adsabs/AstroCLIMB huggingface dataset:
Paper: ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides
Authors: A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, and M. Zíbar
Figure caption: Cumulative percentage of observable planets as a function of the telescope size.
Paper: ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides
Authors: A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, and M. Zíbar
Figure caption: Distributions of the achieved uncertainties on the midtransit time from all the ExoClock observations.
Paper: ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides
Authors: A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, and M. Zíbar
Figure caption: Residuals autocorrelation (left) and Shapiro (right) tests for all the ExoClock observations as a function of the number of data points in each light curve. The red dashed line indicates the upper acceptable limit for each metric, as calculated from time series of white noise.
Paper: ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides
Authors: A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, and M. Zíbar
Figure caption: Uncertainties for the transit-time prediction at the end of 2028 as calculated with the old ephemerides (horizontal axis) and with the new ephemerides as estimated from ExoClock (vertical axis). The dashed line is the line of equal values, and the planets for which the prediction precision has been improved (90%) are plotted on the right of this line.
Paper: ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides
Authors: A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, and M. Zíbar
Figure caption: Difference in the transit-time prediction at the end of 2028 between the old and the new ephemerides, as a function of its uncertainty (quadratically combined). The dashed line is the line of equal values, and the planets for which the drift is greater than 1σ (57%) are plotted above this line.
Paper: ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides
Authors: A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, and M. Zíbar
Figure caption: Comparison of the mean observing rate vs. observing coverage collected from literature data and from the combination of both literature and ExoClock data.
Paper: ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides
Authors: A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, and M. Zíbar
Figure caption: Distribution of planets over the observing coverage (left) and the mean observing rate (right) for the literature data and for the combination of both literature and ExoClock data.
Paper: ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides
Authors: A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, and M. Zíbar
Figure caption: Cumulative probability as a function of the drift in signal-to-noise ratio and comparison with normal distribution.
Paper: The Impact of Observing Strategy on the Reliable Classification of Standard Candle Stars: Detection of Amplitude, Period, and Phase Modulation (Blazhko Effect) of RR Lyrae Stars with LSST
Authors: Nina Hernitschek, and Keivan G. Stassun
Figure caption: Comparison of metric evaluation for RRab light curves. We plot the area (in thousands of square degrees) for which a given fraction of RRab stars with a given distance modulus (17–22) from a light curve with a given time interval (15–55 days) can be identified. The metric was evaluated on simulated 2 yr light curves for OpSim 1.7 databases baseline_nexp2_v1.7_10yrs.db (baseline, blue histograms), pair_times_55_v1.7_10yrs.db (pair times cadence, red histograms), and rolling_scale0.2_nslice2_v1.7_10yrs.db (rolling cadence, orange histograms).
Paper: The Impact of Observing Strategy on the Reliable Classification of Standard Candle Stars: Detection of Amplitude, Period, and Phase Modulation (Blazhko Effect) of RR Lyrae Stars with LSST
Authors: Nina Hernitschek, and Keivan G. Stassun
Figure caption: Comparison of metric evaluation for RRc light curves. We plot the area (in thousands of square degrees) for which a given fraction of RRc stars with a given distance modulus (17–22) from a light curve with a given time interval (15–55 days) can be identified. The metric was evaluated on simulated 2 yr light curves for OpSim 1.7 databases baseline_nexp2_v1.7_10yrs.db (baseline, blue histograms), pair_times_55_v1.7_10yrs.db (pair times cadence, red histograms), and rolling_scale0.2_nslice2_v1.7_10yrs.db (rolling cadence, orange histograms).
Paper: The Impact of Observing Strategy on the Reliable Classification of Standard Candle Stars: Detection of Amplitude, Period, and Phase Modulation (Blazhko Effect) of RR Lyrae Stars with LSST
Authors: Nina Hernitschek, and Keivan G. Stassun
Figure caption: To illustrate how the histograms in Figure 1 and Figure 2 were calculated, this figure shows a single-metric result for a distance modulus of 18.0, and a time interval of 20 days for RRab-like light curves using the pair times cadence. This corresponds to the red histogram in the second panel of the second row in Figure 1. The sky map is plotted in Galactic coordinates. Each HEALPix cell covers 7°33 (achieved using the HEALPix resolution parameter Nside = 8). We highlight that the fraction of correctly recovered period, phase, and amplitude (here as “Fraction Detected”) varies over the survey footprint due to coverage and light-curve length. The generation of sky maps as well as histograms is handled automatically within the lsst.sims.maf.metricBundles Python package provided by the MAF. For further reference, we recommend the documentation described in Section 4.2.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: 5 × 5 cutout example showing KIC 2437745, an ellipsoidal binary in NGC 6791.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Left: 5 × 5 cutout of KIC 2437745, resampled using bilinear interpolation. Right: 5 × 5 cutout of KIC 2437745, resampled using bicubic interpolation. Note the haloing and edge effects, which led us to choose bilinear interpolation for this process.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: One frame of data for KIC 2437745, showing the results of image subtraction. Note that there is high-amplitude variability from the target, as well as a companion star to the top right. Multiple variable stars in the same aperture can lead to blending when using image subtraction photometry, so we select apertures to avoid this, as discussed in Section 2.5. The low-amplitude positive and negative variation is due to small fluctuations between the individual frame and the average.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Uncorrected light curve of KIC 2437745, produced using image subtraction photometry. Dashed lines indicate quarter boundaries.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Stars used for ensemble centroid calculation in NGC 6791 (left) and NGC 6819 (right), plotted on images of the 200 × 200 superstamps. The color scale denotes Kepler magnitude.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: The magnitudes calculated in this study compared to magnitudes from the KIC, with a one-to-one line shown in black. Points are color coded by the adjusted isolation measure, which we used to scale weighted Gaussian apertures for photometry.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Top panel: corrected light curve for KIC 2437745. Middle panel: close-up of quarter 9. Bottom panel: amplitude spectrum calculated using all 17 quarters of data, showing evidence of ellipsoidal variability.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Quarter 9 EC-IRIS (top panel) and Kepler SAP (bottom panel) data for KIC 5023743, a target which exhibits the spurious ∼3 day signal described in Section 3.2. Note that the signal is present in both our light curve and a Kepler SAP light curve, but appears to be higher amplitude in our data. This is due to the differing apertures; EC-IRIS apertures were optimized for faint targets.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Top: KIC 5024943. Bottom: KIC 5025005. Both stars exhibit uneven variations in flux due to their proximity to a bright target. Dashed lines represent quarter boundaries.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Top panels: noise vs. Kp plots for both clusters. Bottom panels: signal-to-noise (S/N) vs. Kp. NGC 6791 is on the left and NGC 6819 is on the right. All plots use noise and S/N measures as outlined in Section 3.3, color coded by adjusted isolation measure. In order to show a clear overview of trends, we set axis limits to exclude outliers in noise, S/N, and Kp. Note that the typical Kp ranges differ for each cluster. Note also that we do not plot the S/N ratio for nonvariable stars, as it is determined based on the highest-amplitude peak of variability, which becomes arbitrary in an amplitude spectrum dominated by noise.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Left panels: NGC 6791. Right panels: NGC 6819. Top row: noise measures for the EC-IRIS and TC-IRIS pipelines, with EC-IRIS on the x-axis and the ratio between TC-IRIS and EC-IRIS on the y-axis. Bottom row: signal-to-noise (S/N) measures plotted for the same two pipelines, with the y-axis inverted. For both noise and S/N, points will lie above the one-to-one line in the case of favorable performance by EC-IRIS, i.e., lower noise and higher S/N. All targets are color coded based on their adjusted isolation measure or aperture size, with brighter points being more isolated; targets where signal was detected are in color, whereas nonvariable targets are in grayscale. As in Figure 10, we do not plot the S/N ratio for nonvariable stars.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Left panels: NGC 6791. Right panels: NGC 6819. Top row: noise measures, with EC-IRIS image subtraction on the x-axis and the ratio between EC-IRIS and custom SAP on the y-axis. Bottom row: signal-to-noise (S/N) measures for EC-IRIS and custom SAP. Points are color coded as in Figure 11, and, as in Figures 10 and 11, we do not plot the S/N ratio for nonvariable stars.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Comparing the retrieved S/N of 230 stars with signal in the sample between EC-IRIS photometry and Kepler SAP photometry, using the same data preparation methods. Points are colored according to how many more quarters of data are available in the IRIS catalog. The y-axis is inverted as in Figure 11 and 12 to indicate that points above the line represent a better result from the EC-IRIS pipeline. Note that the x-axis is shown in log scale to display outliers with very high S/N measurements.
Paper: The Kepler IRIS Catalog: Image Subtraction Light Curves for 9150 Stars in and around the Open Clusters NGC 6791 and NGC 6819
Authors: Isabel L. Colman, Timothy R. Bedding, Daniel Huber, and Hans Kjeldsen
Figure caption: Time series (top) and amplitude spectrum (bottom) for KIC 2570715, an oscillating red giant with only seven available quarters of Kepler SAP data. EC-IRIS data are shown in black, and Kepler SAP in blue. Both light curves in the top panel were produced using the same processing methods. Dashed red lines indicate quarter boundaries.
Paper: CMB/kSZ and Compton-y Maps from 2500 deg2 of SPT-SZ and Planck Survey Data
Authors: L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Benson, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. de Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, D. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, S. Raghunathan, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, and R. Williamson
Figure caption: Relative azimuthally averaged band weights for the minimum-variance thermal SZ Compton-y map (upper left), the CMB-nulled y map (lower left), and the tSZ-nulled CMB/kSZ map (lower right).