adsabs/AstroCLIMB huggingface dataset:
Paper: Low-frequency Radio Recombination Lines Away from the Inner Galactic Plane
Authors: Akshatha K. Vydula, Judd D. Bowman, David Lewis, Kelsie Crawford, Matthew Kolopanis, Alan E. E. Rogers, Steven G. Murray, Nivedita Mahesh, Raul A. Monsalve, Peter Sims, Titu Samson
Figure caption: Top: residuals after fitting and removing a five-term foreground model from simulated spectra in the 50–100 MHz band at LST 18 hr with 6 kHz resolution. The orange curve shows the residuals to a model without RRLs, whereas the blue curve includes modeled Cα, Cβ, and Hα lines. Middle: the residuals rebinned to 390 kHz for comparison with Bowman et al. (2018). Bottom: residuals after the foreground model is fitted and removed when a 200 mK flattened Gaussian global 21 cm absorption signal is also included in the simulated spectra. RRLs contribute to an increase in rms by 12 mK in the data. The difference in amplitude of the best-fit 21 cm profile is only 2 mK, an error of 1%.
Paper: Low-frequency Radio Recombination Lines Away from the Inner Galactic Plane
Authors: Akshatha K. Vydula, Judd D. Bowman, David Lewis, Kelsie Crawford, Matthew Kolopanis, Alan E. E. Rogers, Steven G. Murray, Nivedita Mahesh, Raul A. Monsalve, Peter Sims, Titu Samson
Figure caption: Peak normalized comparison of measured RRL strength and simulated proxy measurements as a function of LST. The average line profile magnitudes for Cα (purple diamonds) and Hα (red squares) are shown along with the Cα integrated optical depths (black circles). The simulated proxy measurement based on the Planck 115.27 GHz CO map (dashed–dotted green line) provides a reasonable predictor of relative RRL strength, particularly when the Galactic center is in the beam. However, it overpredicts the RRL strength at low LST. For reference, the continuum drift scan from EDGES observations (solid blue line) is plotted along with a simulated continuum drift scan using the Haslam et al. (1981) 408 MHz map (dotted black line). As expected, the continuum drift scans show a broader peak than the RRL scans, consistent with synchrotron emission extending farther from the Galactic plane compared to line emission.
Paper: Low-frequency Radio Recombination Lines Away from the Inner Galactic Plane
Authors: Akshatha K. Vydula, Judd D. Bowman, David Lewis, Kelsie Crawford, Matthew Kolopanis, Alan E. E. Rogers, Steven G. Murray, Nivedita Mahesh, Raul A. Monsalve, Peter Sims, Titu Samson
Figure caption: Comparison of simulated delay spectra for a baseline on the HERA radio telescope at LST 6 hr with and without assuming that RRL frequencies need to be masked. The dotted line shows the reference delay spectrum without flagging RRLs. Masking and inpainting RRL frequencies before the delay transform (solid line) raises the foreground leakage by over two orders of magnitude in the delay modes used for redshifted 21 cm science. A similar trend was observed for the other simulated LSTs and baselines in HERA.
Paper: Low-frequency Radio Recombination Lines Away from the Inner Galactic Plane
Authors: Akshatha K. Vydula, Judd D. Bowman, David Lewis, Kelsie Crawford, Matthew Kolopanis, Alan E. E. Rogers, Steven G. Murray, Nivedita Mahesh, Raul A. Monsalve, Peter Sims, Titu Samson
Figure caption: Stacked line profiles (blue) in mid-band EDGES data spanning the frequency range 108–124.5 MHz, with 375 ≤ n ≤ 392 and effective mean frequency of 116.3 MHz. The top panel shows a 2 hr LST bin centered on the Galactic center. A double-Gaussian model (orange) gives a best-fit Cα amplitude of −46 ± 15 mK. The best-fit Hα amplitude of 98 ± 38 mK, peaking 59 kHz below the carbon absorption, is about half of the peak level found at lower frequencies. The bottom panel shows a long 12 hr bin centered on LST 6 hr, yielding stacked line profiles consistent with no detection (best-fit Cα amplitude of 3.4 ± 3.5 mK).
Paper: Low-frequency Radio Recombination Lines Away from the Inner Galactic Plane
Authors: Akshatha K. Vydula, Judd D. Bowman, David Lewis, Kelsie Crawford, Matthew Kolopanis, Alan E. E. Rogers, Steven G. Murray, Nivedita Mahesh, Raul A. Monsalve, Peter Sims, Titu Samson
Figure caption: Same as Figure 6, but for the total radio emission visible by EDGES derived from the Haslam et al. (1981) 408 MHz sky map scaled to 70 MHz using a spectral index of β = − 2.4. The maps are dominated by synchrotron and free–free emission, which extends from the Galactic plane to higher latitudes compared to the CO emission observed by Planck.
Paper: Parameter Estimation for Open Clusters using an Artificial Neural Network with a QuadTree-based Feature Extractor
Authors: Lorenzo Cavallo, Lorenzo Spina, Giovanni Carraro, Laura Magrini, Eloisa Poggio, Tristan Cantat-Gaudin, Mario Pasquato, Sara Lucatello, Sergio Ortolani, Jose Schiappacasse-Ulloa
Figure caption: Superimposed t-SNE maps of synthetic and observed OCs. Synthetic clusters are color coded based on their distance modulus, while observed clusters are plotted with black dots.
Paper: Taxonomic Analysis of Asteroids with Artificial Neural Networks
Authors: Nanping Luo, Xiaobin Wang, Shenghong Gu, Antti Penttilä, Karri Muinonen, Yisi Liu
Figure caption: Spectra of (469) Argentina. The column on the right lists the rotational phase folded with a period of 8.79 hr. Each spectrum is offset for clarity.
Paper: Taxonomic Analysis of Asteroids with Artificial Neural Networks
Authors: Nanping Luo, Xiaobin Wang, Shenghong Gu, Antti Penttilä, Karri Muinonen, Yisi Liu
Figure caption: The confusion matrix. Each diagonal element in green indicates the number of samples having labels consistent with the Bus–Binzel taxonomy, given by the row index, while the elements in that row in yellow show the number of samples mislabeled into a class corresponding to the column of the value.
Paper: Taxonomic Analysis of Asteroids with Artificial Neural Networks
Authors: Nanping Luo, Xiaobin Wang, Shenghong Gu, Antti Penttilä, Karri Muinonen, Yisi Liu
Figure caption: Input data/spectra for the ANN. Blue shows the real and cloned spectra, and the red line represents the average spectrum for each class.
Paper: Taxonomic Analysis of Asteroids with Artificial Neural Networks
Authors: Nanping Luo, Xiaobin Wang, Shenghong Gu, Antti Penttilä, Karri Muinonen, Yisi Liu
Figure caption: Spectra of asteroids (696) Leonora and (780) Armenia.
Paper: Taxonomic Analysis of Asteroids with Artificial Neural Networks
Authors: Nanping Luo, Xiaobin Wang, Shenghong Gu, Antti Penttilä, Karri Muinonen, Yisi Liu
Figure caption: 55 reflectance spectra for 41 asteroids.
Paper: Taxonomic Analysis of Asteroids with Artificial Neural Networks
Authors: Nanping Luo, Xiaobin Wang, Shenghong Gu, Antti Penttilä, Karri Muinonen, Yisi Liu
Figure caption: The arrangement of CCDs, filters, and gratings in the survey module of the CSST.
Paper: Taxonomic Analysis of Asteroids with Artificial Neural Networks
Authors: Nanping Luo, Xiaobin Wang, Shenghong Gu, Antti Penttilä, Karri Muinonen, Yisi Liu
Figure caption: The structure of the artificial neural network. The network contains an input layer, a hidden layer, and an output layer. X represents the input, v and W represent weights, b represents biases, f represents the transfer function, and y represents the output.
Paper: Taxonomic Analysis of Asteroids with Artificial Neural Networks
Authors: Nanping Luo, Xiaobin Wang, Shenghong Gu, Antti Penttilä, Karri Muinonen, Yisi Liu
Figure caption: The blue line is the original data of SMASS II, and the red line is the resampled data.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Top: multitaper power spectrum estimate from the Kepler Q0 observations of KIC 6102338, using the tapers shown in Figure 2. The light blue shading shows the 95% confidence interval. The vertical crossbar shows the expected value of the jackknife variance estimate ﹩\widehat{{\boldsymbol{V}}{\boldsymbol{a}}{\boldsymbol{r}}\{}{\hat{S}}_{{xx}}(f)\}﹩, while the horizontal crossbar has width ﹩\tilde{\varpi }﹩. Green dots indicate signals that exceed the 1 − 1/N significance threshold (Section 3.5). Middle: the p-value given by the F-test for harmonic components, which is performed at each frequency (Section 3.5). Green dots mark the frequencies for which p < 1/N. Bottom: the Schuster periodogram (black) overplotted on the multitaper 95% confidence intervals (orange). The Schuster periodogram has larger variance than the multitaper, which is consistent with the distribution of each estimator (﹩{\chi }_{2}^{2}﹩ vs. ﹩{\chi }_{2K}^{2}﹩).
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Top: the six DPSS tapers with the highest spectral concentrations given N = 1639 and N ϖ = 4 (ϖ = 0.002441, ﹩\tilde{\varpi }=0.1194﹩ day−1). Bottom: the positive half of the K spectral windows W (k)(f) corresponding to each taper, with a vertical dotted line marking the bandwidth ﹩\tilde{\varpi }﹩. The legend at the lower right shows the values of k and λ that correspond to each taper.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Top: PDCSAP fluxes from the Kepler Q16 observations of KIC 6102338. Bottom: MDSS ﹩{w}_{n}^{\left(k\right)}﹩ for the 3534 observations plotted above, constructed with N ϖ = 4 and K = 6. The legend shows the spectral concentration of each W (k)(f). Gray shading highlights time stamps with missing data.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Left: distribution of absolute flux errors in the Kepler Q0 observations of KIC 6102338. Right: distribution of fractional flux errors in the same data set.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Kepler Q0 long-cadence observations of KIC 6102338 after replacing missing data.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Power spectrum estimates from the time series x  n  plotted in Figure 12. Top: the blue line shows the MDMT with ﹩{w}_{n}^{\left(k\right)}﹩ from Figure 12, with shaded 95% confidence intervals. Green stars show signals with significance at least 1 − 1/N according to the F-test. Middle: the p-value associated with the F-statistic at each frequency. Green stars have the same meaning as above. Bottom: the Lomb–Scargle periodogram plotted on top of the multitaper confidence intervals, with the dotted line showing the 1/N false alarm level.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Top: the MDMT power spectrum estimate calculated using the tapers in Figure 5. The shaded blue region shows the 95% confidence interval, while the green dots show oscillatory signals that are significant at the 1-1/N level according to the F-test.  Middle: the p-value given by the F-test for harmonic components, which is performed at each frequency (Section 3.5). Green dots mark the frequencies for which p < 1/N. Bottom: the Lomb–Scargle periodogram (gray) overplotted on the multitaper 95% confidence intervals (orange). The Lomb–Scargle periodogram has a larger variance than the multitaper, which is consistent with the distribution of each estimator (﹩{\chi }_{2}^{2}﹩ vs. ﹩{\chi }_{2K}^{2}﹩).
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Power spectrum estimates from the time series x  n  plotted in Figure 10. Top: the blue line shows the MDMT with ﹩{w}_{n}^{\left(k\right)}﹩ from Figure 10, with shaded 95% confidence intervals. Red stars show signals with significance at least 1 − 1/N according to the F-test. The green circle shows an additional signal with 99.9% significance. Annotations give the frequencies of all significant oscillations. Middle: the p-value associated with the F-statistic at each frequency. The red stars and green circle have the same meaning as above. Bottom: the Lomb–Scargle periodogram plotted on top of the multitaper confidence intervals, with the 1/N false alarm level indicated by the dotted line.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Top: detrended K2 observations of the scallop-shell star EPIC 203354381 with >3σ outliers clipped. Bottom: MDMTs for N ϖ = 6.5 and K = 11. Spectral concentrations are shown in the legend and gaps are highlighted in gray.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Top: x  n , the Kepler Q3 PDC-MAP light curve of KIC 6102338 after removing 3σ outliers. Bottom: MDSS ﹩\,{w}_{n}^{\left(k\right)}﹩ applied to x  n . Gray shading highlights missing data and spectral concentrations λ (k) are given in the legend. For this set of tapers, N ϖ = 4.5 and ﹩\tilde{\varpi }=0.0533﹩ day−1.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Top: multitaper spectral window W(f) (purple) and Lomb–Scargle proxy spectral window W LS(f) (green dashed). Bottom left: Lomb–Scargle pseudowindows for f 0 = 25 day−1 (blue) and f 0 = 80 day−1 (orange dashed). Bottom right: MDMT pseudowindows for f 0 = 25 day−1 (blue) and f 0 = 80 day−1 (orange dashed).
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Top: synthetic signal ﹩{x}_{n}=\sin (2\pi {f}_{1}{t}_{n})﹩, where f 1 = 25 day−1, placed on the CHEOPS 55 Cnc observation time stamps from MJDs 59267.398–59268.466. Bottom: MDSS tapers with N ϖ = 5, K = 7, and ﹩\tilde{\varpi }=7.61﹩ day−1 constructed for the CHEOPS observations. Gray shading highlights time stamps with missing data.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Phase-folded versions of the early (green circles) and late (purple stars) parts of the EPIC 203354381 light curve shown in the top panel of Figure 12. The early and late parts of the data set are before and after BJD = 2456935, respectively.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Spectral windows W (k)(f) from the MDSS tapers applied to the Kepler Q16 observations of KIC 6102338 (Figure 5). The legend indicates the spectral concentrations and the vertical dashed line marks the bandwidth.
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: Left: the heliocentric velocities of our targeted stars within 5′ of BH 261. The clump of 12 stars with radial velocities of ∼−60 km s−1 within the 3.′5 of the cluster are consistent with being BH 261 stars. Right: the radial velocity curve of the first-overtone RR Lyrae, OGLE-BLG-RRLYR-35078, which has both a proper motion and a radial velocity consistent with BH 261. The RRc template from Z. Prudil et al. (2023, in preparation) is used to obtain a center-of-mass radial velocity. The APOGEE DR17 observations are also shown, but not used in determining the radial velocity.
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: The BDBS color–magnitude diagram showing the horizontal branch stars (triangles), giants (circles), and RR Lyrae star (star) for which radial velocities have been determined from AAOmega@AAT. The filled red symbols indicate those stars that have radial velocities consistent with BH 261 (see Table 2), whereas the open triangle and circles are those stars that do not have velocities consistent with the cluster. The underlying BDBS stellar distribution in this field is shown with small gray points and those stars with proper motions consistent with the cluster are shown in blue. The black lines show the MIST (MESA Isochrones and Stellar Tracks, Choi et al. 2016) isochrone from which the cluster’s distance is derived in this work (7.1 kpc).
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: Left: a histogram, in blue, of the [Fe/H] metallicity of our targeted stars as determined from SP_ACE. Five giant stars within the cluster tidal radius with radial velocities consistent with the cluster are highlighted in red. There are five giants with both [Fe/H] metallicities and radial velocities outside the tidal radius; these are candidate extra-tidal giant stars. The tidal radius determined here (Section 3.5) is indicated by the solid line at a distance of 5.′4 from the cluster center. Top right: the observed sample spectra (black) of bh261_1_197.fits of the BH 261 giants within the tidal radius of the cluster. The best-fit spectrum from SP_ACE is overlaid in red, where only the portion of the spectrum sampled by SP_ACE is shown. Note that the Campos wavelength axis used here extends to a longer wavelength range than used in Koch et al. (2017). Bottom right: a comparison between seven APOGEE bulge giants and [Fe/H] derived from SP_ACE using the Campos wavelength range.
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: The Gaia proper motion distribution of the BDBS stars centered in a 3.′2 radius from BH 261. Blue points show stars with proper motions within 1.5 mas yr−1 in both μ  α  and μ  δ  of the mean proper motion of the cluster, as well as those with stars with parallax values smaller than 0.4 mas. The black points indicate stars that were spectroscopically targeted, and those with red highlights are those that were found to be radial velocity members. The star symbol (green) indicates the RR Lyrae star OGLE-BLG-RRLYR-35078.
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: Absolute integrated magnitude (M  V ) and velocity dispersion (log ﹩{\sigma }_{0}^{2}﹩) for clusters analyzed by Baumgardt & Hilker (2018). The open black points indicate globular clusters that are further than 3.35 kpc from the Galactic center, whereas the filled blue points indicate globular clusters in the inner Galaxy—those with galactocentric distances less than 3.35 kpc. The red triangle designates BH 261.
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: The combined BDBS photometry with radial density profile of the BH 261 cluster region determined using Gaia proper motions. The dots show the number of stars per arcmin2 taking the cluster center as the origin. The horizontal dashed black line indicates the field density. The King profile fit is indicated with the green dashed curve and the cluster core radius is indicated by the dotted vertical green line. The red vertical line indicates the assigned radius of BH 261 with the uncertainty region shaded gray. The tidal radius is indicated by the solid vertical line at radius of 5.′38. A rescale of the main plot is shown in the inset.
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: Left: the stars in and around BH 261 targeted spectroscopically with AAOmega@AAT. The field is centered on the GC BH 261. Right: example spectra from AAOmega illustrating the difference in quality between a bright giant (i = 14.678 mag), a faint HB star (i = 16.814 mag), the hot RRc star (i = 15.538 mag), and a typical red clump star (i = 16.515 mag). The spectra have been normalized and are offset for clarity.
Paper: Optimal Frequency-domain Analysis for Spacecraft Time Series: Introducing the Missing-data Multitaper Power Spectrum Estimator
Authors: Sarah Dodson-Robinson, Charlotte Haley
Figure caption: Multitaper power spectrum estimates from the early (top) and late (bottom) parts of the EPIC 203354381 K2 light curve. Green stars mark signals with an F-test p-value < 1/N.