adsabs/AstroCLIMB huggingface dataset:
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: Best-fit 2L2S light curve for MB10328 using constraints from the Keck and HST high-resolution follow-up data. The middle panel is a close-up of the upper pannel, indicating the planetary anomally. The lower plot shows the residuals. The parameters are described in Section 4 and Table 4.
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: Target star identification in Keck and HST using MOA survey data. Target is identified by individual centroid positions in green, with the red box indicating the 1σ error of the scatter.
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: Best-fit MCMC contours (68.3%, 99.5%, 99.7%) of the X and Y pixel positions of the source (red) and lens (cyan). The contours are overplotted on the stacked Keck Narrow image (left) and the one-star residual image (right).
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: Example of a PSF star and its residual from each night of observation that is used to build an empirical PSF model.
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: (Upper) Template spectra used for computing the CCF shown with perturbations from removing individual molecules in the radiative transfer calculation. (Middle) Molecular contribution functions calculated using picaso.jdi.get_contribution. The curve shows the pressure layer where the optical depth per species is approximately unity. (Lower) A visualization where the absorption features are shown per species using colored banding with variable opacity to denote deeper absorption.
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: Detection of the planet 51 Eridani b from moderate resolution spectroscopic observations with JWST/NIRSpec. Top: visualization of the point cloud in sky coordinates (left) and IFU-aligned coordinates (center). In the background at half opacity is the best-fit synthetic WebbPSF from the coordinate correction/centroiding step. In the foreground at full opacity is an interpolation of the continuum-preserving point cloud for the combined planet- and speckle-side observations. The “slit” appears ∼0﹩\mathop{.}\limits^{\unicode{x02033}}﹩05 wide in this figure because that is the scale subtended by the subpixel dither pattern, not the full 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 width of the physical slit aperture. (Right) A demonstration of the offset in IFU Y between the peak intensity of the stellar PSF and the location of the peak of the cross-correlation function, indicating the signal is not a result of amplified stellar noise. Bottom: cross-correlation based detection maps in the IFU Y and planetary radial velocity phase space. (Left) Joint detection map for all planet-side data sets, (right) joint detection map for all speckle-side data sets. The white dashed lines indicate the expected position and velocity of the target.
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: Searching for individual molecules in the atmosphere of 51 Eridani b with “leave one molecule out” cross-correlations. (Top) Cross-correlation functions computed on all four templates showing the effect of removing certain molecules from the atmospheric model across the entire wavelength range. (Middle) Restricted wavelength test in the region of CH4 dominance. (Bottom) Restricted wavelength test in the region of CO dominance.
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: (Upper) Four primary parameters of the Diamondback evolutionary model grid from left to right: luminosity, effective temperature, surface gravity, and radius as a function of age (x-axis) and mass (color). Mass ranges from 0.0005 to 0.08 M⊙ going from dark blue to gold or equivalently 0.524 Mjup to 84 Mjup. (Lower) On the left, the assumption on mass and age for the prior distribution, and on the right the interpolation of that distribution onto the four output parameters of the distribution, which forms the prior on effective temperature, surface gravity, and radius. The prior is assumed flat over the entire grid on all of the other atmospheric parameters.
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: Best-fit model spectra from the first iteration of computing likelihood with no subgrid interpolation or NIRSpec covariance shown in black at R = 100 and in gray at R = 2700 in the upper panel and continuum-subtracted in black at R = 2700 in the two lower panels. (Upper) GPI IFS spectra in bands J, H, K1, and K2, KECK/NIRC2 Lp and Ms photometry, and JWST/NIRCam F410M, F430M, and F460M photometry in red. (Middle) NIRSpec continuum-normalized spectra from slit A1 and slit A2 (lower).
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: Triangle shaped posterior probability visualization for the second iteration of the atmospheric model likelihood calculation. A discrete colormap is used in the covariance plots with edges located at ﹩\mathrm{log}{ \mathcal L }\in [0,-2,-4,-6]﹩ so that the different colored regions in the diagram can be considered to be 1σ, 2σ, and 3σ regions. The mode and 1σ asymmetric limits of the single parameter marginal distributions are plotted with red lines and printed correspondingly in each title.
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: Single parameter marginalized posterior distributions for different combinations of data sets included the calculation of the likelihood. There are seven possible combinations of these data sets. From top to bottom: all data sets, just GPI spectroscopy, just photometry, just NIRSpec spectroscopy, GPI spectroscopy and all photometry, GPI spectroscopy and NIRSpec spectroscopy, and all photometry and NIRSpec spectroscopy. The ﹩\hat{e}﹩ posterior is missing from the subsets that do not include NIRSpec.
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: Artificial planetary signal injected into the continuum-subtracted point cloud for the speckle-side data set is recovered in the CCF at a similar level of significance to the detection of 51 Eridani b in the planet-side data set.
Paper: Direct Spectroscopy of 51 Eridani b with JWST NIRSpec
Authors: Alexander Madurowicz, Jean-Baptiste Ruffio, Bruce Macintosh, Marshall Perrin, Quinn M. Konopacky, Aneesh Baburaj, Kielan Hoch
Figure caption: Correlation profile Ψ for both data sets (slit a1 and a2) on detector NRS1 (upper) and NRS2 (lower) as a function of Δ pixels along the wavelength dimension.
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption:  ﹩{\rm{\Delta }}\mathrm{log}\,(\mathrm{Age})﹩ as a function of APO-K2 log (age) (top) and [C/N]-based log (age) (bottom). The gray gradient shaded regions represent bins of field stars; darker bins imply more stars. The red squares, green circles, and blue triangles represent cluster member stars common to both samples NGC 2682 (M 67), NGC 6791, and NGC 6819, respectively. The vertical dashed lines are the T. Cantat-Gaudin et al. (2020)–determined ages for each cluster, and the respective shaded regions show the error in cluster age. The horizontal gray dashed line is where ﹩{\rm{\Delta }}\mathrm{log}\,(\mathrm{Age})=0﹩, with the surrounding gray region representing a delta of −0.1 and +0.1. The vertical gray dotted line shows the accepted age of the Universe. Median representative error bars are shown in each panel. Clusters member older than the Universe, highlighted with a purple square, were found to be in a binary system (A. M. Price-Whelan et al. 2020).
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption:  ﹩{\rm{\Delta }}\mathrm{log}\,(\mathrm{Age})﹩ as a function of APOKASC3 log (age) (top) and [C/N]-based log (age) (bottom). The gray gradient shaded regions represent bins of field stars; darker bins imply more stars. The green circles and blue triangles represent cluster member stars common to both samples NGC 6791 and NGC 6819, respectively. The vertical dashed lines are the T. Cantat-Gaudin et al. (2020)–determined ages for each cluster, and the respective shaded regions show the error in cluster age. The horizontal gray dashed line is where ﹩{\rm{\Delta }}\mathrm{log}\,(\mathrm{Age})=0﹩, with the surrounding gray region representing a delta of −0.1 and +0.1. The vertical gray dotted line shows the accepted age of the Universe. Median representative error bars are shown in each panel. Cluster members older than the Universe, highlighted with an orange diamond, were found to be rapidly rotating (R. A. Patton et al. 2024), and those highlighted with a purple square were found to be in a binary system (A. M. Price-Whelan et al. 2020).
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Left: locations of the 20 telescopes at 15 different observatories used to measure the RV data analyzed in this work (see Table 4 in Appendix A for observatory details). Right: International Celestial Reference System (J2000) coordinates of the target stars in this study with the number of public RV epochs indicated logarithmically by the color bar. The 44 (of 164) targets with fewer than 20 RV epochs are indicated by red “⨂” symbols—these targets were excluded from the subsequent RV analysis. The ecliptic and galactic planes are shown for reference in yellow and purple, respectively.
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Known exoplanets in the target sample as a function of ﹩{M}_{{\rm{p}}}\,\sin \,i﹩, semimajor axis, maximum angular separation (assuming circular orbits), and incident stellar flux. The sizes of the squares also correspond to the relative ﹩{M}_{{\rm{p}}}\,\sin \,i﹩. The median CL50 limits (Figure 7) are shown by the solid colored lines, and the middle 68% of CL50 limits are bounded by the dashed colored lines. Previously detected planets that were not detected in this study are indicated by red squares, and the locations of the solar system planets are labeled by the first letter of each planet. The green shaded regions in the right panel show the conservative and optimistic habitable zone limits in instellation space.
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Comparison of the lower ﹩{M}_{{\rm{p}}}\,\sin \,i﹩ sensitivity limits in the HZ with the number of RV observation epochs and the span of the RV observations for each target. The color scale corresponds to stellar effective temperature.
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Architectures of systems in our sample with at least one known planet or PC. Both the color and size of each marker correspond to the planet ﹩{M}_{{\rm{p}}}\,\sin \,i﹩. Markers that are outlined in red show the known planets that were not detected in this study. Disputed planet detections are shown as red “?”s inscribed in hexagons, and planet candidates are indicated by blue circles with the text “PC.” Each colored horizontal line shows the minimum ﹩{M}_{{\rm{p}}}\,\sin \,i﹩ sensitivity limit (from the CL50) as a function of semimajor axis, and the colored circles on the left-hand side show stellar effective temperature. Note that HD 33564 has no sensitivity limits because no public RV observations were available.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: The optical design of the PRIME telescope with ray tracing. The top panel presents the entire optical system. The rays traveling to the detector along paths near the optical axis are blocked by the prime-focus camera in reality. These are shown here for illustrative purposes only. The bottom panel provides a close-up view of the prime-focus lens unit.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: Field of view (FOV) of the PRIME telescope (1.45 deg2, with gaps) compared to those of VISTA, Roman (0.28 deg2), UKIRT, Hubble, and the full Moon.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: PRIME 1.8 m telescope.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Completeness as a function of integration time for the same astrophysical scenarios as in Figure 7 for HIP 3765. The three lines represent different levels of accounting for separation and zodiacal light. The solid yellow line for Δmag0(tint, α, Z, κEZ) is the most accurate as it accounts for the most variables and is found by applying Equation (30) to the curves from Figure 7. The dashed blue line for ﹩{\rm{\Delta }}{{\rm{mag}}}_{0}({t}_{{\rm{int}}},0\mathop{.}\limits^{^{\prime\prime} }55,Z,{\kappa }_{{\rm{EZ}}})﹩ shows the effect of calculating the completeness without accounting for the drop in Δmag0 at small separations, which overestimates completeness values for large κEZ. And the dotted purple line for ﹩{\rm{\Delta }}{{\rm{mag}}}_{0}({t}_{{\rm{int}}},0\mathop{.}\limits^{^{\prime\prime} }55,22.6\,{\rm{mag}}\,{{(}^{{\prime\prime} })}^{-2},0.1)﹩ represents the completeness from the curve shown in Figure 6, which consistently overestimates completeness.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Mean completeness error for different stars calculated as the mean difference between the completeness generated with and without α dependence included in the photometric constraint. This was done by calculating the mean difference between the Δmag0(tint, 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩55, Z, κEZ) and Δmag0(tint, α, Z, κEZ) completeness vs. integration time curves shown in Figure 8 for each star. The columns represent different amounts of exozodiacal dust and the rows show the star’s minimum, median, and maximum zodiacal light surface brightness for a telescope on an L2 orbit. The increase in mean completeness error as star distance increases shows that not accounting for the effects of α on Δmag0 leads to a systematic overestimation of completeness. The effect becomes more pronounced for greater amounts of exozodiacal dust assumed. This figure shows that not accounting for α in the photometric constraint results in significant errors for a completeness-based yield calculation. Note that the Z and κEZ values are the same for the two photometric constraints being used within each frame of the figure.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: The refined photometric constraint Δmag0(tint, α, Z, κEZ) for HIP 3765. Each column has a constant value of κEZ and each row has a constant value of Z. The zodiacal light values were generated using EXOSIMS to simulate the range of zodiacal light values of observing the star for an HWO-like telescope (see Appendix B for parameters) at L2.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Percentage errors of the analytic polynomial approach to calculating Δmag0 for the EXOCAT (M. C. Turnbull 2015) target list. The ground truth Δmag0 values are found using the numeric method from Section 2.1. Like in Figure 5 the Roman narrow-field imager is used for the comparison. All errors on Δmag0 are under 0.35%. A clear trend is that dimmer stars produce larger errors. The figure shows over 2000 stars from the EXOCAT target list (M. C. Turnbull 2015), cutting out a handful of stars with incomplete stellar information, an angular diameter larger than the coronagraph inner working angle (IWA), a V magnitude under three, and binary companions.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Plot of the photometric constraint Δmag0(tint) values overlaid on the PDF of an Earth-like planet orbiting HIP 3765 (7.4 pc from Earth) if observed with a notional design of the HWO. The completeness for 30 days of integration time is 0.8. For this figure we fix the values of α, Z, and κEZ to reproduce what a photometric constraint like the one used in D. R. Keithly et al. (2020) looks like.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: The photometric constraints of Roman’s narrow-field imager and spectrometer when observing the planet 47 UMa c. The narrow-field imager’s photometric constraints were calculated with 25 hr of integration time and the spectrometer’s photometric constraints were calculated with 100 hr of integration time. The planet’s joint density function was generated by plandb.sioslab.com, which pulls orbital information from the NASA Exoplanet Archive (J. L. Christiansen et al. 2025). In this case, the orbit fits were pulled from P. C. Gregory & D. A. Fischer (2010). Roman’s wide-field imager is not displayed because the planet is never at a large enough separation to be detected by the wide-field imager.