adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for Protoplanets around MWC 758 and MWC 480 in Br-γ Using Kernel Phase and SCExAO/CHARIS
Authors: Alexander Chaushev, Steph Sallum, Julien Lozi, Jeffrey Chilcote, Tyler Groff, Olivier Guyon, N. Jeremy Kasdin, Barnaby Norris, Andy Skemer
Figure caption: Contrast curves for the RDI-calibrated kernel-phase data sets for MWC 758 and MWC 480. The contrast curves are calculated using a χ 2 interval method, which measures the difference in χ 2 between the data and a range of simulated test binaries. The figures also show the contrast curve for spectral bin 7 (pink dashed line), corresponding to where we might expect to find line emission in the case of Br-γ emission. While the SDI calibration is more sensitive than RDI for finding relative changes in the flux ratios, the RDI contrast benefits from being able to simultaneously fit all 17 spectral bins of the data. For both MWC 758 and MWC 480, lines are included to show the expected contrast of a companion for masses of 20, 40, and 80 M j. These masses were computed using the COND models (Baraffe et al. 2003). We use ages of 8 and 6 Myr for MWC 758 and MWC 480, respectively (Vioque et al. 2018). Assuming that any companion was formed shortly after the star, the continuum observations are only sensitive to brown dwarf mass objects.
Paper: Searching for Protoplanets around MWC 758 and MWC 480 in Br-γ Using Kernel Phase and SCExAO/CHARIS
Authors: Alexander Chaushev, Steph Sallum, Julien Lozi, Jeffrey Chilcote, Tyler Groff, Olivier Guyon, N. Jeremy Kasdin, Barnaby Norris, Andy Skemer
Figure caption: Full-frame example images from the MWC 480 (left panel) and MWC 758 (middle panel) CHARIS high-resolution K-band data sets, at the Br-γ spectral bin. The black contours and shaded region on the MWC 458 image are taken from 1.3 mm ALMA continuum observations (Liu et al. 2019) and show the distinct ring structure around the inner disk of MWC 480. The black lines on the MWC 758 image show contours from a Stokes Q  ϕ  image taken with VLT/SPHERE (Ren et al. 2020). These contours show the distinct spiral arms of the system. The panel on the right shows a 64-by-64 pixel cutout of the MWC 758 image, the same size as used in the kernel-phase analysis. Two lines are shown for scale, one at a radius of λ/D (red solid) and the other at 2λ/D (white dashed). Using a maximum baseline length of 5.8 m (see Section 3 for a discussion), a λ of 2163 nm gives a λ/D of 77 mas, corresponding to 12 au at 160 pc or just under 5 pixels on the detector.
Paper: Searching for Protoplanets around MWC 758 and MWC 480 in Br-γ Using Kernel Phase and SCExAO/CHARIS
Authors: Alexander Chaushev, Steph Sallum, Julien Lozi, Jeffrey Chilcote, Tyler Groff, Olivier Guyon, N. Jeremy Kasdin, Barnaby Norris, Andy Skemer
Figure caption: Steps in computing the kernel phases. Left panel: the discretized “gray” pupil model overlaid on the full SCExAO/CHARIS pupil. Middle panel: the UV plane of a single frame of HD 245009 computed with a discrete Fourier transform showing the phases and the sampling points used. The orange circle represents the 5.8 m baseline cutoff, while the white circle shows the full 7.74 m pupil. Right panel: example kernel phases from one frame of one of the PSF calibrators.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption: (a)–(c): TESS time-series photometry of HIP 65426 for Sectors 11, 38, and 64. (d): Amplitude spectra of each TESS sector in linear-linear space.
Paper: Verification of Astrometrically Accelerating Stars from Hipparcos and Gaia. I. Methodology and Application to HIP 44842
Authors: Valeri V. Makarov, Andrei Tokovinin
Figure caption: Left panel: histogram of GPM—HGPM proper-motion differences for 102,549 Hipparcos/Gaia stars in mas yr−1. Right panel: histogram of standardized GPM—HGPM proper-motion differences for the same sample of stars. Note the logarithmic scale of both axes.
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Computed probability distributions of ﹩{\rm{\Delta }}\mathrm{log}z﹩. Light curves with a positive ﹩{\rm{\Delta }}\mathrm{log}z﹩ favor the GP+transit model, whereas a negative ﹩{\rm{\Delta }}\mathrm{log}z﹩ indicates a light curve that favors the GP-only model. Left: distribution for flipped light curves, which contain no transits, used as the control sample to define a normal distribution. Significant (2–3σ) outliers are defined based on the normal distribution fit to the control sample. Right: distribution for light curves (with no flip). This ﹩{\rm{\Delta }}\mathrm{log}z﹩ distribution contains several outliers favoring the GP+transit model at the 2–3σ level not present in the control sample.
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Displayed is the Spitzer 3.6 μm light curve for 2MASS J11193254-1137466AB over a span of 10 hr, depicted by the light gray line. The data is also binned for clarity, and the corresponding binned data points are marked by red error bars. Superimposed on the plot is the GP+transit model that best fits the data (shown in blue), along with the isolated transit component (depicted by the black dashed line). The transit event with a significance of 2.6σ is observed between the time marks of 0.3 and 0.35 days. The transit fit has a depth of 0.59% and a duration of 43 minutes. This event is described in more detail in Limbach et al. (2021), the only difference here being the inclusion of the impact parameter in our transit model, which changed the best-fit parameters slightly.
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Transit probability of an exosatellite on a 1 day orbit as a function of the host mass. The colored blue circles denote the targets in this sample, including all hosts with masses <30 M Jup. The median transit probability of our sample is 14.3% and increases sharply inversely with host mass. Hosts with masses >30 M Jup (black dots) were excluded from this study—see He et al. (2017) for transit search of higher-mass ultracool dwarfs.
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: The Spitzer 3.6 μm light curve for 2MASS J21171431-2940034, spanning a duration of 21 hr, is illustrated by the light gray line. Overlaid is the best-fit GP+transit model (shown in blue), as well as the isolated transit model (displayed as a black dashed line). The 2.7σ transit event occurs just past the 0.6 day mark. The transit model that best fits this event has a transit depth of 0.34% ± 0.12% or 0.77 ± 0.26 R ⊕. Using the best-fit impact parameter, transit duration (65 ± 25 minutes) and host mass (7 ± 2 M Jup), we derive an orbital period of ﹩{1.5}_{-1}^{+2}﹩ days, similar to Io and Trappist-1b (although there is very significant uncertainly).
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Edge-on transit durations for an exosatellite on a half day (gray open squares) and 3 days (red solid diamonds) orbit about each of FFP and brown dwarf in this sample. Typical transit durations range between 30 minutes and 2.5 hr for short-orbit edge-on exosatellites transiting FFPs and low-mass brown dwarfs.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: Histograms of the planet radius distribution using the input Thompson et al. (2018) Kepler DR25 values (top; black), assuming all systems are around the primary star (middle; blue) and all systems are around the secondary star (bottom; orange). The top row shows the ρ ≤ 100 au sample (left) and the ρ > 300 au sample (right), and the full sample is shown in the bottom row. The dashed green curve shows the median completeness of all systems, described in the text. The full sample does not show evidence for a statistically significant gap, agreeing with Sullivan et al. (2023), while the ≤100 au sample has few sub-Neptunes. The >300 au sample shows a radius gap that appears to be shifted to smaller planetary radii. The revised planetary radius histograms have longer tails toward larger radii compared to the input samples because of the planetary radius bias caused by binaries.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: The fractional difference between the primary and secondary PRCF calculated in this work vs. the PRCF of Furlan et al. (2017). The vertical and horizontal lines at 1.0 denote perfect agreement. The majority of systems agree fairly closely between this work and Furlan et al. (2017), but there are many outliers with disagreement up to 60% in primary PRCF, and even more in secondary PRCF. This is likely because of better distances from Gaia and stellar parameter revision improving stellar radius estimates.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: Radius vs. T eff for all observed systems, showing both initial Kepler values from DR25 (magenta points; Berger et al. 2018) and the revised primary star values from this work (navy points), with the initial and revised values for each system connected by a black line. The underlying curves are MIST isochrones at various ages. The lower panel indicates the percent residual between the 1 Gyr evolutionary model and the final primary star radius for accepted systems.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: Histograms of the input (Berger et al. 2018 or Mathur et al. 2017) stellar temperatures (black, top panel), revised primary star temperatures (blue, middle panel), and secondary star temperatures (orange, bottom panel). The three figures show the ≤100 au and >300 au samples on the top row, and the full sample below. The ≤100 au sample has more cool primary stars than the >300 au sample, likely because the small-separation binaries are systematically more nearby than the wider binaries, meaning that lower-mass stars are detectable.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: The angular separation and estimated contrast in the Kepler bandpass for all systems in our sample. The systems are distributed through contrast–separation space, with a high concentration of bright, small-separation secondaries.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: Planet radius from Thompson et al. (2018) plotted against projected physical separation. Before any parameter revision, it is already apparent that there may be a dearth of larger planets in small-separation binaries.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Distribution of measurements for Hα emission for a random control subsample (blue), a set of stars similar to our candidates (black dashed line), and our candidates set (dark red line). Left panel shows the distribution of the pseudoequivalent width of the Hα line provided by Gaia DR3 (negative values indicate emission). Middle panel shows our measurement using Equation (11) (positive values indicate emission). Right panel shows those measurements against each other.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Age estimates and evolution stage provided by FLAME in Gaia DR3, for our candidates (dark red), a set of similar stars (gray), and a control sample (blue), restricted to the stars that have −0.5 < [M/H] < +0.5. The error bars depict the lower (16th percentile) and upper (84th percentile) ages to cover the 68% confidence interval. The x-axis (Evolution Stage) goes from 100 (zero-age main sequence) to 490 (red giant branch). 360 would be the main-sequence turnoff.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: SED and blackbody fitting for our excess candidates. Yellow triangles are the observations gathered and used by Ariadne to compute the SED (dashed dark red line). Red points are the unWISE (for W1 and W2) and AllWISE (for W3 and W4) values. Blue points are the prediction of our model (averaged over the seven folds). The best-fit blackbody is depicted as a gray dashed line. The final SED computed as Ariadne SED + blackbody is depicted as a solid black line. The letters above W3 and W4 are the AllWISE photometric quality flag.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Left panel shows the distribution of the Stetson index (Equation (12)) of our control sample (blue), of a set of stars similar to our candidates (black dashed line), and of our candidates (dark red line). Right panel shows the distribution of the percentile score of our candidates’ Stetson index with respect to the control sample (blue) and with respect to a set of similar stars (black dashed line).
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Blackbodies and stellar properties. Top left panel shows the fractional luminosity against the angular size, colored by the blackbody’s temperature. Top right panel shows the blackbody’s temperature against angular size, colored by the effective temperature of the star provided by Gaia. Bottom panels show the same space colored by the absolute magnitude M  G  (left) and G (right).
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Map of the recovery rate of blackbody injections in a sample of stars similar to our candidates (∼1500 stars). Our candidates’ blackbody estimates are shown as cyan dots.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Observed flux (in W2 band) vs. predicted flux from Ariadne SED-only (red points) and Ariadne SED + blackbody (blue points) fits, fitted on the flux residuals in bands K  s , W1, W2, and W3. The 1-to-1 line is depicted as a dashed gray line.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: NeoWISE time series for two of our candidates, in W1 (blue) and W2 (red) bands. Left panel shows a candidate with a high percentile score with respect to the control sample. Right panel shows a candidate with a low percentile score.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: K2's Radial P r distribution across a 4–34 pixel radius circle around the photocenter in the Red (left) and I-filter (right) domains at Epoch 1. We derived local values within each annulus of two pixels in width. P  U  (offset +2% for clarity) and null parameters (N  Q  and N  U  in the same color scheme as P  Q  and P  U , respectively) are plotted together for validity check of the derived P  Q  values. Intensity profiles in counts are also given. P  Q  with red edges indicates data points selected according to the criteria mentioned in the main text. Due to overlapping with background stars, there are apparent fluctuations in the distributions of the parameters.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: ZTF zr-band intensity image of K2 (upper row) and its enhanced version divided by azimuthal median (lower row) taken at or near the time of VLT polarimetric observations: on UT 2022 May 11.4 for Epoch 1, UT 2022 June 26.4 for Epoch 2, and UT 2022 July 19.3 for Epoch 3. All images were normalized on the same brightness scale and aligned with the north on top and the east on the left. Anti-sunward (﹩{{\boldsymbol{r}}}_{\odot }﹩) and negative velocity (﹩-{\boldsymbol{v}}﹩) vectors at each epoch are given. Green circles in the center encircle the outer boundary of the polarimetric aperture.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Polarization-phase curve of cometary dust in the Red domain (620−730 nm, left panel) and the I-filter domain (730−900 nm, right panel) quoted from the NASA/PDS comet polarimetric archive (Kiselev et al. 2017 and references therein) and the literature published afterward: 67P/Churyumov-Gerasimenko (Rosenbush et al. 2017; Kwon et al. 2022) which were lumped into the category of JFCs and 2I/Borisov (Bagnulo et al. 2021). Pre-perihelion (inbound) and post-perihelion (outbound) data were distinguished with filled and open symbols, respectively. The solid curve and its shade area indicate the fitted average trend (Equation (6)) and its 1σ error, respectively. The number of data points used for fitting is 29 for JFCs and 181 (= 96 inbound + 85 outbound) for OCCs in the Red domain and 17 for JFCs and 21 (= 19 inbound + 2 outbound) for OCCs in the I-filter domain.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Polarization maps of K2. Rows represent maps in each filter at a particular epoch. The photocenter of the coma is located at the center of each panel (0, 0). Patches of bright and dark stains aligned in a certain direction are caused by background star tracklets. In Epoch 2, central ∼3-by-3 pixels are saturated.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Same as Figure 4 but for the Epoch 3 data.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Spectral gradient of polarization or PC of cometary dust as a function of phase angle α. Pre-perihelion and post-perihelion measurements are distinguished by filled and open circles, respectively. Epochs 1, 2, and 3 are denoted by E1, E2, and E3, respectively.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: PCA example. Primary (PC1) and secondary (PC2) eigenvectors are shown as white and purple arrows, respectively. ϕ out and ϕ in denote a primary axis’ position angle of the outer and inner coma components, respectively. Two epochs were arbitrarily chosen as examples in which the inner and outer coma components presented similar or different angle alignments. Scale bars at the bottom show the projected physical distance from the comet center in kilometers, equivalent to 0.′4 at each epoch.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: 60 s exposure dust acquisition images of K2 in the Red domain (FILT_691_55) with VLT/FORS2 at three epochs of observations. Two dashed horizontal lines bracket the sky area covered by the polarization strip. ﹩{{\boldsymbol{r}}}_{\odot }﹩ and ﹩-{\boldsymbol{v}}﹩ denote the anti-sunward vector and the negative velocity direction of the comet, respectively. Photocenters are marked with a red “X” symbol in the center. Contours represent 90%, 70%, 50%, 30%, and 10% of the brightness peak.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Same as Figure 4 but for the Epoch 2 data.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: Distribution of observation moments for targets and idle. The five target stars are distributed around 135° of ecliptic longitude. The lower figure is a partial enlargement of the black box in the upper figure. The order of observation is determined by the position of the target star and the number of observations. At this ecliptic longitude, the distribution of target stars is also relatively sparse, providing idle time in between observations. This idle time can be used to intersperse with other observing tasks.