adsabs/AstroCLIMB huggingface dataset:
Paper: Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph
Authors: Satoshi Itoh, Taro Matsuo, Motohide Tamura
Figure caption: Schematics of the whole configuration of the new method. The abbreviation FT means “Fourier Transform” of the Fraunhofer diffraction of light between focal and pupil planes. The parts encircled by the cyan dashed curve compose the 1DDLC. The red dotted curve encircled the newly added parts in the new method.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. II. Speckle Observations of 16 Low-separation Systems
Authors: Ilija Medan, Sébastien Lépine, Zachary Hartman, Keivan G. Stassun
Figure caption: Here we show the reconstructed images in the 832 nm band from the speckle pipeline for each of the binaries with a third component detected in the speckle field.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: The redshifted spectrum for an example spaxel from GCMS. This spaxel is located in the overlap region near the center, approximately 5.63 kpc from the galaxy center. The location of the pixel is R.A.: 207.°0931702, decl.: 25.°6792436. 1 spaxel is approximately 0.°001389 for both R.A. and decl. The Balmer emission lines (Hα and Hβ) along with the other sky lines within the available bandwidth are also shown. Wavelengths are multiplied by 1.0513 to account for the redshift of VV 191b, where z = 0.0513. The known sky lines at 5577 Å is successfully removed and mitigated in the combination of individual exposures into a single cube. The feature at ∼5300 Å is suspected to be reflected artificial light, and the absorption feature at ∼5900 Å is a known flat-fielding effect that is dependent on telescope position. Both of these features will be corrected in a future iteration of the pipeline.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: The three panels show the dust map of VV 191b spiral foreground galaxy in the F606W filter from HST with different contours from the Balmer emission lines: the ratio (Hα/Hβ, left panel), Hα (middle panel), and Hβ (right panel), respectively. Color bars display the transmission from the grayscale dust maps, ranging from 0 to 1, with 1 meaning full transmission (no dust). Left: Balmer Decrement contour map with three different levels: The magenta level represents Hα/Hβ = 2.75, green represents Hα/Hβ = 3, and red has Hα/Hβ = 3.75. The Hα (middle) and the Hβ (right) contour maps are the other two figures. Note that the latter two maps are on the scale of 10−17 (Hα) and 10−17 (Hβ), with levels labeled on the figures. The maps of the separate Balmer lines by themselves have small peak detection values after subtracting out the stellar continuum. Hα and Hβ lie in the range of ∼10−18–10−17 erg s−1 cm−2 Å−1 arcsec−2 for the spiral galaxy, respectively. For the Hα contour, the three levels are 1 × 10−17 in magenta, 3 × 10−17 in green, and 5 × 10−17 in red. Similarly, for the Hβ contour, the three levels displayed are 10−18, 4−18, and 7 × 10−18.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Hα and Hβ maps of the dust lane region in spaxels, respectively. Similarly to those in Figure 4, these maps are shown in spaxels to show perspective on spaxel size as well as the size of the dust region in comparison to the WCS coordinates in Figures 7 and 8. This figure displays the zoomed-in dust region, while Figure 4 shows the full VV 191 galaxy pair. The white spaces in the two figures indicate emission line readings of <10−18. The maps are given in log units with a Gaussian interpolation (three pixels across).
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: The dust lane region highlighted in Figure 7 is shown in detail. Left: The A  V  map derived from HST/JWST imaging is shown. Right: map of Balmer decrement in dust lane region ranging values from 2 to 4. The left figure is smoothed using Gaussian interpolation. The attenuation is derived from the pixelated dust lane region, meaning the sizes of spaxels between the left and right figures are the same.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Top left: The Balmer decrement (Hα/Hβ) map of VV 191b. The ratio values are ranged from 0.5 to 4 (the theoretical value for no attenuation is 2.86). The following two maps are the Hα map (top right) and the Hβ map (bottom left) of the spiral foreground. Bottom right: histogram of over 11,000 values for the Balmer decrement values over the same regions as the three maps, ranged from 0 to 14. The hexagonal shapes are the GCMS fibers projected on the spaxel map.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: The logarithm base 10 of the Hα and Hβ maps of the top right and bottom left panels of Figure 3. The maps cover the same area as Figure 3, but are now labeled in pixels instead of WCS coordinates to give perspective on size of pixels. Both maps are smoothed using the Gaussian interpolation (three pixels across).
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Hα and Hβ peaks peaks zoomed in from the same example spaxel taken by GCMS as in Figure 1. The continuum (horizontal green line) is derived from interpolated data for both Hα and Hβ, calculated by taking the sigma clipped mean of the outermost pixels of the peak along with two pixels farther out. The red pixels represent each pixel in the spectra (same units) taken for the spectra. The units for the flux F  λ  are the same as defined in Figure 1 and divided by a normalization factor of 10−17. Spectrum is plotted with the LINE ID PLOT package.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Top: Flux for each individual emission line for both Hα (red) and Hβ (blue) for the entire foreground galaxy VV 191b. These emission line measurements are constrained all the way to the center spaxel (R/R  P  = 0). Units for flux (F  λ ) are erg s−1 cm−2 Å−1 arcsec−2 and divided by a normalization factor of 10−17. Bottom: Balmer decrement values for each spaxel in the dust lane region are matched with the distance to the center spaxel of VV 191b spiral foreground galaxy and then converted to distance in kpc by the WCS.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Left: JWST F090W image of the VV 191 occulting pair that encloses the area in which we selected our dust lane region. Right: JWST F606W dust map, with a zoomed-in view of the selected region shown in the lower right corner.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: Spearman’s rank correlation coefficients between the parameters of mid-IR PDFs of intensity at 21 μm and global galaxy properties. Stronger positive (negative) correlations are indicated in green (pink). We present rank correlations among the most important observation-specific parameters (galaxy inclination i, distance d), intrinsic properties (SFR surface density ΣSFR, stellar mass surface density ﹩{{\rm{\Sigma }}}_{{M}_{* }}﹩, H I mass surface density ﹩{{\rm{\Sigma }}}_{{M}_{\mathrm{HI}}}﹩, and CO luminosity surface density ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{CO}}}﹩), and extrinsic properties (average SFR, total stellar mass M *, H I mass M HI, CO luminosity L CO, average [O/H], and effective radius R  e ), as well as the H II region luminosity function slopes α from Santoro et al. (2022), with PDF parameters (H II region power-law index m, diffuse lognormal mean μ and dispersion σ) and region-wise flux contributions (median intensity I 50 and percent of total flux in field of view for centers, H II regions, and the diffuse ISM).
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The PDFs of emission of the galactic disk (r ≥ 1 kpc) after masking the center, at 7.7, 10, 11.3, and 21  μm for NGC 4303, tagged by emission from within and outside of H II regions. Top: images of the galactic disk of NGC 4303 in each MIRI filter, with the masked central region shaded. Hα-identified H II regions are overlaid in blue contours. Middle: PDFs of inclination-corrected intensity from the disk (excluding the masked central region), colored by the intensity color bar used to display each image. The PDFs of emission from within H II regions and outside of H II region masks are included in hatched blue and orange, respectively. Bottom: the same disk-only PDFs shown in the middle row, but now with the y-axis in log-stretch to highlight the power-law tail. It is evident that the emission from H II regions builds up the power-law component, and the diffuse ISM outside of H II regions shows a lognormal PDF.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: Summary of the galactic disk PDF parameters at each wavelength, including the H II region power-law index (m) in the left panel and the diffuse component lognormal mean (μ) and variance (σ) in the middle and right panels, respectively, as included in Table 2. The PDFs at 21 μm show significantly more pronounced power law components, while the mean intensity of the diffuse lognormal component is systematically higher in PAH-tracing 7.7 and 11.3 μm. The lognormal PDF widths remain generally consistent across the four filters.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The galactic disk PDFs (in black) of our full sample of 19 galaxies at 7.7, 10, 11.3, and 21 μm show an overall lognormal distribution with a power-law tail at higher intensities. The power law component can be primarily attributed to emission from individual H II regions (blue), and the lognormal component comes from emission from outside H II regions (red). Vertical dashed lines indicate the rms noise level in each filter for reference. The best-fit lognormal mean μ and dispersion σ are included for each PDF.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The disk PDFs (in black) of our sample of 19 galaxies at 7.7, 10, 11.3, and 21 μm decomposed by contributions from H II regions (blue) and outside (red). These are the same PDFs as in Figure 6, but in log-stretch to highlight the power-law component. The best-fit power law is shown in dark blue. The corresponding best-fit H II region power-law index m and log–log intercept c for each PDF are included for each panel.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: Median and 16th–84th range of mid-IR intensities in the diffuse ISM (red), H II region (blue), and central components (yellow) at 7.7, 10, 11.3, and 21 μm. AGN-classified galaxies (see Table 1 for AGN classification) are represented with diamonds. Targets are arranged in decreasing order of SFR from top to bottom. The overall brightness of both the disk and centers generally increases with SFR. The H II regions and centers (“bright” regions) show a significantly larger dynamical range of intensities at 21 μm.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: 21 μm images and PDFs of the galactic disk of NGC 0628 convolved to progressively lower resolutions, similar to Figure 11—0.″674 (the native resolution of the F2100W filter), 0.″85 (our working resolution), 4.″0, 7.″5, and 15.″0. This corresponds to physical resolutions of 32, 40, 190, 356, and 712 pc, respectively, in NGC 0628. While the power law is very prominent at high resolution, the power-law component is rapidly diluted at lower resolutions that do not resolve individual star-forming regions in the disk.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: 7.7 μm images and PDFs of the galactic disk of NGC 0628 convolved to progressively lower resolutions—0.″269 (the native resolution of the F770W filter), 0.″674 (the native resolution of the F2100W filter), 0.″85 (our working resolution), 4.″0, 7.″5, and 15.″0. This corresponds to physical resolutions of 12, 32, 40, 190, 356, and 712 pc, respectively, in NGC 0628. The two-component PDF only emerges at high angular resolution when individual star-forming regions can be resolved from the surrounding diffuse emission.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The fraction of total flux coming from the diffuse ISM (red), H II regions (blue), and central regions (yellow) at 7.7, 10, 11.3, and 21 μm. Targets are arranged in decreasing order of SFR from top to bottom. While the contribution from the centers varies, a significant fraction of the flux in the disk comes from diffuse emission.
Paper: The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves
Authors: Anna Zuckerman, James R. A. Davenport, Steve Croft, Andrew Siemion, Imke de Pater
Figure caption: Scatter plot demonstrating injection and recovery accuracy for a sample lightcurve. Each point represents the injected properties of recovered transits. In the left-hand plot, orange triangles represent transits flagged for large TTVs, and the orange filled area represents the region of parameter space which should produce a TTV flag. In the right-hand plot, orange triangles represent transits flagged as missing, blue squares represent transits flagged for large depths, and the orange and blue regions represent the corresponding regions of parameter space expected to produce flags. Not all transits injected in the shaded regions are flagged due to imperfect recovery of the injected properties.
Paper: The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves
Authors: Anna Zuckerman, James R. A. Davenport, Steve Croft, Andrew Siemion, Imke de Pater
Figure caption: Four of the six transits flagged as missing are clearly present on visual inspection of the data. Top left: Kepler-314c, transit 166, is flagged as missing but is clearly visible in the raw data. Missing data at the edge of the fit window and short-timescale stellar variability make the fitting difficult and produce a false positive. Top right: Kepler-472, transit 92 is flagged as missing yet is clearly present on visual inspection. Bottom left: Kepler-564, transit 105 is mis-fit due to two quality masked data points exactly at the transit minimum, which effectively hide the transit. Bottom right: similarly, the model fits adjacent stellar variability instead of transit 63 of Kepler-732b because of a single missing data point in the fit, as well as short-timescale stellar variability which alters the shape of the transit.
Paper: The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves
Authors: Anna Zuckerman, James R. A. Davenport, Steve Croft, Andrew Siemion, Imke de Pater
Figure caption: Example detrended, stitched, and masked lightcurves. Orange points are data that have been removed from our analysis due to quality issues flagged by the Kepler pipeline.
Paper: The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves
Authors: Anna Zuckerman, James R. A. Davenport, Steve Croft, Andrew Siemion, Imke de Pater
Figure caption: Kepler-1655b transits 17 (top) and 22 (bottom) are flagged as “missing” and are not obviously present on visual inspection, but are ultimately rejected due to poor linear trend removal and due to stellar variability which could mask a present transit.
Paper: The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves
Authors: Anna Zuckerman, James R. A. Davenport, Steve Croft, Andrew Siemion, Imke de Pater
Figure caption: Kepler-548b, transit 132, is an apparently very unusual transit with both a large TTV and a shallow depth. However, the transit appears to have a normal shape when viewed using the precotrending SAP flux values, and thus the anomaly can be credited to artifact of the Kepler cotrending process.