adsabs/AstroCLIMB huggingface dataset:
Paper: Eight New Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Michael C. Cushing, Robert A. Stiller, Jeffrey A. Munn, Frederick J. Vrba, Justice Bruursema, Stephen J. Williams, Michael C. Liu, Alexia Bravo, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Dan Caselden, Martin Kabatnik, Arttu Sainio, Thomas P. Bickle, William Pendrill, Nikolaj Stevnbak Andersen, Melina Thévenot
Figure caption: Gemini/GNIRS spectra in full-resolution (gray) and smoothed (black) compared to spectral standards (red–orange). The spectra are normalized between 1.27 and 1.29 μm and offset by integer values for clarity. The spectral standards are: 2MASSI J1010148−040649 (L6; I. N. Reid et al. 2006), 2MASSW J1632291+190441 (L8; A. J. Burgasser 2007), DENIS-P J0255-4700 (L9; A. J. Burgasser et al. 2006a), SDSSp J125453.90−012247.4 (T2; A. J. Burgasser et al. 2004), 2MASS J12095613−1004008 (T3; A. J. Burgasser et al. 2004), and 2MASS J15031961+2525196 (T5; A. J. Burgasser et al. 2004).
Paper: Eight New Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Michael C. Cushing, Robert A. Stiller, Jeffrey A. Munn, Frederick J. Vrba, Justice Bruursema, Stephen J. Williams, Michael C. Liu, Alexia Bravo, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Dan Caselden, Martin Kabatnik, Arttu Sainio, Thomas P. Bickle, William Pendrill, Nikolaj Stevnbak Andersen, Melina Thévenot
Figure caption: Color vs. near-infrared spectral type diagram for L and T dwarfs from the UHS survey in A. C. Schneider et al. (2023; gray circles) compared to candidate and confirmed Hyades L and T dwarfs (colored circles). Median colors for each spectral type for field-age objects are labeled gray squares. The error bars on the median values represent the 16 and 84 percentile ranges as determined in A. C. Schneider et al. (2023).
Paper: Eight New Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Michael C. Cushing, Robert A. Stiller, Jeffrey A. Munn, Frederick J. Vrba, Justice Bruursema, Stephen J. Williams, Michael C. Liu, Alexia Bravo, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Dan Caselden, Martin Kabatnik, Arttu Sainio, Thomas P. Bickle, William Pendrill, Nikolaj Stevnbak Andersen, Melina Thévenot
Figure caption: The positions and proper motion vectors of our new substellar Hyades candidates (red) and known L and T type candidate members of the Hyades (blue; A. C. Schneider et al. 2022) compared to all known Hyades members (gray) within the halo radius (18 pc) from the Gaia Catalog of Nearby Stars (Gaia Collaboration et al. 2021).
Paper: Eight New Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Michael C. Cushing, Robert A. Stiller, Jeffrey A. Munn, Frederick J. Vrba, Justice Bruursema, Stephen J. Williams, Michael C. Liu, Alexia Bravo, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Dan Caselden, Martin Kabatnik, Arttu Sainio, Thomas P. Bickle, William Pendrill, Nikolaj Stevnbak Andersen, Melina Thévenot
Figure caption:  J − W2 vs. K − W2 colors for known L and T dwarfs from the UKIRT Hemisphere Survey (A. C. Schneider et al. 2023) compared to discoveries from A. C. Schneider et al. (2022) and new candidates presented in this work. Note that the color cut requiring new candidates have K − W2 colors greater than 1.0 mag effectively eliminates the late-M-type objects that contaminated the A. C. Schneider et al. (2022) sample.
Paper: Eight New Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Michael C. Cushing, Robert A. Stiller, Jeffrey A. Munn, Frederick J. Vrba, Justice Bruursema, Stephen J. Williams, Michael C. Liu, Alexia Bravo, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Dan Caselden, Martin Kabatnik, Arttu Sainio, Thomas P. Bickle, William Pendrill, Nikolaj Stevnbak Andersen, Melina Thévenot
Figure caption: Spectral binary fits for CWISE J041259.89+085049.6 and CWISE J045800.69+100456.9. The individual components used in the fits are 2MASSI J0825196+211552 (L7; J. D. Kirkpatrick et al. 2000; A. J. Burgasser et al. 2010), 2MASSW J1632291+190441 (L8; J. D. Kirkpatrick et al. 1999; A. J. Burgasser 2007), SDSS J125453.90−012247.5 (T2; S. K. Leggett et al. 2000; A. J. Burgasser et al. 2004), and WISEPC J223937.55+161716.2 (T3; J. D. Kirkpatrick et al. 2011).
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: The timing of the photometric measurements. The top panel shows the dates of the color measurements and the bottom marks the dates of both the single-band measurements that go into the color measurements as well as the supplemental K’ photometry.
Paper: Eight New Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Michael C. Cushing, Robert A. Stiller, Jeffrey A. Munn, Frederick J. Vrba, Justice Bruursema, Stephen J. Williams, Michael C. Liu, Alexia Bravo, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Dan Caselden, Martin Kabatnik, Arttu Sainio, Thomas P. Bickle, William Pendrill, Nikolaj Stevnbak Andersen, Melina Thévenot
Figure caption: Comparison of the near-infrared spectrum of CWISE J042222.17+213900.5 to the likely AB Dor member WISEA J020047.29−510521.4 (A. C. Schneider et al. 2017).
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Left: slopes (﹩{\theta }_{{H}-{K}^{\prime} }﹩) in CMD space against K’ variability metric (﹩{\chi }_{\nu }^{2}﹩) over the H − K’ color baseline. Sources more likely to belong to the extinction Gaussian are colored in black, while those that are less likely are colored in white. As a reference, points marked with a star are considered in the K’ – L’ modeling. Right: results of the error-corrected Gaussian mixture model (ecGMM) for the entire H − K’ population of slopes in the CMD. The model prefers two groupings. In H − K’, the extinction population—in black—has slopes around 55° ± 5° and this group comprises around 30% of the sample. The rest of the population—represented by the gray Gaussian—has ﹩\langle {\theta }_{H-K{\rm{{\prime} }}}\rangle ﹩ inconsistent with extinction variability effects.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Color–magnitude relationships for several stars that show significant color variations. On the left are the K’ vs. H − K’ CMDs, and on the right are the K’ vs. K’ − L’ diagrams. Plotted are individual measurements for each star as well as the best-fit linear models; the linear models are parameterized by an angle θ from the horizontal. The overplotted gray lines are 100 randomly sampled points from the Markov Chain Monte Carlo (MCMC) chains.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Bottom: CMD (mean K’ vs. mean H − K’) of extinction variable sources (marked in black) and nonvariables found in H − K’ (marked in gray crosses). The error bars on the extinction sources are derived from the observed ﹩{\rm{\Delta }}K{\rm{^{\prime} }}﹩. Top: histogram of mean H − K’ color for nonvariables (in gray) and sources that have variability consistent with extinction (in shaded black).
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: All nine dipping sources’ time series in K’. K’ single-band data are marked with open circles, the H − K’ color samplings are marked with black circles, and the K’ – L’ color samplings are marked with black squares. We fit a Gaussian model to each dip in K’, which is shown by the dashed gray line.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Average L’ relative photometric uncertainty as a function of stellar brightness. The points plotted are the average uncertainties for each star’s relative brightness across all epochs and include both the statistical and zero-point uncertainties. Only the nonvariable stars highlighted in Table D1 are shown.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Left: slopes (﹩{\theta }_{{K}^{\prime} -{L}^{\prime} }﹩) in color–magnitude space against the K’ variability (﹩{\chi }_{\nu }^{2}﹩) for the 12 sources that are variable in K’ over the K’ − L’ sampling and are consistent with extinction variability in H − K’. Right: results of the one-component ecGMM. The model prefers a mean slope ﹩\langle {\theta }_{{K}^{\prime} -{L}^{\prime} }\rangle ﹩ around 73° ± 2°.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Average extinction variability in R. Schödel et al. (2010)'s extinction map (in gray) compared to the change in magnitude (﹩{\rm{\unicode{x00394}K}}^{\prime} ﹩) for each extinction event (in red). The changes in extinction, ﹩{\rm{\unicode{x00394}K}}^{\prime} ﹩, that we observe are on average consistent with the extinction variations seen in R. Schödel et al. (2010), although we observe changes that are around a magnitude larger.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Extinction map from R. Schödel et al. (2010), which has a resolution of ∼1″. Extinction sources are marked in black and tend to be in more extinguished regions; Sgr A* is marked with a star at the center of the field. Our experiment’s resolution—∼50 mas—is smaller than the black points.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Location on an L’ image (2021 August 15) for all extinction variability sources. Three known L’ features, identified by K. Mužić et al. (2007), are also marked in red.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Wavelength (in units of μm) compared to the relative extinction (in reference to K’) at our experiment’s effective wavelengths: H = 1.654 μm, K’ = 2.125 μm, and L’ = 3.741 μm. Plotted are values found by other studies such as S. Nishiyama et al. (2009), R. Schödel et al. (2010), and T. K. Fritz et al. (2011). Both S. Nishiyama et al. (2009) and R. Schödel et al. (2010) are plotted assuming the derived broken power-law slopes and their errors from each paper. For T. K. Fritz et al. (2011), the value is calculated assuming the first column of their Table 9 for the NIRC2 H, K’, and L’ filters. We plot the effect of grain size (using R  V  as a proxy) on the relative extinction, assuming the model as presented in J. C. Weingartner & B. T. Draine (2001). In general, our results (in black) are consistent for H. We find more extinction at L’ with our methods, suggesting a grayer extinction in the mid-infrared, possibly due to larger dust grains local to the GC.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption: Plot of mean HH-K’ − K’ and K’ − L’ color for sources that are detected in all three wavelengths. Nonvariable sources are plotted in gray and their L’ information is provided in Table D1. We plot the movement in color–color space of sources where we measure a slope in both the H − K’ and K’ − L’ CMDs. The sources which are consistent with extinction follow our average local reddening vector as they change color; the mean colors tend to follow the integrated reddening along the line of sight, assuming the result of T. K. Fritz et al. (2011), which is marked by the dashed gray line.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption:  K’ vs. H − K’ CMD for extinction variability stars. The overplotted gray lines are 100 randomly sampled points from the MCMC chains (1).
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption:  K’ vs. H − K’ CMD for extinction variability stars. The overplotted gray lines are 100 randomly sampled points from the MCMC chains (3).
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption:  K’ vs. K’ − L’ CMD for extinction variability stars. The overplotted gray lines are 100 randomly sampled points from the MCMC chains.
Paper: The Galactic Center in Color: Measuring Extinction with High-proper-motion Stars
Authors: Zoë Haggard, Andrea M. Ghez, Shoko Sakai, Abhimat K. Gautam, Tuan Do, Jessica R. Lu, Matthew Hosek, Mark R. Morris, Sean Granados
Figure caption:  K’ vs. H − K’ CMD for extinction variability stars. The overplotted gray lines are 100 randomly sampled points from the MCMC chains (2).
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: TTV diagram for analyzing 230 midtransit times of TrES-2b. The dashed black line and red and blue curves represent the linear, orbital decay, and apsidal precession models. The lines are drawn for 100 randomly chosen sets of parameters from the Markov chains of posteriors of the orbital decay (brown) and apsidal precession (cyan) models. The models are extrapolated for the next ∼17 yr to illustrate the broad spectrum of possible solutions.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Generalized Lomb–Scargle periodogram computed for the timing residuals of TrES-2b.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Top panel: time-series data of TrES-2b observed by TESS within sector 40. Middle panel: corresponding OOT time-series data along with the best-fit GP model (red curve). Bottom panel: detrended time-series data corresponding to the top panel.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: A comparative analysis of midtransit times derived from both observer data and our calculations, where O − C represents the deviation of the observed midtransit times from our derived midtransit times. The sky blue shaded region shows the maximum deviation range from the central line.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Top panel: time-series data of TrES-2b observed by TESS within sector 26. Middle panel: corresponding OOT time-series data along with the best-fit GP model (red curve). Bottom panel: detrended time-series data corresponding to the top panel.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Top panel: time-series data of TrES-2b observed by TESS within sector 55. Middle panel: corresponding OOT time-series data along with the best-fit GP model (red curve). Bottom panel: detrended time-series data corresponding to the top panel.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Top panel: time-series data of TrES-2b observed by TESS within sector 54. Middle panel: corresponding OOT time-series data along with the best-fit GP model (red curve). Bottom panel: detrended time-series data corresponding to the top panel.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Top panel: time-series data of TrES-2b observed by TESS within sector 41. Middle panel: corresponding OOT time-series data along with the best-fit GP model (red curve). Bottom panel: detrended time-series data corresponding to the top panel.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: The normalized relative flux of TrES-2b as a function of the time (the offset from midtransit time and in TDB-based BJD) of individual transits taken from ETD. The points are the data of the raw flux, solid red lines are the best-fit models for the model flux, and E is the calculated epoch number.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: The normalized relative flux of TrES-2b as a function of the time (the offset from midtransit time and in TDB-based BJD) of individual transits observed by TESS. The points are the data of the raw flux, solid red lines are the best-fit models for the model flux, and E is the calculated epoch number.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Same as Figure A10 but for the remaining epochs.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Same as Figure A7 but for the remaining epochs.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Top panel: time-series data of TrES-2b observed by TESS within sector 75. Middle panel: corresponding OOT time-series data along with the best-fit GP model (red curve). Bottom panel: detrended time-series data corresponding to the top panel.
Paper: Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
Figure caption: Top panel: time-series data of TrES-2b observed by TESS within sector 74. Middle panel: corresponding OOT time-series data along with the best-fit GP model (red curve). Bottom panel: detrended time-series data corresponding to the top panel.
Paper: Improving Power Spectrum Estimation Using Multitapering: Efficient Asteroseismic Analyses for Understanding Stars, the Milky Way, and Beyond
Authors: Aarya A. Patil, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, David J. Thomson
Figure caption: Power spectrum analysis of the pseudowindow generated using the irregular sampling times of the Kepler-91 light curve shown in the top left panel. The top right panel displays the synthetic light curve composed of two sinusoidal signals sampled at the times t  n  of the Kepler-91 series. The bottom panel shows a zoomed-in version of the LS (black) and NUFFT (gray) periodograms of the synthetic light curve x ⋆(t  n ) as compared to the true PSD (orange). The two estimates of the true spectrum are nearly identical, and both show inconsistency and spectral leakage compared to the true PSD. Note that the bottom panel is in log scale, whereas its inset is in linear scale to better view the difference between the signals and the noise.
Paper: Improving Power Spectrum Estimation Using Multitapering: Efficient Asteroseismic Analyses for Understanding Stars, the Milky Way, and Beyond
Authors: Aarya A. Patil, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, David J. Thomson
Figure caption: Both panels show the same pseudowindow as that in the bottom panel of Figure 3, but for the NUFFT and mtNUFFT periodograms. The top panel shows the spectral leakage properties of the mtNUFFT periodogram with NW = 1 and K = 1, i.e., the single-tapered power spectrum estimate, in blue, whereas the bottom panel shows the NW = 1.5, K = 2 mtNUFFT estimate in dark pink. It is clear that the mtNUFFT estimates have smaller spectral leakage than NUFFT. In the bottom panel, we observe that as NW increases, the variance of the estimate reduces but the frequency resolution worsens.
Paper: Improving Power Spectrum Estimation Using Multitapering: Efficient Asteroseismic Analyses for Understanding Stars, the Milky Way, and Beyond
Authors: Aarya A. Patil, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, David J. Thomson
Figure caption: Schematic diagram illustrating the estimation of the mtNUFFT periodogram described in Section 2.2.3. The left panel shows the Kepler-91 time series for which we compute the power spectrum estimate. The middle panels show three DPSS or Slepian tapers with time-bandwidth product NW = 2 and order k = 0, 1, 2 (number of tapers K = 2NW − 1), their corresponding tapered time series, and the single-tapered NUFFT periodograms. The rightmost panel shows the multi-tapered NUFFT or mtNUFFT periodogram that is constructed by averaging the three single-tapered estimates with adaptive weights d  k (f).
Paper: Improving Power Spectrum Estimation Using Multitapering: Efficient Asteroseismic Analyses for Understanding Stars, the Milky Way, and Beyond
Authors: Aarya A. Patil, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, David J. Thomson
Figure caption: Distributions of best-fit parameters for realizations from a simulated p-mode with frequency ν 0, width w 0 and height h 0. The left panel shows the deviation of the frequency estimates ν from the true value ν 0, whereas the middle and right panels show this deviation for the width and height estimates respectively. The blue and orange distributions are obtained by fitting the LS and mtNUFFT periodograms respectively, and their mean values are shown using dotted blue and orange lines. The standard deviations of the two frequency distributions in the left panel are on the order of 8 × 10−4, whereas the Libbrecht formula for the precision limit of infinite SNR p-modes is 4 × 10−4.