiang-Chuan Tuo, Qian Zhong, Zhen-Yu Tang, Qian Liu, Fei Xie, Shuang-Nan Zhang, En-Wei Liang
Figure caption: The analytical results showing the impact of positional errors on the reconstructed polarization degree and angle. Errors are applied separately to the azimuth η and the inclination δ in the detector reference frame. The true polarization degree, P0, is set at 20%, 50%, and 80% for Panels A, B, and C, respectively. Panels 1, 2, and 3 correspond to an energy of 2 keV, while Panels 4, 5, and 6 correspond to 10 keV. Pairs of panels (1,4), (2,5), and (3,6) represent inclinations δ of 0°, 20°, and 50°, respectively. Each plot includes results for true polarization angles φ0 of 0° and 90°. Solid lines in the plots indicate the results for the polarization degree, while dashed lines represent the results for the polarization angle.
Paper: Polarization Reconstruction Study of Wide Field-of-view Photoelectric Polarimeter for POLAR-2/LPD
Authors: Zu-Ke Feng, 祖科 冯, Hong-Bang Liu, 宏邦 刘, Di-Fan Yi, Li-Rong Xie, Cong Dai, Huan-Bo Feng, Jian-Chao Sun, Jiang He, Yuan-Hao Wang, Rui-Ting Ma, Bin-Long Wang, Qian-Nan Mai, Jiang-Chuan Tuo, Qian Zhong, Zhen-Yu Tang, Qian Liu, Fei Xie, Shuang-Nan Zhang, En-Wei Liang
Figure caption: Simulation results of GRB localization at different flux levels for POLAR-2/BSD. Each point in the figure represents a simulation, with the y-axis showing the deviation between reconstructed and input positions.
Paper: Polarization Reconstruction Study of Wide Field-of-view Photoelectric Polarimeter for POLAR-2/LPD
Authors: Zu-Ke Feng, 祖科 冯, Hong-Bang Liu, 宏邦 刘, Di-Fan Yi, Li-Rong Xie, Cong Dai, Huan-Bo Feng, Jian-Chao Sun, Jiang He, Yuan-Hao Wang, Rui-Ting Ma, Bin-Long Wang, Qian-Nan Mai, Jiang-Chuan Tuo, Qian Zhong, Zhen-Yu Tang, Qian Liu, Fei Xie, Shuang-Nan Zhang, En-Wei Liang
Figure caption: Statistical results of reconstructed polarization degree for GRBs at different SNRs (1, 5, and 10), derived using the bootstrap method with 20,000 events per extraction from a large sample of simulated data. The GRB energy spectrum is modeled by a power-law distribution with a spectral index of 1.6, an off-axis angle of 45°, and a polarization angle φ0 of 90°.
Paper: The Spatial Distribution of Globular Cluster Systems in Early-type Galaxies: Estimation Procedure and Catalog of Properties for Globular Cluster Systems Observed with Deep Imaging Surveys
Authors: Sungsoon Lim, Eric W. Peng, Patrick Côté, Laura Ferrarese, Joel C. Roediger, Chengze Liu, Chelsea Spengler, Elisabeth Sola, Pierre-Alain Duc, Laura V. Sales, John P. Blakeslee, Jean-Charles Cuillandre, Patrick R. Durrell, Eric Emsellem, Stephen D. J. Gwyn, Ariane Lançon, Francine R. Marleau, J. Christopher Mihos, Oliver Müller, Thomas H. Puzia, Rubén Sánchez-Janssen
Figure caption: (Left) Inverse concentration index, Δm4−8, vs. g-band magnitude for sources in the NGC 4472 region. The red dotted box shows the pointlike source region used for this galaxy. (Right) (﹩{u}^{* }-g^{\prime} ﹩)-(﹩g^{\prime} -i^{\prime} ﹩) color–color diagram of pointlike sources in the NGC 4472 region. The red dashed polygon shows the globular cluster (GC) selection region used in this study, with red sources showing GC candidates.
Paper: The Spatial Distribution of Globular Cluster Systems in Early-type Galaxies: Estimation Procedure and Catalog of Properties for Globular Cluster Systems Observed with Deep Imaging Surveys
Authors: Sungsoon Lim, Eric W. Peng, Patrick Côté, Laura Ferrarese, Joel C. Roediger, Chengze Liu, Chelsea Spengler, Elisabeth Sola, Pierre-Alain Duc, Laura V. Sales, John P. Blakeslee, Jean-Charles Cuillandre, Patrick R. Durrell, Eric Emsellem, Stephen D. J. Gwyn, Ariane Lançon, Francine R. Marleau, J. Christopher Mihos, Oliver Müller, Thomas H. Puzia, Rubén Sánchez-Janssen
Figure caption: (Left) Inverse concentration index, Δm4−8, vs. g-band magnitude for sources in the NGC 524 region. The red dotted box shows the pointlike source region used for this galaxy. (Right) (﹩g^{\prime} -r^{\prime} ﹩)-(﹩g^{\prime} -i^{\prime} ﹩) color–color diagram of pointlike sources in the NGC 524 region. The red dashed polygon shows the GC selection region used in this study, with red sources showing GC candidates.
Paper: The Spatial Distribution of Globular Cluster Systems in Early-type Galaxies: Estimation Procedure and Catalog of Properties for Globular Cluster Systems Observed with Deep Imaging Surveys
Authors: Sungsoon Lim, Eric W. Peng, Patrick Côté, Laura Ferrarese, Joel C. Roediger, Chengze Liu, Chelsea Spengler, Elisabeth Sola, Pierre-Alain Duc, Laura V. Sales, John P. Blakeslee, Jean-Charles Cuillandre, Patrick R. Durrell, Eric Emsellem, Stephen D. J. Gwyn, Ariane Lançon, Francine R. Marleau, J. Christopher Mihos, Oliver Müller, Thomas H. Puzia, Rubén Sánchez-Janssen
Figure caption: Comparison of NGC,total from the ACSVCS results (E. W. Peng et al. 2008) with this study. Left panel: Direct comparison of the total number of GCs from between this study and ACSVCS. The black dashed line and the red dotted line show the one-to-one relation and the linear fit, respectively. E. W. Peng et al. (2008) used additional data to fit GC density profiles for several galaxies because of large spatial distribution of GCs, and we mark them with large open circles. Right panel: Similar to the left panel, but total numbers of GCs in this study are limited within ﹩1.^{\prime} \,67\,﹩ similar to the ACS/WFC field of view. The dashed line shows the one-to-one relation. E. W. Peng et al. (2008) used additional background observations to estimate the number of GCs, but they used local background (in an ACS/WFC field) for several galaxies, so these galaxies are marked with cyan filled circles. This study uses Gaussian functions of the ACSVCS GCLF to correct for the magnitude limit, but several ACSVCS galaxies do not have a Gaussian form of the GCLF, so we have marked them with red filled circles.
Paper: The Spatial Distribution of Globular Cluster Systems in Early-type Galaxies: Estimation Procedure and Catalog of Properties for Globular Cluster Systems Observed with Deep Imaging Surveys
Authors: Sungsoon Lim, Eric W. Peng, Patrick Côté, Laura Ferrarese, Joel C. Roediger, Chengze Liu, Chelsea Spengler, Elisabeth Sola, Pierre-Alain Duc, Laura V. Sales, John P. Blakeslee, Jean-Charles Cuillandre, Patrick R. Durrell, Eric Emsellem, Stephen D. J. Gwyn, Ariane Lançon, Francine R. Marleau, J. Christopher Mihos, Oliver Müller, Thomas H. Puzia, Rubén Sánchez-Janssen
Figure caption: GC luminosity functions and their fitting results, with the fixed peak magnitude of the Gaussian function. (a) GCLF of NGC 4365. The gray histogram shows the background-subtracted GCLF, and the blue histogram represents the background. GCs are within 2Re,GCS, and the background area is chosen between 5Re,GCS and 8Re,GCS. The dashed line represents the fitted Gaussian function with a fixed peak magnitude. (b) GCLF of NGC 4267, with notations the same as in panel (a). (c) GCLF of NGC 4473, with notations also the same as in panel (a). (d) Comparison of GCLF widths from this study and D. Villegas et al. (2010). The X- and Y-axes show σGCLF from this study and D. Villegas et al. (2010), respectively. The dotted line indicates a one-to-one correspondence.
Paper: The Spatial Distribution of Globular Cluster Systems in Early-type Galaxies: Estimation Procedure and Catalog of Properties for Globular Cluster Systems Observed with Deep Imaging Surveys
Authors: Sungsoon Lim, Eric W. Peng, Patrick Côté, Laura Ferrarese, Joel C. Roediger, Chengze Liu, Chelsea Spengler, Elisabeth Sola, Pierre-Alain Duc, Laura V. Sales, John P. Blakeslee, Jean-Charles Cuillandre, Patrick R. Durrell, Eric Emsellem, Stephen D. J. Gwyn, Ariane Lançon, Francine R. Marleau, J. Christopher Mihos, Oliver Müller, Thomas H. Puzia, Rubén Sánchez-Janssen
Figure caption: Comparison of Re,gc from literature with this study. The downward triangle shows NGC 4365 (C. Blom et al. 2012); the triangle shows NGC 4278 (C. Usher et al. 2013), and pentagons show three galaxies from the SLUGGS survey (S. S. Kartha et al. 2014, 2016), diamonds, NGC 4472 and NGC 4406 (J. R. Hargis & K. L. Rhode 2014), squares (J. P. Caso et al. 2019), and circles (B. J. De Bórtoli et al. 2022).
Paper: The Spatial Distribution of Globular Cluster Systems in Early-type Galaxies: Estimation Procedure and Catalog of Properties for Globular Cluster Systems Observed with Deep Imaging Surveys
Authors: Sungsoon Lim, Eric W. Peng, Patrick Côté, Laura Ferrarese, Joel C. Roediger, Chengze Liu, Chelsea Spengler, Elisabeth Sola, Pierre-Alain Duc, Laura V. Sales, John P. Blakeslee, Jean-Charles Cuillandre, Patrick R. Durrell, Eric Emsellem, Stephen D. J. Gwyn, Ariane Lançon, Francine R. Marleau, J. Christopher Mihos, Oliver Müller, Thomas H. Puzia, Rubén Sánchez-Janssen
Figure caption: Comparison of the GC number density profile in NGC 4486 with the literature. X-axis is the radial distance from the center of NGC 4486, and Y-axis is the GC number density. Gray circles and red dashed line show data points and fitted results from this study. For comparison with previous studies, the background is subtracted, and the effect of the magnitude limit is corrected with the GCLF for GC number density. Magenta diamond and green inverted triangle represent results from D. E. McLaughlin (1999) and W. E. Harris (2009), respectively.
Paper: The Spatial Distribution of Globular Cluster Systems in Early-type Galaxies: Estimation Procedure and Catalog of Properties for Globular Cluster Systems Observed with Deep Imaging Surveys
Authors: Sungsoon Lim, Eric W. Peng, Patrick Côté, Laura Ferrarese, Joel C. Roediger, Chengze Liu, Chelsea Spengler, Elisabeth Sola, Pierre-Alain Duc, Laura V. Sales, John P. Blakeslee, Jean-Charles Cuillandre, Patrick R. Durrell, Eric Emsellem, Stephen D. J. Gwyn, Ariane Lançon, Francine R. Marleau, J. Christopher Mihos, Oliver Müller, Thomas H. Puzia, Rubén Sánchez-Janssen
Figure caption: The GC specific frequencies (﹩{S}_{N,g^{\prime} }﹩) are plotted against the absolute ﹩g^{\prime} ﹩-band magnitudes of their host galaxies. Gray filled circles show GC systems from this study; well-fitted systems (error of Re,gc < 50%) are shown with large heavy symbols, and MATLAS galaxies are highlighted.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Comparison of the results from the traditional classification method and our new classification method. (a) The relationship between the EHD parameter and T90,i. The black dashed line serves as the classification boundary, clearly separating GRBs into type I and type II, with green and red symbols representing GRBs with T90 > 2 s and T90 < 2 s, respectively. (b) Distribution of the classification results from the EHD−T90,i relation according to our new classification method. Green diamonds and red triangles represent GRBs classified as type II (EHD_II) and type I (EHD_I) under the EHD parameter classification method, respectively. Special GRBs, including GRB 200826A, GRB 230307A, GRB 211211A, and GRB 170817A, are highlighted with unique symbols. The magenta diamond represents the Platinum sample that closely follows the Dainotti relation (3D).
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Comparison with the unsupervised ML classification results of S. Bhardwaj et al. (2023). The blue, red, yellow, and green symbols represent IS GRBs, ULGRBs, XRR, and XRF, respectively.
Paper: ExoMolHR: A Relational Database of Empirical High-resolution Molecular Spectra
Authors: Jingxin Zhang, Christian Hill, Jonathan Tennyson, Sergei N. Yurchenko
Figure caption: Comparison of the line intensities (cm molecule−1) from ExoMol, ExoMolHR (top), and HITRAN (bottom) databases at T = 296 K of 1H216O, 15N1H3, 12C1H4, and 32S16O2. The highlighted points in the upper panels show intensities provided by ExoMolHR, while the darker background shows the full coverage given by the POKAZATEL, CoYuTe-15, MM, and ExoAmes line lists of 1H216O, 15N1H3, 12C1H4, and 32S16O2, respectively.
Paper: ExoMolHR: A Relational Database of Empirical High-resolution Molecular Spectra
Authors: Jingxin Zhang, Christian Hill, Jonathan Tennyson, Sergei N. Yurchenko
Figure caption: Compare the densities of wavenumbers (left) and line intensities (middle) of the ExoMol, ExoMolHR, and HITRAN databases at T = 296 K for 1H216O, 14N1H3, 12C1H4, and 32S16O2. The ExoMol line lists provide full coverage using the POKAZATEL, CoYuTe, MM, and ExoAmes line lists of 1H216O, 14N1H3, 12C1H4, and 32S16O2, respectively. The 2D plots of the densities between wavenumbers and line intensities (cm molecule−1) for ExoMolHR databases at T = 296 K are displayed on the right panels.
Paper: ExoMolHR: A Relational Database of Empirical High-resolution Molecular Spectra
Authors: Jingxin Zhang, Christian Hill, Jonathan Tennyson, Sergei N. Yurchenko
Figure caption: Comparison of the line intensities (cm molecule−1) from ExoMolHR (top) and ExoMol (bottom) databases at temperatures T = 1000 and 2000 K of 1H216O, 48Ti16O, and 51V16O.
Paper: ExoMolHR: A Relational Database of Empirical High-resolution Molecular Spectra
Authors: Jingxin Zhang, Christian Hill, Jonathan Tennyson, Sergei N. Yurchenko
Figure caption: Process flowchart for ExoMolHR database generation.
Paper: ExoMolHR: A Relational Database of Empirical High-resolution Molecular Spectra
Authors: Jingxin Zhang, Christian Hill, Jonathan Tennyson, Sergei N. Yurchenko
Figure caption: Four steps for getting the intensity file from the ExoMolHR website.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Count maps and light curves of the GRB 240205926 event recorded by four detectors (n3, n4, n5, and b0).