adsabs/AstroCLIMB huggingface dataset:
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Top: secondary eclipse depth (Stokes ΔI) vs. effective particle radius for SiO2, MgSiO3, and MnS particles. The pure Rayleigh secondary eclipse depth (dashed line) is calculated for geometric albedo Ag = 0.60. The Hubble secondary eclipse constraint is shown in the light gray box (T. M. Evans et al. 2013), which strongly favors MnS particles. Bottom: same as the top but for peak linear polarization (Stokes Δp), which strongly favors silicate particles. Lower limits to measured peak polarization are labeled on the right. Best-fit particle radii for data obtained at morning and evening terminators are shown (Section 3.4).
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Confidence of rejection of SiO2, MgSiO3, MnS, and pure Rayleigh models with various effective radii or geometric albedos based on B-band polarimetry data obtained near the HD 189733b evening terminator. The presence of 1 nm SiO2 particles (the low end of sizes consistent with JWST secondary eclipse spectra, J. Inglis et al. 2024) is inconsistent with polarimetry with 2.9σ confidence.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Top left: Stokes q data from Figure 1 plotted as a function of LST, whose heartbeat nature is due to telescope polarization. Polarization modulates rapidly as the target crosses the meridian (vertical dashed line). Top right: Stokes q data as a function of HD 189733b orbital phase, where orbital phase 0 and 1 represent midtransit (planet between host star and observer) and orbital phase 0.5 represents the center of the secondary eclipse (host star between planet and observer). Bottom: same as as the top but for Stokes u.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: B-band geometric albedo confidence limit from polarimetry data in the Gemini North orbital phase region (Figure 4), which places a 2σ lower limit to B-band geometric albedo of Ag > 0.26. The 1σ range in Ag from a Hubble secondary eclipse detection is shown in the gray region (T. M. Evans et al. 2013).
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Intrinsic B-band linear polarization of HD 189733b. Top: POLISH2 polarization measurements (gray points) compared to the best-fit SiO2 model (red and purple curves at left and right, respectively) as well as the model multiplied by a scaling factor of 1.53 to fit polarization measurements (blue and gold curves at left and right, respectively). Top left and right plots are identical, as the direction of the x-axis is reversed from left to right panels. Center: flux from the best-fit SiO2 model (blue-and-red curve at left, thin black curve at right) compared to flux from the model multiplied by 0.32 (thin black curve at left, gold-and-purple curve at right) to fit a Hubble secondary eclipse measurement (T. M. Evans et al. 2013, gold point at right). Bottom: intrinsic planetary linear polarization pintrinsic = Δp/ΔI obtained by dividing polarization models in top panels (choice of two models blue = gold or red = purple) by flux models in center panels (choice of two models blue = red or gold = purple). This generates four intrinsic polarization combinations following blue, red, gold, and purple curves from top to bottom panels. Models that produce pintrinsic > 100% are unphysical (horizontal, dashed line), which include those using T. M. Evans et al. (2013) secondary eclipse constraints. Blue (left panel) and gold data points (right panel) are shown, while red (left panel) and purple data points (right panel) are removed for clarity. Thin black curves at left and right mirror colored curves at right and left to guide the eye.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Intrinsic B-band linear polarization of HD 189733b (blue and red data points) in the Gemini North orbital phase overlap region (Figure 4). This is obtained by normalizing polarization measurements by the photometric phase curve of the best-fit SiO2 model (Figures 5 and 14, left center panel). The intrinsic polarization model (purple curve) is given by normalizing the best-fit polarization phase curve, scaled by 1.53, to this photometric phase curve (blue curve at bottom left in Figure 14). Also shown are blue optical measurements of solar system bodies measured from the ground (B. Lyot 1929; D. L. Coffeen & T. Gehrels 1969; A. Dollfus & D. L. Coffeen 1970, Venus) and from Pioneer 10 and 11 (M. G. Tomasko & P. H. Smith 1982; P. H. Smith & M. G. Tomasko 1984; M. G. Tomasko & L. R. Doose 1984, Jupiter, Saturn, and Titan). Ground-based observations of Uranus, obtained at effective orbital phases < 0.01 (J. J. Michalsky & R. A. Stokes 1977; S. J. Wiktorowicz et al. 2026), are consistent with Rayleigh scattering with 36.22% ± 0.89% efficiency (gold curve). HD 189733b appears to have intrinsic linear polarization slightly larger than Jupiter and Titan. Phase angles of solar system observations are converted to HD 189733b’s orbital phase.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Peak flux vs. peak polarization of scattered light from HD 189733b dominated by pure Rayleigh, SiO2, MgSiO3, or MnS scatterers. Peak polarization and flux increase monotonically as single scattering albedo, and thereby geometric albedo Ag, is increased for Rayleigh scattering models. Silicate models deviate from pure Rayleigh models for effective particle radii reff > 0.02  μm, while MnS models appear Rayleigh-like for reff < 0.05  μm. SiO2 and MgSiO3 peak polarization diverge for reff > 0.08  μm, while they diverge in flux for reff > 0.2  μm. Large MgSiO3 particles tend to be more reflective and polarized than SiO2 with the same effective radius. Numbers attached to each model point indicate reff of the scattering population in microns, and the color bar only applies to the Rayleigh scattering models. Measured 1σ, 2σ, and 3σ lower limits to measured linear polarization are shown.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Same as Figure 5 but for pure Rayleigh scattering only. Top: B-band Stokes q linear polarization measurements of HD 189733 vs. orbital phase compared to models containing pure Rayleigh scatterers. Blue and red data points indicate measurements obtained at the Lick 3 m and Gemini North, respectively. Peak polarization increases nonlinearly with increasing geometric albedo Ag. The best-fit, pure Rayleigh model occurs for Ag = 0.60 (dashed gold curve), which is essentially the theoretical limit for a pure Rayleigh atmosphere. Middle: same as the top but for Stokes u. Bottom: planetary flux modulation ΔI vs. orbital phase for pure Rayleigh models of varying geometric albedo. The T. M. Evans et al. (2013) Hubble secondary eclipse measurement, Ag = 0.226 ± 0.091, is shown in the light gray box.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Left: Stokes q (top) and u (bottom) data along with best-fit SiO2 models with one- (evening only, purple curve) and two-particle size distributions (evening and morning, gold curve), whose sizes are given in Table 7. One- and two-particle models overlap at the evening terminator, but they diverge at the morning terminator potentially due to grain growth via condensation on the night side of the planet. Center: same as the left but for MgSiO3. Right: same as the left but for MnS.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Same as Figure 10 but for MnS particles. While polarization measurements are best fit by reff ∼ 0.04  μm particles (solid blue curve at top and middle), the fit is worse than for silicates. Unlike for silicates, the MnS model that fits polarization measurements best also acceptably fits Hubble secondary eclipse photometry (solid blue curve at bottom) from T. M. Evans et al. (2013).
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Confidence of rejection of SiO2, MgSiO3, MnS, and pure Rayleigh models with various effective radii or geometric albedos based on B-band polarimetry data obtained near the HD 189733b morning terminator. This is in contrast to evening terminator data (Figure 8) and may suggest grain growth on the planet’s night side.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Same as Figure 10 but for MgSiO3 particles. While polarization measurements are best fit by ﹩{r}_{\,\rm{eff}\,}=0.03{5}_{-0.020}^{+0.047}﹩ μm particles (dashed blue curve at top and middle), Hubble secondary eclipse photometry (T. M. Evans et al. 2013) is best fit by 0.01 μm particles (solid dark blue curve at bottom).
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Same as Figure 10 but for SiO2 particles. While polarization measurements are best fit by ﹩{r}_{\,\rm{eff}\,}=0.03{8}_{-0.023}^{+0.047}﹩  μm particles (dashed blue curve at top and middle), Hubble secondary eclipse photometry (T. M. Evans et al. 2013) is best fit by 0.01 μm particles (solid dark blue curve at bottom).
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: B-band circular polarization (Stokes v) of the HD 189733 system measured at the Lick 3 m (blue points) and Gemini North (red points) as a function of HD 189733b’s orbital phase. Both Lick 3 m and Gemini North measurements are strikingly consistent, which would require intrinsic planetary circular polarization to be vintrinsic = 27.0% ± 2.8% (dashed gold curve). This is over 2 orders of magnitude larger than physically motivated models (L. Rossi & D. M. Stam 2018) and observations of solar system atmospheres. Near transit (orbital phases <0.25 and >0.75), the presence of circular polarization that is larger than the flux modulation from the planet (solid gold curve) precludes circular polarization originating from the planet. Therefore, another synchronously rotating mechanism appears to be present. Measured system circular polarization is larger than modeled linear polarization modulation from the planet (purple curve).
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: GJ 3222b, which is currently the lowest-mass exoplanet amenable to polarimetric scattered light characterization due to its high eccentricity (Tables 8 and 9). Left: top view of the planetary orbit, where the observer is located toward the bottom and the planet orbits counterclockwise. GJ 3222b’s highly eccentric orbit is fortuitously placed such that a highly polarizing geometry occurs for Rayleigh scattering while the planet is close enough to the host star to intercept a detectable fraction of stellar photons. Therefore, GJ 3222b has similar peak linear polarization to an exoplanet on a very close, circular orbit. The purple point indicates periastron and green indicates apastron. Center: zoom of the orbit centered on the star indicating gold and red-orange locations of the linear polarization peaks before and after periastron (purple point), respectively. Right: logarithmic stretch of GJ 3222b’s expected Rayleigh-like linear polarization signature, which rapidly peaks (gold point) prior to periastron (purple point), peaks again (red-orange point) after periastron, and rapidly dives back to undetectable levels. Blue points are spaced 30 minutes apart, and the sequence of gold/purple/red-orange geometries takes 73 minutes during each 10.7-day orbit.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Radius vs. equilibrium temperature for transiting Jovians in the NASA Exoplanet Archive (blue points), values binned in equilibrium temperature to guide the eye (red points), and R–T fits using a power law (K. Edmondson et al. 2023, Equation (4a), gold curve) and a four-parameter logistic equation from this work (4PL, Equation (4b), purple curve). The power law is not only unphysical for low Teq, but it overpredicts planetary radius for 725 K <Teq < 1750 K hot Jupiters (gold curve vs. red, binned data points). The 4PL fit accurately reproduces mean R–T measurements (purple curve vs. red points) and naturally accounts for cold Jovians such as Jupiter. Dashed vertical lines indicate where the power law and 4PL fits intersect.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Top: Gemini POLISH HD 189733 Stokes q (blue points) and u (red points) measurements vs. linear polarization orientation Θ from Figure 1 prior to telescope polarization subtraction. Solid lines indicate ﹩q={q}_{\,\rm{max}\,}\cos 2{\rm{\Theta }}﹩ and ﹩u={u}_{\,\rm{max}\,}\sin 2{\rm{\Theta }}﹩. Bottom: Stokes v measurements vs. Θ. No obvious sinusoidal trend is observed, suggesting residual instrumental crosstalk is negligible.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Estimated SNR of detection of the known transiting (dark circles) and nontransiting (open circles) exoplanets vs. Bmag assuming HD 189733b-like atmospheres and one full orbit of observation at Gemini North (Table 8). We model 21 exoplanets to be detectable with greater confidence than the HD 189733b detection in this work (red annotation). Exoplanet parameters are obtained from the NASA Exoplanet Archive.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Schematic of the processing stages leading to the single-transit statistic shown for simulated data. The final result is then passed to the periodicity search module. (1) The initial flux is taken, and bad segments are identified (marked in red). The green shading indicates the simulated planet. (2) The flux is conditioned: outliers are cleaned, low-frequency trends and peaks unresolved by PSD measurement are removed, and gaps are filled. (3) The flux is whitened using the measured PSD. (4) The single-transit statistic is obtained from matched filtering with one of the whitened templates. We note that templates are defined to have zero baseline and positive deviation at transits, therefore the statistic is negative at transits. (5) Large nontransit-like scores are identified and masked using the veto. They are included in the mask, and their score is zeroed. The masked points are represented with orange dots and will not have a contribution during the periodicity search. We can see that true transits passed the veto, but the points around them, where the shape is shifted and does not match the template, were masked.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Illustration of regular high-pass filtering compared to the piecewise detrending method shown for one of the Kepler targets (KIC003852808). Top left: Kepler flux (blue line) and its low-frequency Fourier component (black line). Bottom left: the flux, after subtracting the low-frequency trend, has a spurious drop, which may produce a false positive. Top right: Kepler flux (blue line) and its trend obtained using the piecewise detrending module. Bottom right: with the piecewise detrending, the break is mitigated.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Top panel: example of PSD estimation for several simulated noise samples. The black line is the true PSD used to generate the noise. The blue lines represent individual measurements, while the orange line shows the average PSD from these measurements. The red vertical line marks the resolution limit of frequencies whose power can be measured. Power below this threshold is removed. Bottom panel: relative error of the measurements from the top panel. The blue lines correspond to different noise samples. The black line is the average of the blue lines. The orange line is the error of their average (marked by the orange line in the top panel).
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Schematic of data conditioning on a simulated light curve represented in Fourier domain. (1) The original correlated (red noise) flux, including an additional noise peak. (2) The flux after detrending the low frequencies that cannot be resolved by the measured PSD. (3) The flux whitened after the PSD was measured and the whitening filter was constructed. (4) The flux after the peak detection and removal. (5) The final whitened flux, which will be used for statistic score calculation.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: The template bank of 58 templates used by the pipeline. The colors represent the template prior probability. The templates are normalized by their maximum and centered for demonstration purposes. During the SES calculation, these templates will be whitened and cross correlated with the whitened data.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Schematic representation of the pipeline (refer to the legend for color coding). The main flow shows how the light curve is processed to find the optimal IMES detection score. The module framed in the dashed line contains additional searches that are needed to evaluate the statistical significance of a threshold-crossing event.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Example of a trigger statistical significance analysis for one Kepler target, KIC006934045. The horizontal axis represents the IMES statistic, and the vertical axis shows the probability density of obtaining a given IMES per star in a search in the selected period range (0.35 days around the trigger period of approximately 266 days). Black vertical line: IMES value of the trigger obtained in the main search. Orange solid line: background distribution obtained from 5 · 104 scrambled searches. Orange dashed line: extrapolation of the background distribution (orange solid line). Red dotted line: same as the orange solid line, but the trigger was masked before running the scrambled searches. The extrapolation for this background distribution is not shown in this plot. Blue solid line: foreground distribution obtained in the injection–recovery campaign, normalized to the expected transiting planet rate in this period range. Blue dashed line: foreground distribution including injections for which the pipeline failed to detect the correct timing.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: SNR recovery fraction and detection efficiency in simulated light curves. Top panel: dependence of the recovered SNR2 on the injected SNR2 for different numbers of transits. The duration of the injected transits was 0.4 days. Each point is an average of multiple simulations, with the error bars showing the 1σ dispersion. The solid horizontal line shows the empirical detection threshold of the IMES corresponding to Pplanet ≈ 0.5. The dashed horizontal line shows the scores obtained in this simulation when no planet was injected. Bottom panel: relative number of injections that were identified at correct times and crossed the empirical detection threshold. They are plotted as a function of the injected SNR2 and for different numbers of transits.
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 inpainting filter compared to linear interpolation (shown for target KIC007742408). Gray regions represent masked points. Blue lines depict data with gaps filled using linear interpolation. Orange lines correspond to the gap filling with the inpainting filter. Top panel: Kepler flux. Interpolation just connects the two points outside the mask. The inpainting filter fills the gap as described in the text, leaving data outside the gaps unchanged. Middle panel: flux after applying the whitening filter. Cross talk between points inside and outside the gap modifies the data outside the gap in the linear interpolation case. Bottom panel: statistic score after matched filtering with a template. The blue line corresponding to linear interpolation exhibits two dips which might mimic transits. The inpainted orange line does not contain these peaks.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Distribution of different scores from empty scrambled searches and searches with injection. Solid lines: UMES, CMES, and IMES scores from empty scrambled searches. These distributions define the corresponding threshold. Black dashed–dotted line: nominal background density distribution defining the detection threshold. Vertical dotted line: threshold UMES, CMES, and IMES values, at which the corresponding score distributions cross the threshold density. Dashed lines: UMES, CMES, and IMES scores from injected searches.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Distributions of IMES detection score for the regular search and scrambled search over about 1.5 · 105 targets. The vertical axis shows the number of obtained triggers in this IMES bin. Blue line: scores from the regular, nonscrambled search. Orange line: scores from the scrambled search. Black vertical line: approximate empirical threshold for which the triggers result in Pplanet ≈ 0.5.
Paper: An Independent Search for Small Long-period Planets in Kepler Data. I. Detection Pipeline
Authors: Oryna Ivashtenko, Barak Zackay
Figure caption: Folded and binned time series for the trigger analyzed in Figure 12. Gray dots represent the folded time series, meaning that their time axis was taken modulo the trigger period. Black dots represent the binning of the gray dots. The plots are zoomed in on the transit; the full plots would span the entire orbital period of about 266 days. Top panel: folded whitened flux (Section 4.3.4). The red line shows the best-match whitened template from the template bank, with its amplitude estimated using Equation (N5). Bottom panel: folded SES time series obtained by cross correlating the closest whitened template with the whitened flux (Section 4.4.1). The red line represents the cross correlation of this template with itself, showing the expected SES response.