adsabs/AstroCLIMB huggingface dataset:
Paper: Stability and Detectability of Exomoons Orbiting HIP 41378 f, a Temperate Jovian Planet with an Anomalously Low Apparent Density
Authors: Caleb K. Harada, Courtney D. Dressing, Munazza K. Alam, James Kirk, Mercedes López-Morales, Kazumasa Ohno, Babatunde Akinsanmi, Susana C. C. Barros, Lars A. Buchhave, A. Collier Cameron, Ian J. M. Crossfield, Fei Dai, Peter Gao, Steven Giacalone, Salomé Grouffal, Jorge Lillo-Box, Andrew W. Mayo, Annelies Mortier, Alexandre Santerne, Nuno C. Santos, Sérgio G. Sousa, Emma V. Turtelboom, Andrew Vanderburg, Peter J. Wheatley
Figure caption: Top: K2 transit light curve for HIP 41378 f from Campaigns 5 (blue points) with best-fit planet-only model (red dashed line). As in Figure 5, additional models with injected signals from a 0.53 R ⊕ moon and an Earth-size moon are shown by the black solid line and dashed–dotted line. The inset panel shows a zoomed-in view near mid-transit, demonstrating that the effects of moons are below the noise level of the data. Note that the 15 ppm difference in mid-transit flux between the moon-free and 0.53 R ⊕ moon cases is slightly greater in the K2 bandpass than the HST bandpass (Figure 5) due to differences in the stellar limb-darkening coefficients. Middle: Same as the top panel, but with data from K2 Campaign 18. Short-cadence data are shown by the transparent points, while the opaque points have been binned to match the long-cadence data. Bottom: Simulated 10 minute cadence PLATO data for a single transit of HIP 41378 f assuming the presence of no moon (red points) and an Earth-size moon (black points). The underlying Pandora models for each case are shown by the lines with corresponding colors, and a zoomed-in view near mid-transit is shown in the inset panel.
Paper: Multicolor Photometry of Tiny Near-Earth Asteroid 2015 RN35 across a Wide Range of Phase Angles: Possible Mission-accessible A-type Asteroid
Authors: Jin Beniyama, Ryou Ohsawa, Chrysa Avdellidou, Shigeyuki Sako, Satoshi Takita, Masateru Ishiguro, Tomohiko Sekiguchi, Fumihiko Usui, Shinichi W. Kinoshita, Kianhong Lee, Asami Takumi, Marin Ferrais, Emmanuël Jehin
Figure caption: Lomb–Scargle periodogram of 2015 RN35. The number of harmonics is two. The three periodograms were created using lightcurves obtained with the TRAPPIST-South telescope on 2022 December 19, 22, and 26. Four peak frequencies in each case are indicated.
Paper: Stability and Detectability of Exomoons Orbiting HIP 41378 f, a Temperate Jovian Planet with an Anomalously Low Apparent Density
Authors: Caleb K. Harada, Courtney D. Dressing, Munazza K. Alam, James Kirk, Mercedes López-Morales, Kazumasa Ohno, Babatunde Akinsanmi, Susana C. C. Barros, Lars A. Buchhave, A. Collier Cameron, Ian J. M. Crossfield, Fei Dai, Peter Gao, Steven Giacalone, Salomé Grouffal, Jorge Lillo-Box, Andrew W. Mayo, Annelies Mortier, Alexandre Santerne, Nuno C. Santos, Sérgio G. Sousa, Emma V. Turtelboom, Andrew Vanderburg, Peter J. Wheatley
Figure caption: HST white light curve posterior distributions for the planet-only model shown in Figure 5.
Paper: Multicolor Photometry of Tiny Near-Earth Asteroid 2015 RN35 across a Wide Range of Phase Angles: Possible Mission-accessible A-type Asteroid
Authors: Jin Beniyama, Ryou Ohsawa, Chrysa Avdellidou, Shigeyuki Sako, Satoshi Takita, Masateru Ishiguro, Tomohiko Sekiguchi, Fumihiko Usui, Shinichi W. Kinoshita, Kianhong Lee, Asami Takumi, Marin Ferrais, Emmanuël Jehin
Figure caption: Stacked images of 2015 RN35 in g, r, and i bands with a total integration time of 1200 s in 2023 January 16. Nonsidereally stacked images (top) and sidereally stacked images (bottom) are shown. Horizontal and vertical bars indicate 2015 RN35. The field of view covers ﹩1\buildrel{\,\prime}\over{.} \,75\times 1\buildrel{\,\prime}\over{.} \,75﹩. North is to the top and east is to the left.
Paper: Multicolor Photometry of Tiny Near-Earth Asteroid 2015 RN35 across a Wide Range of Phase Angles: Possible Mission-accessible A-type Asteroid
Authors: Jin Beniyama, Ryou Ohsawa, Chrysa Avdellidou, Shigeyuki Sako, Satoshi Takita, Masateru Ishiguro, Tomohiko Sekiguchi, Fumihiko Usui, Shinichi W. Kinoshita, Kianhong Lee, Asami Takumi, Marin Ferrais, Emmanuël Jehin
Figure caption: rms residuals between observed and model lightcurves of 2015 RN35 fixing P 1 at 1149.7 s. Residuals using two-dimensional Fourier series with m of 3 and m of 4 are shown by solid and dashed lines, respectively. Five periods with smaller rms in either case are indicated.
Paper: Stability and Detectability of Exomoons Orbiting HIP 41378 f, a Temperate Jovian Planet with an Anomalously Low Apparent Density
Authors: Caleb K. Harada, Courtney D. Dressing, Munazza K. Alam, James Kirk, Mercedes López-Morales, Kazumasa Ohno, Babatunde Akinsanmi, Susana C. C. Barros, Lars A. Buchhave, A. Collier Cameron, Ian J. M. Crossfield, Fei Dai, Peter Gao, Steven Giacalone, Salomé Grouffal, Jorge Lillo-Box, Andrew W. Mayo, Annelies Mortier, Alexandre Santerne, Nuno C. Santos, Sérgio G. Sousa, Emma V. Turtelboom, Andrew Vanderburg, Peter J. Wheatley
Figure caption: (a) K2 C5 light curve posterior distributions for the planet-only model shown in the top panel of Figure 9. (b) K2 C18 light curve posterior distributions for the planet-only model shown in the middle panel of Figure 9.
Paper: Multicolor Photometry of Tiny Near-Earth Asteroid 2015 RN35 across a Wide Range of Phase Angles: Possible Mission-accessible A-type Asteroid
Authors: Jin Beniyama, Ryou Ohsawa, Chrysa Avdellidou, Shigeyuki Sako, Satoshi Takita, Masateru Ishiguro, Tomohiko Sekiguchi, Fumihiko Usui, Shinichi W. Kinoshita, Kianhong Lee, Asami Takumi, Marin Ferrais, Emmanuël Jehin
Figure caption: Lightcurves of 2015 RN35. The reduced g-, r-, i-, and z-band magnitudes are presented as circles, triangles, squares, and diamonds, respectively. Bars indicate the 1σ uncertainties. The error-weighted average of magnitude in each lightcurve is presented with a dashed line. Shaded areas indicate the standard errors of the weighted averaged magnitudes.
Paper: Multicolor Photometry of Tiny Near-Earth Asteroid 2015 RN35 across a Wide Range of Phase Angles: Possible Mission-accessible A-type Asteroid
Authors: Jin Beniyama, Ryou Ohsawa, Chrysa Avdellidou, Shigeyuki Sako, Satoshi Takita, Masateru Ishiguro, Tomohiko Sekiguchi, Fumihiko Usui, Shinichi W. Kinoshita, Kianhong Lee, Asami Takumi, Marin Ferrais, Emmanuël Jehin
Figure caption: Phased lightcurves of 2015 RN35. All lightcurves in reduced r magnitude are folded with a period of 1149.7 s. Phase zero is set to JD 2459932.5. Bars indicate the 1σ uncertainties of measurements. The model curve fitted to the lightcurves is shown by the dashed line.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: 6 hr estimated CDPP in parts per million as a function of G-band magnitude from the perturbed PSF (top) and aperture (middle) light curves. CDPP estimates the noise properties of Kepler data, where lower values indicate a more precise light curve. The bottom panel shows a direct comparison of PSF and aperture CDPP values. The black and orange lines follow the CDPP distribution maximum in a brightness bin (0.1 mag width). As expected, the noise increases as flux decreases, reaching the 100 ppm value for objects fainter than G = 16, where the Kepler target selection bias is shown as a hard cutoff in bin counts. The gray dashed line shows the point at 13.25 mag where on average PSF photometry achieves lower CDPP values than aperture photometry. See Section 3.1.2 for details.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: PSF data (left column), model (middle column), and residuals (right column) evaluated on a stack of 250 TPFs in channel 37 observed during quarter 5. The top row shows the data and model in Cartesian coordinates, while the bottom row is in polar coordinates. Each data point corresponds to a pixel located δ x (radius) and δ y (angle) from the center of its corresponding source, and the color maps show the normalized flux value. The red marker in the top left panel represents the magnitude of the PSF centroid offset, which is <0.″8 with respect to the origin. A small fraction of data points have larger residuals due to remaining contaminated pixels that are clipped during model fitting.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Mean normalized pixel time series for uncontaminated pixel data in 250 TPFs in channel 37, quarter 5 (same as Figure 6). The 3 panels show the time series of each pixel data (left) after binning (as described in Section 2.5), the perturbed full model based on the Kepler pipeline CBVs (middle), and the normalized residuals (left). The pixel time series are sorted by flux value with fainter pixels at the bottom. The middle panel shows the “perturbed” version of the PSF model fit for all sources. Our model results in flux time series for each pixel, where the sources in the pixels are fit for flux at each time. The perturbed version of the full model is a good estimate of the data, as shown by the small residuals (≤2%). Data points with significant residuals are either the remaining contaminated pixels or belong to true variable sources.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Example of background model estimated using the kbackground package for a stack of 200 TPFs in channel 44 observed during quarter 5. The left (center) panel shows the pixel flux data (model) as a function of time, and each row on the y-axis represents the median average time series across column pixels. The color maps the flux deviation from the mean value across all cadences. Because the rolling band signal is more prominent in the row direction, we model it as a function of time and pixel row and average over the column dimension. The right panel shows the flux value averaged from all background pixels as a function of time, the data are shown in black and the model in blue, and red markers are cadences with an extra offset in the model due to outlier.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Perturbed PSF model for a stack of 250 TPFs in channel 37, quarter 5. The four panels show the spatial distribution of data points (top row) used to fit the perturbed model (bottom row) at the first (left column) and last cadence (right column). The shift in color shows the PSF profile change due to velocity aberration and other effects within the observing quarter.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Example of first four CBV vectors for channel 37, quarter 5. The colors are the different components: light colors are the original vector values, bold lines are the smooth version using a b-spline function, and vertical dashed lines show data gaps after the spacecraft performs data downlink.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Spatial distribution (2D histogram) of Kepler targets (left) and KBonus background sources (right) brighter than the 19th magnitude in the G-band across the Kepler field of view. KBonus background sources are stars that are fully or partially contained within a Kepler TPF but are not primary targets, and therefore the Kepler pipeline did not analyze them. The overdensities on the left correspond to particular stellar clusters, while on the right the overdensities closely follow the true underlying distribution of stars.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption:  G-band magnitude distribution of Kepler targets (red), KBonus background sources (green), and both (blue). Kepler targets are the stars defined by the primary mission. These are in the center of the TPF, and the Kepler pipeline created light curves for each of them. KBonus background sources are stars that are fully or partially contained within a Kepler TPF but are not primary targets, and therefore the Kepler pipeline did not analyze them.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Five LPV light-curve examples selected from the Gaia DR3 variable catalog. Red light curves are PDCSAP photometry, while black light curves are our PSF photometry. KIC identifier, G-band magnitude, and reference periods (when available) are in the title of each panel. Missing quarter data are due to nondetection or subpar PSF estimation (e.g., PSF fraction below 0.5 threshold).
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Next five LPV light-curve examples. Similar to Figure C1.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: KOI 932.01 false-positive candidate due to centroid offset. Figure layout and legends are the same as for Figure 14. The contaminant is KIC 9166862, which hosts the confirmed planet Kepler-731 b.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: KOI 021.01 false-positive candidate due to centroid offset. Figure layout and legends are the same as for Figure 14.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: KOI 254.01 false-positive candidate due to centroid offset. Figure layout and legends are the same as for Figure 14.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Confirmed exoplanet Kepler-686 b with an orbital period of 1.59 days. Similar to Figure A1.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Confirmed multiplanet system Kepler-238 e, Kepler-238 d, and Kepler-238 c, with orbital periods 23.65, 13.23, and 6.16 days, respectively. Similar to Figure A1.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Similar to Figure A1 for confirmed exoplanet Kepler-473 b with an orbital period of 14.56 days.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Confirmed exoplanet Kepler-770 b with an orbital period of 18.93 days. Similar to Figure A1.
Paper: Hot Jupiters from Disruption of Resonant Chains in Postdisk Evolution
Authors: Dong-Hong Wu, Ying He
Figure caption: Evolution of semimajor axis, orbital eccentricity, and resonant angles during a migration process and postdisk phase. Libration of resonant angles ﹩3{\lambda }_{i+1}-2{\lambda }_{i}-{\widetilde{\omega }}_{i}﹩ or ﹩3{\lambda }_{i+1}-2{\lambda }_{i}-{\widetilde{\omega }}_{i+1}﹩ indicates the 3:2 mean motion resonance between planet i and planet i + 1. λ  i  = M  i  + Ω i  + ω  i , and ﹩{\widetilde{\omega }}_{i}={{\rm{\Omega }}}_{i}+{\omega }_{i}﹩.
Paper: Hot Jupiters from Disruption of Resonant Chains in Postdisk Evolution
Authors: Dong-Hong Wu, Ying He
Figure caption: Top panel: cumulative density function of planetary masses for super-Earth in stable and unstable planetary systems. Bottom panel: cumulative density function of orbital period for Jupiter at the end of disk migration in stable and unstable planetary systems.
Paper: Hot Jupiters from Disruption of Resonant Chains in Postdisk Evolution
Authors: Dong-Hong Wu, Ying He
Figure caption: The distribution of the epoch that the last instability occurs in the planetary systems.
Paper: Hot Jupiters from Disruption of Resonant Chains in Postdisk Evolution
Authors: Dong-Hong Wu, Ying He
Figure caption: The frequency of nearby companions as a function of the orbital period of Jupiter. The errors are given as binomial errors. Our simulation results are shown in blue, while the results considered the observational bias of the Kepler satellite are shown in red.
Paper: Hot Jupiters from Disruption of Resonant Chains in Postdisk Evolution
Authors: Dong-Hong Wu, Ying He
Figure caption: The frequency of nearby companions as a function of the orbital period of Jupiter. The errors are given as binomial errors. Our fiducial simulation results are shown in blue, while the simulations including the GR effect are shown in red, and simulations including both the GR effect and tidal dissipation are shown in green.
Paper: Hot Jupiters from Disruption of Resonant Chains in Postdisk Evolution
Authors: Dong-Hong Wu, Ying He
Figure caption: The mutual inclination between Jupiter and its closest companion as a function of Jupiter’s orbital period.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Radial-velocity measurements of the bright star are compared with velocities measured from the He I profile (upper panel) and Si II emission (middle panel) in the envelope spectra. The mean of the combined He I and Si II emission velocities is shown in the bottom panel. The filled red squares are the mean velocities in phase intervals that are 0.1 unit wide where at least two velocity measurements were made. The dashed red lines show a least-squares fit to all of the phase-binned velocities, while the solid red lines show a least-squares fit that does not include the outlying point in the binned measurements that has v brightstar > 0 km s−1. That the velocities measured from the He I profile and the Si II emission lines are anticorrelated with the velocities measured for the bright star over much of the orbital velocity range of the bright star is consistent with them tracking the orbital motion of the companion.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: He I spectra that sample three orbital phase intervals near periastron after removing light from the brighter star. Each spectrum is labeled with the night in 2022 on which it was recorded, in the format MMDD, where MM is the month, and DD is the day of the month. The orbital phase of each spectrum is shown in brackets under the date of observation. The character of the He I trough changes with time in all three phase intervals, indicating cycle-to-cycle variations in the medium in which the He I trough forms. There is also evidence for line splitting near the trough center in the middle panel, and this is attributed to flows in the envelope that are driven by variations in the tidal field (see the text). He I emission become evident in the right-hand panel.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Maps of the area around V1507 Cyg at 408 Mhz (left panel) and 1420 MHz (right panel). Both were recorded as part of the CGPS. The 1420 MHz map has been smoothed to match the angular resolution of the 408 MHz map. Each map covers 180′ × 180′,  with north at the top and east to the left. V1507 Cyg, marked by the blue star, is at or near the center of a diffuse emission structure that is most obvious in the 1420 MHz map. The intermediate-age cluster NGC 6834 and the diffuse source IRAS 19445+2810, discussed in the text, are also labeled. Neither of these appear to be associated with the H I emission that is centered on V1507 Cyg.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Residual spectra that are the result of subtracting the mean Hα profile (shown in green) from the phase-binned spectra in Figure 8. The vertical dotted and dashed red lines mark the same features as in Figure 8. The red hash marks above each curve indicate the expected location of Hα at that phase if it followed the radial-velocity curve of the brighter star. The corresponding cyan hash marks indicate the expected location of Hα based on the radial velocities of the companion, as inferred from the solid line in the middle panel of Figure 7. The peak in the residuals propagates in a manner that is consistent with the motion of the brighter star, as expected if the bulk of the emission is associated with that star.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Hα profiles in phase-binned spectra. The contribution from the brighter star, which is assumed to have Hα based on the template β Ori spectrum, has been removed. The mean of the profiles is shown in green. The overall morphology of the Hα profile at some phases is similar to what is seen in the spectrum of some Herbig AeBe stars (e.g., Hamann & Persson 1992). The vertical red lines mark the approximate locations of the peak in Hα emission (dotted line) and a second bump that is slightly redward of the main peak that is most clearly seen between phases 0.2 and 0.5 (dashed line). The absorption trough between 6559 and 6560 Å that is present between phases 0.0 and 0.4 is likely due to blueshifted Hα absorption.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Same as Figure 5, but showing Hα. The overall shape of Hα emission varies with time in each phase interval in a more-or-less consistent manner, in the sense that the red bump appears in spectra recorded after 2022 June. The depth of the trough to the left of the main emission feature weakens with the appearance of the red bump, suggesting that they might be related. The relative height of Hα emission is roughly constant with time in the left-hand panel, and changes only slightly with time in the middle panel. However, significant changes in the height of Hα occur with time in the right-hand panel, in the sense that the peak height of the emission weakens with time. This is accompanied by a decrease in depth of the blue absorption trough.
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: The minimum RV masses ﹩M\sin i﹩ and orbital periods P of planets in our Sun-like star sample (filled circles). Planets are colored by median values of ages in the posterior PDFs that are obtained by the stellar isochrone fitting described in Section 2.2. The red and cyan rectangles show the definition of hot and cold Jupiters in our analysis, respectively. The background color map and white contours represent the mean detection efficiencies (survey completeness) of planets in the Sun-like star sample calculated from the injection-recovery simulation results published in R21.
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: Black crosses show the absolute Gaia G-band magnitudes M  G  and the effective temperatures T eff of 697 CLS stars for which we derived isochrone parameters. The 382 stars in our Sun-like sample defined in Section 2 are shown as orange circles. Among them, 37 stars (cyan squares) host cold Jupiters, and 9 stars (red stars) host hot Jupiters.