adsabs/AstroCLIMB huggingface dataset:
Paper: A Machine Learning–based Direction-of-origin Filter for the Identification of Radio Frequency Interference in the Search for Technosignatures
Authors: Pavlo Pinchuk, Jean-Luc Margot
Figure caption: Sample signal with lower S/N in the top image compared to the bottom image. The CNN score for this image pair is 0.2706, which corresponds to a label of “0.”
Paper: A Machine Learning–based Direction-of-origin Filter for the Identification of Radio Frequency Interference in the Search for Technosignatures
Authors: Pavlo Pinchuk, Jean-Luc Margot
Figure caption: Histogram of the S/N detected in the top half of each scan. The blue vertical line shows the S/N cutoff value of 6 used to remove signals with low power in the top half of the scan.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Optical setup of the common-path VNC based on a Savart plate.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Optical setup of polarization-based speckle nulling for a common-path VNC using an SLM.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Laboratory demonstration of speckle-nulling wave-front control of case 3. Coronagraphic images acquired (a) before and (b) after speckle nulling (“SN” in the figure) are shown together with (c) a numerically simulated image. The plus sign indicates the positions of the model star. The color scales differ between the experimentally acquired and simulated images.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Numerical simulation of speckle nulling using an SLM for a common-path VNC. Coronagraphic images (a) before and (b) after speckle nulling (“SN” in the figure) are shown using a logarithmic color scale. Four red circles show radii of 4, 20, 37, and 116 λ/D, which roughly correspond to the orbits of Earth, Jupiter, Saturn, and Neptune as seen from 10 pc away assuming D = 4 m and λ = 500 nm. The green square represents the Nyquist limit of a 32 × 32 DM.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Left: experimentally acquired speckle images (with close-ups of the regions indicated by red solid squares) of case 2 at the first (left) and 30th (right) iterations. Right: radially averaged profiles of the cross-correlation maps of the speckle images between adjacent iterations. The cross-correlations are evaluated over one quadrant region of the images indicated by the red dashed squares.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Laboratory demonstration of speckle-nulling wave-front control of case 2. Coronagraphic images acquired (a) before and (b) after speckle nulling (“SN” in the figure) are shown together with (c) a numerically simulated image. Magnified images around the dark hole region are also shown in the bottom row. The plus sign indicates the position of the model star. The color scales differ between the experimentally acquired and simulated images.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Laboratory demonstration of speckle-nulling wave-front control of case 1. Coronagraphic images acquired (a) before and (b) after speckle nulling (“SN” in the figure) are shown together with (c) a numerically simulated image. The plus sign indicates the position of the model star. The color scales differ between the experimentally acquired and simulated images.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Target dark hole regions registered for the laboratory demonstration. The target regions for cases 1, 2, and 3 are indicated by the black rectangles and square. The asterisks and dotted squares indicate the positions of a model star and a Nyquist limit of a 32 × 32 DM, respectively.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Estimated correction parameters α  m  (in units of voltage level) for rejecting the mth-brightest speckles (m from 1 to 5) as a function of iteration number. The results for case 1 are shown.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Optical configuration of a laboratory demonstration of speckle-nulling wave-front control for a common-path VNC.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Measured mean contrasts over dark hole regions for the three cases as a function of iteration number.
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: Violin plot (gray) showing posterior distributions of the different Gaussian process results for Asteroid 221 Eos, spanning 10, 20, 30, 40, 50, and 60 days (20, 40, 60, 80, 100, and 120 data points). Colored diamonds in green, teal, and blue represent the top three best period estimates in the Lomb–Scargle periodograms. The lines show the period that was used to simulate the data (yellow, dotted–dashed), double (blue, dashed) that period, and 1/3 of the true period (blue, dotted). Our posterior probability distributions for the light curves with 30 and 40 days of observations contain a small number of samples more than 5 standard deviations (averaged across all samples) above the mean, which, for the sake of this visualization, have been masked.
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: Top: three example realizations drawn from a Gaussian process with a periodic covariance function. All three realizations were drawn from a Gaussian process with a period of P = 3.0 and an amplitude of A = 1, but variable intra-period length scale Γ. Bottom left: visualization of the covariance function that generated the realizations in the top panel. Given the period of P = 3, points that are integer multiples apart from each other will be exactly correlated, and thus generate a periodic pattern. The variations within each period depend on the value of Γ: if Γ is large, the correlation between points that are close together is near zero, generating rapidly varying structure within each period. If Γ is small, the correlation between data points is always high, generating smooth, nearly sinusoidal realizations. Bottom right: two-dimensional representation of the covariance function with Γ = 20 from the left panel. The light yellow bands are regions of high covariance spaced at intervals of multiples of P; the dark purple bands in between show regions where the covariance between data points for a given Δx is near 0.
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: Left: 30 days (60 data points) of simulated observations of asteroid 3200 Phaethon with varying magnitude measurements and uncertainties. Uncertainties are fractions of the standard deviation of the distribution of magnitudes, ranging from 10% to 100%. For each case, magnitude measurements are varied by sampling from normal distributions with μ equal to the original magnitudes and σ equal to the magnitude error, respectively. Right: the marginalized posterior distribution of the period parameter near the true period, 3.604 hr. The solid blue line indicates the mean of the samples, and the dashed lines indicate ±1σ of the distribution. The full marginalized posterior distributions (Figure 18) can be found in the Appendix.
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: Violin plot (gray) showing posterior distributions of the different Gaussian process results for Asteroid 3200 Phaethon, spanning 20, 60, 80, 100, and 120 data points (or 10, 30, 40, 50, and 60 days). Diamonds in green, teal, and blue represent the top three best period estimates of Lomb–Scargle periodograms, respectively. Lines mark the period that was used to simulate the data (yellow, dotted–dashed), double that period (blue, dashed) and half that period (blue, dotted).
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: This figure shows the normalized distribution of recorded asteroid period values from the Lightcurve Database (LCDB) as of 2020 March (gray) and the kernel density estimate distribution of our period prior (blue).
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: Asteroid 3200 Phaethon light curve with simulated observations over 10 days total. Magnitudes are simulated without phase functions and normalized to 1. Gray lines denote the densely simulated light curve of 3200 Phaethon from the shape model available in the DAMIT database and the blue markers are the simulated photometric observations obtained from the light curve. Left: 8 observations over the first 4 days of observations, shortened from 10 days for viewing clarity. Right: the light curve for all 10 days of observations, folded at the asteroid’s estimated rotational period.
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: Simulated light curve of asteroid Eos 221 over 10 days. Blue markers are 20 simulated observations and the gray line is the original simulated light curve obtained from the DAMIT database.
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: Posterior probability density (blue) for the asteroid’s axis ratio, based on the Gaussian process model. For comparison, we show the standard estimate (solid black line) from the maximum/minimum data points and their observational uncertainties (dashed black lines).
Paper: Characterizing Sparse Asteroid Light Curves with Gaussian Processes
Authors: Christina Willecke Lindberg, Daniela Huppenkothen, R. Lynne Jones, Bryce T. Bolin, Mario Jurić, V. Zach Golkhou, Eric C. Bellm, Andrew J. Drake, Matthew J. Graham, Russ R. Laher, Ashish A. Mahabal, Frank J. Masci, Reed Riddle, Kyung Min Shin
Figure caption: LSP for asteroid 3200 Phaethon for 60 days of observations (N = 120 observations). The dashed yellow line indicates the highest peak in the periodogram, similar to the period found in Hanuš et al. (2018a).
Paper: EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry
Authors: Rachael M. Roettenbacher, Samuel H. C. Cabot, Debra A. Fischer, John D. Monnier, Gregory W. Henry, Robert O. Harmon, Heidi Korhonen, John M. Brewer, Joe Llama, Ryan R. Petersburg, Lily L. Zhao, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Claire L. Davies, Tyler Gardner, Cyprien Lanthermann, Gail Schaefer, Benjamin Setterholm, Catherine A. Clark, Svetlana G. Jorstad, Kyler Kuehn, Stephen Levine
Figure caption: Comparison of three models of activity-based RV variations. The red curve and shaded regions depict the GP model and confidence intervals (also shown in Figure 2). The orange curve depicts the RV variations obtained by rotating the LI-reconstructed stellar surface and integrating the stellar spectrum over a pixelated disk. For reference, snapshots of the disk model are shown for several selected timestamps of RV exposures. The features on the surface are responsible for the RV variations in the model, and a faint dashed line connects each snapshot to the corresponding point on the RV model curve. The gray curve represents an FF′ model (Aigrain et al. 2012), which serves as a benchmark for the LI surface model. The bottom panel shows the residuals for the LI surface model, GP model, and FF′ model in orange, red, and gray, respectively. The rms scatter of residuals after subtracting the GP is 0.76 m s−1, which is largely a reflection of the EXPRES measurement uncertainties and intra-night scatter. The rms scatter of residuals after subtracting the LI surface model and best-fit offset is 1.98 m s−1, compared to the 2.20 m s−1 rms from subtracting the FF′ model. All three are a reduction from the original rms scatter of 4.72 m s−1 of this subset of RVs, which were selected based on their overlap with TESS photometry. In both the plot and the rms calculations, the marginal Keplerian contribution has been subtracted.
Paper: EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry
Authors: Rachael M. Roettenbacher, Samuel H. C. Cabot, Debra A. Fischer, John D. Monnier, Gregory W. Henry, Robert O. Harmon, Heidi Korhonen, John M. Brewer, Joe Llama, Ryan R. Petersburg, Lily L. Zhao, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Claire L. Davies, Tyler Gardner, Cyprien Lanthermann, Gail Schaefer, Benjamin Setterholm, Catherine A. Clark, Svetlana G. Jorstad, Kyler Kuehn, Stephen Levine
Figure caption: Top: Binned TESS light curve (blue solid line) and LI-reconstructed light curve (red dashed line) of ϵ Eri. The binned light curve is normalized to the maximum value for each rotation. Two stellar rotations were reconstructed using LI with the gap in TESS data separating the rotations. The vertical black dashed lines indicate the times of the interferometric MIRC-X observations discussed in Section 4.2. Bottom: LI-reconstructed surfaces of the binned TESS light curve. The visible pole is marked with a white line and the surface rotates counterclockwise around this pole. The surface temperature ranges from a spot temperature of T spot = 4100 K to a photospheric temperature of T phot = 5100 K. The surfaces are shown at the times of the MIRC-X observations.
Paper: EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry
Authors: Rachael M. Roettenbacher, Samuel H. C. Cabot, Debra A. Fischer, John D. Monnier, Gregory W. Henry, Robert O. Harmon, Heidi Korhonen, John M. Brewer, Joe Llama, Ryan R. Petersburg, Lily L. Zhao, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Claire L. Davies, Tyler Gardner, Cyprien Lanthermann, Gail Schaefer, Benjamin Setterholm, Catherine A. Clark, Svetlana G. Jorstad, Kyler Kuehn, Stephen Levine
Figure caption: Best-fit GP and 1-Planet model that was fit to the combination of archival ϵ Eri RVs with new EXPRES RVs (dark blue scatter points). The archival data set is identical to that analyzed by Mawet et al. (2019), with the addition of CHIRON RVs (Giguere et al. 2016). For clarity, the MAP offset values (γ  k ) have been subtracted from each RV data set. A zoomed-in panel of the EXPRES RVs is shown on the right. The GP mean (red line) predominantly tracks the 7 yr planetary signal (black line), with deviations owing to stellar activity. The quasiperiodic activity signal is more clearly seen in the zoomed-in panel. The period of oscillations is usually close to the periodic timescale hyperparameter, which was fixed to the 11.4 day stellar rotation period. By choosing a quasiperiodic kernel, the GP can accommodate small variations in period and amplitude, as well as gradual changes in the activity signal’s phase. The characteristic timescale for these variations is set by the parameter L. The GP 1σ and 2σ confidence intervals are depicted as lightly shaded regions around the GP mean. CES+LC and CES+VLC correspond to data obtained with the Coudé Echelle Spectrograph with the Long Camera and Very Long Camera, respectively. Lick data are color-coded by their corresponding upgrade epoch.
Paper: EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry
Authors: Rachael M. Roettenbacher, Samuel H. C. Cabot, Debra A. Fischer, John D. Monnier, Gregory W. Henry, Robert O. Harmon, Heidi Korhonen, John M. Brewer, Joe Llama, Ryan R. Petersburg, Lily L. Zhao, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Claire L. Davies, Tyler Gardner, Cyprien Lanthermann, Gail Schaefer, Benjamin Setterholm, Catherine A. Clark, Svetlana G. Jorstad, Kyler Kuehn, Stephen Levine
Figure caption: Top: MIRC-X observations of ϵ Eri from 2020 November 2 (left) and 2020 November 5 (right). The observed data are shown in black with one baseline of each triangle shown in the closure phase and triple amplitude panels. The model data for a limb-darkened, spotted surface are plotted in red. Bottom: The spotted, limb-darkened (power-law) stellar surface models used to generate the interferometric data in red. The visible pole is marked with a white line and the surface rotates counterclockwise around this pole. As in Figure 3, the surface temperature ranges from a spot temperature of T spot = 4100 K to a photospheric temperature of T phot = 5100 K. The surface models are presented such that they are on the plane of the sky where north (toward the celestial pole) is up and east is to the left. Because of the sparse uv plane coverage, these starspot detections are marginal. More data are needed for future studies aiming to image the star and determine the inclination and position angle of the rotational pole.
Paper: EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry
Authors: Rachael M. Roettenbacher, Samuel H. C. Cabot, Debra A. Fischer, John D. Monnier, Gregory W. Henry, Robert O. Harmon, Heidi Korhonen, John M. Brewer, Joe Llama, Ryan R. Petersburg, Lily L. Zhao, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Claire L. Davies, Tyler Gardner, Cyprien Lanthermann, Gail Schaefer, Benjamin Setterholm, Catherine A. Clark, Svetlana G. Jorstad, Kyler Kuehn, Stephen Levine
Figure caption: Left: LI-reconstructed pseudo-Mercator surface of ϵ Eri for the first rotation observed by TESS (ending before TJD 2,459,157). At phase 0.0, as viewed by TESS, the center of the star is at longitude 90°. As time increases, the longitude of the center of the star decreases. Right: LI-reconstructed pseudo-Mercator surface of ϵ Eri for the second rotation observed by TESS (starting after TJD 2,459,157).
Paper: EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry
Authors: Rachael M. Roettenbacher, Samuel H. C. Cabot, Debra A. Fischer, John D. Monnier, Gregory W. Henry, Robert O. Harmon, Heidi Korhonen, John M. Brewer, Joe Llama, Ryan R. Petersburg, Lily L. Zhao, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Claire L. Davies, Tyler Gardner, Cyprien Lanthermann, Gail Schaefer, Benjamin Setterholm, Catherine A. Clark, Svetlana G. Jorstad, Kyler Kuehn, Stephen Levine
Figure caption: Left: The best-fit interferometric fit for the 2020 November 2 data set with the LI reconstruction and its latitude and longitude grid overlaid, assuming i = +70°. The LI reconstruction is rotated ∼335° east of north in order to have the LI and MIRC-X starspots lie on the same line of longitude. The visible pole is marked with a white line and the surface rotates counterclockwise around this pole. Right: Same as the left figure, but for the 2020 November 5 data set. This position angle determination is tentative due to the limited interferometric data.
Paper: EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry
Authors: Rachael M. Roettenbacher, Samuel H. C. Cabot, Debra A. Fischer, John D. Monnier, Gregory W. Henry, Robert O. Harmon, Heidi Korhonen, John M. Brewer, Joe Llama, Ryan R. Petersburg, Lily L. Zhao, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Claire L. Davies, Tyler Gardner, Cyprien Lanthermann, Gail Schaefer, Benjamin Setterholm, Catherine A. Clark, Svetlana G. Jorstad, Kyler Kuehn, Stephen Levine
Figure caption: Ground-based APT light curve of ϵ Eri. Top: Differential (b + y)/2 photometry (in magnitudes) from the T8 (black circles) and T4 (gray diamonds, latest data set) telescopes. The long-term trends are shown in red for the T8 data and in blue for the T4 data. Bottom: The same photometry as above, but with the long-term trends removed. The signature that remains is assumed to be rotational variation and not overall brightening or dimming trends.