adsabs/AstroCLIMB huggingface dataset:
Paper: Validation of 13 Hot and Potentially Terrestrial TESS Planets
Authors: Steven Giacalone, Courtney D. Dressing, Christina Hedges, Veselin B. Kostov, Karen A. Collins, Eric L. N. Jensen, Daniel A. Yahalomi, Allyson Bieryla, David R. Ciardi, Steve B. Howell, Jorge Lillo-Box, Khalid Barkaoui, Jennifer G. Winters, Elisabeth Matthews, John H. Livingston, Samuel N. Quinn, Boris S. Safonov, Charles Cadieux, E. Furlan, Ian J. M. Crossfield, Avi M. Mandell, Emily A. Gilbert, Ethan Kruse, Elisa V. Quintana, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Britt Duffy Adkins, David Baker, Thomas Barclay, David Barrado, Natalie M. Batalha, Alexander A. Belinski, Zouhair Benkhaldoun, Lars A. Buchhave, Luca Cacciapuoti, David Charbonneau, Ashley Chontos, Jessie L. Christiansen, Ryan Cloutier, Kevin I. Collins, Dennis M. Conti, Neil Cutting, Scott Dixon, René Doyon, Mohammed El Mufti, Emma Esparza-Borges, Zahra Essack, Akihiko Fukui, Tianjun Gan, Kaz Gary, Mourad Ghachoui, Michaël Gillon, Eric Girardin, Ana Glidden, Erica J. Gonzales, Pere Guerra, Elliott P. Horch, Krzysztof G. Hełminiak, Andrew W. Howard, Daniel Huber, Jonathan M. Irwin, Giovanni Isopi, Emmanuël Jehin, Taiki Kagetani, Stephen R. Kane, Kiyoe Kawauchi, John F. Kielkopf, Pablo Lewin, Lindy Luker, Michael B. Lund, Franco Mallia, Shude Mao, Bob Massey, Rachel A. Matson, Ismael Mireles, Mayuko Mori, Felipe Murgas, Norio Narita, Tanner O'Dwyer, Erik A. Petigura, Alex S. Polanski, Francisco J. Pozuelos, Enric Palle, Hannu Parviainen, Peter P. Plavchan, Howard M. Relles, Paul Robertson, Mark E. Rose, Pamela Rowden, Arpita Roy, Arjun B. Savel, Joshua E. Schlieder, Chloe Schnaible, Richard P. Schwarz, Ramatholo Sefako, Aleksandra Selezneva, Brett Skinner, Chris Stockdale, Ivan A. Strakhov, Thiam-Guan Tan, Guillermo Torres, René Tronsgaard, Joseph D. Twicken, David Vermilion, Ian A. Waite, Bradley Walter, Gavin Wang, Carl Ziegler, Yujie Zou
Figure caption: Top: coordinates of the TESS planet candidates in this paper (white circles), validated TESS planets in this paper (black circles), validated TESS planets (blue squares), confirmed TESS planets (blue diamonds), and confirmed pre-TESS planets (red hexagons). The ecliptic plane and ecliptic poles (i.e., the JWST continuous viewing zones) are shown as dashed black lines. Bottom: emission spectroscopy metric versus apparent K  s  magnitude for each planet candidate and planet. The dashed lines indicate the minimum values a target should have to be observed with JWST.
Paper: Parallax of Star-forming Region G027.22+0.14
Authors: S. B. Bian, Y. Xu, J. J. Li, Y. W. Wu, B. Zhang, X. Chen, Y. J. Li, Z. H. Lin, C. J. Hao, D. J. Liu
Figure caption: Results from combining the parallax fits for three maser spots. The left panel plots the data and fits of positions changing with time, and the right shows the parallax signatures after proper motions were removed. The best-fitting models in R.A. and decl. are shown as solid dashed lines. Different marks indicate different maser spots as shown in the figure legend.
Paper: Parallax of Star-forming Region G027.22+0.14
Authors: S. B. Bian, Y. Xu, J. J. Li, Y. W. Wu, B. Zhang, X. Chen, Y. J. Li, Z. H. Lin, C. J. Hao, D. J. Liu
Figure caption: Distance PDF for G027.22+0.14 calculated with a Bayesian distance estimator (Reid et al. 2016, 2019). Each probability is indicated in a differently colored curve (see the legend in the upper-right corner). The name of spiral-arm segments are in short form: N1N/F = Norma arm (near/far); 3kF = 3 kpc arm far; ScF = Scutum arm far. P is the probability of a component.
Paper: Parallax of Star-forming Region G027.22+0.14
Authors: S. B. Bian, Y. Xu, J. J. Li, Y. W. Wu, B. Zhang, X. Chen, Y. J. Li, Z. H. Lin, C. J. Hao, D. J. Liu
Figure caption: Plan view of the Milky Way from the north Galactic pole following Reid et al. (2019). The background map combines BeSSeL Survey and VERA project results. The green pentagram with a 1σ parallax distance error indicates the source reported in this paper (see the legend in the upper left corner). The locations of maser sources with measured parallaxes are indicated with solid dots. Solid curved lines trace the centers of spiral-arm models from Reid et al. (2019), and the dotted lines enclose 90% of the sources.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: Sample background observations showing every good event in the plane of event energy vs. PI_ratio. The curved red line shows the NICER pipeline’s boundary between events that appear as if in focus (left of the line), vs. events originating far from the detector anode (right of the line). The integration areas for the first two background model parameters, ibg and hrej, are also shown. The observations were chosen to illustrate how the two background components are always present, but the fraction of events in each group can vary widely.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: The in-focus background rate at 0.4–12 keV (R BG) vs. the first two parameters of the 3C50 model, ibg (top panel) and hrej (bottom panel). The plotted data corresponds to all of the 3556 GTIs represented in Table 1. Rough correlations are seen in each panel, with a steeper dependence in the case of ibg.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: Plot of ibg vs. hrej. This plane is divided into five cells (horizontal) covering hrej < 5.0 and seven cells (vertical) with ibg < 10.0. The cells are referenced by (ibg, hrej) number with 11 on the lower left and 75 to the upper right. Cell boundaries in units of ibg, hrej are given in Table 3. These intervals define the bins in which the background spectra per GTI are combined to create the stage 1 background library for the 3C50 model. The stage 1 library contains 33 such spectra, with cells 15 and 71 unoccupied.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: Top panel: values of R BG, the in-focus and in-band count rate for the background GTIs, are plotted for each successive cell of the stage 1 library. The cells are counted by their ibg, hrej number, ranging from 11 to 75. The cell id numbers and their ordinal number within the cell are used to stretch out the points along the x-axis (see the text). The dashed line shows the high-rate filter that clips the brightest outliers to be excluded when computing the library spectra. Bottom panel: reduced chi square values for each cell, after filtering out the high points (top panel), assuming that R BG is constant within each cell. The levels of intrinsic scatter in each cell are 20%–40%, motivating a step to normalize each library selection using the ibg i  value of each target spectrum.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: The stage 1 library for the 3C50 background model consists of these 33 spectra, arranged with ibg number (1–7) increasing vertically and hrej number (1–5) increasing to the right. The spectra are substantially brighter and flatter with increasing ibg cell number (vertical steps), while a more shallow brightness increase, a stronger soft component at 0.2–4 keV, and brighter emission lines are seen with increased hrej cell number (from left to right). Cell 11 (lower left) is the closest that the library comes to an isolation of the cosmic diffuse X-ray background.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: The 3C50 model was applied to GTIs of the background observations using only the stage 1 library. The residuals from this exercise are shown at 0.4–12 keV (top panel) and 0.3–0.4 keV (bottom panel). The plot symbols distinguish GTIs during ISS night (black cross) and ISS day (red triangle). The positive residuals during ISS daytime are associated with the seepage of sunlight into the XTI, which expands the ∼0.1 keV noise component to the point that it can encroach into the soft X-ray region that is valuable for NICER science.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: The stage 2 library for the 3C50 background model consists of 12 spectra that represent the soft excess caused by various levels of sunlight intrusion into the XTI. These spectra were determined from the residuals of the stage 1 model for 1076 GTIs during ISS day. The 12 spectra correspond to different levels in the nz 52 parameter, which closely tracks the amount of optical light leak.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: The final residuals from the application of the 3C50 model to the background observations, plotted vs. the original count rate at 0.4–12 keV, R BG. The horizontal axis is truncated at 5 c s−1 for clarity; only 6% of the observations exceed this level. The model residuals are shown at 0.4–12 keV (R BGnet; top panel) and 0.3–0.4 keV (S1net; bottom panel). The plot symbols distinguish GTIs during ISS night (black cross) and ISS day (red triangle).
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: A map of the background observations in Earth longitude and latitude, with the magnitudes of the 3C50 model residuals, R BGnet, represented with the symbol types. The c s−1 ranges and symbols are: ±0.1 (black “x”s); ±1.0, excluding the previous level (small black triangles); ±2.0, excluding previous levels (cyan circles); −5.0 to −2.0 (medium magenta squares); 2.0 to 5.0 (medium green triangles); <−5.0 (large red triangles); and >5.0 (large blue squares). The points terminate in latitude at the inclination of the ISS orbit (52 deg). The highest residual count rates from the 3C50 model reside in the polar horns in the ISS orbit. The region void of points in the lower right quadrant is the exclusion zone for the SAA, and there are no indications of problems near the chosen SAA boundaries.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: Top panel: NICER light curve of the Crab Nebula at 0.4–12 keV, after background subtraction with the 3C50 model and the application of level 1 filtering, which excluded only two GTIs. The selected data (431 GTIs) have a mean and rms deviation of 10,526 ± 65 c s−1. Most of the the 0.6% variations can be seen as a gentle 900 day wave in the light curve. Middle panel: the deadtime fraction for Crab observations (see the text), showing the low level of NICER deadtime (0.5%–1.5% for the Crab) and the annual cycle tied to increases in undershoot and noise events when Crab observations are conducted in sunlight. Bottom panel: the deadtime-corrected light curve for the Crab Nebula, suggesting that the subtle 900 day waves in intensity may be real.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption:  NICER observations of the SNR in the SMC, E0102, yielded background-subtracted spectra with the 3C50 model for 941 GTIs through 2020 June 12, accumulating 408 ks exposure time. The soft light curve (0.3–2.0 keV) extracted from all of the GTIs is shown in the left panel, while the same data with level 2 filtering (804 GTIs, 352 ks) is shown in the right panel (see Section 6). These measurements have a mean and rms of 25.60 ± 0.62 c s−1 and 25.63 ± 0.42 c s−1, respectively, while the rms statistical uncertainty is 0.32 c s−1.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: Estimates of the in-band background rate using the relationship R est = 2.91 ∗ ibg + 4.67 ∗ hrej. Each point corresponds to one GTI, and the equation is determined with a least-squares fit confined to the range 0.5 < R BG < 300 c s−1. The error bars consider only the statistical uncertainties in R BG, ibg, and hrej. The dashed line is a reference for the match between this relationship and the measured rate (R BG). The estimator is valuable for showing background temporal variability, e.g., at 1 s timescale, that can help to determine whether fast flaring behavior originates from the target or from activity in the background.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: The application of the 1 s background estimator to two GTIs from observations of SwiftJ1858 when the source, an X-ray binary system containing an accreting neutron star, was in a flaring state. The first GTI shows that the rapid flaring is from the X-ray source (blue), and this behavior has been observed many times with NICER and other instruments. However, the second GTI shows a light curve with unusual rapid flaring in the background (red), demonstrating that this particular sequence of flares is from the background, rather than the X-ray source.
Paper: An Empirical Background Model for the NICER X-Ray Timing Instrument
Authors: Ronald A. Remillard, Michael Loewenstein, James F. Steiner, Gregory Y. Prigozhin, Beverly LaMarr, Teruaki Enoto, Keith C. Gendreau, Zaven Arzoumanian, Craig Markwardt, Arkadip Basak, Abigail L. Stevens, Paul S. Ray, Diego Altamirano, Douglas J. K. Buisson
Figure caption: The relationship between the 3C50 model parameters and those of the NICER Environmental Model. The plot of hrej vs. the cutoff rigidity (COR_SAX) is the best correlation seen between any two hypothetical background parameters in this study. On the other hand, ibg and K  p  pair with their model partners in different ways.
Paper: A Search for Analogs of KIC 8462852 (Boyajian’s Star): A Second List of Candidates
Authors: Edward G. Schmidt
Figure caption: The NSVS light curves for the stars classified as slow dippers. The upper horizontal line is the continuum level and the lower line is three standard deviations below it.
Paper: A Search for Analogs of KIC 8462852 (Boyajian’s Star): A Second List of Candidates
Authors: Edward G. Schmidt
Figure caption: The HR diagram of the dipper candidates. Squares, circles, and a star represent slow dippers from Paper I, dipper candidates from the present paper, and Boyajian’s star, respectively. The small dots represent the statistical sample from Paper I. The two irregular quadrilateral areas delineated by light lines are the two regions defined in Paper I and the large rectangle defined by bold solid lines is the modified region defined here.
Paper: A Search for Analogs of KIC 8462852 (Boyajian’s Star): A Second List of Candidates
Authors: Edward G. Schmidt
Figure caption: (a) The distribution of the dipper candidates on the sky. The slow dippers are represented by circles, and Boyajian’s star by a star. The solid curve shows the location of the galactic plane. The dashed box delineates the area of the sky studied in Paper I and the dashed line through it separates the tiles of the clump from those of the comparison region. (b) and (c) The distribution of the slow dippers in the ﹩x^{\prime} z^{\prime} ﹩ and ﹩x^{\prime} y^{\prime} ﹩ planes, respectively. Filled circles denote stars between α = 254° and 303° and open circles represent stars outside this region. Boyajian’s star is represented by a star and the Sun by the usual symbol.
Paper: A Hot Mars-sized Exoplanet Transiting an M Dwarf
Authors: Caleb I. Cañas, Suvrath Mahadevan, William D. Cochran, Chad F. Bender, Eric D. Feigelson, C. E. Harman, Ravi Kumar Kopparapu, Gabriel A. Caceres, Scott A. Diddams, Michael Endl, Eric B. Ford, Samuel Halverson, Fred Hearty, Sinclaire Jones, Shubham Kanodia, Andrea S. J. Lin, Andrew J. Metcalf, Andrew Monson, Joe P. Ninan, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Kepler Photometry of KOI-4777. (a) displays the raw PDCSAP photometry from all 17 quarters of the Kepler mission. We have excluded observations with nonzero data quality flags. (b) shows the photometry after detrending with a Gaussian process and phasing to the observed ephemeris from the supplemental Kepler DR 25 catalog. In the bottom panel, we bin the phase-folded data into 2 minutes bins to show the shape of the transit.
Paper: A Hot Mars-sized Exoplanet Transiting an M Dwarf
Authors: Caleb I. Cañas, Suvrath Mahadevan, William D. Cochran, Chad F. Bender, Eric D. Feigelson, C. E. Harman, Ravi Kumar Kopparapu, Gabriel A. Caceres, Scott A. Diddams, Michael Endl, Eric B. Ford, Samuel Halverson, Fred Hearty, Sinclaire Jones, Shubham Kanodia, Andrea S. J. Lin, Andrew J. Metcalf, Andrew Monson, Joe P. Ninan, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Detection of KOI-4777.01 with ARPS. The periodogram is displayed from 0.2 to 50 days of KOI-4777.01 (KIC 6592335) obtained with the transit comb filter method in the ARPS analysis of Kepler light curves (Caceres et al. 2019b, 2019a). The strongest peak is at P = 0.412 days and its harmonics are marked in green.
Paper: A Hot Mars-sized Exoplanet Transiting an M Dwarf
Authors: Caleb I. Cañas, Suvrath Mahadevan, William D. Cochran, Chad F. Bender, Eric D. Feigelson, C. E. Harman, Ravi Kumar Kopparapu, Gabriel A. Caceres, Scott A. Diddams, Michael Endl, Eric B. Ford, Samuel Halverson, Fred Hearty, Sinclaire Jones, Shubham Kanodia, Andrea S. J. Lin, Andrew J. Metcalf, Andrew Monson, Joe P. Ninan, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Stellar neighborhood around KOI-4777. (a) presents the cumulative Kepler footprint on a POSS-I red image from 1951. The blue dashed polygon is the region of the sky observed at least once in all seventeen quarters of the Kepler data. The red solid polygon is the cumulative region of sky contained at least once within the aperture pixel mask. KOI-4777 is marked as a star. Gaia EDR3 detects no bright ΔG < 4 companions within the entire Kepler footprint. (b) is similar to Panel A but overlaid on a PS1 i image taken in 2011 when Kepler was observing this star. KOI-4777 has moved slightly but no other bright stars have moved into the aperture or Kepler footprint. When KOI-4777 was observed by Kepler, there were no bright stars in the aperture that could cause significant dilution.
Paper: A Hot Mars-sized Exoplanet Transiting an M Dwarf
Authors: Caleb I. Cañas, Suvrath Mahadevan, William D. Cochran, Chad F. Bender, Eric D. Feigelson, C. E. Harman, Ravi Kumar Kopparapu, Gabriel A. Caceres, Scott A. Diddams, Michael Endl, Eric B. Ford, Samuel Halverson, Fred Hearty, Sinclaire Jones, Shubham Kanodia, Andrea S. J. Lin, Andrew J. Metcalf, Andrew Monson, Joe P. Ninan, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Robo-AO Imaging of KOI-4777. This figure displays the 5σ contrast curve observed by Ziegler et al. (2018) using Robo-AO in a long-pass filter with a hard cutoff at 600 nm (LP-600). The data show there are no bright companions within 4″ of the host star. The inset image is an 8″ cutout centered on KOI-4777 in this long-pass filter. The contrast curve and image were obtained from the Robo-AO KOI survey (http://roboaokepler.org/koi_pages/KOI-4777.html).
Paper: A Hot Mars-sized Exoplanet Transiting an M Dwarf
Authors: Caleb I. Cañas, Suvrath Mahadevan, William D. Cochran, Chad F. Bender, Eric D. Feigelson, C. E. Harman, Ravi Kumar Kopparapu, Gabriel A. Caceres, Scott A. Diddams, Michael Endl, Eric B. Ford, Samuel Halverson, Fred Hearty, Sinclaire Jones, Shubham Kanodia, Andrea S. J. Lin, Andrew J. Metcalf, Andrew Monson, Joe P. Ninan, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Rotation period of KOI-4777. (a) displays the median-normalized Kepler SAP photometry, after detrending with seven CBVs, along with our Gaussian-process (GP) model as the dashed–dotted line. (b) shows the GLS periodogram, (c) the time lags derived via wavelet decomposition, and (d) shows the autocorrelation function of the photometry in panel (a). Each method in panels (b)–(d) shows a significant peak between 25 and 50 days.
Paper: A Hot Mars-sized Exoplanet Transiting an M Dwarf
Authors: Caleb I. Cañas, Suvrath Mahadevan, William D. Cochran, Chad F. Bender, Eric D. Feigelson, C. E. Harman, Ravi Kumar Kopparapu, Gabriel A. Caceres, Scott A. Diddams, Michael Endl, Eric B. Ford, Samuel Halverson, Fred Hearty, Sinclaire Jones, Shubham Kanodia, Andrea S. J. Lin, Andrew J. Metcalf, Andrew Monson, Joe P. Ninan, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: (a) Displays the photometric model and the phased Kepler light curve. For clarity, we only show the phase-folded data after rebinning to 2 minutes bins (similar to Figure 1(b)). (b) presents the RVs after phasing the data to the ephemeris derived from the joint fit. For panels (a) and (b), the best-fitting model is plotted as a dashed line while the shaded regions denote the 1σ (darkest), 2σ, and 3σ range of the derived posterior solution.