adsabs/AstroCLIMB huggingface dataset:
Paper: Estimating Microlensing Parameters from Observables and Stellar Isochrones with pyLIMASS
Authors: E. Bachelet, M. Hundertmark, S. Calchi Novati
Figure caption: Various distributions for six parameters of prime interest from the Roman sample. From top to bottom, the distribution of the parameters accuracy, normalized accuracy, uncertainties, and precision are displayed. The displayed range of parameters has been limited to the [10%, 90%] percentiles for plotting purposes.
Paper: Estimating Microlensing Parameters from Observables and Stellar Isochrones with pyLIMASS
Authors: E. Bachelet, M. Hundertmark, S. Calchi Novati
Figure caption: (Left) Simulated V vs. U distribution (top left) and the different reconstructed GM distributions with different numbers of Gaussian components. As more components are added to the model, the simulated distribution is reconstructed with more fidelity. (Right) BIC (plain blue) and AIC (dashed red) from a validation sample vs. the number of Gaussian components used in the GM model. Both metrics reach a plateau after ∼20 components, indicating potential overfitting afterward.
Paper: Estimating Microlensing Parameters from Observables and Stellar Isochrones with pyLIMASS
Authors: E. Bachelet, M. Hundertmark, S. Calchi Novati
Figure caption: Same as Figure 5, but for the microlensing event OGLE-2005-169Lb. The measurements of G06, Ba15, and Be15 are displayed in black, orange, and red, respectively.
Paper: Estimating Microlensing Parameters from Observables and Stellar Isochrones with pyLIMASS
Authors: E. Bachelet, M. Hundertmark, S. Calchi Novati
Figure caption: Summary of the proposed algorithm. The first step is to collect the observables and inject them in the GM object. Then, the observables distributions are fitted by the GM model to find the best hyperparameters θ  f . Finally, the likelihood function of the GM model is used in conjunction with user-defined priors, stellar isochrones, and microlensing parameters to explore the posterior probability p(P∣X).
Paper: Helium in Exoplanet Exospheres: Orbital and Stellar Influences
Authors: Vigneshwaran Krishnamurthy, Nicolas B. Cowan
Figure caption: Expected atmospheric mass loss vs. F XUV. The red circles and blue triangles are helium-observed planets, scaled similarly to those in Figure 3. The dashed horizontal black lines indicate the evaporation time (t eva) equaling stellar age for different efficiencies (ϵ), while the dashed blue line indicates the upper-limit efficiency of 6% (ε=0.06) for all the helium-detected planets. The accompanying histogram illustrates that planets with detected helium (blue) tend to prefer F XUV flux in the range of 103–105 erg s−1 cm−2.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: The 10 primary transits of TOI-1338 b in TESS observations. We binned the data into the 30 minutes cadence for clarity of display. Red lines are the synthetic light curves from the best-fit photodynamical model of TOI-1338 b (see Section 3). The residuals between the best-fit model and observation are shown below. Cadences affected by stray light flagged by SPOC are marked in blue. The photodynamical modeling used all primary transits except for the one in Sector 30.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: Dynamical stability (in terms of the displacement of MEGNO 〈Y〉 factor from 2) for three sets of photodynamical solutions from Table 2. Each solution is integrated for 50 kyr. The closer the 〈Y〉 is to 2, the more stable the system is in the integrated time. The stability analysis shows that the majority of esp-only solutions are stable while the other sets of solutions are more prone to be unstable within the integrated time, mainly due to the different eccentricity of TOI-1338 c from the different solutions (see Section 3.5).
Paper: Helium in Exoplanet Exospheres: Orbital and Stellar Influences
Authors: Vigneshwaran Krishnamurthy, Nicolas B. Cowan
Figure caption: Planet radius vs. age. The red circles and blue triangles are helium-observed planets, scaled as in Figure 3 and colored by their instantaneous F XUV/F Ly α . The accompanying histograms illustrate that older small planets do not have exosphere helium. Well-known planets are labeled.
Paper: Helium in Exoplanet Exospheres: Orbital and Stellar Influences
Authors: Vigneshwaran Krishnamurthy, Nicolas B. Cowan
Figure caption: The cumulative XUV flux (normalized with Earth) with the escape velocity of the planets. The cosmic shoreline (﹩{I}_{\mathrm{XUV}}\propto {v}_{\mathrm{esc}}^{4}﹩), shown in dashed black line, is reconstructed from Zahnle & Catling (2017). The planets below this line are expected to have retained their atmosphere, while those above are expected to have lost it. Some of the planets that exhibit exosphere helium despite lying above the cosmic shoreline are labeled.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: The comparisons between the fitted nine transit midtime posteriors derived from direct fitting (blue; Section 2.2), photodynamical model (red; Section 3.3), and GP correction (orange; see text in Section 3.4).
Paper: Helium in Exoplanet Exospheres: Orbital and Stellar Influences
Authors: Vigneshwaran Krishnamurthy, Nicolas B. Cowan
Figure caption: Planet radius vs. semimajor axis. The red circles and blue triangles are helium-observed planets, scaled as in Figure 3 and colored by their instantaneous F XUV/F Ly α . The accompanying histograms illustrate that small planets with detected helium (blue filled) are rarer compared to the giant planets.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: An example of the Target Pixel File of TOI-1338 (the zeroth target) in Sector 6 and the pipeline aperture (orange squares) from SPOC. The three closest nearby sources to TOI-1338 have angular separations of 54.″1, 58.″9, and 60.″7, respectively, all of them having ΔG > 2.7 mag. This figure is produced by tpfplotter (Aller et al. 2020).
Paper: A Contact Binary Misclassified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches
Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader
Figure caption: Comparison between the disentangled spectra of the components and the PHOENIX template model identified as the best match to the observed data. The secondary has been scaled for a light ratio such that l 2/l tot = 0.2. Noticeably, the disentangled spectra are very similar. The lower-left and right panels are cutouts around Hγ and Hβ, respectively. In all panels the normalized template has been shifted vertically by 0.3 for clarity.
Paper: A Contact Binary Misclassified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches
Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader
Figure caption:  χ 2 surface explored in the K 1, K 2 grid search, with the green dashed contour indicating 1σ. The semiamplitudes inferred from this exploration were K 1 = 54.7 ± 7.2 km s−1 and K 2 = 177 ± 21 km s−1. The K 1 inferred assuming the binary was single lined (﹩{34.8}_{-2.5}^{+2.6}﹩  km s−1) is discrepant with the value inferred using this technique at the 2σ  level.
Paper: A Contact Binary Misclassified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches
Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader
Figure caption: Comparison of disentangled spectra with the input spectrum around Hγ and Hβ for six different light contribution fractions. All secondary spectra are scaled by their light contribution except the bottom row, which is scaled assuming l 2/l tot = 0.05. These results suggest that we could reliably detect the presence of a luminous companion if it was contributing at least 20% of the total light of the system.
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: Blazhko side peak in SDSS 3478713: the top panel shows spectra around the first-overtone frequency f 1 for the r-band LC. After prewhitening the LC with f 1 and its three harmonics, we observed f 0 and the linear combinations of these frequencies. Again prewhitening the LC with them, we observed the Blazhko side peak f 1 − f  m  as shown in the bottom panel.
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: Period–period plot: x-axis is the fundamental period P 0 and the y-axis is the first-overtone period P 1. Colored symbols represent our stars in different passbands. The silver circles and crosses are OGLE’s classical and anomalous RRd stars from Soszyński et al. (2019), respectively. The silver triangles are RRd stars from Prudil et al. (2017). The black line shows the fitting from this work plotted for all the data sets.
Paper: A Contact Binary Misclassified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches
Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader
Figure caption: Top: phase-folded RVs overplotted with the best-fit Keplerian model. Bottom: residuals of model minus data as a function of orbital phase. The blue data point is the RV from the SOAR spectrum. The WiFeS RVs are in black.
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: Petersen diagram: period ratio P 1/P 0 observed in RRd stars are plotted against fundamental period P 0. The colored points are RRd stars from the current study in gri bands. The silver circles and crosses are OGLE-classified (Soszyński et al. 2019) classical and anomalous RRd stars, respectively. The silver triangles on the left bottom corner are RRd stars with short periods documented by Prudil et al. (2017).
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: Combined data sets: LCs of SDSS 2488976 in gri bands are shown as an example. The square points are SDSS data and the round points are ZTF data, respectively, with ∼10 yr gap in between. The gap is shrunken by the broken axes.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Observed data and the 2L1S wide (the solid black, yellow, cyan, and magenta lines) and 1L1S models (the dashed gray line) for KMT-2017-BLG-0849 and its bump-type anomaly. Different data sets are shown with different colors. The third panel shows the cumulative Δχ 2 distribution of models relative to the Wide A model.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Scatterplot of the hotter MCMC of Δξ vs. ﹩\mathrm{log}q﹩ of KMT-2017-BLG-0849, where Δξ is the offset between the center of the caustic and the intersection of the source trajectory and the planet–host axis. We find Δχ 2 barriers of ∼20 between the Wide A and Wide B models, ∼70 between the Wide A and Wide C models, and Δχ 2 ∼ 90 between the Wide B and Wide D models. The respectively color coding is purple, red, yellow, green, cyan, blue, magenta, and gray for Δχ 2 < (1, 4, 9, 16, 25, 36, 49, 64). We use black dots to symbolize Δχ 2 > 64.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Caustic-crossing geometries of KMT-2017-BLG-0849 models. In each panel, the red lines represent the caustics, the solid black line represents the source trajectory, the radius of the green dot represents the source radius, and the line with an arrow indicates the direction of the source motion.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Scatterplot of the hotter MCMC of Δξ vs. ﹩\mathrm{log}q﹩ for the wide models of OGLE-2017-BLG-0364. The distribution is derived by multiplying the photometric error bars by a factor of ﹩\sqrt{3}﹩ and then multiplying the resulting χ 2 by 3.0 for the plot. We find three local minima and their parameters are provided in Table 4. The symbols are similar to those in Figure 2.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Geometries of the KMT-2017-BLG-1057 and KMT-2017-BLG-2331 models. The symbols are similar to those in Figure 3.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: The observed data and the 2L1S and 1L2S models of OGLE-2017-BLG-0364.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Observed data and the 2L1S model for KMT-2017-BLG-1057. The symbols are similar to those in Figure 1.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: A close-up of the anomaly with the 2L1S close and 1L2S models of KMT-2017-BLG-0849. The symbols are similar to those in Figure 1.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Caustic-crossing geometries of OGLE-2017-BLG-0364.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Demonstration of the inadequacy of a simple LR model for NGC 3377. The left panel shows the average recovery fraction binned across the CMD, which highlights sharp cutoffs in color and magnitude as well as asymmetric complex behavior (highlighted with a red box). The right panel shows the predictions from a simple LR model which incorrectly smooths over both of these behaviors, leading to an overly broad completeness transition that is “tilted” in the CMD.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Predicted completeness/recovery fraction ﹩\hat{f}(m)﹩ from our best-fit NN models binned in magnitude (orange line) vs. the true completeness fraction f(m) from the ASTs (black line) for NGC 1275 (left) and NGC 3377 (right). The input magnitude distribution versus the recovered magnitude distribution is shown for reference in light gray and blue, respectively (i.e., the black line is the ratio of the blue and gray). The top panels show the behavior as a function of the (unknown) input magnitudes m in, which behave much like a logistic function (see Figure 11). The bottom panels show the behavior over the measured (known) magnitudes, which shows that the NNs can reproduce the same complex behavior highlighted in Figure 11.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Similar to Figure 15, but now plotting the predicted recovery fraction (orange) and the true recovery fraction (black) against all input parameters for NGC 1275 (top) and NGC 3377 (bottom), with the density of individual predictions shown in blue tones. This includes magnitude (far left), color (center left), sky noise (top center right), crowding (top far right), and background density (bottom right). These individual panels highlight that our NN model predictions behave sensibly in not only magnitude (declining steeply near the detection limit) but also color (declining outside of the main color range) and sky noise/crowding (declining in noisier and more crowded regions). They also highlight that mean trends can mask a lot of complex behavior that the NN model is able to successfully capture in the predicted individual recovery probabilities. Note that in the upper right panel, the vertical streaks of points are due to the quantized nature of the crowding variable for NGC 1275.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Change in the classification accuracy (recovered vs. lost with a decision boundary of ﹩\hat{p}({\bf{X}})=0.5﹩) for our NN models based on the size of the training set for the three AST scenarios explored in this work: ASTs for NGC 1275 drawn from a flat LF (red), for NGC 1275 drawn from a steep LF (purple), and for NGC 3377 drawn from a steep but truncated LF (blue). The accuracy for each scenario from a simple logistic regression model (as shown in Figure 12) is highlighted as horizontal dashed lines. The behavior of the four specific NN models shown in Figure 21 (below) is also highlighted. We find that only a few tens of thousands of ASTs are needed to capture the majority of the behavior seen in the data, although additional ASTs often still help to improve performance.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Dependence of stellar recovery over the measured CMD from the NGC 1275 ASTs. Top left: Individual input artificial stars classified by whether they were recovered (purple) or not (gray). Top right: Recovery fraction estimated in bins across the CMD (note that the color scale is nonlinear to emphasize the behavior closer to 1). Bottom left: As the top left panel, but now colored by the predicted recovery probability from our NN model. Bottom right: As the top right panel, but now colored by the predicted recovery fraction from our NN model. We find excellent agreement across the CMD, with the top/bottom right panels providing strong evidence that the NN predictions are able to smoothly interpolate over the true recovery fraction even in the presence of shot noise.