adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Strongly Lensed Arcs in Galaxy Clusters with Transformers
Authors: Peng Jia, Ruiqi Sun, Nan Li, Yu Song, Runyu Ning, Hongyan Wei, Rui Luo
Figure caption: This figure shows (a) the original simulated image, (b) the image after grayscale transformation, and (c) the mask of lensed arcs. As we can see, the structure of this image is almost invisible in the original image. After grayscale transformation, we can easily see various galaxy structures and even directly observe the CGSL, which would be beneficial to development of the algorithm. We can see that the mask of lensed arcs ignores the foreground and shows the boundary of the CGSL, which is an arc in this image.
Paper: Detection of Strongly Lensed Arcs in Galaxy Clusters with Transformers
Authors: Peng Jia, Ruiqi Sun, Nan Li, Yu Song, Runyu Ning, Hongyan Wei, Rui Luo
Figure caption: The data flowchart of the DETR. It includes an encoder and decoder part that could learn features of extended targets for detection.
Paper: M33 Cepheids from CFHT/MegaCam Survey
Authors: Samuel Adair, Chien-Hsiu Lee, 見修 李
Figure caption: This plot shows the color–magnitude diagram of our visually examined periodic variables in the Wesenheit magnitude vs. r–i color. The red region indicates the instability strip where we identify 1622 Cepheids.
Paper: M33 Cepheids from CFHT/MegaCam Survey
Authors: Samuel Adair, Chien-Hsiu Lee, 見修 李
Figure caption: Wesenheit magnitude vs. log(P) of our 1622 Cepheids identified from the instability strip region. The red points are FO Cepheids classified by the amplitude ratio. The black line is a visual cut to identify the type II Cepheids.
Paper: M33 Cepheids from CFHT/MegaCam Survey
Authors: Samuel Adair, Chien-Hsiu Lee, 見修 李
Figure caption: Distributions of amplitude ratio vs. log (period) from r filter. The red line shows the boundary to separate the FO type Cepheids from the FM type and type II Cepheids, where the FO type Cepheids are located under the line.
Paper: M33 Cepheids from CFHT/MegaCam Survey
Authors: Samuel Adair, Chien-Hsiu Lee, 見修 李
Figure caption: The period–luminosity relation slopes we obtained plotted against the wavelength of the filter that corresponds to the slope (seen in magenta). The other lines are slopes from previous results.
Paper: M33 Cepheids from CFHT/MegaCam Survey
Authors: Samuel Adair, Chien-Hsiu Lee, 見修 李
Figure caption: An example of light curves from 30,308 with Fourier decomposition in the g, r, and i filters.
Paper: M33 Cepheids from CFHT/MegaCam Survey
Authors: Samuel Adair, Chien-Hsiu Lee, 見修 李
Figure caption: We show the residual of period–luminosity relationship and the best-fitted linear relation in the g, r, and i filters and for the extinction-free Wesenheit magnitudes.
Paper: M33 Cepheids from CFHT/MegaCam Survey
Authors: Samuel Adair, Chien-Hsiu Lee, 見修 李
Figure caption: We show the period–luminosity relationship and the best-fitted linear relation in the g, r, and i filters and for the extinction-free Wesenheit magnitudes.
Paper: Searching for Barium Stars from the LAMOST Spectra Using the Machine-learning Method: I
Authors: Fengyue Guo, Zhongding Cheng, Xiaoming Kong, Yatao Zhang, Yude Bu, Zhenping Yi, Bing Du, Jingchang Pan
Figure caption: Comparisons of the Sr abundances calculated by our work ([Sr/Fe]LGBM) and values determined from N19 ([Sr/Fe]N19). The yellow line represents that the predicted value is equal to the target value. The yellow dot represents the point at which ∣[Sr/Fe]4077 Å − [Sr/Fe]4215 Å∣ ≥ 0.5 in N19. The left shows the differences between [Sr/Fe]LGBM and [Sr/Fe]N19 in the prediction of 4077 Å (Sr II), and the right shows these differences in the prediction of 4215 Å (Sr II).
Paper: Searching for Barium Stars from the LAMOST Spectra Using the Machine-learning Method: I
Authors: Fengyue Guo, Zhongding Cheng, Xiaoming Kong, Yatao Zhang, Yude Bu, Zhenping Yi, Bing Du, Jingchang Pan
Figure caption: This is a process diagram of how LGBM constructs a decision tree for classification or prediction. The model discretizes the input features and establishes the histogram. Then according to these established histograms, features are selected as nodes to split and build a decision tree. Each decision tree would give a possible result, and the final result will be calculated according to the results of all the decision trees.
Paper: Searching for Barium Stars from the LAMOST Spectra Using the Machine-learning Method: I
Authors: Fengyue Guo, Zhongding Cheng, Xiaoming Kong, Yatao Zhang, Yude Bu, Zhenping Yi, Bing Du, Jingchang Pan
Figure caption: Local continuum spectra for Sr-only (J081757.34+062400.7) and Ba-only (J234340.04+283123.2) candidates randomly selected from the N19 data set. The zoom-in ranges of wavelengths are feature bands of 70 Å, and the light blue part is feature bands of 20 Å.
Paper: Searching for Barium Stars from the LAMOST Spectra Using the Machine-learning Method: I
Authors: Fengyue Guo, Zhongding Cheng, Xiaoming Kong, Yatao Zhang, Yude Bu, Zhenping Yi, Bing Du, Jingchang Pan
Figure caption: Distribution of barium stars adopted as positive samples in the plane of T eff–﹩\mathrm{log}g﹩, the colors indicate the [Fe/H] of stars. The triangle symbols indicate the barium star sample provided by L18, and the dot symbols indicate samples provided by N19.
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: The 2L1S model geometries of the best fit and possible solutions (right-side panels) of KMT-2021-BLG-2294. The left-side panels show the locations of the solutions in the (s,q) parameter space. The color scheme of the space is identical to Figure 3.
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: The APRX contours of KMT-2021-BLG-0119. Each color indicates the χ 2 difference between the best fit and chains. That is, ﹩{\rm{\Delta }}{\chi }^{2}\left(\equiv {\chi }_{\mathrm{chain}}^{2}-{\chi }_{\mathrm{best}-\mathrm{fit}}^{2}\right)={n}^{2}﹩, where n = 1 (red), 2 (yellow), 3 (green), 4 (light blue), 5 (blue), and 6 (purple).
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: The comparison of STD large ρ *, STD small ρ *, and ARPX models of KMT-2021-BLG-0119.
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: Light curve of KMT-2021-BLG-2294 with model curves and their residuals. The geometries of 2L1S models are presented in Figure 9.(The data used to create this figure are available.)
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: The color–magnitude diagrams of three events. The color and magnitudes of the KMTNet CMD (black dot) are aligned to the OGLE-III (gray dot) instrumental scales. The colored circles indicate the positions of RGC (red), source (blue/cyan), and blend (green/dark green) shown in Table 5.
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: The light curve of KMT-2021-BLG-0192 with STD model curves and residuals. The geometries of 2L1S models are presented in Figure 6.(The data used to create this figure are available.)
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: Geometries of best fit and possible solutions (s ± cases) caused by the ρ * degeneracy of KMT-2021-BLG-0192.
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: The (π E,E , π E,N ) distributions of APRX models of KMT-2021-BLG-0192. The color scheme is identical to Figure 3.
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: Cumulative Δχ 2 plots between STD and APRX models of KMT-2021-BLG-0119.
Paper: Unifying High- and Low-resolution Observations to Constrain the Dayside Atmosphere of KELT-20b/MASCARA-2b
Authors: David Kasper, Jacob L. Bean, Michael R. Line, Andreas Seifahrt, Madison T. Brady, Joshua Lothringer, Lorenzo Pino, Guangwei Fu, Stefan Pelletier, Julian Stürmer, Björn Benneke, Matteo Brogi, Jean-Michel Désert
Figure caption: Full retrieval results for KELT-20b. Red indicates the retrieval on just the MAROON-X data (both channels and both nights together), and blue indicates the joint retrieval with the HST/WFC3 and Spitzer/IRAC data. The numerical values above each histogram panel are the median and 68% confidence interval. Both data sets by themselves provide sufficient evidence for the inversion. Isothermal atmospheres (i.e., log(γ 1) = 0) are strongly ruled out by the MAROON-X data alone as there is a hard edge to the log(γ 1) in the MAROON-X Only data. There are no posterior samples below a log(γ 1) value of 0.27 and this minimum value is excluded at >99.974%.
Paper: Unifying High- and Low-resolution Observations to Constrain the Dayside Atmosphere of KELT-20b/MASCARA-2b
Authors: David Kasper, Jacob L. Bean, Michael R. Line, Andreas Seifahrt, Madison T. Brady, Joshua Lothringer, Lorenzo Pino, Guangwei Fu, Stefan Pelletier, Julian Stürmer, Björn Benneke, Matteo Brogi, Jean-Michel Désert
Figure caption: Pressure levels probed by the observations as dictated by the location of the τ = 2/3 level at each wavelength. As described in the text, the retrieval cannot precisely constrain the exact location of temperature with pressure due to the log(κ IR)-log g-metallicity degeneracy. Here, we show a representative surface from the 3× solar 1D-RC model. The approximate pressure levels probed by each data set by which species are indicated by the shaded boxes.
Paper: Unifying High- and Low-resolution Observations to Constrain the Dayside Atmosphere of KELT-20b/MASCARA-2b
Authors: David Kasper, Jacob L. Bean, Michael R. Line, Andreas Seifahrt, Madison T. Brady, Joshua Lothringer, Lorenzo Pino, Guangwei Fu, Stefan Pelletier, Julian Stürmer, Björn Benneke, Matteo Brogi, Jean-Michel Désert
Figure caption: Continuation of Figure 6.
Paper: The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Arthur D. Adams, Emily Rauscher
Figure caption: The uniform brightness curve and the first 10 eigencurves with uniform components added for our Warm Jupiter model, at a range of rotation rates with ψ LOS = 30°. Rotation rates span the scale from “slow” where the planet rotates a small fraction of a full rotation across eclipse (N tot < 1), to “fast” where the planet rotates through a considerable fraction of a full rotation. At the fastest rate the planet’s rotation period approaches the duration of ingress or egress (N i,e → 1). For reference, with our prototypical 10 day Warm Jupiter, N tot = 1 corresponds to ω rot/ω orb ≈ 71, and N i,e = 1 corresponds to ω rot/ω orb ≈ 432. One might notice that some eigencurves dip below the baseline where the planet is completely behind the star and contributes nothing to the observed flux. The eigencurves are initially generated from spherical harmonics, which each have zero net global brightness. Therefore, the eigencurves themselves start out as combinations of maps which each have zero net brightness. To “reconstitute” the eigencurves, we plot them here as additions on top of the uniform brightness curve. This allows for an eclipse curve composed of a single eigenmode to be unphysical, i.e.,  have net negative flux at some points.
Paper: The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Arthur D. Adams, Emily Rauscher
Figure caption: The first 10 modes of eigenmaps identified by PCA for the Warm Jupiter case with ψ sky = 60°. We show the maps in a Mollweide projection that shows all longitudes and latitudes. The reference hemisphere, which is the hemisphere that faces the observer at the midpoint phase of ingress, is centered in each projection and outlined with a dotted white circle. Green dashed contours represent the equator and ±45° latitude lines, with arrows indicating the direction of rotation. Rotation rates span the scale from “slow” where the planet rotates a small fraction of a full rotation across eclipse (N tot < 1), to “fast” where the planet rotates through a considerable fraction of a full rotation. At the fastest rate the planet’s rotation period approaches the duration of ingress or egress (N i,e → 1). For reference, with our prototypical 10 day Warm Jupiter, N tot = 1 corresponds to ω rot/ω orb ≈ 71, and N i,e = 1 corresponds to ω rot/ω orb ≈ 432.
Paper: The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Arthur D. Adams, Emily Rauscher
Figure caption: The uniform brightness curve and the first 10 eigencurves with uniform components added for our Warm Jupiter model, at a range of rotation rates with ψ LOS = 60°. Rotation rates span the scale from “slow,” where the planet rotates a small fraction of a full rotation across eclipse (N tot < 1), to “fast” where the planet rotates through a considerable fraction of a full rotation. At the fastest rate, the planet’s rotation period approaches the duration of ingress or egress (N i,e → 1). For reference, with our prototypical 10 day Warm Jupiter, N tot = 1 corresponds to ω rot/ω orb ≈ 71, and N i,e = 1 corresponds to ω rot/ω orb ≈ 432. One might notice that some eigencurves dip below the baseline where the planet is completely behind the star and contributes nothing to the observed flux. The eigencurves are initially generated from spherical harmonics, which each have zero net global brightness. Therefore, the eigencurves themselves start out as combinations of maps which each have zero net brightness. To “reconstitute” the eigencurves, we plot them here as additions on top of the uniform brightness curve. This allows for an eclipse curve composed of a single eigenmode to be unphysical, i.e.,  have net negative flux at some points.
Paper: The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Arthur D. Adams, Emily Rauscher
Figure caption: The uniform brightness curve and the first 10 eigencurves with uniform components added for our Warm Jupiter model, at a range of rotation rates with ψ sky = 60°. Rotation rates span the scale from “slow” where the planet rotates a small fraction of a full rotation across eclipse (N tot < 1), to “fast” where the planet rotates through a considerable fraction of a full rotation. At the fastest rate the planet’s rotation period approaches the duration of ingress or egress (N i,e → 1). For reference, with our prototypical 10 day Warm Jupiter, N tot = 1 corresponds to ω rot/ω orb ≈ 71, and N i,e = 1 corresponds to ω rot/ω orb ≈ 432. One might notice that some eigencurves dip below the baseline where the planet is completely behind the star and contributes nothing to the observed flux. The eigencurves are initially generated from spherical harmonics, which each have zero net global brightness. Therefore, the eigencurves themselves start out as combinations of maps which each have zero net brightness. To “reconstitute” the eigencurves, we plot them here as additions on top of the uniform brightness curve. This allows for an eclipse curve composed of a single eigenmode to be unphysical, i.e.,  have net negative flux at some points.
Paper: The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Arthur D. Adams, Emily Rauscher
Figure caption: The first 10 modes of eigenmaps identified by PCA for the Warm Jupiter case with ψ LOS = 60°. We show the maps in a Mollweide projection that shows all longitudes and latitudes. The reference hemisphere, which is the hemisphere that faces the observer at the midpoint phase of ingress, is centered in each projection and outlined with a dotted white circle. Green dashed contours represent the equator and ±45° latitude lines, with arrows indicating the direction of rotation. Rotation rates span the scale from “slow” where the planet rotates a small fraction of a full rotation across eclipse (N tot < 1), to “fast” where the planet rotates through a considerable fraction of a full rotation. At the fastest rate the planet’s rotation period approaches the duration of ingress or egress (N i,e → 1). For reference, with our prototypical 10 day Warm Jupiter, N tot = 1 corresponds to ω rot/ω orb ≈ 71, and N i,e = 1 corresponds to ω rot/ω orb ≈ 432.
Paper: The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Arthur D. Adams, Emily Rauscher
Figure caption: The first 10 modes of eigenmaps identified by PCA for the Warm Jupiter case with ψ LOS = 30°. We show the maps in a Mollweide projection that shows all longitudes and latitudes. The reference hemisphere, which is the hemisphere that faces the observer at the midpoint phase of ingress, is centered in each projection and outlined with a dotted white circle. Green dashed contours represent the equator and ±45° latitude lines, with arrows indicating the direction of rotation. Rotation rates span the scale from “slow” where the planet rotates a small fraction of a full rotation across eclipse (N tot < 1), to “fast” where the planet rotates through a considerable fraction of a full rotation. At the fastest rate the planet’s rotation period approaches the duration of ingress or egress (N i,e → 1). For reference, with our prototypical 10 day Warm Jupiter, N tot = 1 corresponds to ω rot/ω orb ≈ 71, and N i,e = 1 corresponds to ω rot/ω orb ≈ 432.