adsabs/AstroCLIMB huggingface dataset:
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: Evolutionary tracks and stellar mass dependence for XUV and bolometric luminosity. Colors and corresponding ages are the same for all panels. Top left: time-integrated cumulative XUV luminosity (relevant for photoevaporation) for a selection of key ages, including the approximate age (∼4.6 Gyr; Berger et al. 2020b) of the Kepler field, using evolutionary tracks from Johnstone et al. (2021). Gray dashed lines indicate log–log relations fit independently at each time. Top right: the exponential dependence ξ of integrated XUV luminosity on stellar mass for the log–log fits of ﹩L\propto {M}_{* }^{\xi }﹩ as a function of stellar age. Bottom left: similar to the XUV luminosity panel, but now using bolometric evolutionary tracks (relevant for core-powered mass loss) using data from Baraffe et al. (2015). Bottom right: similar to the integrated XUV exponent panel, but now using integrated bolometric luminosity.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: Best-fit parameters as a function of stellar mass. Each panel represents a different free parameter, and each mass bin was fit independently. Vertical error bars indicate 1σ uncertainties as the 16th and 84th percentile values from the posterior. Horizontal error bars represent the stellar mass range of each bin.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: The occurrence of small planets marginalized over orbital period (2 ≤ P orb ≤ 100 days) as a function of planet radius. Each panel represents a different stellar mass bin, with the full FGK sample shown in the lower right. Black points are the observed marginalized occurrence as calculated by epos for a selection of planet radius bins. Blue lines indicate the best-fit distributions evaluated for that bin.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: The occurrence of small planets marginalized over planet radius (1 ≤ R p ≤ 3.5 R ⊕) as a function of orbital period. Each panel represents a different stellar mass bin, with the full FGK sample shown in the lower right. Black points are the observed marginalized occurrence as calculated by epos for a selection of orbital period bins. Blue lines indicate the best-fit distributions evaluated for that bin. Gray lines represent the best-fit distributions scaled by the average detection efficiency computed for stars in that bin.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: Similar to Figure 4, but without considerations of reliability for both the best-fit model and the epos-derived occurrence rates. The results of the inverse detection efficiency method change more under the effects of reliability implementation than those of our forward model, likely due to the former’s stronger susceptibility to biases in bins with a low number of observations.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: Orbital period and radius distributions for the planets in our samples, with density contours weighted by planet completeness. Each panel represents a different stellar mass bin, with the full FGK sample shown in the lower right. The location of the radius valley (black dashed line) follows the scaling of Wu (2019), and is used to separate the super-Earth (green) and sub-Neptune (blue) populations.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: left) A comparison of residuals between the measured midtransit times and a calculated linear ephemeris (reported in the plot legend). The gray shaded region indicates the uncertainty in the ephemeris extending to ±1σ using our best estimates in Table 7. The pink shaded region indicates an uncertainty based on the prior listed in Table 1. Some midtransit measurements are not used in the joint analysis because they were measured from partial transits. right) An ephemeris estimate for mideclipse times. The pink shaded region shows the uncertainty in a linear solution if we use the Spitzer measurement (Laughlin et al. 2009) as E mid along with the period from Bonomo et al. (2017). The gray shaded region indicates an uncertainty based on the orbital information listed in Table 7.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: A transit light curve of HD 80606 b measured with the TESS spacecraft using data from Sector 21. The TESS light curve is contaminated with light from a neighboring star causing the transit depth to appear smaller (by about ∼48%) than it really is. The plate scale of TESS is ∼21″ × 21″ and that is also coincidentally the distance between the nearby stellar companion, HD 80607, and HD 80606. Light contamination from the roughly equal brightness companion was summed in the aperture used for TESS photometry and will contribute to a smaller measured depth than observations from platforms with a higher imaging resolution, where the light sources can be treated separately. Despite the contamination shrinking the measured depth, we can still detect it to ∼44σ, which is enough to constrain the time of midtransit to within ∼3 minutes. The binned data is purely for visualization purposes and is at two different cadences, 30 minutes in black and 60 minutes in white with a black outline, while the transparent points are the original data.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: Posteriors for the joint fit between the radial velocity measurements, a transit light curve from TESS and historical measurements for midtransit and mideclipse. Measurements from Table 3 are included in an ephemeris estimate during the fitting process and added into the likelihood function. The best-fit radial velocity model can be found in Figure 4, the best-fit transit model is shown in Figure 1 and the final ephemeris is shown in Figure 6. The data points in each correlation plot are color coded to the likelihood, with darker colors representing higher likelihoods. The contours represent the Nσ boundary using the uncertainty reported in each column’s title.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: Top: the combined light curve showing the complete transit of HD 80606 b on 2021 December 7–8 along with a model fit to the observations (red line). The data are binned to a resolution of 30 minutes for each individual data set and 60 minutes for the combined data set (empty circles) for the purposes of visualization. Each observation is fit simultaneously with Equation (1) and requires a separate airmass model for detrending. A mosaic of individual light curves can be found in the Appendix. Bottom: residuals for the light-curve model are displayed at the native resolution except for a binned version shown in white circles. The standard deviation of the residual scatter is reported in the legend on the top subplot.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: Posteriors for the global light-curve solution on 2021 December 7–8. All of the observations shown in Figure 3 are fit simultaneously in order to constrain the time of midtransit and transit depth from a global light-curve model. Each observation was acquired at a different airmass and requires individual treatment in order to detrend properly, and those coefficients make up a majority of this distribution. The data points in each correlation plot are color coded to the likelihood, with darker colors representing higher likelihoods. The contour represents roughly the 1σ boundary using the uncertainty reported in each plot’s title. Each value in the prior starts as a uniform distribution.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: Position vectors for the HD 80606 system showing the planet and star plotted over the course of one orbital period for the planet. The colored segments represent chunks of the orbit spanning ∼1 day. The big plot has a viewing angle 90° above the line of sight. The small subplot also has a top-down view but of the star’s orbit. The markers indicate where midtransit, mideclipse, and periastron occur for the planet.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: Data from 2000 to 2022 show the extremely eccentric orbit of HD 80606 b. The time series RV measurements are plotted in the top panel, the best-fit model is in the middle panel, and the residuals are on the bottom panel. The standard deviation of the residuals is listed in the legend of the top subplot for each data set.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: A mosaic of observations for the transit of HD 80606 b on the night of 2021 December 7–8. A global light-curve model is overplotted in red. All of these observations are stitched together into a single time series shown in Figure 3.
Paper: Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST
Authors: Kyle A. Pearson, Charles Beichman, B. J. Fulton, Thomas M. Esposito, Robert T. Zellem, David R. Ciardi, Jonah Rolfness, John Engelke, Tamim Fatahi, Rachel Zimmerman-Brachman, Arin Avsar, Varun Bhalerao, Pat Boyce, Marc Bretton, Alexandra D. Burnett, Jennifer Burt, Charles H. Cynamon, Martin Fowler, Daniel Gallego, Edward Gomez, Bruno Guillet, Jerry Hilburn, Yves Jongen, Tiffany Kataria, Anastasia Kokori, Harsh Kumar, Petri Kuossari, Georgios Lekkas, Alessandro Marchini, Nicola Meneghelli, Chow-Choong Ngeow, Michael Primm, Subham Samantaray, Masao Shimizu, 正雄 清水, George Silvis, Frank Sienkiewicz, Vishwajeet Swain, Joshua Tan, Kalée Tock, Kevin Wagner, Anaël Wünsche
Figure caption: A map of the facilities in the global network of small telescopes used to observe the transit on 2021, December 7/8.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: The fractional occurrence of super-Earths (green) and sub-Neptunes (blue) relative to their combined planet occurrence. Each panel represents a different stellar mass bin, with the full FGK sample in the lower right. The colored numbers in each panel indicate the number of observed candidate planets of a given type within a particular orbital period bin (and stellar mass bin). Dashed points represent the observed occurrence as calculated by epos for a selection of orbital period bins. Solid lines indicate the best-fit distributions as evaluated for that bin. The horizontal gray line marks a fractional occurrence of 0.5, corresponding to an equal abundance of super-Earths and sub-Neptunes, and the orbital period where each fit matches this condition is marked by a vertical purple line. Shaded regions indicate 1σ envelopes.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: Top: the best-fit values of P central as calculated for each stellar mass bin. Vertical error bars represent the 1σ uncertainties in P central as drawn from their posteriors. In orange, we present log–log fits between stellar mass and orbital period, which has a dependence on stellar mass of α = 1.4 ± 0.5. Bottom: similar to above, but now plotting the median and 1σ uncertainties of P trans evaluated from the best-fit fractional occurrence curves; the orange line represents represents a log–log fit between stellar mass and transition period with α = 1.7 ± 0.2. In both panels, the rightmost vertical axis presents the same information converted to semimajor axis, with log–log fits shown by the dotted–dashed blue (top: α = 1.1 ± 0.3; bottom: α = 1.5 ± 0.1).
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: Graphical representation of the functional form adopted in this work to describe the close-in population of exoplanets. Top: a broken power law governs the overall orbital period distribution. Bottom: a transition function describes how the fractional occurrence behaves with period for super-Earths (green; 1 R ⊕ − R valley) and sub-Neptunes (blue; R valley − 3.5 R ⊕). Dots represent the relevant period free parameters (top: P break; bottom: P central). The purple line indicates the point P trans where sub-Neptunes become more common than super-Earths.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: The occurrence of super-Earths (green; 1 R ⊕ − R valley) and sub-Neptunes (blue; R valley − 3.5 R ⊕) as a function of orbital period. Each panel represents a different stellar mass bin, increasing from top to bottom. The colored numbers in each panel indicate the number of observed candidate planets of a given type within a particular orbital period bin (and stellar mass bin). Black vertical lines indicate the approximate orbital period where the occurrence curves cross.
Paper: The Demographics of Kepler's Earths and Super-Earths into the Habitable Zone
Authors: Galen J. Bergsten, Ilaria Pascucci, Gijs D. Mulders, Rachel B. Fernandes, Tommi T. Koskinen
Figure caption: The occurrence of super-Earths (green; 1 R ⊕ − R valley) and sub-Neptunes (blue; R valley − 3.5 R ⊕) as a function of orbital period, calculated for all planets in the full FGK sample (0.56–1.63 M ⊙). The colored numbers indicate the number of observed candidate planets of a given type within a particular orbital period bin. The black vertical line indicates the approximate location where the super-Earth and sub-Neptune curves cross.
Paper: A Silent Revolution in Fundamental Astrophysics
Authors: Zeki Eker, Faruk Soydugan, Volkan Bakış, Selçuk Bilir, Ian Steer
Figure caption: Independent BC–T eff relation at Gaia G, G BP, and G RP and Johnson B and V (Bakış & Eker 2022).
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: Upper panels: histogram plots of Figure 10, with respect to the rotation period and the semi-amplitude of the photometric variation. All the targets and the targets that are detectable in the J and Kp bands with a threshold of 1% are shown with gray, red, and the black diagonals, respectively. Lower panels: the rates of the detectable numbers to the total numbers of samples in the J and Kp bands (the red and black lines, respectively), corresponding to the upper panels. The vertical dashed lines represent the parameter ranges shown in Figure 12.
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: Histograms showing the number distributions of the minimum detectable radius ratio R p/R s (left) and the planetary radius R p[R ⊕] (right) with SDE = 7 for a given orbital period in each cluster. In the right panels, the vertical dotted and dashed lines denote the Earth and Neptune radii, respectively. The solid, dashed, and dotted lines of the histograms denote the different orbital periods of the injected planets (5 days, 10 days, and 15 days, respectively).
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: The distributions of PSs, CPs, and PCs in K2 with respect to the stellar rotation period (left column) and the semi-amplitude of the light curve (right column). From top to bottom: scatter plot of A vs. P rot; histograms of all PSs, CPs, and PCs; and line graphs showing the frequencies of CP and CP + PC among all PSs, respectively. In the top panel, the sizes and colors are the sizes and orbital periods, respectively, of the targets flagged as CPs (red) or PCs (blue).
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: Explanations of the analysis in Subsection 5.1 for three typical targets. For each target, the top panel plots the periodogram derived by FFT. The red, blue, and black data represent the sinusoidal modulation detected by the LS periodogram, white noise, and other correlated noise, respectively. In the middle panels, the range is narrowed to approximately 5 days, to clarify the details of the light curves reproduced by inverse FFT. The color relation is same as in the top panels. The bottom panels plot the original light curves in the Kp band (upper) and reproduced light curves assuming J-band observations (lower).