adsabs/AstroCLIMB huggingface dataset:
Paper: A Phenomenon Resembling Early Superhumps in a New SU UMa-type Dwarf Nova with a 2 hr Orbital Period
Authors: Rebecca S. Boyle, Colin Littlefield, Peter Garnavich, Ryan Ridden-Harper, Paula Szkody, Patricia Boyd, Krista Lynne Smith
Figure caption: The shared-axis, detrended light curve (top), and time-resolved power spectrum (bottom) of K2BS5 starting just before the maximum of the superoutburst. Frequency units are cycles day−1. Double-wave oscillations near the orbital period begin slightly before BKJD 3024 and transition rapidly into stage A superhumps, marked by the frequency drop on the power spectrum mid day 3024. Stage A is also relatively short lived, rising rapidly to higher frequency stage B. While the superhumps are not present during the rebrightening event, they do reappear just before it, between BKJD 3037 and BKJD 3039. Both the fundamental and second harmonic are visible on the power spectrum. Note: different intensity cuts were used in the second and third panels of the figure to improve signal visibility of the second harmonic.
Paper: A Phenomenon Resembling Early Superhumps in a New SU UMa-type Dwarf Nova with a 2 hr Orbital Period
Authors: Rebecca S. Boyle, Colin Littlefield, Peter Garnavich, Ryan Ridden-Harper, Paula Szkody, Patricia Boyd, Krista Lynne Smith
Figure caption: LBT quiescent spectrum of K2BS5 with no reddening correction (black line) and after correction for a reddening of E(g − r) = 0.29 mag (blue line). Wavelength units are given in angstroms and flux density units in erg s−1 cm−2 Å−1.
Paper: A Phenomenon Resembling Early Superhumps in a New SU UMa-type Dwarf Nova with a 2 hr Orbital Period
Authors: Rebecca S. Boyle, Colin Littlefield, Peter Garnavich, Ryan Ridden-Harper, Paula Szkody, Patricia Boyd, Krista Lynne Smith
Figure caption: Top: transition from double-wave oscillations to Stage A superhumps. The expected times of superhump maxima are indicated with black arrows (for the double-wave oscillations) and blue arrows (for Stage A superhumps). Both the double-wave oscillations and Stage A superhumps show stable, periodic maxima. Double-wave oscillations persisted for ∼15 cycles before transitioning into Stage A superhumps in just several superhump cycles. Bottom left: power spectra of the double-wave oscillations and Stage A superhumps. Bottom right: phase-averaged profile of double-wave oscillations.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: We computed an l1 periodogram of TOI-1136 RV data, determining the best white-noise value for the noise model through cross-validation. Instrument offsets are fit by the compressed sensing model. Unlike other periodograms, multiple peaks can have significance. However, the rotation period (8.53 days), signals near the rotation period (8.36 days), and aliases of the rotation period (4.40, 4.36, 2.87 days) dominate the periodogram. Once again, planet periods are not significantly detected, and a more complicated model is required to remove the activity and uncover the planet signals.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: TTV observed-calculated plots for each of the six inner transiting planets (b–g), from top to bottom, left to right. Red lines indicate the maximum-likelihood TTV model predictions from a seven-planet model, while green lines indicate a six-planet model. Light blue lines indicate the final prediction of 100 randomly selected chains. We do not include a fit to the single transit of TOI-1136 (h). We also highlight TESS sector 75, where TOI-1136 will receive additional observations. The two models predict significant TTV differences during this sector.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: A plot of the GP fit to the RV activity signal of TOI-1136, calculated from photometry. This activity prediction is estimated via the FF′ method described in Aigrain et al. (2012). The above plot illustrates our fit to season 2. After assessing convergence, we use the frequency posteriors of this GP fit as priors on the GP hyperparameters for our TTV+RV fits in the next section.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: Top: total RV model to TOI-1136, planets and GP. Middle: residuals to seven-planet GP fit. Bottom: phase folds to each planet in TOI-1136 after subtracting the activity model and each other planet. RVs are adjusted for instrumental offsets. We note that APF’s lower precision was not ideal for tracking planetary reflex, but helped to constrain the stellar activity. The RV data used in our analysis are available as “data-behind-the-figure”.(The data used to create this figure are available.)
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: Our posterior transit fit to the single transit of the candidate planet. Fits indicate that the planet likely has a radius near 2.68 R ⊕. We use the SES (Equation (2)) to verify the significance of the transit.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: An autocorrelation function (ACF) of TOI-1136's TESS photometry. A clear frequency pattern with well-defined parabolas fit to the peaks of the ACF indicates a solid detection of the system’s rotation period.
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: The MCMC corner plot with a third body of TIC 63597006, because we see a obvious periodic signal which could be caused by a third body on the O − C diagram. The fit model include the binary parameters (inclination incl, mass ratio q, fill-out factor f, temperature ratio T 2/T 1) and the third body parameters (third light fraction L 3).
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: The MCMC corner plot for TIC 55007847. The fit model includes the orbital parameters (inclination incl), binary paramters (mass ratio q, fill-out factor f and temperature ratio T 2/T 1) and starspot parameters (the relative temperature T spot/T 1, the colatitude of starspot col, the longitude of starspot long, and the angular radius of starspot R spot).
Paper: Deep Paβ Imaging of the Candidate Accreting Protoplanet AB Aur b
Authors: Lauren I. Biddle, Brendan P. Bowler, Yifan Zhou, Kyle Franson, Zhoujian Zhang
Figure caption: EWs and stellar color and companion flux density corresponding to simulated Paβ emission lines injected into the stellar continuum (top) and companion continuum (bottom). The solid gray line in the top panel indicates the real measured stellar J cont − Paβ and the shaded region bounded by dashed lines represents the 1σ uncertainty on the measurement. The green star marks the simulated quantity that matches the observed stellar J cont − Paβ. The bottom panel shows the EW estimations for both an unresolved source and spatially resolved source. The uppermost boundary of each of the shaded regions indicates the upper limit of the companion flux density determined in Section 3.4. The pink and maroon stars mark the simulated quantities that match the measured upper limits on the companion’s flux density if it were unresolved or resolved, respectively. EW values are negative for emission lines.
Paper: Deep Paβ Imaging of the Candidate Accreting Protoplanet AB Aur b
Authors: Lauren I. Biddle, Brendan P. Bowler, Yifan Zhou, Kyle Franson, Zhoujian Zhang
Figure caption: SED of AB Aur b. The adopted upper limit of the flux density in Paβ for an unresolved source is indicated by the pink downward-pointing arrow, whereas the upper limit of the flux density for a spatially resolved source is shown depicted as a maroon arrow. The green circles are the optical (HST) and NIR (Subaru) photometry reported by Currie et al. (2022), and the CHARIS spectrum they report is represented in light-green. The orange square point indicates the Hα excess identified by Zhou et al. (2022) with HST.
Paper: Deep Paβ Imaging of the Candidate Accreting Protoplanet AB Aur b
Authors: Lauren I. Biddle, Brendan P. Bowler, Yifan Zhou, Kyle Franson, Zhoujian Zhang
Figure caption: The PSF-subtracted image (left column) and corresponding S/N Map (right column) showing several 5σ injected sources that are unresolved (top row) and spatially resolved (bottom row). The synthetic sources are located at PA = 270° with separations 0.″4, 0.″6, 0.″8, and 1.″0. The FOV is slightly smaller than that in Figure 3 for enhanced visual clarity.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Zoomed-in comparison of BOSS and LAMOST spectra for some of the sources for which spectra from both instruments are available. All spectra have been interpolated onto a common wavelength grid. The shown sources have SNR ∼ 100 for BOSS, and  ∼30 for LAMOST. Both BOSS and LAMOST spectra were normalized through dividing out the median flux within the presented wavelength range, and different sources were arbitrarily offset.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Distribution of the T eff and ﹩\mathrm{log}g﹩  from the training set colored according to the weight applied to the loss.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Photometric interpolation of T eff and ﹩\mathrm{log}g﹩ values for cool dwarfs using the data from Cifuentes et al. (2020).
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Architecture of the neural net model used in this paper.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Distribution of the T eff and ﹩\mathrm{log}g﹩ of the sources that form the training set; BOSS objects are in red and LAMOST in blue.
Paper: Radio Emission from High-redshift Active Galactic Nuclei in the JADES and CEERS Surveys
Authors: Muhammad A. Latif, Ammara Aftab, Daniel J. Whalen
Figure caption: Radio flux densities for AGNs observed in JADES for α = 0.3 with detection limits for ngVLA (left column) and SKA (right column). The dotted, dashed and dotted–dashed red and brown lines are H II region and SN flux densities for SFRs of 1, 3 and 10 M ⊙ yr−1, respectively. The black solid, dashed and dotted horizontal bars show ngVLA and SKA detection limits for integration times of 1, 10 and 100 hr, respectively.
Paper: Radio Emission from High-redshift Active Galactic Nuclei in the JADES and CEERS Surveys
Authors: Muhammad A. Latif, Ammara Aftab, Daniel J. Whalen
Figure caption: The AGN radio flux vs. the expected flux from the host galaxy (which includes both contributions from H II regions and SN remnants) for α = 0.3. The dot symbols show the highest flux from FPs and triangles represent the lowest flux expected from FPs at given frequencies of 0.1 and 8 GHz. The sources for which SFRs are unknown, we assume fixed values of 3 and 10 M ⊙ yr−1 while for other sources SFRs are listed in Table 1.
Paper: Radio Emission from High-redshift Active Galactic Nuclei in the JADES and CEERS Surveys
Authors: Muhammad A. Latif, Ammara Aftab, Daniel J. Whalen
Figure caption: Radio flux densities for UHZ1 for α = 0.3 (top row) and 0.7 (bottom row) with detection limits for ngVLA (left column) and SKA (right column). The dotted, dashed and dotted–dashed red and brown lines are H II region and SN flux densities for SFRs of 1, 3 and 10 M ⊙ yr−1, respectively. The black solid, dashed and dotted horizontal bars are H II region and SN flux densities for SKA and ngVLA limits for integration times of 1, 10 and 100 hr, respectively.
Paper: Radio Emission from High-redshift Active Galactic Nuclei in the JADES and CEERS Surveys
Authors: Muhammad A. Latif, Ammara Aftab, Daniel J. Whalen
Figure caption: Radio flux densities for AGNs observed in CEERS, JADES, and UNCOVER for α = 0.3 with detection limits for ngVLA (left column) and SKA (right column). The dotted, dashed, and dotted–dashed red and brown lines are H II region and SN flux densities for SFRs of 1, 3, and 10 M ⊙ yr−1, respectively. The black solid, dashed, and dotted horizontal bars show ngVLA and SKA limits for integration times of 1, 10, and 100 hr, respectively.
Paper: Radio Emission from High-redshift Active Galactic Nuclei in the JADES and CEERS Surveys
Authors: Muhammad A. Latif, Ammara Aftab, Daniel J. Whalen
Figure caption: Radio flux densities for AGNs observed in JADES for α = 0.3 with detection limits for ngVLA (left column) and SKA (right column). The dotted, dashed and dotted–dashed red and brown lines are H II region and SN flux densities for SFRs of 1, 3, and 10 M ⊙ yr−1, respectively. The black solid, dashed, and dotted horizontal bars show ngVLA and SKA detection limits for integration times of 1, 10, and 100 hr, respectively.
Paper: Radio Emission from High-redshift Active Galactic Nuclei in the JADES and CEERS Surveys
Authors: Muhammad A. Latif, Ammara Aftab, Daniel J. Whalen
Figure caption: Radio flux densities for AGNs observed in CEERS, JADES and UNCOVER for α = 0.3 with detection limits for ngVLA (left column) and SKA (right column). The dotted, dashed and dotted–dashed red and brown lines are H II region and SN flux densities for SFRs of 1, 3 and 10 M ⊙ yr−1, respectively. The black solid, dashed, and dotted horizontal bars show ngVLA and SKA detection limits for integration times of 1, 10, and 100 hr, respectively.
Paper: Radio Emission from High-redshift Active Galactic Nuclei in the JADES and CEERS Surveys
Authors: Muhammad A. Latif, Ammara Aftab, Daniel J. Whalen
Figure caption: Radio flux densities for AGNs observed in CEERS, JADES and UNCOVER for α = 0.7 with detection limits for ngVLA (left column) and SKA (right column). The dotted, dashed and dotted–dashed red and brown lines are H II region and SN flux densities for SFRs of 1, 3 and 10 M ⊙ yr−1, respectively. The black solid, dashed and dotted horizontal bars show ngVLA limits for integration times of 1, 10 and 100 hr, respectively.
Paper: Radio Emission from High-redshift Active Galactic Nuclei in the JADES and CEERS Surveys
Authors: Muhammad A. Latif, Ammara Aftab, Daniel J. Whalen
Figure caption: Radio flux densities for AGNs observed in JADES for α = 0.7 with detection limits for ngVLA (left column) and SKA (right column). The dotted, dashed and dotted–dashed red and brown lines are H II region and SN flux densities for SFRs of 1, 3 and 10 M ⊙ yr−1, respectively. The black solid, dashed and dotted horizontal bars show SKA limits for integration times of 1, 10 and 100 hr, respectively.
Paper: Estimating Galaxy Parameters with Self-organizing Maps and the Effect of Missing Data
Authors: Valentina La Torre, Anna Sajina, Andy D. Goulding, Danilo Marchesini, Rachel Bezanson, Alan N. Pearl, Laerte Sodré
Figure caption: The top panel shows the comparison of distribution of simulated and UVISTA colors, obtained from magnitudes brighter than the peak of the observed magnitude’s distribution in each band. The colors g − r on the left and Y − J on the right are shown as an example of two similar color distributions. The middle and bottom panels show the comparison of component maps obtained from training SOM with simulated galaxy colors (middle) and UVISTA (bottom). A comparison between the middle and the bottom panels shows that the two data sets yield the same component maps, meaning that if the input objects have the same color distribution, as in the top panel, then even the SOMs will be similar. For this test, we trained the two SOMs with the same color set considered in this paper.
Paper:  ethraid: A Simple Method for Characterizing Long-period Companions Using Doppler, Astrometric, and Imaging Constraints
Authors: Judah Van Zandt, Erik A Petigura
Figure caption: The top panel shows a 7.5 yr subset of HD 117207's RV time series, divided into four slices based on the epoch in which the RVs were measured. Panels (a)–(d) show the RVs from each slice, along with the linear/quadratic trend fit to those RVs using radvel. We show the measurement error of each RV with horizontal black lines. We used ethraid to model each trend/curvature pair, along with HGCA astrometry, in panels (e)–(h), respectively. The gold star in each panel shows HD 117207 b’s semimajor axis and ﹩{m}_{c}\sin i﹩ values measured by long-baseline RV surveys: a = 3.744 au, ﹩{m}_{c}\sin i=1.87﹩                      M J, where we have approximated a conversion from ﹩{m}_{c}\sin i﹩ to m  c  by dividing by the median ﹩\sin i﹩ value of 0.866. The overlap between ethraid's predicted parameters and the true values in all four panels demonstrates ethraid's reliability in estimating companion parameters over a range of orbital phases.
Paper:  ethraid: A Simple Method for Characterizing Long-period Companions Using Doppler, Astrometric, and Imaging Constraints
Authors: Judah Van Zandt, Erik A Petigura
Figure caption:  ethraid's fitting algorithm. The steps are the same for RVs (left), astrometry (center), and direct imaging (right): ethraid samples a set of model orbital parameters, forward models the data-specific parameters, evaluates the model likelihood, and finally marginalizes many such likelihoods to derive the posterior PDF. Arrows represent inputs used in a given step: blue arrows show inputs from the previous step, red arrows show inputs provided by the user, and purple arrows show inputs that are fixed in the code. The bottom row shows three of the plots available to the user through the plot command. Left: The 2D m  c –a posteriors for each of the RV (green), astrometry (blue), and imaging (gray line) data sets, plus the combined posterior (red) conditioned on all three. The dark/light regions of each posterior show 68/95% confidence intervals. For imaging, the gray contour marks the 95% confidence boundary, with models below/above the contour ruled in/out by the data. Right: CDFs of the marginalized a and m  c  posteriors. The vertical red lines indicate 95% confidence intervals. ethraid also produces corresponding PDFs by default.