adsabs/AstroCLIMB huggingface dataset:
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Example of the removal of sharp peaks in the Fourier domain for one of the Kepler targets (KIC000757280). Top panel: the absolute value of the Fourier transform of Kepler data (blue line) alongside the measured PSD, which does not resolve the peaks (orange line) Middle panel: notch filters designed by the pipeline for the identified peaks. Bottom panel: Fourier transform of the data after applying the notch filters, showing the peaks removed.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Shape quality piecewise χ2 veto, illustrated for Kepler target KIC008590354. The blue points represent the whitened flux around a trigger that was identified by the template shown in the black line. Orange lines show the template split into segments, with independent amplitude fits for each. Orange shading represents the 1σ confidence interval for these fits. The three panels show the splitting of the template into two, three, and four parts. In this case, the test identified inconsistency in the segment amplitudes, indicating that the template does not adequately describe the data.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Example of the distribution of SESs in units of SNR before and after vetting and non-Gaussianity correction for Kepler target KIC008590354. Blue line: SES distribution with a non-Gaussian tail caused by the flux’s non-Gaussianity. Orange line: same distribution after veto. Green line: after the non-Gaussianity correction was applied.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Illustration of SES distribution estimation for one of the Kepler targets (KIC008553579). Blue line: distribution of SESs in units of SNR. Orange line: fit by the two-Gaussian mixture model. This function will be used to compute the non-Gaussianity correction (Equation (8)). The green line shows a Gaussian distribution for reference.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Illustration of a box-shaped and a smooth template match in the case of white noise (upper panel) and red correlated noise (lower panel). Left panel: examples of box templates and smooth templates in the time domain. The top plot shows the nonwhitened template, which would be used if the noise is white. The bottom plot shows the whitened templates, which have to be used if the noise is correlated. Middle panel: the two templates in the Fourier domain. The green line shows the fiducial PSD that was used for whitening in this example. Right panel: the cosine angle closeness metric between the templates as a function of their duration. The solid line corresponds to the match of nonwhitened templates, or to the case when the noise is not correlated. The dashed lines stand for the whitened templates, which have to be used if the noise is correlated.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Left panel: estimation (performed on simulated noise) of SNR losses due to the PSD measurement errors as a function of the PSD estimator slice length. Different lines represent losses due to different sources of PSD measurement error discussed in the text. The thick blue line shows their sum, which is the total SNR loss. Right panel: loss in SNR2 caused by planetary transit biasing the PSD measurement. Different colors denote cases of different SNRs of the overfitted transit. Dashed lines correspond to the case when a preliminary detrending (high-pass filtering) was performed. For long transit durations, detrending already removes a significant part of their SNR concentrated at low frequencies, therefore the residual loss from the PSD overfitting becomes less significant.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Comparison of the detection efficiency of the UMES, CMES, and IMES scores. Vertical axis: all injections that crossed the detection threshold for the corresponding score. The detection thresholds and the injection distributions are shown in Figure 16. The timings of the transits were identified correctly for all the injections that crossed the detection threshold. Left panel: detection fraction presented as a function of the UMES score of the injections. Right panel: same data as the left panel presented as a function of the IMES score.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Distribution of the scaled density parameter of Kepler stars from the Gaia–Kepler crossmatch catalog (M. Bedell 2022). Objects excluded from the search, filtered based on stellar mass and radius, are shown in different colors, with the purple contour indicating the stars ultimately selected. Vertical black dashed lines mark the density bin edges used for the prior calculations.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Blue shading: histograms of the distributions of the stellar and planetary parameters used in the Monte Carlo simulation for the template bank and prior generation. Triangles: parameters of the templates in the template bank, color coded by the template prior values. Magenta dots: parameters of transits which got poor coverage by the bank (<0.97 match).
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Receiver operating characteristic curves for injections in the UMES range of 50 to 80. Vertical axis: fraction of injections (Figure 16) that crossed the detection threshold. Left panel: detection fraction as a function of chosen background rate density (horizontal line in Figure 16). Right panel: detection fraction as a function of the measured false positive rate.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: The distribution of cosine angles (i.e., the closeness metric, see Appendix A) between generated transit models and their best-matching template from the bank, assuming a fiducial averaged whitening filter. It was obtained using a Monte Carlo simulation covering the parameter space of interest.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Pplanet for confirmed Kepler candidates as function of Kepler period. Color coding represents planetary radius in units of Earth radius.
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: A comparison between posteriors from the seven orbit models, listed in the legend. We find no obvious discrepancy between any data set. The bottom-left panel is a corner plot, and the top-right panel shows the predicted location on 2025 January 1, near the planet’s maximum separation from the star and the epoch of recent JWST observations. All contours encompass the volume contained within the 1σ two-dimensional Gaussian equivalent. The inclination and position angle of the outer disk model from M. Booth et al. (2023) fitted to ALMA data is overplotted as dashed lines. The ❉ indicates two models containing only RV data and only absolute astrometry data, respectively, and whose posteriors are therefore completely independent. The models indicated by ✦ include RV data, but distinct sets of astrometric data, making the position angles effectively independent. The posterior represented by black contours include all available RV and astrometric data. We draw the reader’s attention in particular to the Ω vs. i and Ω vs. m subpanels, which illuminate how each data source progressively constrains the orientation of the orbit.
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: Comparison of the orbit posteriors incorporating different sources of data. The blue dots mark the location of the planet on 2025 January 1. The colors of the orbit draws match those in Figure 2 for easier cross-referencing. The bottom-right panel shows the outer debris disk model fit to ALMA data by M. Booth et al. (2023). The red symbol indicates two models containing only RV data and only absolute astrometry data, respectively, and whose posteriors are therefore completely independent. The models indicated by the blue symbol include RV data, but distinct sets of astrometric data, making the position angles they indicate on 2025 January 1 effectively independent.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Injection parameters generated for one of the triggers using the scheme described in the text. Notation: ιi is the injected inclination, ei is the injected eccentricity, wi is the injected argument of periastron, duri is the injected transit duration, ﹩{({R}_{p}/{R}_{s})}_{i}﹩ is the injected planet-to-star radius ratio, and ﹩{\rho }_{r}^{2}﹩ is the recovered detection score. Blue distributions represent injections whose timing was successfully identified by the pipeline, while orange represents those missed. The 1D histograms are normalized to units of density. The total number of successful and failed injections is shown in the legend.
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: Orbits sampled from the RV, Hipparcos, DR3 model (blue) and the complete RV, Hipparcos, FGS, DR2 and DR3 model (black) compared against all data. This shows how the addition of the DR2 and FGS data constrains the motion of the star in the R.A. direction. The horizontal bars in the proper-motion panels show the time range over which each measurement is fit by their respective catalogs. The light blue markers show binned FGS data, with the size of the marker indicating the number of data points in the bin.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Same as Figure 15 but for the UMES score (i.e., without non-Gaussianity correction, template marginalization, and peak integration). Top panel: recovered UMES as a function of the injected SNR2 for various numbers of transits. The deviation from the identity shows the SNR loss not associated with the non-Gaussianity correction. Bottom panel: fraction of successfully detected injections crossing the fiducial detection threshold of 55.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Comparison of IMES and UMES scores to Kepler MES2 for confirmed faint KOIs. Points are color coded by orbital period. Left panel: IMES score vs. Kepler MES2. The diagonal line represents the identity, and the dashed horizontal line indicates the empirical detection threshold discussed in Section 7. Right panel: UMES score vs. Kepler MES2. The detection threshold is not provided because it is harder to define it for the UMES score due to the non-Gaussian background (see Section 8.2).
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: Covariances between R.A. and decl. velocity at each proper-motion epoch, for the RV, Hipparcos, FGS, DR2 and DR3 model. The “H” epoch is the net proper motion at the Hipparcos epoch calibrated to the DR3 velocity reference by the HGCA, “G-H” is the long-term proper motion derived from the HGCA, “DR2” is the Gaia DR2 reported proper motion after correcting for frame rotation, and “DR3” is the Gaia DR3 proper motion. Both the DR2 and DR3 values have uncertainties inflated according to the multipliers given in the HGCA, DR2 (T. D. Brandt 2018) and eDR3 versions (T. D. Brandt 2021).
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: Maximum a posteriori sample from the complete RV and astrometry model. RV data from each instrument. The scatter in the RV data is well modeled by a GP with a quasiperiodic kernel, just as reported in previous works.
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: Zoom in of Figure 3 showing the dense sampling of HARPS data over 1.5 days in 2004 October. The blue line and band show the GP model mean and standard deviation, respectively. The planet’s contribution to the RV signal is essentially flat over this short time range. The inclusion of these data in particular causes an apparent eccentricity signal if not modeled with a GP. Dropping these data leads to a low-eccentricity solution, even without a GP.
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: Predicted locations of planet b in 1 yr increments. The contours represent 1σ Gaussian equivalent volumes. Both 1σ and 3σ contours are plotted for the full model, indicated in black. The dark outlined panels in the bottom row correspond to notable imaging epochs.
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: Marginal mass and inclination posteriors for planet b based on contributions from different data sets. We find that the model including all data, shown in black, finds a mass of 1.00 ± 0.10 MJup, which is somewhat higher than previous estimates but in the range we would expect for a planet aligned with the outer debris disk. The white contours indicate 1σ and 3σ, while the gray bands indicate the 68.5% CI.
Paper: Revised Mass and Orbit of ε Eridani b: A 1 MJup Planet on a Near-circular Orbit
Authors: William Thompson, Eric L. Nielsen, Jean-Baptiste Ruffio, Sarah Blunt, Christian Marois
Figure caption: Marginal eccentricity posteriors from leave-one-instrument-out cross-validation of RV data sets. The legend specifies which data set is ignored. We find that the GP model (left) is more predictive of held out data than the model without a GP (right). Dropping the HARPS (pre) data from the no-GP model also makes the eccentricity nearly consistent with zero ([0.02, 0.12]).
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Pre-detrended QLP light curves from Sectors 7, 34, 61, 87, and 88 for TIC-107150013. There are no events with comparable significance to the event in Sector 61 at ∼2987 days. The increase in noise in later sectors is due to their shorter cadences, which are associated with higher per-point uncertainties. Sector 7 was observed at 30-minute cadence, Sector 34 was observed at 10 minutes, and Sectors 61–88 were observed at 200 s. The light curves potentially indicate stellar variability over timescales on the order of tens of days, but TESS alone is not able to constrain the amplitude and period of this variability owing to systematic differences between TESS orbits.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Expected FFP detection rate per dex in mass, across all currently available TESS sectors from QLP (Sectors 1–71). The range of values corresponds to different underlying mass functions, based on the central best-fit values describing the Sumi et al. power law and the ±1σ uncertainties (T. Sumi et al. 2023). TESS is most sensitive to FFP events between 0.01 < M/M⊕ < 0.1.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Detrended QLP light curves from Sector 61 (top) and Sector 62 (bottom) for TIC-123147666, which feature a brightening event that was initially identified in Sector 61 as a potential microlensing event before repeating events were identified in other TESS sectors. This event is likely caused by tidal distortion in a highly eccentric binary star system. The heartbeat nature of the event is more obvious in Sector 62, further emphasizing the need for multiple sectors when performing microlensing searches with TESS.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Flux- and pixel-level data associated with the source star TIC-107150013, which features a high-SNR (SNR = 31) transient signal at 2987 days. The direct image reflects the typical field near the target (pink star), while the difference image reflects the pixels undergoing the largest brightening over the event. White circles show the locations of all stars down to 4 mag fainter than the target star, with sizes scaled by brightness. The difference image is consistent with the signal being colocated with the target star.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Examples of BLS-detected brightening events corresponding to flares (left) and scattered light (right). The flare event has a skew shape parameter α = 137 based on a fit to a skew normal distribution (red line), which indicates strong asymmetry. The scattered light event reflects the most common type of microlensing false positive in TESS data, representing ∼80% of BLS-detected events.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Pixel-level data demonstrating typical signatures for asteroids (left) compared to isolated events (right), using examples associated with TIC-141479395 and TIC-432012378, respectively. These data were produced by subtracting the mean out-of-event image from each image within 1.5τ of the center of a given event and finding the maximum value of each pixel.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: The primary brightening event associated with TIC-107150013 (left) and the secondary smaller bump earlier in the light curve (right) overlaid with colored lines showing the best-fit FSPL lensing model (black), M. Pitkin et al. (2014) flare model (orange), and J. R. A. Davenport et al. (2014) flare model (green). We also show a M. Pitkin et al. (2014) flare + flare model (dotted orange) and FSPL + flare model (dotted black) for the primary event only (see text). The bottom panel shows the residual light curve and each model after removal of the baseline models chosen to interpret the events (FSPL model for the primary event; J. R. A. Davenport et al. 2014 model for the secondary event).
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Hypothetical lens masses (blue) and relative velocities (red) at different lens distances based on the FSPL fits to the TGLC light curve. The shaded regions correspond to the 16th−84th percentiles of the fit results for θE and tE, with uncertainties from Rs and ds propagated, while the solid line corresponds to the median values. Note that some regions are more likely than others, as discussed in 4.2.2. The dotted gray line corresponds to 13MJup, which we assume is the largest possible planetary mass.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: All flares manually flagged as symmetric and microlensing-like out of a subset of 291 flares compiled by M. N. Günther et al. (2020). These flares would all have been rejected by our automated vetting tests, due to large intrinsic red noise and the presence of other flares in the light curve, but suggest a possible symmetric flare occurrence rate up to ∼1%. See Section 4.3 for details.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Histogram of flare energies for 57,961 flares measured by Z. Yang et al. (2023) from TESS Sectors 1–30, compared to the measured flare energy of the primary brightening event associated with TIC-107150013.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: The TESS event associated with the source star TIC-107150013, as seen in TGLC (left) and QLP (right) Sector 61 light curves. The red lines show the median PSPL fits, while the black lines show the median FSPL model fits. Based on comparing BIC values for each result, the FSPL fits are overwhelmingly preferred. The residuals show the light curve after removal of the FSPL model.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Detrended Sector 61 light curves for TIC-107150013, as extracted by TGLC (top) and QLP (bottom). The black points show the data binned in 1 hr bins. The signal at 2987 days is visually consistent between the two light curves, with similar shape, duration, and amplitude.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: Corner plot displaying the emcee posteriors from the FSPL fit to the TGLC light curve of TIC-107150013.
Paper: Searching for Free-floating Planets with TESS: Results from Sectors 61–65
Authors: Michelle Kunimoto, William DeRocco, Nolan Smyth, Steve Bryson, B. Scott Gaudi
Figure caption: 20 s cadence SPOC PDCSAP light curve for TIC-107150013 from Sectors 87 and 88. There are no repeated signals resembling the event from Sector 61, nor any indications of flares.