adsabs/AstroCLIMB huggingface dataset:
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Spectra and contribution functions of the retrieved forward model fit to the SpeX data for 2M 2224. The forward model spectra (using the MLE parameter values) are in color, with the data in gray. Immediately beneath the spectra are the contribution functions for the two principal carbon- and oxygen-bearing species; CO2 is not included in the retrieval, as it was excluded from the retrieval in Burningham et al. (2017), inviting a more direct comparison of our results. The deepest contours, outlined in solid colors, enclose the regions where the contribution function reaches >1% of the total contribution within the atmospheric column at a given wavelength bin. Each successive contour denotes 2 orders of magnitude smaller fractional contribution (here, 10−4).
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Initial retrieval fits to the HD 106906 b spectrum. The data are down-sampled to a maximum resolution of ≈500, a factor of 4–8 lower than the original. The fit using the full data set is shown in light red. The shaded pink regions indicate where Daemgen et al. (2017) identified contiguous or near-contiguous regions of suspected high telluric contamination that could not be reliably fully removed in reduction, thus introducing potential residual systematics. The fits with each band individually are shown in the various nonred colors in each band (purple for J, green for H, and yellow for K  s ). The fit using the data across all bands, but without the high-telluric regions, is shown in darker red. Both the full and single-band fits perform most poorly in fitting the data in the high-telluric regions, especially on the blue ends of each band.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Single-parameter (1D) and parameter vs. parameter (2D) posterior distributions of cloud parameters from the samples in the cloudy (red) and cloud-free (blue) forward model fit to data simulated from the cloudy forward model of an L dwarf (see Section 4). The cloud opacity is modeled as a power law in wavelength, as described in Section 3.3. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 4.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: The vertical temperature–pressure profiles of the retrieved forward model fit to the SpeX data for 2M 2224. We show the MLE, median, and 95% confidence interval of the retrieved T–P profiles, with the retrieved T–P profiles of retrievals from Burningham et al. (2017) and Burningham et al. (2021) also plotted for comparison. The latter profile is shown to highlight how the retrieved vertical structure changes as longer-wavelength data are included. The median retrieved τ = 1 pressure for the retrieved deck cloud models of Burningham et al. (2017) is shown as a dashed line.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Single-parameter (1D) and parameter vs. parameter (2D) posterior distributions of cloud parameters from the samples in the model fit to the SpeX data for 2M 2224. The cloud opacity is modeled as a power law in wavelength, as described in Section 3.3. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 5. Median values for the equivalent parameters in the run in Burningham et al. (2017) are listed in Table 5.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: A selection of parameters of the retrieved forward model fit to the SpeX data for 2M 2224, shown as 1D and 2D histograms in a corner plot of the retrieved posterior distributions for selected parameters. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 5. Median values for the equivalent parameters in the run in Burningham et al. (2017) are listed in Table 5.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: A selection of parameters of the retrieved forward model fits to data simulated from forward models of an L dwarf, shown as 1D and 2D histograms in a corner plot of the retrieved posterior distributions. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 4.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Single-parameter (1D) and parameter vs. parameter (2D) posterior distributions of gas parameters from the samples in the model fit to the SpeX data for 2M 2224. The cloud opacity is modeled as a power law in wavelength, as described in Section 3.3. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 5. Median values for the equivalent parameters in the run in Burningham et al. (2017) are listed in Table 5.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Single-parameter (1D) and parameter vs. parameter (2D) posterior distributions of gas parameters from the samples in the cloudy (red) and cloud-free (blue) forward model fit to data simulated from the cloudy forward model of an L dwarf (see Section 4). The cloud opacity is modeled as a power law in wavelength, as described in Section 3.3. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 4.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Predicted transits for TOI-199 c, which does not transit. Blue and orange points indicate the PDCSAP and tesseract light curves, respectively, as in Figure 1. The vertical dashed line indicates the expected time of midtransit. Model transits from batman are shown for two radii, R  c  = 1.03 R  J  (solid lines) and R  c  = 0.6 R  J  (dotted lines), and for two impact parameters, b = 0 (green) and b = 0.75 (purple).
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption:  N-body orbital evolution of the TOI-199 system for an extent of 30,000 yr. The initial orbit is taken from our TTV+RV best fit (see Table 3) and is stable for at least 10 Myr. Left to right: evolution of the semimajor axes a  b  (blue) and a  c  (red), the eccentricities e  b  (blue) and e  c  (red), and the evolution of Δω = ω  b  – ω  c , respectively. See the text for details.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Top: RV measurements (FEROS: blue, HARPS: red, CHIRON: purple, and CORALIE: green) and best-fit two-planet model (gray line) for the combined data. Bottom left: TTVs (blue circles) and fitted model with Exo-Striker (gray line) for TOI-199 b (top panel) and residuals to the model (bottom panel). The model has been smoothed with a quadratic spline. Bottom center and right: phase-folded representation of the two planetary signals after the RV signal of the other companion was subtracted. The respective RV residuals are shown under each panel, accordingly. The more precise HARPS RVs, which are the main driver of the fit, are highlighted. The black squares show the binned phase-folded RVs.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Evolution models of TOI-199 b and TOI-199 c compared to a simple model for Saturn. All models assume a central ice–rock core surrounded by a hydrogen and helium envelope of solar composition. ﹩{M}_{\mathrm{core}}﹩ corresponds to the mass of the ice–rock core while M env corresponds to the mass of the solar-composition envelope. The ranges of ﹩{M}_{\mathrm{core}}﹩ and M env compatible with the observational constraints are shown for TOI-199 b. The blue error bar corresponds to observational constraints on the age and the radius of TOI-199 b. We also show the range of radii expected for likely extreme compositions of TOI-199 c in red.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Corner plot of the posterior distributions of the fitted planet parameters for TOI-199 b for the joint modeling of the TESS and ASTEP TTVs, and the HARPS, FEROS, CHIRON, and CORALIE RVs. The distributions are explored using nested sampling. The red crosses indicate the median values, and the black contour lines the 1σ, 2σ, and 3σ confidence levels. For ω  b , note that it is a circular argument and thus, e.g., −10° = 350°.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Corner plot of the posterior distributions of the planet parameters for TOI-199 c from the joint modeling of the TESS and ASTEP TTVs, and the HARPS, FEROS, CHIRON, and CORALIE RVs. The distributions are explored using nested sampling. The red crosses indicate the median values, and the black contour lines the 1σ, 2σ, and 3σ confidence levels. For ω  c , note that it is a circular argument and thus, e.g., 370° = 10°.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Radius–period diagram for giant planets with masses measured to better than 20% and radii measured to better than 10%, similar to our accuracies for TOI-199 b. The markers are color coded by eccentricity and scaled by planet mass. TOI-199 occupies a scarcely populated region of this space.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Mass–radius diagram for warm (T eq < 1000 K) giant planets with masses measured to better than 20% and radii measured to better than 10%, similar to our accuracies for TOI-199 b. The markers are color coded by equilibrium temperature and scaled by the TSM. TOI-199 b is significantly cooler than other well-characterized planets with similar masses and radii, and has a high TSM.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Orbital configuration of the TOI-199 system. The conservative and optimistic HZs are shown in dark and light green, respectively. TOI-199 c is in the HZ.
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: [Left] RV signal for Earth-mass, Jupiter-mass, and Saturn-mass objects on Earth-like, Jupiter-like, and Saturn-like eccentric orbits, respectively, around a solar-mass star with varying orbital periods. THE is pushing toward the 0.1 m s−1 detection limit for Earth-like exoplanets, with 10 yr of nightly observations with target 1σ measurement error of ∼0.3 m s−1 per observation. [Right] Astrometric signal for Earth-mass, Jupiter-mass, and Saturn-mass objects around solar-mass stars with varying periods on circular orbits. Gaia astrometry will have a ∼34.2 μas 1σ measurement error per field-of-view passing for the along-scan (AL) direction for bright stars. Roman astrometry has a target ∼5–20 μas 1σ measurement error per observation for bright stars. With Gaia and Roman, the astrometric observations can have a baseline of up to ∼25 yr. As the radial velocity signal increases with shorter orbital periods and the astrometric signal increases with larger orbital periods, we can see how the two observing methods are complementary in period space. We emphasize that these (target) measurement errors are not a detection threshold, but rather a per observation estimated measurement error.
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Left: Recovered median and 1σ MCMC period and mass vs. Roman observing plan for exoplanetary systems with an Earth-like exoplanet and CGG-like companion exoplanet (a: Jupiter-like, b: Saturn-like) around a Sun-like star at 10 pc. Each data point represents the median of the multiple iterations of simulations that we ran and subsequent MCMC models that we fit in order to account for correlated noise and biases in our small number of astrometric observations. The error bars are the median of the MCMC 1σ results. Right: Period and mass 1σ uncertainty vs. Roman observing plan. Here, the data points are the mean of the upper and lower 1σ error bars on the left plots. The error bars on these plots represent the median absolute deviation among the 1σ values for the different MCMC runs. Takeaway: These figures show three main things: (1) An observing program with only THE RVs and Gaia astrometry can recover Earth-like and CGG exoplanets around nearby Sun-like stars. (2) A modest astrometric observing program with Roman of the THE stars could extend the astrometric baseline to ∼25 yr and improve the precision of the recovered CGG masses and periods. (3) Roman astrometry will not improve the precision of the detection of Earth-like exoplanets around stars at 10 pc beyond the Gaia astrometric observations.