adsabs/AstroCLIMB huggingface dataset:
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Variation of the width of the N-pdf with (a) peak excitation temperature, (b) radius, and (c) kinematic distance of the clouds. The red color and blue color correspond to the clouds in the LN and LN+PL categories, respectively.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Histograms of the distance-independent physical parameters, i.e., (a) pixel number, (b) column density, and (c) excitation temperature of the selected clouds.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Histograms of the distance-dependent physical parameters, i.e., (a) kinematic distance, (b) mass, and (c) radius of the selected clouds.
Paper: Binding Energy Evaluation Platform: A Database of Quantum Chemical Binding Energy Distributions for the Astrochemical Community
Authors: Giulia M. Bovolenta, Stefan Vogt-Geisse, Stefano Bovino, Tommaso Grassi
Figure caption: Binding energy distributions for Group H, ASW–X systems, using HF-3 c/MINIX geometries and including ZPVE correction. According to the benchmark results, the energy has been computed at ω − PBE/def2-TZVP level of theory for all species except HNC (B97-2/def2-TZVP), H2CO (CAM-B3LYP/def2-TZVP), CH3OH (TPSSH/def2-TZVP), HF, and HCN (MPWB1K/def2-TZVP). D3BJ dispersion correction has been applied to all DFT energies. Each identified binding mode has been fitted with a Gaussian function, using a bootstrap method (see Appendix F). Mean (μ) and standard deviation (σ) of the Gaussian fit are reported for the main binding mode (BM1, solid line) and the minor binding mode (BM2, dashed line). The numbers on the plot represent the percentage of minimum energy structures that belong to a specific mode. Columns 2 and 5 report a graphic representation of an example of BM1 and BM2. The atoms in proximity of the binding site have been highlighted. The color scheme for the atoms is red for O, gray for C, white for H, blue for N, yellow for S, and green for F.
Paper: Binding Energy Evaluation Platform: A Database of Quantum Chemical Binding Energy Distributions for the Astrochemical Community
Authors: Giulia M. Bovolenta, Stefan Vogt-Geisse, Stefano Bovino, Tommaso Grassi
Figure caption: Three-step computational procedure used in this work for building a binding energy distribution. BSC stands for binding site candidate; opt 1 stands for optimization at gradient generalized approximation (GGA) exchange-correlation DFT functional and opt 2 for optimization at a higher level of theory that further refines the geometry. The color scheme for the atoms is red for O, white for H, blue for N, and yellow for the generic target atom X.
Paper: Blacklight: A General-relativistic Ray-tracing and Analysis Tool
Authors: Christopher J. White
Figure caption: Errors in midplane Kerr deflection angles using the DP, RK4, and RK2 schemes. The error for each ray is plotted against the total number of steps used to integrate that ray. Colors correspond to the user-specified numerical control parameters. The DP integrator is a robust choice, with the RK methods providing versatility for users needing more control over the computation–accuracy trade-off.
Paper: Blacklight: A General-relativistic Ray-tracing and Analysis Tool
Authors: Christopher J. White
Figure caption: Schematic illustrating the arrangement of pixels into blocks suitable for refinement. The root grid samples 82 rays (black points) in as many pixels (gray squares), which are arranged into four blocks of 42 pixels (black squares). The upper right block is refined into four new blocks (solid blue squares) of 42 pixels each (pale blue squares), sampled at their respective centers (blue points).
Paper: Blacklight: A General-relativistic Ray-tracing and Analysis Tool
Authors: Christopher J. White
Figure caption: Comparison of the fiducial image (upper left), made with only the standard σ ≤ 1 cut, with the result of various other cuts on the data. Only sufficiently magnetized (β −1 ≥ 2) plasma contributes to the upper right image. The lower panels exclude plasma further than (left) or nearer than (right) the plane orthogonal to the line of sight passing through the origin.
Paper: Blacklight: A General-relativistic Ray-tracing and Analysis Tool
Authors: Christopher J. White
Figure caption: Deflection angles obtained by Blacklight when integrating the geodesic equation for rays in the midplane around a spinning black hole. The line is calculated from the analytic formula, with the differences shown in the lower panel. This test uses the DP integrator with f abs, f rel = 10−8.
Paper: Blacklight: A General-relativistic Ray-tracing and Analysis Tool
Authors: Christopher J. White
Figure caption: Images produced by Blacklight for the five parameterized models in Gold et al. (2020), showing the expected features and brightnesses. In order to match the color scales in that work, I  ν  in erg s−1 cm−2 sr−1 Hz−1 is multiplied by 105(75/128)2 f −1, where f is 1.6465, 1.436, 0.4418, 0.2710, and 0.0255 for the five tests, respectively.
Paper: Blacklight: A General-relativistic Ray-tracing and Analysis Tool
Authors: Christopher J. White
Figure caption: Results of a fast-light calculation performed with a snapshot from the fiducial simulation (left), together with a comparable slow-light calculation using 160 snapshots spaced by Δt = 1 GM/c 3. Though the images largely agree, the time-variability properties of the light curves generated from sequences of such images could well be different.
Paper: Blacklight: A General-relativistic Ray-tracing and Analysis Tool
Authors: Christopher J. White
Figure caption: Comparison of the fiducial image (left) with the result of treating spacetime as flat (right). The effect of gravity here is to magnify the image relative to flat-spacetime expectations, as well as to produce a photon ring.
Paper: Blacklight: A General-relativistic Ray-tracing and Analysis Tool
Authors: Christopher J. White
Figure caption: Stokes parameters for the fiducial image in units of erg s−1 cm−2 sr−1 Hz−1.
Paper: X-Ray Intraday Variability of the TeV Blazar Markarian 421 with XMM-Newton
Authors: A Priyana Noel, Haritma Gaur, Alok C. Gupta, Alicja Wierzcholska, Michał Ostrowski, Vinit Dhiman, Gopal Bhatta
Figure caption: (a) A plot of τ var vs. the mean photon flux ﹩\overline{x}﹩ for all observations. An arbitrarily normalized dashed line τ var = 4 ks × Flux/(400 cts s−1) is provided for reference, showing the expected τ var values for the same Δx and Δt used in all data sets. (b) The minimum variability timescale τ var plotted against the observation dates, given in modified Julian date, for all observations.
Paper: X-Ray Intraday Variability of the TeV Blazar Markarian 421 with XMM-Newton
Authors: A Priyana Noel, Haritma Gaur, Alok C. Gupta, Alicja Wierzcholska, Michał Ostrowski, Vinit Dhiman, Gopal Bhatta
Figure caption: (a) Fractional variability F var in the soft- and hard-energy bands plotted vs. the duration of the observation; fitted correlation lines are provided for both distributions. (b) F var in the hard vs. the soft bands. The lines F var(hard) = F var(soft) and F var(hard) = 2.5F var(soft) are provided for reference. (c) F var in the total-energy band vs. flux, with the correlation line represented by the dashed line
Paper: X-Ray Intraday Variability of the TeV Blazar Markarian 421 with XMM-Newton
Authors: A Priyana Noel, Haritma Gaur, Alok C. Gupta, Alicja Wierzcholska, Michał Ostrowski, Vinit Dhiman, Gopal Bhatta
Figure caption: Fractional variability F var vs. the parameters of the Gaussian fits of the DCF maximum. (a) The amplitude A. (b) The width σ. (c) The time lag μ. The red lines represent linear fits to the presented distributions, without considering the two “nonvariable” outliers with the lowest F var. The dashed lines in panel (c) are for a reference, as explained in the text.
Paper: X-Ray Intraday Variability of the TeV Blazar Markarian 421 with XMM-Newton
Authors: A Priyana Noel, Haritma Gaur, Alok C. Gupta, Alicja Wierzcholska, Michał Ostrowski, Vinit Dhiman, Gopal Bhatta
Figure caption: HR–I diagram of all the plots combined into one, with the color bar (a) depicting the chronology of the observation, from the first observation taken on 2000 May 25 to the last observation taken on 2017 May 4, and (b) showing the distribution of the derived τ var within the observations.
Paper: X-Ray Intraday Variability of the TeV Blazar Markarian 421 with XMM-Newton
Authors: A Priyana Noel, Haritma Gaur, Alok C. Gupta, Alicja Wierzcholska, Michał Ostrowski, Vinit Dhiman, Gopal Bhatta
Figure caption: Obs. ID 0136541001. (a) The LC with the considered flare marked by the vertical lines. (b) The LC of the flaring part. (c) HR–I diagram of the flaring portion of the LC, plotted in color over the whole LC (plotted in gray) HR–I diagram (Figure 1.5, panel (c)), with a colorbar showing increasing time in seconds.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: The results from the dusty sound wave test. The left and middle panels are the time evolution of the normalized density and the normalized velocities of gas and dust located at x = 0, to be compared with Figure 3 of Benítez-Llambay et al. (2019). The solid lines represent the analytical solutions, and the triangle and circle markers are the numerical results from test runs with 256 cells. The right panel demonstrates the numerical convergence, where we calculate the mean L1 error after one wave period, and show how it varies with the number of grid cells using the “VL2-Implicit” and “RK2-Implicit” drag integrators.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Left: the evolution of the maximum and mean dust-to-gas ratios ϵ over time in the global run and the local BA-5122. The calculations of ϵ in the global run are conducted over r ∈ [0.4, 2.4]. Right: dust CDFs of the global run and the local BA-5122, similar to Figure 7. The dust CDFs of the global run are calculated by the normalized dust density ρ d r 0.5 on r ∈ [0.4, 2.4]. The color-shaded regions are the temporal standard deviations from ﹩600\ {{\rm{\Omega }}}_{0}^{-1}﹩ and ﹩800\ {{\rm{\Omega }}}_{0}^{-1}﹩.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Snapshots of the KHI tests with two dust species with AMR. The top (bottom) six panels are the cases without (with) dust feedback at t = 1.2 (t = 1.6). The abbreviations “nofb” and “fb” are for the cases without and with feedback, respectively. From left to right, the panels are for gas, dust species 1, and dust species 2. The stopping times of the dust are T s,1 = 10−2 and T s,2 = 10−8. The first and third rows are the gas and dust densities from the AMR runs with up to three refinement levels. The second and fourth rows are the relative differences between the AMR runs and the uniform grid runs, at a resolution matching the finest AMR refinement level of 3. The edges of the meshblocks in the AMR runs are also indicated by the black solid lines.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: The dust CDFs of the AB test (top) and the BA test (bottom), similar to Figure 10 of Benítez-Llambay et al. (2019). The left panels are the CDFs calculated by counting the number of cells whose dust density exceeds a certain threshold. The right panels are the CDFs calculated by additional weighting by dust density. The color-shaded regions are the temporal standard deviations based on many snapshots (from ﹩30\ {{\rm{\Omega }}}_{0}^{-1}﹩ to ﹩40\ {{\rm{\Omega }}}_{0}^{-1}﹩ for the AB test, and from ﹩600\ {{\rm{\Omega }}}_{0}^{-1}﹩ to ﹩800\ {{\rm{\Omega }}}_{0}^{-1}﹩ for the BA test). The initial dust densities are ρ d,0 = 1.0 and ρ d,0 = 0.2 for the AB and BA tests, respectively.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Dust densities of the AB test (top) and the BA test (bottom), with different spatial resolutions at ﹩t=40\ {{\rm{\Omega }}}_{0}^{-1}﹩ for the AB test and ﹩t=800\ {{\rm{\Omega }}}_{0}^{-1}﹩ for the BA test.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Snapshots of the dust densities in the SMR test of the AB test, with two levels of refinement. From top to bottom, and from left to right, the panels are at ﹩t=5\ {{\rm{\Omega }}}_{0}^{-1}﹩, ﹩10\ {{\rm{\Omega }}}_{0}^{-1}﹩, ﹩15\ {{\rm{\Omega }}}_{0}^{-1}﹩, and ﹩40\ {{\rm{\Omega }}}_{0}^{-1}﹩. The edges of each meshblock are marked by the solid black lines, and the meshblocks with different levels are labeled in the top left panel. Each meshblock contains 642 cells, and there are 8, 16, and 64 meshblocks at levels 0, 1, and 2.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Different snapshots of the dust densities (scaled by r −0.5) in the global unstratified BA test in cylindrical coordinates. From top to bottom, the panels are at ﹩t=100\ {{\rm{\Omega }}}_{0}^{-1}﹩, ﹩200\ {{\rm{\Omega }}}_{0}^{-1}﹩, ﹩400\ {{\rm{\Omega }}}_{0}^{-1}﹩, and ﹩800\ {{\rm{\Omega }}}_{0}^{-1}﹩, where Ω0 is the orbital frequency at r 0 ≡ 1. The strength of the gas pressure gradient is η = 0.0075. The top and right axes are scaled by η r 0, for reference. The effective resolution is the same as BA-5122 in Figure 6.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Normalized velocities (top) and densities (bottom) of the dusty wave tests, with one (left) and three (right) dust species, to be directly compared with Figure 5 of Benítez-Llambay et al. (2019). The gas profile is shown in red, while the other colors correspond to the dust species, with the insets showing the zoomed-in profiles across the shock. The analytical solutions are shown with the solid lines, while the numerical results are shown with the filled circles.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Code performance measured by CPU time per cell in micron seconds, shown as a function of the total number of species (gas and  N   d  species of dust).
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: An example of the N-pdf fitting process. Panel (a) shows the spatial distribution of the H2 column densities of the Mon OB1 GMC, while panel (b) shows the corresponding N-pdf overlaid with the fitted LN and LN+PL functions. The horizontal green dashed line marks the 10-counts level in the statistic bins, while the vertical green dashed line marks the reference detection limit of the H2 column density. The vertical blue dashed line shows the location of b  r . The model selected by BIC and the reduced chi-squared, χ  ν , of the LN and LN+PL fittings are shown in the figure. The meanings of the numbers to the right of χ  ν  are given in the text. The lower subpanel in panel (b) shows the distribution and histograms of the residuals of the two fittings. Panel (c) presents the corner map of the fitted parameters. The two vertical dashed lines, from left to right, in the marginalized distributions of the parameters are the 16% and 84% quantiles, respectively. The median values of μ, σ  s , b  r , and α are presented on top of the corresponding histograms. The differences between the two quantiles and the median values are adopted as 1σ errors of these parameters.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Spatial extents (top panel) and l–v extents (bottom panel) of the molecular clouds for which we have created N-pdfs, with each contour corresponding to an individual 13CO cloud. The background image in the top panel is the integrated intensity map of the 13CO emission, T mb, in the velocity range from −17 to 65 km s−1, while in the bottom panel we show the peak intensity map extracted along the direction of Galactic latitude. The black numbers and the red numbers in the top panel are the distances of the molecular clouds measured by Zucker et al. (2019) and Chen et al. (2020), respectively, while the effective extents of the corresponding molecular clouds are indicated with rectangles and circles. The yellow, magenta, and red dashed lines in the bottom panel show the locations of the Local, Perseus, and Outer spiral arms, respectively, which are derived from CO and HI observations (Weaver 1970; Cohen et al. 1980).
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: RGB map of the integrated intensity of the 12CO, 13CO, and C18O J = 1 − 0 emission, T mb. Red, green, and blue colors correspond to the integrated intensity of the 12CO emission in the velocity range from −17 to 65 km s−1, 13CO emission from −5 to 55 km s−1, and C18O emission from 0 to 33 km s−1, respectively. The units of the integrated intensities are K km s−1. The H II regions and H II region candidates from Anderson et al. (2014) are overlaid as pink circles and magenta circles, respectively, while the supernova remnants from Green (2019) are indicated by the green ellipses. The corresponding names of the H II regions in the Sharpless catalog (Sharpless 1959) are shown with pink letters, while the names of the supernova remnants are shown with green letters. Some well-known GMCs, like Rosette, Mon OB1, Canis Major, and Maddalena, are indicated with orange letters.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Examples of N-pdfs of the categories (a) LN, (b) UN (BIC proposing LN), and (c)UN (BIC proposing LN+PL), respectively. The horizontal and vertical green dashed lines and the reduced chi-squared have the same meaning as those in Figure 3. The names of the clouds are given in the upper right corner of panels (a)−(c). The fitted N-pdfs of the LN and the LN+PL models are indicated in red and blue, respectively. The lower panels in panels (a)−(c) present the residuals of the fittings for the N-pdfs. The zoom-in histograms in the lower panels show the distributions of the residuals.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons of M ⋆ and SFR distributions among our three fields. Sources are separated into three redshift bins with cuts listed in the panel titles. The upper right corner of each panel lists the median value of each distribution, and the numbers of sources plotted are shown in the same locations of the upper panels. The distributions are generally consistent among different fields.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Distribution of (a) skewness and (b) kurtosis of the column densities of the selected clouds.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Pie chart of the classification of N-pdfs into LN, LN+PL, and UN.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons of M ⋆ and SFR distributions among our three fields for X-ray AGNs. The legends list the median values of the distributions.
Paper: Binding Energy Evaluation Platform: A Database of Quantum Chemical Binding Energy Distributions for the Astrochemical Community
Authors: Giulia M. Bovolenta, Stefan Vogt-Geisse, Stefano Bovino, Tommaso Grassi
Figure caption: Sublimation radius on the midplane of a typical protoplanetary disk for different species obtained by employing the binding energies obtained in this work and compared with values available in the literature. For the sake of comparison, Ferrero et al. (2020) is the average between their upper and lower limits. See the references in Figure 5.
Paper: Binding Energy Evaluation Platform: A Database of Quantum Chemical Binding Energy Distributions for the Astrochemical Community
Authors: Giulia M. Bovolenta, Stefan Vogt-Geisse, Stefano Bovino, Tommaso Grassi
Figure caption: Binding energy distributions for Group D, ASW–X systems, using HF-3 c/MINIX geometries except for CO (M05/def2-TZVP). ZPVE correction has been included only for C2H2, see Section 3.2. The energy has been computed at ω-PBE/def2-TZVP level of theory for all species except CH4 (TPSSH/def2-TZVP). D3BJ dispersion correction has been applied to all DFT energies. See Figure 2’s caption for further details.
Paper: Binding Energy Evaluation Platform: A Database of Quantum Chemical Binding Energy Distributions for the Astrochemical Community
Authors: Giulia M. Bovolenta, Stefan Vogt-Geisse, Stefano Bovino, Tommaso Grassi
Figure caption: Box plot comparison between BE distributions computed in this work, considering only the main binding mode, and BEs present in previous theoretical studies (upper panels; Das et al. 2018; Ferrero et al. 2020; Sameera et al. 2021) and existing databases (lower panels: KIDA (Wakelam et al. 2017) and UMIST (McElroy et al. 2013)).
Paper: Binding Energy Evaluation Platform: A Database of Quantum Chemical Binding Energy Distributions for the Astrochemical Community
Authors: Giulia M. Bovolenta, Stefan Vogt-Geisse, Stefano Bovino, Tommaso Grassi
Figure caption: Box plot comparison between BE distributions presented in this work and He et al. (2016) experimental results. The box plot median corresponds to the mean of the main binding mode we identified.
Paper: Binding Energy Evaluation Platform: A Database of Quantum Chemical Binding Energy Distributions for the Astrochemical Community
Authors: Giulia M. Bovolenta, Stefan Vogt-Geisse, Stefano Bovino, Tommaso Grassi
Figure caption: Binding energy distributions computed using the best performing DFT functional from the energy benchmark for each molecule, with (blue) or without (orange) including D3BJ correction. Upper panel: Group D; lower panel: Group H.