adsabs/AstroCLIMB huggingface dataset:
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Velocity dispersion as a function of effective radius. CO and its isotopic clumps with αvir > 2 are points labeled with black circles and linearly fitted with a black dashed line, while clumps with αvir ≤ 2 are unlabeled points and linearly fitted with a black dotted–dashed line. The cyan solid line is the referenced line of the Larson relation σ ∝ R0.5.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Variation of σv/R0.5 with surface density Σ. The three black dashed lines mark the positions at which the virial coefficients αvir are 2, 1, and 0.4, respectively.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Virial parameter vs. clump mass. The two horizontal lines represent αvir = 2 and αvir = 0.4. The three dashed lines represent the linear fit to the corresponding clumps.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: The 12CO, 13CO, C18O, and HCO+ line profiles toward the infall candidates. The red dashed line indicates the center velocity of the C18O line obtained by Gaussian fitting. Clump numbers indicate the serial numbers of the C18O clumps; see Table A3.
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: Illustration of GP augmentation applied to simulated light curves. Each band displays the mean GP flux prediction as a solid line, with a shaded contour representing one-standard-deviation uncertainty in the flux prediction. The middle column presents the initial fit. The left column shows the augmented data for a “low-redshift” scenario (achieved by reducing the wavelength parameter in the GP model). The right column illustrates the augmented data for a “higher redshift” case (accomplished by increasing the wavelength parameter in the GP model). The top row demonstrates the augmentation solely by adjusting the wavelength parameter, whereas the bottom row reflects adjustments made after considering the distance difference. For ease of comparison, each panel includes error bars that align with the original light curve. (Note: Since these scenarios do not precisely reflect real redshifts, we use quotation marks around lower and higher “z” to indicate this distinction from actual redshift values.)
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: Example of GP real-time interpolation applied to simulated light curves. A solid vertical line divides the light curve into segments for early classification (left) and full classification (right). Each band’s mean GP flux prediction is shown as a solid line, surrounded by a shaded contour indicating the one-standard-deviation uncertainty in the flux prediction. The GP model produces relatively consistent interpolation but performs poorly in forecasting future data points.
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: The semisupervised classification architecture comprises two distinct pathways. The unsupervised component (denoted as the orange pathway) is purposed to discern the low-dimensional distribution inherent in the data. It functions by reconstructing the original full light curve from its partial counterpart, thereby establishing a linkage between the partial and full light curves. Meanwhile, the supervised component (depicted in green) is tasked with generating the predicted probability of classification for each class. Both pathways are concurrently trained and they utilize a shared encoder module, represented in gray.
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: Illustrations of well sampled simulated light curves in expected WFST cadence. From left to right, the light curves represent the following classes: AGN, KN, and SNIa (the first line); SNIa-91bg, SNIax, and SNIbc (the second line); SNII, SLSN, and TDE (the third line).
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: Redshift distributions of three data sets representing the following transient classes: KN, SLSN, SNIa, SNIa-91bg, SNIax, SNIbc, SNII, and TDE.
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: Comparison of confusion matrices (normalized over true labels) between the benchmark model (right panel) and our framework (left panel).
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: The detailed structure of the benchmark model (left panel) and the encoder module of our framework (right panel).
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: Decoder module of our framework.
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: The latent space analysis reveals distinct patterns in model performance: the left panel highlights misclassified data points within the context of the full test set, while the right panel visualizes reconstructed light curves sampled from diverse regions of the latent space, demonstrating its structural heterogeneity.
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: Latent space distribution. The left panel is the different distribution of the Cart and test data set; The right panel is the different distribution of the train data set and the test data set.
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: The latent space representation of the early light curve in the test data set. The two axes are the latent features learned by the unsupervised path.
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: Comparison of ROC curve and corresponding AUC between the benchmark model (right panel) and our framework (left panel).
Paper: Real-time Light Curve Classification Framework for the Wide Field Survey Telescope Using Modified Semisupervised Variational Autoencoder
Authors: Yongling Tang, 永灵 唐, Lulu Fan, 璐璐 范, Zhen Wan, 振 宛, Yating Liu, 雅婷 刘, Yan Lu, 岩 陆
Figure caption: The macro precision, recall, and F1 scores of our framework are compared with those of the benchmark model across different phases of the light curve.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Comparison of N-bearing species relative to HNCO in low- and high-mass protostars. The abundances are compiled from the literature as follows: Sgr B2 (N) from A. Belloche et al. (2013), 101899 and 126348 from P. Nazari et al. (2022), B1-c and S68N from P. Nazari et al. (2021), and IRAS 16293 A and B from H. Calcutt et al. (2018), S. Manigand et al. (2020), N. F. W. Ligterink et al. (2017), and S. Zeng et al. (2019). The red downward arrow indicates the upper limit due to tentative detection. For ﹩{{\rm{CH}}}_{3}{{\rm{CH}}}_{2}{\rm{CN}}﹩, ﹩{{\rm{CH}}}_{{\rm{2}}}{\rm{CHCN}}﹩, and NH2CHO in IRAS 16293 A and B, the column density of HNCO is adopted from S. Manigand et al. (2020). For ﹩{{\rm{HOCH}}}_{2}{\rm{CN}}﹩ in IRAS 16293 B, the column density of HNCO is adopted from N. F. W. Ligterink et al. (2017).
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Detected COMs toward the disk of V883 Ori. The horizontal dotted line in gray represents the noise level (1σ) in the data, the black line represents the data, and different colors represent the different species identified in this study, the dashed lines to facilitate distinguishing similar colors. The gaps between the SPWs are excluded from the fit and shaded in lavender.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Continuation of Figure 8.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: In black are the observed spectra, and in blue is the cumulative model adding the contribution from each molecule. The gaps between the SPWs are excluded from the fit and shaded in lavender.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Posterior distributions for the excitation temperature Tex and the column density Ntot for various COMs.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Continuation of Figure 16.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Continuation of Figure 22.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Predicted emission of the molecule glycolaldehyde at Tex = 150 K and Ntot = 4.0 × 1016 cm−2.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Continuation of Figure 26.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Kiel diagram of queried giants from APOGEE DR17. Hexagonal histograms represent the ∼6.5 × 105 unique systems in the full catalog. The marginal distributions on the top and right of the figure depict the full sampling of Teff and log g for DR17. Our initial sample of log g < 3.5 dex and ﹩v\sin i﹩ > 0 km s−1 is plotted as a 2D histogram with 100 bins per axis going from blue to yellow with increasing bin count. The gray background highlights the Teff range where we remove stars not consistent with the giant branch. Partial evolutionary tracks with equal mass spacing are given from 1 M⊙ to 2.5 M⊙.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Critical period over projected rotational period vs. projected rotational period. To help determine the Pcrit of individual systems in the figure contour lines of constant Pcrit are drawn for reference. The stars in the red box are considered to be critically rotating and categorized as breakup giants. The triangle marker highlights BU giant 2M12072913+0036598, which has E0(NUV) = –8.45 and is classified as a semiregular variable.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Infrared (top) and optical (bottom) CMD diagrams used to select subsubgiants. In both panels the histogram is the DR17 catalog and the red dashed line is a 14 Gyr, [M/H] = 0.5 isochrone. The gold circular points are the stars in our sample that are to the red of the isochrone in both CMDs and classified as SSGs. The blue square points are stars redder than the isochrone, but are consistent with the single/binary main sequence so we don’t classify them as SSGs.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: NUV − J vs. J − Ks plot of our sample, colored by [M/H]. A grid of Castelli–Kurucz model atmospheres displayed as triangle markers to show large changes in NUV − J due to changes in [M/H]. The K. Findeisen & L. Hillenbrand (2010) locus is plotted as a black line.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Comparison of ASPCAP ﹩v\sin i﹩ and literature orbital period and eccentricity values. Circles are SB1 solutions from the Joker VAC and triangles and squares are SB1 solutions and astrometric solutions from Gaia DR3, respectively. The X markers are subsubgiants. All markers are colored by Eζ(NUV) divided into three colors with breaks at 0 and −1. The gray backgrounds highlight regions where ﹩v\sin i﹩ < 10 km s−1. In the top left panel a maximum eccentricity curve using a period of 15 days is shown for reference. A key is given in the top right panel to help identify different sources for orbit solutions and giants in our defined synchronized and Sub-subgiant categories. The dashed line in the bottom left panel is a synchronization line assuming a radius of 4 R⊙ and inclination of 90°. The vertical dotted line also in the bottom left panel marks an orbital period of 50 days, which empirically bounds the synchronized giants with ﹩v\sin i﹩ > 10 km s−1. Lastly, in the bottom right panel the dashed line is a one-to-one line with dotted lines shown for factors of 2.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Eζ(NUV) vs. ﹩v\sin i﹩ for giant categories defined in Section 3.2. Color scheme for categories is Single, Binary, Synchronized, SSG, and BU. The BU and SSG categories are given as open circle so overlap with other categories can be seen. Dashed line is rotation activity relation as defined in Equation (6).
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: NUV − J vs. J − Ks plot of our sample, with BU giants colored red. The K. Findeisen & L. Hillenbrand (2010) locus is plotted as a black line. VSX designations (C. L. Watson et al. 2006) are given for the three high-infrared excess systems and defined as the following. SRD = semiregular variable, L = slow irregular variable, TTS = T Tauri star.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Quotient of stellar radius by Roche limit (R*/RL) at varying mass ratios (q) for BU giants. Gray background highlight region where RLOF occurs. X markers indicate a mass equal to the Chandrasekhar limit for the secondary.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Top panel: difference between D. Dixon et al. (2020)-defined NUV excess E0(NUV) and NUV excess defined from fitted CK atmospheres ES(NUV) vs. [M/H]. E0(NUV) minus the linear regression line ζ([M/H]) yields Eζ(NUV) which serves as an estimate for ES(NUV). Bottom panel: histograms comparing the E0(NUV) − ES(NUV) and Eζ(NUV) − ES(NUV) distributions.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Cumulative distribution functions for ﹩v\sin i﹩, Eζ(NUV) and Gaia activity index (α) in units of sample fraction for giant categories defined in Section 3.2. Color scheme is identical to Figure 8.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: Comparison between our SED estimated radii and radii calculated from D. J. Stevens et al. (2017) color-derived angular diameters. A one-to-one line and a robust linear fit line are depicted as the dashed green line and dashed cyan line, respectively.
Paper: Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Authors: Don Dixon, Keivan G. Stassun, Robert D. Mathieu, Jamie Tayar, Lyra Cao
Figure caption: E0(NUV) vs. white-dwarf companion Teff for simulated white-dwarf giant binaries. Each line represents a 5000 K giant of varying size and the white-dwarf size is set to 1 R⊕.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Galactic Cartesian velocities of SYNTHPOP simulated stars in the (l, b) = (0∘, 0∘) field belonging to the 7–10 Gyr thin disk subpopulation. We limit the figure to a single population for clarity, as each population has its own velocity dispersions and asymmetric drift. The ∣V∣ panel shows the absolute velocity in the direction of Galactic rotation, where true V values are negative for the far disk. The U panel shows the velocity component within the Galactic plane and perpendicular to the direction of Galactic rotation, where the velocity dispersion has a gradient. Finally, the W panel shows velocity perpendicular to the Galactic plane. See Appendix A for a full description of the coordinate system.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Comparison between input distributions (thick shadowed line) and distributions of generated stars (stepped line) for initial mass functions (left), age (center), and metallicity (right). For IMFs, we show the Chabrier (red), Kroupa (green), and an arbitrary, unphysical piecewise power law (blue) distributions. For age, we show two different uniform distributions (red, green) and a Gaussian (blue). For metallicity, we show two single Gaussian distributions (red, blue), and a double Gaussian (green). In all cases, the generated stars follow the input distributions.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Stellar density for the (left to right) thin disk, thick disk, halo, and bulge profiles used in the Besançon (A. C. Robin et al. 2003) Model. Each panel shows the stars produced (stepped line) and the specified distribution (shadowed line) along four different lines of sight. Large scatter at small and large distances are due to small volumes and/or low densities resulting in very small numbers of stars generated. Note that the bulge population is defined by a number density rather than mass density. Two of the fields point too far from the Galactic center to contain any bulge stars.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Comparison between the color–magnitude diagram generated by SYNTHPOP (dots) and MIST web interpolator isochrones (thick shadow) for three different single-age, single-metallicity populations. B and V are shown in absolute Vega magnitudes in the Bessell filter system.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: The structure of a SYNTHPOP model’s definition. Two .synthpop_conf Configuration json files control the model settings. In these, a Model directory is selected, which contains some number of .popjson json files specifying the Populations.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: Cumulative montly submission rate to the NEOCP averaged over 2019–2023 as a function of lunation. Illustrations of the moon as a function of lunation are shown along the top axis.