adsabs/AstroCLIMB huggingface dataset:
Paper: OGLE-2014-BLG-1760: A Jupiter–Sun Analogue Residing in the Galactic Bulge
Authors: Natalia E. Rektsini, Clément Ranc, Naoki Koshimoto, Jean-Philippe Beaulieu, David P. Bennett, Andrew A. Cole, Sean K. Terry, Aparna Bhattacharya, Étienne Bachelet, Ian A. Bond, Andrzej Udalski, Joshua W. Blackman, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Bayesian posterior probability distributions for the planetary companion mass, host mass, their projected separation, and the distance to the lens system are shown with only light-curve constraints in gold and with the additional constraints from our Keck follow-up observations in red. The centers 68.3% (1σ) of the distributions are shaded in darker colors (dark red and dark gold), and the remaining central 95.4 %  (3σ) of the distributions are shaded in lighter colors. The vertical black line marks the median of the probability distribution for the respective parameters. The priors used for the Bayesian analysis are the estimates from the final light-curve model. We show that the medians of the Bayesian probability are within 2σ of the constrained parameter distributions for the lens mass and distance.
Paper: OGLE-2014-BLG-1760: A Jupiter–Sun Analogue Residing in the Galactic Bulge
Authors: Natalia E. Rektsini, Clément Ranc, Naoki Koshimoto, Jean-Philippe Beaulieu, David P. Bennett, Andrew A. Cole, Sean K. Terry, Aparna Bhattacharya, Étienne Bachelet, Ian A. Bond, Andrzej Udalski, Joshua W. Blackman, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Mass–distance estimate for the lens. The purple curve represents the constraint from the K-band lens flux measurement for isochrones up to 10 Gyr, the red dotted lines represent the flux uncertainties, the gold curve shows the Einstein angular radius measurement, and the aquamarine curve represents the microlensing parallax constrained by the (AO) results. The intersection between the three curves defines the estimated solution of the lens physical parameters.
Paper: OGLE-2014-BLG-1760: A Jupiter–Sun Analogue Residing in the Galactic Bulge
Authors: Natalia E. Rektsini, Clément Ranc, Naoki Koshimoto, Jean-Philippe Beaulieu, David P. Bennett, Andrew A. Cole, Sean K. Terry, Aparna Bhattacharya, Étienne Bachelet, Ian A. Bond, Andrzej Udalski, Joshua W. Blackman, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Two-dimensional parallax distribution based on the Galactic model (genulens). The color-scale shows the relative probability, the black cross indicates the microlensing parallax coordinates predicted using our (AO) Keck constraints.
Paper: OGLE-2014-BLG-1760: A Jupiter–Sun Analogue Residing in the Galactic Bulge
Authors: Natalia E. Rektsini, Clément Ranc, Naoki Koshimoto, Jean-Philippe Beaulieu, David P. Bennett, Andrew A. Cole, Sean K. Terry, Aparna Bhattacharya, Étienne Bachelet, Ian A. Bond, Andrzej Udalski, Joshua W. Blackman, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Best-fit model of the light curve of OGLE-2014-BLG-1760. The 2L1S best-fit model is indicated by the black curve. The bottom panel shows the residual from the best-fit model and the OGLE, MOA, and RoboNet data. The right panel presents the enlargement of the caustic-crossing and the cusp of the light curve and the top right-corner panel shows a close-up of the anomaly. The figures were produced using the software described in C. Ranc (2020).
Paper: OGLE-2014-BLG-1760: A Jupiter–Sun Analogue Residing in the Galactic Bulge
Authors: Natalia E. Rektsini, Clément Ranc, Naoki Koshimoto, Jean-Philippe Beaulieu, David P. Bennett, Andrew A. Cole, Sean K. Terry, Aparna Bhattacharya, Étienne Bachelet, Ian A. Bond, Andrzej Udalski, Joshua W. Blackman, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: The marginalized posterior distributions of the new light-curve best-fit model. On the diagonal we show the one-dimensional cumulative density function of each parameter. The 68.3% (1σ), 95.5% (2σ), and 99.7% (3σ) confidence intervals are represented by dark violet, median blue, and light green, respectively.
Paper: OGLE-2014-BLG-1760: A Jupiter–Sun Analogue Residing in the Galactic Bulge
Authors: Natalia E. Rektsini, Clément Ranc, Naoki Koshimoto, Jean-Philippe Beaulieu, David P. Bennett, Andrew A. Cole, Sean K. Terry, Aparna Bhattacharya, Étienne Bachelet, Ian A. Bond, Andrzej Udalski, Joshua W. Blackman, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: 2L1S light-curve model described by the black line with the V-band data. The green points showing the OGLE-V data around the microlensing event, the only V-band observations. In the bottom panel, we show the residual from the best-fit model and the OGLE-V data.
Paper: OGLE-2014-BLG-1760: A Jupiter–Sun Analogue Residing in the Galactic Bulge
Authors: Natalia E. Rektsini, Clément Ranc, Naoki Koshimoto, Jean-Philippe Beaulieu, David P. Bennett, Andrew A. Cole, Sean K. Terry, Aparna Bhattacharya, Étienne Bachelet, Ian A. Bond, Andrzej Udalski, Joshua W. Blackman, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Close-up (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2) frames of the six stars used to construct the PSF model (right) and their residuals, after profile-fitting photometry subtraction (left).
Paper: A Coronagraphic Pilot Study of the Circumstellar Environments around Red Supergiants: CD -31°4916’s Dust Morphology
Authors: Jamie R. Lomax, Emily M. Levesque, John P. Wisniewski, John H. Debes
Figure caption: GPI imagery of CD -31°4916’s circumstellar material with an overlay of the contours derived from the HST imagery (blue). The location the central star is marked by the plus sign, while GPI’s inner working angle is shown as a solid white circle. The region bounded by the black line marks the locations under HST’s BAR5 occulter and areas that were masked out due to diffraction spikes (see the right-hand side of Figure 2).
Paper: A Coronagraphic Pilot Study of the Circumstellar Environments around Red Supergiants: CD -31°4916’s Dust Morphology
Authors: Jamie R. Lomax, Emily M. Levesque, John P. Wisniewski, John H. Debes
Figure caption: GPI imagery of CD -31°4916’s circumstellar material with an overlay of the contours derived from the HST imagery after removal of light leaking out from under the occulter. The location the central star is marked by the plus sign, while GPI’s inner working angle is shown as a filled white circle. The black box-like region marks the locations under HST’s BAR5 occulter and areas that were masked out due to diffraction spikes (see the right-hand side of Figure 2).
Paper: A Coronagraphic Pilot Study of the Circumstellar Environments around Red Supergiants: CD -31°4916’s Dust Morphology
Authors: Jamie R. Lomax, Emily M. Levesque, John P. Wisniewski, John H. Debes
Figure caption: HST imagery of CD -31°4916’s circumstellar material after subtracting out light leaking out from behind the occulting bar from the central star (see Section 4). The overlay of the contours derived from the displayed imagery to help guide the eye. The location the central star is marked by the plus sign.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Planet visibility fractions as a function of stellar distance for different coronagraph configurations. The visibility fraction represents the portion of a planet’s orbit during which it remains detectable between the coronagraph’s IWA and OWA. Different colored lines represent various OWA values ranging from 360 to 2520 mas, with a fixed IWA of 60 mas. Solid lines show results for circular orbits (e = 0), while dashed lines show results for eccentric orbits (0 < e < 1). The shaded regions represent 1σ uncertainties derived from our orbital simulations across the ExEP stellar sample. For all cases, we assumed that the semimajor axes were uniformly distributed between 5 and 30 au. This analysis demonstrates that an OWA of at least 800 mas is required to maintain visibility fractions above 0.6 for stars out to 20 pc.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Phase curves showing reflected flux as a function of orbital phase for different planetary albedo values ranging from 0.1 to 0.5. The orbital phase runs from 0 to 1, where phase 0 corresponds to the inferior conjunction and phase 0.5 to the superior conjunction. All curves assume a Lambertian scattering law and identical orbital geometry. Despite the range of albedo values spanning a factor of 5, this variation is relatively minor compared to the typical dynamic range of planet-to-star contrast ratios, justifying our adoption of a single representative albedo value of 0.2 for detectability calculations.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: The phase curve of a planet over one rotation at eight different illumination phases. The images at the right show renderings of the planet’s illuminated surface throughout the observation. Each curve represents a different viewing geometry, the observer-planet–star angle, with the corresponding planetary illumination phase shown by the colored circles in the legend. The top (blue) curve shows a fully illuminated planet, while the lower curves show various partial illumination scenarios down to a completely dark planet (purple). The gray curve represents the classical edge-on viewing case exhibiting the full range of phase variations.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Schematic representation of coronagraph working angles. The IWA and OWA define the detectable region (dotted pattern) where exoplanets can be observed. The coronagraph blocks the central star, while planets can be detected between the IWA (red circle) and OWA (blue circle). Green dots represent detectable planets, while gray dots indicate planets that fall outside the observable region. The dashed lines represent the orbits of planets.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Properties of stars in the ExEP catalog. Left: Distribution of V magnitudes, showing a peak between V = 5–6, indicating a sample dominated by bright stars. Right: Distribution of distances, showing a relatively uniform spread of targets out to 20 pc, with most stars between 5 and 20 pc, making this a sample of nearby stars.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Parameter recovery precision across 100 independent orbital simulations combining RV and astrometric measurements after six epochs of astrometric observations covering around a year (one epoch every two months). The left panel shows relative precision in recovered inclination values, while the right panel shows uncertainties in eccentricity. Each point represents the percentage uncertainty for a single simulation. The varying levels of precision reveal a key limitation in orbital characterization: planets with periods significantly longer than our observational baseline show markedly higher uncertainties. We highlight several cases (numbered 8 and 95) with uncertainties reaching up to 50% for inclination and 60% for eccentricity. These outliers share a common feature—their orbital periods (128 and 133 yr, respectively) are much longer than our observational baseline, resulting in coverage of only a small fraction of their complete orbits. This temporal sampling limitation, rather than specific inclination values or other orbital elements, proves to be the primary factor determining parameter recovery precision.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Orbital fits for the two cases showing poor precision in their orbital parameters (simulations 8 and 95). Each panel displays the projected orbit in the plane of the sky, where ΔR.A. and Δdecl. are given in mas. The white circles represent the actual observations, while the star symbol indicates the position of the central body. The color gradient along the orbit traces the mean anomaly from 0 (yellow) to 2π (dark blue), illustrating the object’s motion along its orbit. The orbital parameters are shown above each panel: semimajor axis (a) in astronomical unit, eccentricity (e), inclination (i) in degrees, the argument of periapsis (ω) in degrees, and longitude of ascending node (Ω) in degrees. These problematic cases all share extremely long orbital periods with 128 yr in simulation 8 and approximately 150 yr in simulation 95, resulting in our observations covering only 1%–2% of a complete orbit. This limited orbital coverage is the primary factor limiting precise parameter determination.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Corner plot showing posterior distributions of orbital parameters from two different models: astrometry-only (blue) and combined RV+astrometry (orange) for a simulated planetary system. The star is at 20 pc, and the astrometric measurements span two months between epochs. The top right panels show the predicted astrometric separation (in mas), position angle (in degrees), and RV measurements (in m s−1) over time. The corner plot displays joint and marginal posterior distributions for the total mass (M), planetary semimajor axis (b_a), eccentricity (b_e), and inclination (b_i). The true system parameters correspond to a nearly circular orbit (e = 0.07) at inclination (i = 64°). The addition of precursor RVs to the astrometric data significantly improves parameter constraints, particularly for eccentricity and semimajor axis.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: The accuracy of exoplanet orbital parameter determination using RV measurements combined with astrometry. The top panels show the correlation between inferred and true values for orbital inclination (left) and eccentricity (right), with blue triangles representing RV-only measurements, yellow diamonds representing astrometry-only measurements, open circles showing combined RV+Astrometry measurements, and the dashed line indicating perfect recovery. The error bars show 1σ uncertainty. The bottom panels display histograms of the measurement errors (inferred minus true values) for inclination (left) and eccentricity (right), with blue bars showing the RV-only results, yellow bars showing astrometry-only results, and white bars showing combined RV+astrometry results. The combined approach significantly improves parameter recovery, where RV alone shows large systematic uncertainties, while both methods achieve relatively good precision.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Corner plot showing posterior distributions of orbital parameters from two different models: RV-only (blue) and combined RV+astrometry (orange) for a simulated planetary system. The star is at 20 pc, and the astrometric measurements span two months between epochs. The top right panels show the predicted astrometric separation (in mas), position angle (in degrees), and RV measurements (in m s−1) over time. The corner plot displays joint and marginal posterior distributions for the total mass (M), planetary semimajor axis (b_a), eccentricity (b_e), inclination (b_i), and planetary mass (b_mass). The true system parameters correspond to a quite eccentric orbit (e = 0.2) at low inclination (i = 10°). The addition of astrometric measurements to the RV data significantly improves parameter constraints, particularly for inclination and eccentricity.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Comparison of orbital inclination constraints for two planetary systems using different observation timing strategies. Histograms show the posterior distributions of inclination measurements for observations scheduled every two months within one year (light red) and observations randomly distributed across the five-year mission timeline (dark red). The true inclination for each system is shown by the vertical dashed line. Each strategy’s orbital period (P) and measurement uncertainties are indicated. All four cases demonstrate significant improvement in precision when using sparse sampling over the extended baseline, with uncertainty reductions of 1–3 orders of magnitude. This improvement is achieved despite still not covering the full orbit in longer-period systems, but covering a good fraction of it with this sampling, highlighting the importance of extended temporal baselines for orbital characterization.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Evolution of orbital solution constraints with an increasing number of simulated astrometric observations, shown in relative R.A. (ΔR.A.) and decl. (Δdecl.) coordinates in mas. Each panel shows the ensemble of possible orbits (colored lines) consistent with the simulated measurements (black circles) for different numbers of observations from one to eight. The star symbol indicates the position of the star. The color scale represents the mean anomaly from 0 to 2π. The progressive reduction in the spread of possible orbits demonstrates how additional observations improve orbital constraints, with significant convergence achieved by six observations.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Reduction in the uncertainty in % of orbital parameters as a function of the number of astrometric observations (epochs) with an uncertainty of 1° for 100 simulated planets. The black lines show the uncertainty in orbital inclination, while the purple lines show the uncertainty in eccentricity. Both parameters show rapid improvement with initial observations, with uncertainties dropping significantly after five epochs. Additional observations beyond six epochs yield diminishing returns, suggesting this as an optimal number of visits for orbital characterization with HWO for wide-separation planets.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Comparison of eccentricity absolute uncertainties (Δe) and inclination absolute uncertainties (Δi) between RV-only (blue triangles), astrometry-only (yellow diamonds), and combined RV+astrometry (white circles) solutions across 100 simulated planetary systems. While the RV+astrometry solutions show higher uncertainties in some cases, particularly for nearly circular orbits, the absolute uncertainty for eccentricity remains below 0.1.