adsabs/AstroCLIMB huggingface dataset:
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Posteriors and covariances for the circum-secondary MCMC of the MuSCAT2 quad-band transit light curves for a set of model parameters: effective temperature of the host [H] secondary star and contaminant [C] primary star, impact parameter, and host stellar density, plotted against the flux contamination ratio. The upper limit to a flux ratio from the primary contributing 19% of the light to the system rules out the circum-secondary scenario as it is not physically possible to have a bound primary companion that is both hotter and less luminous than the secondary.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Full RV time-series plot for the Gaussian process (GP) model with the 8.99 day prior on η  P  (top 2), and the 9.94 day prior on η  P  (bottom 2), unphased. Residuals (data − model) are shown in the lower plots. In both cases, the GP models do not significantly improve our recovery of K  b .
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Top: pi charts of the prior probabilities, likelihoods, and posterior probabilities of TOI 620 assuming it is a planet or an EB, BEB, or HEB at 1 or 2 times the period, from vespa. Bottom: the probability of the planet scenario, and the position of TOI 620 in ﹩\mathrm{log}\delta ﹩                      –T–T/τ space compared to other planets taken from galactic population statistics, also from vespa.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Sector 35 DAVE Report for TOI 620. The top panel shows phased transit data, with TESS data in red, binned data in blue, and repeated data in the gray region. The transit model is the black curve. The middle panel shows autocorrelated flux over the same phase. The bottom six panels depict different phased scenarios showing primary, odd, even, secondary, tertiary, and positive transits.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Sector 8 DAVE Report for TOI 620. The top panel shows phased transit data, with TESS data in red, binned data in blue, and repeated data in the gray region. The transit model is the black curve. The middle panel shows autocorrelated flux over the same phase. The bottom six panels depict different phased scenarios showing primary, odd, even, secondary, tertiary, and positive transits.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Photocenter difference images and PSFs for Sectors 8 (top 4) and 35 (bottom 4). The black-outlined star indicates the TIC position, while the red circle is the observed photocenter. The white dashed line indicates the TESS target pixels used to extract the light curve, just as the orange outlines showed in the TPF plot (Figure 2).
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: RV time-series plot for the circum-secondary case (left) and HEB case (right) phased to the period of b, with the black model representing the planet’s MAP model fit.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: The MCMC transit model for TOI 620 b in the circum-secondary case from EXOFASTv2 in the B band. The model is the red line, and the data are the black points. It is clearly visible that the transit depth in the data is deeper than what the model predicts from the flux dilution of the secondary by the primary. The reduced χ 2 for this model is 9.07.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Comparison of time-series radial velocities (RVs) acquired by different spectrographs on the night of the transit of V1298 Tau b. Offsets and trends of varying slopes between instruments are apparent. The gray shaded band indicates the predicted transit window. The chromaticity of the RV trend is apparent from the PEPSI data. We note that wavelength ranges indicated are the approximate regions from which RV information is extracted, and not necessarily the complete wavelength ranges of the spectra.
Paper: Uncertainty in Grain Size Estimations of Volatiles on Trans-Neptunian Objects and Kuiper Belt Objects
Authors: A. Emran, V. F. Chevrier
Figure caption: Plots for single scattering albedo of pure CH4 at 39 K (a), α-N2:CH4 at 35 K (b), and β-N2:CH4 at 38 K (c) for a grain 10 μm radius. The dashed solid line presents δ-Eddington corrected Mie, dashed yellow represents ISM, and the dotted green represents Hapke slab results. The plots were smoothened using the Savitzky–Golay filter (Savitzky & Golay 1964).
Paper: Limits on the Detection of Planet Nine in the Dark Energy Survey
Authors: Matthew Belyakov, Pedro H. Bernardinelli, Michael E. Brown
Figure caption: Histogram comparing the distribution of perihelion distance for the entire reference population in blue, the remaining population after the ZTF search in orange, and what remains after DES in green.
Paper: Limits on the Detection of Planet Nine in the Dark Energy Survey
Authors: Matthew Belyakov, Pedro H. Bernardinelli, Michael E. Brown
Figure caption: 2D histogram in albedo vs. g − r space, colored by the proportion of the reference population detected. Redder and higher albedo objects are more easily detected, while the bluer, low albedo range significantly depresses detection.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: The power spectrum of HAT-P-7’s light curve, after removal of HAT-P-7 b’s signal. The light and dark gray curves show HAT-P-7’s power spectrum smoothed by convolution with a Gaussian envelope with standard deviations of 0.3 μHz and 2.4 μHz, respectively. The red curve shows the best-fit model to the power spectrum, and dashed lines show individual components of the fit. HAT-P-7’s power spectrum shows evidence for several different signals, at least two of which (namely the broad supergranulation signal and the possible rotation signal at 1.7 days or 6.7 μHz) have timescales similar to HAT-P-7 b’s orbital period. The blue curve is the power spectrum of an array of Gaussian random white noise with the same time axis and standard deviation as HAT-P-7’s light curve (with the planetary signal removed). Compared to the power spectrum of purely white noise, HAT-P-7’s light curve shows excess noise on timescales close to the planetary orbital period that is unaccounted for in our phase curve analysis. The excess correlated astrophysical noise in HAT-P-7’s light curve could contribute to the apparent variations in HAT-P-7 b’s phase curve.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: A possible relationship between the level of apparent variations in the phase-curve parameters and the amount of low-frequency variability in injected light curves. The x-axis shows the ratio between the standard deviation of the Kepler light curve (excluding transits and eclipses) and the point-to-point scatter of the same. A larger ratio indicates dominance of longer-scale variations, such as those from stellar rotation signals. The y-axis shows the χ 2/d. o. f. value of measurements of the phase (ϕ) of the sine at the planet’s orbital period over time. Injected curves are shown in green, while HAT-P-7 is shown in dark blue. The possible relationship between this metric designed to quantify red noise in the light curve and the apparent statistical significance (using χ 2/d. o. f. as a proxy) of variations implies that the variations seen in HAT-P-7 b’s phase curve may be due to these low-frequency variations. KIC10801359 is the outlier visible in the lower-right-hand corner of the plot. It shows ∼ 50–500 ppm amplitude photometric variability on short (∼1 day) timescales, but is qualitatively similar to other noisy light curves that show higher reduced χ 2/d. o. f. values.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Measurements of the phase offset of the peak of the injected phase curves for each of the different stars in our injection/recovery tests. The Kepler Input Catalog (KIC) identifier of the injected star is shown in each panel, along with the reduced χ 2/d. o. f. value for each time series. The vertical dotted lines show where the Kepler light curves are broken into quarters. Even though we know the true signal injected into these planets was stationary and did not vary in time, we measure strong variations in these time series. Qualitatively, these variations are similar to those found in the actual light curve of HAT-P-7 b, and quantitatively their apparent statistical significance can exceed that of the variations in HAT-P-7 b’s phase curve. Our oversampled phase-offset variation result for HAT-P-7 b is shown at the bottom for comparison. It is possible that the variations measured in HAT-P-7 b’s phase curve could be caused by the same effects as in our injection/recovery tests.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Excess noise vs. recovered phase offset in HAT-P-7 b and the injected light curves. Excess noise is defined in Equation (11), where a high excess noise indicates a poor fit quality. The high excess noise of some of the injected light curves (KIC10801359, KIC10794838) makes them poor comparisons against the HAT-P-7 b result. However, some of the injections which show comparable excess noise to the HAT-P-7 b result also show a similar phase-offset range (the injections in the same range as HAT-P-7 b are shown in color in the second plot). This suggests that stellar variability can cause similar phase-offset variability results as those we recovered for HAT-P-7 b.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Measurements of the amplitude of the injected phase curves for each of the different stars in our injection/recovery tests. Like Figure 11, the Kepler Input Catalog (KIC) identifier of the injected star is shown in each panel, along with the reduced χ 2/d. o. f. value for each time series. The vertical dotted lines show where the Kepler light curves are broken into quarters. The amplitude time series also show apparent variations, even though the injected signal had no time variations. There are apparently effects other than true atmospheric variability that can introduce variations as large as we see in HAT-P-7 b’s phase curve. Our oversampled amplitude variation result for HAT-P-7 b is shown at the bottom for comparison. We note that while the stars with the highest χ 2/d. o. f. values show high-amplitude photometric variability, even apparently quiet stars yield χ 2/d. o. f. values similar to HAT-P-7.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: An illustration of how oversampling can create the appearance of variability in time series. Top: a time series of Gaussian random noise, sampled at the times of the measurements of HAT-P-7 b’s orbital phase by Armstrong et al. (2016). Middle: the same distribution of Gaussian random noise shown in the top panel but smoothed by a box filter with an oversampling factor of 10. Bottom: our phase-offset variation result, sampled using a sliding window of 10 orbits. In all three panels, the vertical dotted lines show where the Kepler light curve is broken into quarters. The sliding window makes the result appear smoother by oversampling the data, but qualitatively similar to the smooth variations in the Gaussian random noise in the previous panel.