adsabs/AstroCLIMB huggingface dataset:
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: Filters used in this work plotted with respect to scaled spectra of components of the total sky. The earthshine spectrum is approximated by an E-490 solar spectrum following Giavalisco et al. (2002) and is shown in black. The zodiacal light spectrum is shown in gray and described in Section 3.1. Both spectra are shown with relatively “high” scaling from Giavalisco et al. (2002) Figure 2. Four HST filters that span the visible wavelength portion of the scattered earthshine and zodiacal light spectra are chosen for this study. A portion of the CERES shortwave filter from weather satellites, which extends to 5 μm, is shown in purple.
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: The location of fields used in this study in four selected filters. Field location is plotted in galactic coordinates, with the galactic plane from ±15° shown in shaded gray. The ecliptic plane is plotted in black. ACS F435W, F606W, and F814W are chosen due to the quantity of data available with existing archival sky surface brightness estimates over the entire sky. ACS F850LP is chosen because of data in the GOODS North fields, which are known to have high levels of earthshine contamination.
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: Total observed sky is plotted as a function of ecliptic latitude to illustrate the change in minimum sky backgrounds due to the planar distribution of zodiacal dust within the solar system. Scatter upwards from the minimum backgrounds shows some correlation with Sun altitude, indicating a likely increased contribution from earthshine stray light. However, the correlation with Sun altitude is not perfect, indicating other underlying parameters impact the observed sky. Single fields observed over a range of Sun altitudes and/or zodiacal levels are apparent as vertical stripes.
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: Earthshine observations by the CERES instruments are provided in 1° × 1° latitude and longitude grids with a temporal resolution of 3 hr on the illuminated side of Earth. This figure illustrates one image from CERES projected onto a map of Earth over Australia. Data used here are from the CERES shortwave filter covering 0.3–5 μm.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Condensate mixing ratio (mole fraction) of MnS, KCl, and Na2S clouds for a T7.0 brown dwarf with log g = 5.0. The mole fraction for each cloud type provides us with the vertical cloud structure of 2M0050–3322.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Normalized light curve for an edge-on 2M0050–3322 as predicted by GCMs (Tan & Showman 2021b). We show four consecutive periods of the light curve.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Edge-on map for 2M0050–3322 predicted by GCMs (Tan & Showman 2021b).
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Left: maximum flux J-band spectrum for 2M0050-332 (orange), and minimum J-band spectrum for 2M0050-332 (blue). Right: maximum flux H-band spectrum for 2M0050-332 (orange), and minimum H-band spectrum for 2M0050–3322 (blue).
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Visual representation of the different cloud layers in the atmosphere of 2M0050–3322 showing the pressure levels at which each of them condensates, and the top of the atmosphere for reference. We show the traced pressure levels by the different near-infrared wavelengths in our MOSFIRE J- and H-band spectra.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Left: ratio of the maximum divided by the minimum spectra of 2M0050–3322 in the J band. Right: ratio of the maximum divided by the minimum spectra of 2M0050–3322 in the H band.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Sensitivity plot for Keck 1/MOSFIRE. MOSFIRE would be able to measure the predicted light curve for a T7.0 brown dwarf similar to 2M0050–3322 50%–60% of the time with the observation strategy followed in this work.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Correlation between the imaging J-band target’s noncorrected light curve and the noncorrected calibration stars’ light curves.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Correlation between the imaging J-band target’s corrected light curve and the corrected calibration stars’ light curves.
Paper: MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary
Authors: E. Bachelet, Y. Tsapras, Andrew Gould, R. A. Street, David P. Bennett, M. P. G. Hundertmark, V. Bozza, D. M. Bramich, A. Cassan, M. Dominik, K. Horne, S. Mao, A. Saha, J. Wambsganss, Weicheng Zang, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Stela Ishitani Silva, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Andrzej Udalski, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Left: observations and 2L1S-P model (u 0 ≤ 0 and no orbital motion) centered at the peak magnification. Right: the corresponding model geometry, where red lines represent the caustics, dashed lines represent the critical curve, and the blue line is the source trajectory. The north and east vectors are also represented. The lens center of mass is fixed at (0, 0).(The data used to create this figure are available.)
Paper: MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary
Authors: E. Bachelet, Y. Tsapras, Andrew Gould, R. A. Street, David P. Bennett, M. P. G. Hundertmark, V. Bozza, D. M. Bramich, A. Cassan, M. Dominik, K. Horne, S. Mao, A. Saha, J. Wambsganss, Weicheng Zang, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Stela Ishitani Silva, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Andrzej Udalski, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Color composite of g, r, i reference images of the ROME survey. The inset is 2′ × 2′ zoom-in around MOA-2019-BLG-008. The NGC6451 cluster center is visible, while some of the stars of the Basel5 cluster are also visible (its center is on the left, outside of the image; see Kharchenko et al. 2013). As indicated by the white cross, north is up and east is to the left.
Paper: MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary
Authors: E. Bachelet, Y. Tsapras, Andrew Gould, R. A. Street, David P. Bennett, M. P. G. Hundertmark, V. Bozza, D. M. Bramich, A. Cassan, M. Dominik, K. Horne, S. Mao, A. Saha, J. Wambsganss, Weicheng Zang, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Stela Ishitani Silva, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Andrzej Udalski, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: OGLE and MOA long-term baseline trends.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Recovery of HIP 67522b. Upper panel: PSF flux (in dark gray) and penalized spline trend (in blue). Lower panel: Detrended light curve (PSF flux divided by the trend). The multi-transit signature (in red) can be clearly seen. Right: Upper panel shows phase-folded light curve of HIP 67522b (gray data points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Comparison of phase-folded light curve of HIP 67522b using two-minute cadence data (orange) and 30-minute cadence data (black). Right: Upper panel shows phase-folded light curve of HIP 67522b using two-minute cadence (dark gray points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Recovery of TOI 451 d. Upper panel: PSF flux (in dark gray) and penalized spline trend (in blue). Lower panel: Detrended light curve (PSF flux divided by the trend). The multi-transit signature (in red) can be clearly seen. Right: Upper panel shows phase-folded light curve of TOI 451 d (gray data points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Schematic of pterodactyls. *Before passing to triceratops, we conducted a centroid test whenever the Target Pixel File (TPF) was available on MAST.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Equatorial locations of stars in selected clusters used in this study.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Skye Excess Metric for Sectors 3, 10, 11, and 12, respectively. Red dashed line depicts the 3σ threshold.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Left: cartoon schematic illustrating how increasing V ⊥ results in increased R peri. The red dashed circle is the cluster R 200. The cyan filled circle is an infaller halo at the moment of entering the cluster. The blue arrow labeled “V ⊥” shows the perpendicular component of the halo’s orbital velocity. Right: R peri vs. V ⊥ plot (normalized axes) for the full sample (teal) and for cluster-mass hosts only (red). There is a clear trend, which is independent of host mass. The smooth black curve is an approximate fit to the trend (﹩{R}_{{\rm{peri}}}=0.27{V}_{\perp }^{3}+0.40\,{V}_{\perp }﹩), which we apply in Section 3.3.2. The scatter about the trend is small. The black contour contains 95% of the “All” sample, meaning most objects are found within ±0.1 of the fit line.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Plots illustrating the relation between R peri and V ⊥. The main panel is R peri vs. V ⊥, and the contour encompasses 68% of the data points. The upper histogram shows the normalized V ⊥ distribution (a vertical integration of the R peri vs. V ⊥ plot) and the side panel shows the normalized R peri distribution (a horizontal integration of the R peri vs. V ⊥ plot). We subsample by various parameters: in the upper left we split by host mass, upper right by mass of the infaller halo, bottom left by the mass ratio of the infaller to the host, and lower right by the time of infall (see legend for line colors). A short line on the histogram axis indicates the median value for each distribution.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Age of the universe in gigayears at the time of infall (t inf) vs. mass ratio plots. Top left: pixels are colored by the median R peri of halos that fall within them. Black contours indicate 100, 200, 300, and 400 objects in a pixel. Top right: pixels are colored by median V ⊥. Bottom left: pixels are colored by the R peri value that would be expected if dynamical friction were heavily suppressed (see text for details). R peri values are based only on the median V ⊥ value, using the fit line from the right panel of Figure 4 (see text for details). Bottom right: pixel-by-pixel subtraction of the upper-left and lower-left panels to show how much the measured R peri values reduce compared to those when dynamical friction is heavily suppressed in the sample. Pixels are blank if they contain fewer than 20 halos.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Tidal mass loss of infaller halos with small pericentres (R peri < 0.2;  left panel) and large pericentres (R peri > 0.5;  center panel). The y-axis is the halo mass of the infaller normalized by its mass at the time of infall. The x-axis is time since pericentre passage in gigayears, with negative x-values being before the infaller reaches pericentre. Halos with small R peri values suffer stronger and more rapid tidal mass loss. Right panel: orbital velocity at pericentre normalized by host velocity dispersion (V peri) vs. R peri. Halos with smaller pericentres tend to have higher normalized pericentre velocities.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Four representative examples of clusters (shown top to bottom; labeled “Cluster A–D”). A deep-pink sphere shows the location and R 200 of the clusters at z = 0. Blue lines show the trajectories of infaller halos, colored darker blue according to their proximity to the cluster. The left column (labeled “All Tracks”) shows the tracks of all the infallers and highlights the filamentary connections of each cluster. The middle and right columns (labeled “Lo V ⊥” and “Hi V ⊥,” respectively) presents the infaller tracks of low- and high-V ⊥ subsamples, with equal numbers shown for a fair visual comparison.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Left: cluster-to-cluster variations in the R peri vs. V perp plot. Magenta symbols are the median R peri and V ⊥ values for the first infallers into each individual cluster (i.e., one symbol per cluster). Teal symbols are all the individual first infallers into clusters (not split by cluster host). Right: mass evolution of infallers, normalized by mass at infall time for the six clusters with the highest median V ⊥ value (red line; labeled “V ⊥  <  0.6”), and the six clusters with the lowest median V ⊥ value (blue line; labeled “V ⊥  >  0.84”). The bold line is the median mass evolution track, and shading shows the standard deviation.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: The main R peri distribution (teal filled) for all the infaller sample. The lines are from Wetzel (2011). The blue curve is the result when the cluster potential was treated as a point mass. The magenta curve is the result when an analytical extended host potential was used. The small vertical lines along the x-axis indicate the median value of the three distributions in the legend.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Evolution of infaller halo masses (normalized by halo mass at infall time) plotted against time since pericentre passage in gigayears. Halos with higher mass ratios (﹩{M}_{{\rm{rat}}}={M}_{inf}﹩/M host) suffer more rapid tidal mass loss near pericentre, due to the dependency of V ⊥ on mass ratio, combined with dynamical friction for objects with M rat > 0.1.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption:  R peri distributions of all isolated infallers (gray histograms, same in all the panels for comparison), and infallers that are in a group when they enter the cluster. Left to right, the panels show substructures that have a low, medium, and high mass ratio with the cluster. The small vertical lines on the x-axes indicate the medians of the distributions.
Paper: Analytic Light Curve for Mutual Transits of Two Bodies Across a Limb-darkened Star
Authors: Tyler A. Gordon, Eric Agol
Figure caption: Posterior plots for the impact parameter of each planet vs. the mutual inclination. Left: joint posterior distribution for the impact parameters of planets b and d with darker colors indicating higher probability. The distribution is multimodal, which presents a difficulty for MCMC methods. Dashed lines represent the line along which the impact parameters for both planets are equal, and the error bars represent the impact parameters found by the Kepler team and for each of the visits (V1 and V2) with the Hubble Space Telescope from Libby-Roberts et al. (2020). This figure can be compared to Figure 4 in Masuda (2014). We have made no attempt to account for the possible failure of the MCMC chains to fully explore all of the modes. Therefore the apparent densities of each mode relative to the others should not be interpreted as a preference for one mode over another. We merely intend to show that multiple modes exist and to demonstrate the use of our model with an MCMC sampler. Upper right: kernel density estimate of the posterior for the mutual inclination between planets b and d marginalized over all other parameters. The dashed line is the estimate from Masuda (2014) and the purple shaded region shows the 1σ confidence interval from that paper. The green shaded region represents the 1σ confidence interval from this work. We find agreement between our determination of the mutual inclination and the value found by M14, with the exception that our posterior admits a wider range of mutual inclination angles than was found by M14. Again, we caution that the multimodality of the posterior presents an issue for our MCMC analysis and thus the relative heights of the modes in this plot may not represent the actual relative probabilities of true transit parameters having been drawn from each mode.