adsabs/AstroCLIMB huggingface dataset:
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Two-dimensional histograms of the darkest subregions for all the images in every filter in ACS/WFC. The color bar indicates the percentage of images (N Darkest/N Total × 100%, where N Darkest is the number of darkest subregions and N Total is the total number of images) in this filter that contain a darkest subregion in the corresponding location. In other words, regions that are more blue/purple have systematically lower sky-SB levels across the entire filter. These histograms resemble the ACS/WFC flat fields, indicating that a residual flat field exists in the majority of images in our database.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Two-dimensional histograms of the darkest subregions for all the images in every filter in WFC3/UVIS. The color bar indicates the percentage of images (N Darkest/N Total × 100%, where N Darkest is the number of darkest subregions and N Total is the total number of images) in this filter that contain a darkest subregion in the corresponding location. In other words, regions that are more blue/purple have systematically lower sky-SB levels across the entire filter. White indicates regions that are always ignored due to detector artifacts or regions that always contain a bright object. These histograms resemble the WFC3/UVIS flat fields, indicating that a residual flat field exists in the majority of images in our database.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Comparison of the systematically brightest and darkest subregions. The error bars for both plots show the 16th and 84th percentiles of the y-axis distribution. Left: median ratio of the brightest subregions over the darkest subregions. The bluest filters are excluded because the sky-SB is nearly zero. Right: median difference of the brightest subregions over the darkest subregions. The left y-axis shows units of MJy sr−1 and the right axis shows nW m−2 sr−1 at 0.6 μm.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Relationship of the sky-SB measurements in this work (using the Pro-med algorithm) and the measurements in SKYSURF–2. The x-axis shows sky-SB measurements from SKYSURF–2, and the y-axis shows the difference in sky-SB values between this work and SKYSURF–2. The red lines indicate the median differences shown in Table 4 used for DL estimations. The red lines agree with the darkest sky-SB measurements from SKYSURF–2.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: One-to-one relationship of the sky-SB measurements in this work (using the Pro-med algorithm) and the measurements in SKYSURF–2. The x-axis shows sky-SB measurements from SKYSURF–2 and the y-axis shows sky-SB measurements from this work. The gray line is a one-to-one relationship.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: Top: projected starspots on TOI-3884's stellar surface for an aligned system using the APO ﹩{i}^{{\prime} }﹩ filter transit observed on 2022 April 5 assuming a spot temperature of 2900 K and a photospheric temperature of 3200 K (spot contrast of 0.5) for the three-spot model (red) and one-spot model (blue). The planet’s crossing path is defined by the blue dotted lines, with the central dotted line corresponding to the equator of the planet and the outer dotted lines denoting the full extent of the planet, and the central latitude of the transit is marked with a red vertical line. The large red spot in the middle has a relative radius R spot = 0.44R  s , with the two smaller red spots having radii R spot = 0.10Rs  and 0.07R  s , respectively. The large blue spot has a relative radius R spot = 0.63R  s  and is mostly out of the transit chord. The fractional spotted area for the three-spot model in the transit chord for these stellar surface features (assuming that there are no spots anywhere else on the star) is 11%. Middle: best-fit three-spot model for the aligned system (red line) compared to the best-fit one-spot model (blue line) and the no starspot transit model (cyan line), with the APO 20 s ﹩{i}^{{\prime} }﹩-band data as black points with error bars. Bottom: residuals from the three-spot best-fit starspot model (red) and one-spot best-fit model (blue).
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: Top: projected starspots on TOI-3884's stellar surface for a polar starspot with a stellar spin axis tilt of −65° and λ = 75° using the APO SDSS ﹩{i}^{{\prime} }﹩ filter transit observed on 2022 April 05 assuming a spot temperature of 2900 K and a photospheric temperature of 3200 K (spot contrast of 0.5). The large spot in the middle has a relative radius R spot/R  s  = 0.29, with the two smaller spots having radii R spot/R  s  = 0.16 and 0.09, respectively. The fractional spotted area in the transit chord for these stellar surface features assuming that there are no spots anywhere else on the star is 3%. The black line shows the path of the equator of the planet as it crosses the star. Bottom: best-fit starspot model for the oblique (not aligned) system (red line) compared to the no starspot transit model (cyan line), with the APO 20 s ﹩{i}^{{\prime} }﹩-band data shown as black points with error bars.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: Light curves for individual ground-based observations and the phase-folded TESS sectors 22, 46, and 49. Light-blue points were masked in order to fit the transit shape during our analysis, and the best-fit nonspotted transit model is plotted in red, with the appropriate dilution terms included for the TESS sectors (0.98, 0.86, 0.84, respectively). Residuals for the respective transit models are plotted in the bottom panel for each light curve.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: The HPF RVs phased to the best-fit period of TOI-3884b. The best-fit model and the 1σ quantile are plotted in blue. Mid-transit occurs at phase 0.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: TESS sector 46 short-cadence (2-minute) data, shown with black points, with the aligned starspot model (red line) and polar starspot model (cyan line). The same pattern can be seen in TESS sector 49 short-cadence data, though it is not reproduced here.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: Comparing the width of the CCFs of TOI-3884 (red curves) in six different orders in HPF in six different panels to the CCFs of a slowly rotating calibration star, Ross 128. The gray dashed lines show the unbroadened calibration star, and the black lines show the calibration star artificially broadened to the best-fit value. The TOI-3884 spectra show evidence for rotational broadening.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: Top: TESS sector 22 long-cadence light curve, with the TOI-3884b transits denoted in blue. Differing transit depths are an artifact of the 30-minute cadence. Bottom: short 2-minute cadence of the TESS sectors 46 and 49, with the transit model in blue. Both sets of light curves use the PDCSAP flux without additional out-of-transit GP detrending required.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: The full HPF RV time series with the best-fit model plotted in blue, with the 1σ quantile included as a lighter shade.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: NESSI 5σ contrast curve of TOI-3884 with the ﹩{z}^{{\prime} }﹩ filter. The inserted image is the final speckle image, which shows no nearby sources with Δmag > 3.5 outside 0.″2.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Einstein ring crossing time, t E, distribution at (l, b) = (0.°125, −0.°125) (left panels) and at (l, b) = (0.°125, −2.°625) (right panels). The top panels show the distribution of all simulated events (red) and detected microlensing events (blue) with a 16 minute cadence by the assumed PRIME survey. The bottom panels show the distribution of detected microlensing events (blue) and detected planetary events (black). The vertical lines show the median value of each histogram. The dashed green and orange lines show the detection efficiency of microlensing events and planetary events depending on t E, respectively.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Source magnitude, H  S , distribution at (l, b) = (0.°125, −0.°125) (left panels) and at (l, b) = (0.°125, −2.°625) (right panels). The top panels show the distribution of all simulated events (red) and detected microlensing events (blue) with a 16 minute cadence. The bottom panels show the distribution of detected microlensing events (blue) and detected planetary events (black). The dashed green and orange lines show the detection efficiency of microlensing events and planetary events depending on H  S , respectively.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Mean detection efficiency of microlenisng events along each line of sight, ϵ ML(l, b). Each plot shows the detection efficiency for different cadences. With the same observation cadence, the detection efficiency is lower at the Galactic center than away from the Galactic center. See the text for an explanation of these trends. At the same field, the lower the observation cadence, the lower the detection efficiency.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Microlensing detection maps along each line of sight. Each plot shows the number of detections with 16, 32, 48, and 96 minute cadences. This figure is obtained by multiplying the star counts, N source (Figure 5), event rate, Γsource (Figure 7), and mean detection efficiency of microlenising events, ϵ ML (Figure 9).
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Comparison of star counts in the Stanek window (l, b = [0.°25, −2.°15]) in KGM (blue line) for the bulge population as a function of the H-band magnitude to those by HST observation in Terry et al. (2020; red points). Stars with H > 19.5 mag are underestimated in the Galactic model.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Map of the event rate per source, Γsource, calculated using source and lens catalogs, generated by genstars. The event rates per source are mainly determined by the stellar density, so at the NSD region (∣b∣ < 0.°5, ∣l∣ < 1.°5) the event rate is the highest among other fields.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Detection efficiency of planetary signatures, ϵ PL(M  p ), depending on the planet mass, which are obtained by taking the average of all 875 fields and are summed across semimajor axis, 0.3 < a < 30 au. The red, green, blue, and black color plots shows detection efficiency with 16, 32, 48, and 96 minute cadences, respectively.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Comparison of the event rate per source calculated from the source and lens catalogs from genstars (blue line) with that measured in Mróz et al. (2019; red points). Due to the high extinction around the Galactic plane, there is no measurement of the event rate at ∣b∣ < 1° by OGLE. Outside of the Galactic plane, the two values of the event rate are almost coincident.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Detection efficiency of microlensing events depending on t E. The solid and dotted lines show the detection efficiency away from the Galactic center, (l, b) = (0.125, −2.625), and at the Galactic center, (l, b) = (0.125, −0.125), respectively. The detection efficiency with 16, 32, 48, and 96 minute cadences are shown in red, green, blue, and black, respectively.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: Simulated population of long-period perturbers capable of exciting the eccentricity of TOI-4127 b to facilitate high-eccentricity tidal migration. We show the perturbers that are detectable via available astrometric and radial velocity observations as pink “x” marks and blue circles, respectively, and the perturbers that cannot yet be detected as black points.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: NEID and SOPHIE RV data for TOI-4127. We show the NEID data in blue and the SOPHIE data in red, as well as the median orbit fit, as determined in Section 3, as a solid black line. We also highlight the times during which TESS was observing the target in Sectors 40 and 47, with colors matching the light curves in Figure 1.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: Phase-folded RV data for TOI-4127 b. We show the NEID data (blue) and SOPHIE data (red), as well as the best-fit model (black) and 3σ uncertainties (gray) in the top panel, and we show the residuals to the fit in the bottom panel.