adsabs/AstroCLIMB huggingface dataset:
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Planet mass (M  p  or ﹩{M}_{p}\sin i﹩) vs. host star metallicity. The red and blue circles are hot (a/R * < 20) and warm (a/R * ≥ 20) Jupiters around M dwarfs, respectively. The vertical red and blue dashed lines are the median metallicity of two samples: 0.28 and 0.06 dex, respectively. The background gray circles and triangles are hot and warm Jupiters around G-type stars, respectively, under the same definition. Both of them have a median iron abundance of 0.14 dex, shown as a vertical black line. The top two panels are the histograms of these four samples.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Power spectra and relative astrometric solution for KOI 4252 on 2021 October 24. The top panels show the observed binary power spectrum (left), the best-fit model (center), and the residuals (right). The bottom left plot shows the full reconstructed image from the speckle pipeline, which often has a reflected image of the companion. The bottom right plot shows a close-in view of the χ 2 values around the best-fit solution, where the best-fit position of the companion is marked with an X. The 1σ, 2σ, and 3σ χ² contour levels (corresponding to ﹩{\chi }_{\min }^{2}+1,{\chi }_{\min }^{2}+4,{\chi }_{\min }^{2}+9﹩) are shown in black.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Top panel: semimajor axis as a function of time. Bottom panel: advance in mid-transit for TOI-4201b for an observation baseline of 6 yr measured from today. For both panels, the colors represent different stellar rotation periods (P rot) from 10 to 40 days, as expected for M dwarfs (McQuillan et al. 2014). The orange line stands for the measured P rot in this work.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Planet mass and radius diagram. The gray circles are giant planets around FGK stars. The colored circles are all transiting gas giants around M dwarfs with mass measurements. Different colors represent different equilibrium temperatures. Three constant-density curves (ρ = 0.5, 1.0, 2.0 g cm−3) are shown as dashed lines for reference. With a density around 1.8 g cm−3, TOI-4201b is one of the densest gas giants transiting M dwarfs.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Top panel: the mass and semimajor axis diagram of all confirmed gas giants around M dwarfs from transit (red) and RV (blue) surveys. Bottom panel: the planet-to-star mass ratio and semimajor axis distribution of gas giants around M dwarfs colored by the detection techniques. The blue shaded region is the mass ratio paucity region proposed by Gan et al. (2022a). In both panels, TOI-4201b is marked as a brown star.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Radius evolution of three TOI-4201b-like planets. The observed values of radius−age appear in the gray box. The evolution models are of a metal-free planet (dashed blue), hot diluted core of 25 M ⊕ (red), and 5M ⊕ core with high atmospheric opacity (green). Models emphasize the requirement of additional energy sources to explain the observed properties of TOI-4201b.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Ratio of the total Gaia DR3 proper motion to the total observed motion for each binary in our sample. The proper motion is at least three times larger compared to the observed relative motion for all systems, so this motion is likely true orbital motion of a bound companion rather than motion of an unbound, line-of-sight companion.
Paper: Fast Globally Optimal Catalog Matching using MIQCP
Authors: Jacob Feitelberg, Amitabh Basu, Tamás Budavári
Figure caption: Simulation Total Runtime vs. Number of Catalogs for DirILP and MIQCP. We set the distance between the object centers to 0.″13. We set the uncertainties for both objects to 0.″04. For these runtimes, we use the algorithm to find a better upper bound on the maximum number of hypothetical objects. We repeat the simulations five times for each setting. MIQCP has a faster total runtime than DirILP.The DirILP line does not have data points for 30 and 35 catalogs because we stopped the program after 45 minutes. We show in Figure 4 exactly what percentage of the runs succeeded in finishing before 45 minutes. The error bars at the end of DirILP and MIQCP are zero because only 1 out of 5 runs finished on time for both methods.
Paper: Fast Globally Optimal Catalog Matching using MIQCP
Authors: Jacob Feitelberg, Amitabh Basu, Tamás Budavári
Figure caption: HSC match with three catalogs. In the first plot, we color each point according to its catalog. We also shade the circle of radius σ around the source center. In the second plot, we show through colors which points are assigned to the same object by the Chainbreaker and MIQCP methods. Their solutions are the same. So, we do not show separate plots. Both methods predict three total objects. DirILP was not able to find a solution for this match within a reasonable amount of time.
Paper: Fast Globally Optimal Catalog Matching using MIQCP
Authors: Jacob Feitelberg, Amitabh Basu, Tamás Budavári
Figure caption: Percent of Optimization Problems Solved vs. Number of Catalogs for DirILP and MIQCP. For these results, we set a reasonable amount of time to 45 minutes. We set the distance between the object centers to 0.″13. We set the uncertainties for both objects to 0.″04. For these runtimes, we use the algorithm to find a better upper bound on the maximum number of hypothetical objects. We repeat the simulations five times for each setting. MIQCP is able to solve more problems within 45 minutes than DirILP.
Paper: Fast Globally Optimal Catalog Matching using MIQCP
Authors: Jacob Feitelberg, Amitabh Basu, Tamás Budavári
Figure caption: HSC match with 4 catalogs. In the first plot, we color each point according to its catalog. We also shade the circle of radius σ around the source center. In the second plot, we use pairwise lines to show which points are assigned to the same object by the Chainbreaker method. MIQCP and DirILP could not find a solution for this match within 45 minutes.
Paper: Fast Globally Optimal Catalog Matching using MIQCP
Authors: Jacob Feitelberg, Amitabh Basu, Tamás Budavári
Figure caption: Simulation with 20 catalogs with object assignment shown through the different colors. The two object centers are denoted with x-ticks in red and blue. MIQCP is able to recover the true solution shown in the top left. Chainbreaker is not able to find a good solution and predicts the wrong number of objects. Chainbreaker also violates constraints by assigning sources within the same catalog to the same object.
Paper: Fast Globally Optimal Catalog Matching using MIQCP
Authors: Jacob Feitelberg, Amitabh Basu, Tamás Budavári
Figure caption: MIQCP Runtime vs. Number of Catalogs with ﹩\hat{N}=2﹩. We manually set the maximum number of hypothetical objects to 2. We set the distance between the object centers to 0.″13. We set the uncertainties for both objects to 0.″04. We repeat the simulations five times for each setting. Comparing to the runtimes in Figure 2, reducing ﹩\hat{N}﹩ dramatically reduces the overall runtime.
Paper: Fast Globally Optimal Catalog Matching using MIQCP
Authors: Jacob Feitelberg, Amitabh Basu, Tamás Budavári
Figure caption: Setup Time vs. Number of Catalogs for DirILP and MIQCP. We set the distance between the object centers to 0.″13. We set the uncertainties for both objects to 0.″04. For these runtimes, we do not use the algorithm to find a better upper bound on the maximum number of hypothetical objects. We repeat the simulations 5 times for each setting. MIQCP has a faster setup time than DirILP.
Paper: Direct Simulation Monte Carlo Modeling of Ammonia in Comet C/2014 Q2 (Lovejoy)
Authors: Hideyo Kawakita, Neil Dello Russo, Ronald J. Vervack, Michael A. DiSanti, Boncho P. Bonev, Hitomi Kobayashi, Daniel C. Boice, Yoshiharu Shinnaka
Figure caption: Observed spatial profiles of H2O (blue squares) and NH3 (red circles) in comet Q2 Lovejoy at 1.29 au from the Sun (Dello Russo et al. 2022) compared with calculated spatial profiles of H2O (dotted line in purple) and NH3 produced solely from its parent molecule (NH3X) with photodissociation lifetimes of 100, 500, and 1000 s (dashed curves in green, orange, and red respectively) at 1 au from the Sun and converted to 1.29 au by using an r                   ﹩{}_{h}^{2}﹩ law. The observed spatial profiles of H2O and NH3 are shifted in logarithmic scale for readability. The mixing ratios of cometary nucleus ice are assumed as H2O:CO2:CO: NH3X = 85:10:4:1 in this plot. The modeled profile of NH3 that is released only from a NH3 nucleus ice (dashed curve in blue) is also shown for comparison. The gray-hatched region indicates the area affected by telluric seeing.
Paper: Direct Simulation Monte Carlo Modeling of Ammonia in Comet C/2014 Q2 (Lovejoy)
Authors: Hideyo Kawakita, Neil Dello Russo, Ronald J. Vervack, Michael A. DiSanti, Boncho P. Bonev, Hitomi Kobayashi, Daniel C. Boice, Yoshiharu Shinnaka
Figure caption: Same as Figure 3 but for NH3 (red circles) and NH2 (gray triangles) in comet Q2 Lovejoy at 1.29 au from the Sun (Dello Russo et al. 2022) compared with calculated spatial profiles of NH3 (dashed line in brown) and its photodissociation product NH2 (dotted line in brown) in the case of the NH3 parent molecules having a lifetime of 1000 s at 1 au. The observed spatial profiles of NH3 and NH2 are shifted in logarithmic scale for readability. The modeled profile of NH2 (solid line in black) based on the combination between the nucleus source and the distributed source of NH3 as shown in Figure 4 is more consistent with the observed spatial profile of NH2. A contribution from NH2 prompt emission appears to further improve the fit with the observed spatial profile (thick dashed line in violet).
Paper: Direct Simulation Monte Carlo Modeling of Ammonia in Comet C/2014 Q2 (Lovejoy)
Authors: Hideyo Kawakita, Neil Dello Russo, Ronald J. Vervack, Michael A. DiSanti, Boncho P. Bonev, Hitomi Kobayashi, Daniel C. Boice, Yoshiharu Shinnaka
Figure caption: Same as Figure 3, but assuming different mixing ratios between a NH3 nucleus source and a distributed source from NH3 parent molecules with a lifetime of 10,000 s at 1 au. The spatial profile in the very inner coma region (within the seeing size) is similar to the nucleus source case (i.e., a ρ −1-profile).
Paper: Physical Properties of the Young Asteroid Pair 2010 UM26 and 2010 RN221
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Composite image showing UM26 and RN221. Tiger stripes at the upper right are caused by the inter-chip gap. The cores of both objects are clipped in order to emphasize faint structures in the sky background caused by imperfectly removed trailed field stars and galaxies. The projected antisolar and negative heliocentric velocity vectors are marked −S and −V, respectively. A scale bar shows 10″ and 15,000 km at the distance of the asteroid pair.
Paper: Direct Simulation Monte Carlo Modeling of Ammonia in Comet C/2014 Q2 (Lovejoy)
Authors: Hideyo Kawakita, Neil Dello Russo, Ronald J. Vervack, Michael A. DiSanti, Boncho P. Bonev, Hitomi Kobayashi, Daniel C. Boice, Yoshiharu Shinnaka
Figure caption: Same as Figure 6 but with the spatial profile of NH2 that is produced from NH3 directly released from the nucleus (dashed line in black), the spatial profile of NH3for the nucleus source (dashed line in blue), and the spatial profile of NH3 for the nucleus source with a correction for the used g factors (solid line in green), see text.
Paper: Direct Simulation Monte Carlo Modeling of Ammonia in Comet C/2014 Q2 (Lovejoy)
Authors: Hideyo Kawakita, Neil Dello Russo, Ronald J. Vervack, Michael A. DiSanti, Boncho P. Bonev, Hitomi Kobayashi, Daniel C. Boice, Yoshiharu Shinnaka
Figure caption: Same as Figure 3, but with calculated spatial profiles of NH3 assuming that the UV optical depth effect (see Figure 1 for H2O, CO2, and CO) of NH3 parent molecules is similar to that of H2O.
Paper: Direct Simulation Monte Carlo Modeling of Ammonia in Comet C/2014 Q2 (Lovejoy)
Authors: Hideyo Kawakita, Neil Dello Russo, Ronald J. Vervack, Michael A. DiSanti, Boncho P. Bonev, Hitomi Kobayashi, Daniel C. Boice, Yoshiharu Shinnaka
Figure caption: Examples of normalized loss rates of major molecular species by photolytic reactions in the coma for a comet with ﹩{Q}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ = 5 × 1029 s−1 (H2O:CO2:CO = 85:10:5) at 1 au from the Sun. Extinction of the solar UV radiation is significant within 1000 km and negligible for outside of 10,000 km in this case.
Paper: Direct Simulation Monte Carlo Modeling of Ammonia in Comet C/2014 Q2 (Lovejoy)
Authors: Hideyo Kawakita, Neil Dello Russo, Ronald J. Vervack, Michael A. DiSanti, Boncho P. Bonev, Hitomi Kobayashi, Daniel C. Boice, Yoshiharu Shinnaka
Figure caption: Number density [m−3], outflow velocity [m s−1], and kinetic temperature [K] of cometary coma in the case of a “pure-water” nucleus with ﹩{Q}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ = 5 × 1029 s−1 at 1 au from the Sun based on our DSMC coma model.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Spectrophotometry of AF Lep b from Mesa et al. (2023; blue), De Rosa et al. (2023; green), and Franson et al. (2023b; purple). Photometry is converted from magnitudes into fluxes (unless already reported in the literature as such) based on zero-points provided by Nielsen et al. (2017). Response curves of the ﹩K1/K2/L^{\prime} ﹩ bands (gray) are obtained from the VLT/SPHERE and Keck/NIRC2 websites.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Fitted orbits of AF Lep b, with the red and blue colors denoting positive and negative ΔRV b−A at epoch J2024.0, respectively. A positive (negative) ΔRV b−A value means the planet moves, relative to its host star, away from (toward) the observer at a given epoch. Specific signs and values of ΔRV b−A have not been observed to date. Thin lines are random orbits drawn from the posteriors, and each thick line corresponds to the maximum-likelihood orbital solution for a given sign of ΔRV b−A. The orbital solutions with positive and negative ΔRV b−A values have similar shapes but the locations of their ascending and descending nodes are nearly swapped. We use a black star to show AF Lep A and black circles to trace the observed relative astrometry of AF Lep b.
Paper: Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
Authors: Megan G. Li, Sofia Z. Sheikh, Christian Gilbertson, Matthias Y. He, Howard Isaacson, Steve Croft, Evan L. Sneed
Figure caption: Histograms comparing the inputs for each of the seven parameters used to calculate drift rates, with low-eccentricity and high-eccentricity options being shown in separate subplots. The simulated parameters are in red, and the NEA sample’s parameters are in blue. The x axes for period and semimajor axes are only shown up to 300 days and 6 au, respectively, for visualization purposes, as mathematical models currently only predict this far. However, the NEA sample has entries past these limits.
Paper: Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
Authors: Megan G. Li, Sofia Z. Sheikh, Christian Gilbertson, Matthias Y. He, Howard Isaacson, Steve Croft, Evan L. Sneed
Figure caption: Histograms for the entirely simulated populations of exoplanets (high eccentricities on the left, low eccentricities on the right). Each population has 5286 planets with 200 drift rates drawn for each planet, giving a total of 1,057,200 drift rates, to mirror Figure 2. The dotted lines on each histogram give the 99% containment boundary. For high eccentricity, 99% of the drift rates fall in ±0.44 nHz. For low eccentricity, 99% of the drift rates fall in ±0.27 nHz.
Paper: Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
Authors: Megan G. Li, Sofia Z. Sheikh, Christian Gilbertson, Matthias Y. He, Howard Isaacson, Steve Croft, Evan L. Sneed
Figure caption: A histogram of all of the calculated drift rate magnitudes for the 5286 planet sample from the NEA with all inclinations set to 90°. 200 drift rates are calculated for each of the 5286 exoplanets for a total of 1,057,200 drift rates. The dotted line at 53 nHz designate the 99% boundary: 99% of calculated drift rates fall between these values. The solid line demonstrates the suggested drift rate upper limits from Sheikh et al. (2019).
Paper: Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
Authors: Megan G. Li, Sofia Z. Sheikh, Christian Gilbertson, Matthias Y. He, Howard Isaacson, Steve Croft, Evan L. Sneed
Figure caption: A histogram of all of the calculated drift rate magnitudes for the 5286 planet sample from the NEA with eccentricities sampled from the low-eccentricity model. 200 drift rates are calculated for each of the 4286 exoplanets for a total of 1,057,200 drift rates. The dotted line at 53 nHz designate the 99% boundary: 99% of calculated drift rates fall between these values. The solid line demonstrates the suggested drift rate upper limits from Sheikh et al. (2019).
Paper: Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
Authors: Megan G. Li, Sofia Z. Sheikh, Christian Gilbertson, Matthias Y. He, Howard Isaacson, Steve Croft, Evan L. Sneed
Figure caption: A histogram of all of the calculated drift rate magnitudes for the 4538 planet sample from the NEA with simulated periods and semimajor axes. 200 drift rates are calculated for each of the 4538 exoplanets for a total of 907,600 drift rates. The dotted line at 0.59 nHz designate the 99% boundary: 99% of calculated drift rates fall between these values.
Paper: Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
Authors: Megan G. Li, Sofia Z. Sheikh, Christian Gilbertson, Matthias Y. He, Howard Isaacson, Steve Croft, Evan L. Sneed
Figure caption: A histogram of all of the calculated drift rate magnitudes for the 5286 planet sample from the NEA with inclinations sampled uniformly in cosine. 200 drift rates are calculated for each of the 4286 exoplanets for a total of 1,057,200 drift rates. The dotted line at 42 nHz designate the 99% boundary: 99% of calculated drift rates fall between these values.