adsabs/AstroCLIMB huggingface dataset:
Paper: Validation of a Third Planet in the LHS 1678 System
Authors: Michele L. Silverstein, Thomas Barclay, Joshua E. Schlieder, Karen A. Collins, Richard P. Schwarz, Benjamin J. Hord, Jason F. Rowe, Ethan Kruse, Nicola Astudillo-Defru, Xavier Bonfils, Douglas A. Caldwell, David Charbonneau, Ryan Cloutier, Kevin I. Collins, Tansu Daylan, William Fong, Jon M. Jenkins, Michelle Kunimoto, Scott McDermott, Felipe Murgas, Enric Palle, George R. Ricker, Sara Seager, Avi Shporer, Evan Tey, Roland Vanderspek, Joshua N. Winn
Figure caption: Histograms of confirmed multiplanet systems (top panel) and multiplanet systems containing USPs (bottom panel) orbiting stars spanning effective temperatures of approximately 2500–6750 K (NASA Exoplanet Archive; 2023 December 8). This temperature range covers M dwarfs (<4000 K) and solar-type, FGK stars (4000–6750 K). There are far more multiplanet systems around solar-type stars, but this difference narrows for systems that include a USP. One of only 10 multiplanet M-dwarf systems with a USP, LHS 1678 is valuable for investigating planet formation and evolution theories.
Paper: Validation of a Third Planet in the LHS 1678 System
Authors: Michele L. Silverstein, Thomas Barclay, Joshua E. Schlieder, Karen A. Collins, Richard P. Schwarz, Benjamin J. Hord, Jason F. Rowe, Ethan Kruse, Nicola Astudillo-Defru, Xavier Bonfils, Douglas A. Caldwell, David Charbonneau, Ryan Cloutier, Kevin I. Collins, Tansu Daylan, William Fong, Jon M. Jenkins, Michelle Kunimoto, Scott McDermott, Felipe Murgas, Enric Palle, George R. Ricker, Sara Seager, Avi Shporer, Evan Tey, Roland Vanderspek, Joshua N. Winn
Figure caption: To better visualize the successful ground-based recovery of each transiting planet, we stack all ground-based observations, excluding those containing transits of multiple planets. Each transit center is set to 0 hr. Individual transit measurements are plotted using small filled circles with colors matching those shown for each date in Figures 2, 3, and 4. The transits binned to 10 minute intervals are shown as white-filled black circles. The transit models are represented by black lines, with the models for each observation stacked on top of each other.
Paper: Validation of a Third Planet in the LHS 1678 System
Authors: Michele L. Silverstein, Thomas Barclay, Joshua E. Schlieder, Karen A. Collins, Richard P. Schwarz, Benjamin J. Hord, Jason F. Rowe, Ethan Kruse, Nicola Astudillo-Defru, Xavier Bonfils, Douglas A. Caldwell, David Charbonneau, Ryan Cloutier, Kevin I. Collins, Tansu Daylan, William Fong, Jon M. Jenkins, Michelle Kunimoto, Scott McDermott, Felipe Murgas, Enric Palle, George R. Ricker, Sara Seager, Avi Shporer, Evan Tey, Roland Vanderspek, Joshua N. Winn
Figure caption: Ground-based transit observations of LHS 1678 c from LCO and MEarth, derived and presented in the same way as in Figure 2. Light curves taken on 2019 July 27, 2019 December 14, 2021 November 8, and 2021 November 15 feature multiple and/or simultaneous transits of another planet, including a partially overlapping transit with LHS 1678 d on 2021 November 8.
Paper: Validation of a Third Planet in the LHS 1678 System
Authors: Michele L. Silverstein, Thomas Barclay, Joshua E. Schlieder, Karen A. Collins, Richard P. Schwarz, Benjamin J. Hord, Jason F. Rowe, Ethan Kruse, Nicola Astudillo-Defru, Xavier Bonfils, Douglas A. Caldwell, David Charbonneau, Ryan Cloutier, Kevin I. Collins, Tansu Daylan, William Fong, Jon M. Jenkins, Michelle Kunimoto, Scott McDermott, Felipe Murgas, Enric Palle, George R. Ricker, Sara Seager, Avi Shporer, Evan Tey, Roland Vanderspek, Joshua N. Winn
Figure caption: Ground-based transit observations of LHS 1678 d from LCO, derived and presented in the same way as in Figures 2 and 3. Light curves on 2021 November 8 and 2022 January 1 demonstrate simultaneous transits, and the light curve on 2021 November 18 shows separate transits of b and d.
Paper: Validation of a Third Planet in the LHS 1678 System
Authors: Michele L. Silverstein, Thomas Barclay, Joshua E. Schlieder, Karen A. Collins, Richard P. Schwarz, Benjamin J. Hord, Jason F. Rowe, Ethan Kruse, Nicola Astudillo-Defru, Xavier Bonfils, Douglas A. Caldwell, David Charbonneau, Ryan Cloutier, Kevin I. Collins, Tansu Daylan, William Fong, Jon M. Jenkins, Michelle Kunimoto, Scott McDermott, Felipe Murgas, Enric Palle, George R. Ricker, Sara Seager, Avi Shporer, Evan Tey, Roland Vanderspek, Joshua N. Winn
Figure caption: Observed minus calculated transit times for LHS 1678b, c, and d reveal no significant signs of TTVs.
Paper: Validation of a Third Planet in the LHS 1678 System
Authors: Michele L. Silverstein, Thomas Barclay, Joshua E. Schlieder, Karen A. Collins, Richard P. Schwarz, Benjamin J. Hord, Jason F. Rowe, Ethan Kruse, Nicola Astudillo-Defru, Xavier Bonfils, Douglas A. Caldwell, David Charbonneau, Ryan Cloutier, Kevin I. Collins, Tansu Daylan, William Fong, Jon M. Jenkins, Michelle Kunimoto, Scott McDermott, Felipe Murgas, Enric Palle, George R. Ricker, Sara Seager, Avi Shporer, Evan Tey, Roland Vanderspek, Joshua N. Winn
Figure caption: TESS photometry from all four sectors folded on orbital period for each planet. Tiny dots are the individual 2 minute cadence measurements, shown also in 13 minute bins as larger green dots. Overlaid as orange curves are the best-fit transit models; shading displays the 1σ (central 68th percentile) range of models consistent with the data.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: KPIC spectrum for the primary star compared to the best-fit models from breads. The pink curve shows the data, with the green curve representing the atmospheric model and the purple curve representing the atmospheric model + telluric model. The blue curve in the lower panel shows the residuals, which are normalized by the data before uncertainty inflation.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Final fit for the moderate-resolution spectrum from OSIRIS. The temperature fit is 2760 ± 12 K, log(g) is 5.2 ± 0.04. This pair of parameters yields a mass fit of 0.09 ± 0.02 M ⊙ for the companion, slightly above but still consistent with the KPIC fit.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Corner plots showing the posteriors for temperature, log(g), [Fe/H], vsin(i), and RV for the primary and companion using KPIC data from 2020.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Same as Figure 4, but for the companion.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Corner plots for 1RXS0342+1216 b’s orbital parameters with the previous system mass of 0.23 M ⊙ (left) and new system mass of 0.38 M ⊙ (right). No new astrometry or radial-velocity data were included in this orbit fit. Full corner plots can be found in Appendix A.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Final median combined image of the companion 1RXS0342+1216 b obtained with NIRC2 on Keck on 2023 February 8.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: Upper panel: a comparison of Z  σ  (blue empty crosses) and ∣S∣ (orange empty circles) for a series of images capturing a moving source (asteroid 3832, Shapiro). The images are taken sequentially within 1 hr during the same night. The first image serves as the reference image. Each sequential new image thus represents a source moving away from its initial position. The distance that the asteroid has crossed since the time of the reference image is shown as a shift in arcseconds and in the FWHM of P  r . Three selected measurements, where the shift is closest to a multiple of FWHMPSF, are marked by gray dashed vertical lines and designated by the letters A, B, and C. Lower panel: for each of the three marked measurements (A, B, C), a set of 30 × 30 pix cutouts of the new, reference, D, ∣S∣, and Z  σ  images around the initial asteroid position are shown. For the ∣S∣ and Z  σ  cutouts, the minimum and maximum values of the color map are fixed to −5σ and 13σ, respectively. For each cutout the dashed circle shows the FWHM of the PSF of the respective image. For ∣S∣ and Z  σ , the shown PSF is that of the D image. Within a shift of ≲2  FWHMPSF, Z  σ  > ∣S∣. Once the asteroid positions in the reference and new images are clearly separated, ∣S∣ overtakes Z  σ .
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: The likelihood function ﹩P({\widehat{D}}_{T}| {{\rm{\Delta }}}_{x},{{\rm{\Delta }}}_{y},{\alpha }_{r},{\alpha }_{n})﹩ evaluated for simulation 7 using the (true) point-source center location  x   c  = ( p  +  q )/2 as a function of model parameters Δ x , Δ y , α  r , and α  n  (see Section 3.4). The evaluation was performed using MCMC sampling. The figure shows the marginal distributions over single parameters (upper diagonal) as well as the marginal distributions for all parameter pairs (off-diagonal). The blue point indicates the true model parameters while the curves indicate the 68%, 95%, and 99.7% confidence regions. The dashed vertical lines indicate the 1σ confidence intervals in the one-dimensional marginals.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: Receiver operating characteristic (ROC) curves for simulations 1–3 (varying levels of flux noise) showing the rates of true-positive events as a function of the false-positive event rate. These curves were generated by varying detector threshold levels η over an appropriately wide range. Each color represents a simulation index (noise level) while solid (dashed) curves represent the resulting performance when using the translient statistic (proper statistic). One can see that for all simulations and at all values of the false-positive rate the translient statistic achieves a higher true-positive detection rate compared to the proper statistic. We also see that lower levels of noise allow the detectors to reach higher true-positive rates at set false-positive rates.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: The likelihood function ﹩P({\widehat{D}}_{T}\,| \,| | {\rm{\Delta }}| | ,\theta ,{\alpha }_{r}-{\alpha }_{n},{\alpha }_{r}+{\alpha }_{n})﹩, similar to Figure 8 and similarly evaluated for simulation 8 (where the translation is small compared to the PSF) but using a different set of variables to display the same distribution. One can see that this change of variables largely decouples most (though not all) of the parameters, leaving a clear dependence between ∣∣Δ∣∣ and α  r  + α  n .
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: The likelihood function ﹩P({\widehat{D}}_{T}| {\alpha }_{r}-{\alpha }_{n},({\alpha }_{r}+{\alpha }_{n})| | {\rm{\Delta }}| | ,\theta )﹩, obtained by linearizing Equation (25) in  k  · Δ. Here evaluation is again for the small translation simulation 8 (as in Figures 8 and 9). One can see that this reduced set of model parameters (in the linearized likelihood) does not show a strong dependence and may therefore be preferable in the small translation limit.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: The likelihood function ﹩P({\widehat{D}}_{T}| {{\rm{\Delta }}}_{x},{{\rm{\Delta }}}_{y},{\alpha }_{r},{\alpha }_{n})﹩, similar to Figure 7 but evaluated for simulation 8, where the translation length is smaller than the resolving width of the PSFs.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: A comparison of Z  σ  (blue empty crosses) and ∣S∣ (orange empty circles) for a series of images capturing a variable star (eclipsing binary). The measured LAST magnitude of the star (green solid circles) is also shown, with its value on the right y-axis. For a stationary variable star, ∣S∣ is dominant.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: ROC curves similar to Figure 5 but for simulations 4–6.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: The top panel shows the along-scan residuals (mas) of the fit of Gaia FPR data set, bottom panel shows the across-scan residuals (mas). The orange bins account for all along-scan outliers beyond ﹩\left|30\right|﹩ mas, some of which may be excluded from the fit. The bin frequency is the number of residuals in the bin divided by the total number of residuals.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Photocenter offset as function of the solar phase angle for objects of 0.1, 1 and 10 km of radius. The equivalent angular correction if observed at 1 au (mas) is included for reference. The dashed lines correspond to the photocenter offset uncertainty term as observed at 1 au (λ = 0.3).
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Orbital fit residuals of asteroid 779 Nina (H = 8.02) using the photocenter correction (blue) and without photocenter correction (orange). Neither solution includes the photocenter offset uncertainty factor (λ = 0). The top panel shows the residuals over time, whereas the bottom panel shows the residuals as function of the solar phase angle. Residuals removed from the fit are shown with a cross symbol, whereas circles are included in the fit.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: The top panel shows the length of the observation arc as function of the absolute magnitude H, for solar system objects with H > 6. The color of the dots represents the number of observation transits. The bottom panel shows the distribution of absolute magnitudes of the objects in Gaia FPR data set, as histogram of object number count and estimated cdf from sorting the objects by H.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: The asteroid position relative to the observer  ρ  and the heliocentric position of the asteroid  r  define the photocenter offset correction direction ﹩\hat{t}﹩ and are related by the solar phase angle α. The correction  t  is the projection into the plane of sky directions ﹩{\hat{i}}_{\mathrm{RA}}﹩ and ﹩{\hat{i}}_{\mathrm{Decl}}﹩ after being scaled using Equation (5).
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Uncertainty in the semimajor axis of the 20,536 asteroids with H < 14 and σ  a,FPR < 10−8 au used in the detailed prediction test. The uncertainties are shown for full arc Gaia FPR observational arc (Long arc), observations until 2017 June (Short arc), with and without the photocenter offset uncertainty factor (λ = 0, dotted, λ = 0.3 otherwise). The estimated cdf corresponds to the objects sorted by σ  a .
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Transit weighted mean of along-scan residuals (mas) from Gaia FPR data set. The orange bins account for all outliers beyond ﹩\left|10\right|﹩ mas in the distribution of the mean. The gray histogram shows the residuals of Figure 4 for reference. The bin frequency is the number of transits in the bin divided by the total number of transits.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Normalized along-scan residuals (mas) with respect to the uncertainty in the measurements shown as estimated pdf. The pdf is estimated by the bin count divided by the number of residuals times the bin width (i.e., count/(N Δ · w  i )). A Gaussian distribution is overlapped for reference.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Uncertainty in the semimajor axis normalized by the semimajor axis. We include the uncertainties using the full observational arc (full FPR) and for short-arc solutions based on data through 2017 June, i.e., the data cutoff for Gaia DR3. The bin frequency is the number of objects in the bin divided by the total number of objects.