adsabs/AstroCLIMB huggingface dataset:
Paper: Line-by-line Velocity Measurements: an Outlier-resistant Method for Precision Velocimetry
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Thomas Vandal, Jean-François Donati, Claire Moutou, Xavier Delfosse, Pascal Fouqué, Eder Martioli, François Bouchy, Jasmine Parsons, Andres Carmona, Xavier Dumusque, Nicola Astudillo-Defru, Xavier Bonfils, Lucille Mignon
Figure caption: Histogram of radial velocities relative to the median velocity for Barnard’s star observed with SPIRou. Line-by-line values have a standard deviation of 2.59 m s−1 for a 2.57 m s−1 median uncertainty. Cross-correlation function values have a 7.53 m s−1 standard deviation.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Galactic Heliocentric (XYZ) coordinates of stars within D < 50 pc and ﹩{\rm{\Delta }}{v}_{\tan }\lt 5﹩  km s−1 of KOI-3876, color-coded by their velocity difference from KOI-3876 and transparency set by their 3D separation from KOI-3876. KOI-3876 is shown as a red X, Kepler-970 as an orange X, and members of Theia 316 from Kounkel & Covey (2019) as blue hollow circles. There is a high overlap between Theia 316 members and the cluster of MELANGE-3 candidates co-moving with and near KOI-3876. A majority of high-probability MELANGE-3 candidates are ≥10 pc from the Theia 316 string in low densities that would likely not trigger the clustering method used in Kounkel & Covey (2019).
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Comparison of the PARSEC model isochrones to candidate members of MELANGE-3. The top shows the corner plot of our MCMC mixture model comparison, with contours corresponding to 1σ, 2σ, and 3σ. The bottom plot shows the Gaia G vs. B  P  − R  P  CMD of stars included in the MCMC (blue circles). Each point is shaded based on its average outlier probability as determined by the relative strength of the two mixture components. Most of those flagged as outliers are likely to be nonmembers or binaries that evaded our selection cuts. KOI-3876 and Kepler-970 are shown as red and orange stars. Both have low (<1%) outlier probabilities. The green lines are 200 PARSEC isochrones with parameters drawn (randomly) from the MCMC posterior. The purple dashed line indicates a “field” (2 Gyr) population, highlighting the fact that much of the age leverage comes from the pre-main-sequence mid-M dwarfs and the small number of AF stars.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Rotation periods of candidate members of MELANGE-3 (dark circles) as a function of Gaia B  P  − R  P  color. Only stars with literature measurements or Q0 or Q1 rotations are shown. For reference, we show rotation periods from ≃110 Myr Pleiades (green squares; Rebull et al. 2016b). Stars are color-coded by their tangential velocity difference compared to KOI-3876. The stars on the Pleiades gyrochrone are also generally closer to KOI-3876 in tangential velocity. Because of the distance to the cluster, we have few rotation periods past M1.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Corner plot of the major transit parameters (P, R  P /R *, b, and ρ *) from our MISTTBORN fit for KOI-3876b (left) and Kepler-970 b (right). The contour levels correspond to 1σ, 2σ, and 3σ of the points (from darkest to lightest). The planet-to-star radius ratio and eccentricity are strongly covariant with impact parameter, as a higher impact parameter requires a deeper transit (and lower eccentricity) to reproduce the observed transit depth (and duration). It is difficult to break this degeneracy with Kepler long-cadence data alone, as the integration time is longer than the ingress/egress. Plot made using corner.py (Foreman-Mackey 2016).
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Galactic coordinates and motions for all 1007 candidate members of MELANGE-3. The red arrow shows KOI-3876. Kepler-970 is shown in orange, and other stars are color-coded by their tangential velocity offset from KOI-3876 with transparency set by their physical distance from KOI-3876. Arrows indicate the direction and (relative) magnitude of the proper motion.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Best-fit template spectrum (G1V; black) and synthetic photometry (green) compared to the observed photometry of KOI-3876 (red). Errors on observed photometry are shown as vertical error bars, while horizontal error bars indicate the approximate width of the filter. BT-SETTL models (blue) were used to fill in regions of high telluric absorption or beyond the template range. The bottom panel shows the photometric residual in units of standard deviations.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Phase-folded light curve of potential member TIC 158415341 (KIC 9700914) from TESS (blue) and Kepler (gray) detrended with the Notch filter. We found TIC 158415341 has a best-fit period of 20.016 days with an initial transit time of 1690.503 BTJD using TESS data, but we failed to detect the transit using Kepler data. We rejected this signal as noise in the TESS data.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Posteriors of the eccentricity (e) for KOI-3876b (red) and Kepler-970 b (orange). For both systems, the e = 0 fit yields a ρ ⊙ greater (i.e., of shorter duration) than the expected value determined in Section 6. Uncertainties are large due to the long (30 m) cadence, so the final eccentricity is consistent with zero in both cases (marginal consistency for KOI-3876b).
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Phase-folded light curves of KOI-3876 (left) and Kepler-970 (right) from Kepler (gray points) with the best-fit transit model (red). The best-fit GP model to the stellar variability has been removed from both the data and the model, for clarity. Both planets show the expected transit shape.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Posterior distributions for the transmission spectrum of WASP-17 b accounting for an active star retrieved with different data sets. The dashed vertical lines in each histogram refer to the median value, the first quantile (lower bound error), and the third quantile (upper bound error) of each parameter. Similarly, the reported values on top of the histograms denote the parameter’s median value, the first quantile, and the third quantile. The values shown are those obtained with the spectrum constituted by STIS visit 1&3, WFC3, Spitzer (Case 1). Inset: transmission spectra with best-fit models and their 1σ uncertainties.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Transmission spectrum of WASP-17 b, constituted by HST/STIS, HST/WFC3, and Spitzer/IRAC channel 1 and 2 data analyzed in this study compared to the data from Sing et al. (2016).
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Posterior distributions for the transmission spectrum of WASP-17 b accounting for a homogeneous star retrieved with different data sets. The dashed vertical lines in each histogram refer to the median value, the first quantile (lower bound error), and the third quantile (upper bound error) of each parameter. Similarly, the reported values on top of the histograms denote the parameter’s median value, the first quantile, and the third quantile. The values shown are those obtained with the spectrum constituted by STIS visit 1&3, WFC3, Spitzer (Case 1). Inset: transmission spectra with best-fit models and their 1σ uncertainties.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Top: white light curve for the HST/STIS G750L transmission observation taken on 2013 March 19 of WASP-17 b. First panel: raw light curve, after normalization. Second panel: light curve, divided by the best-fit model for the systematics. Third panel: residuals for the best-fit model. Fourth panel: autocorrelation function of the residuals. Bottom: spectral light curves fitted with Iraclis for the same observation, where, for clarity, an offset has been applied. Left panel: the detrended spectral light curves with the best-fit model plotted. Right panel: fitting residuals with values for the χ 2, the standard deviation of the residuals with respect to the photon noise (﹩\bar{\sigma }﹩), and the autocorrelation (AC) of the residuals.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Top: white light curve for the HST/STIS G430L transmission observation taken on 2013 March 15 of WASP-17 b. First panel: raw light curve, after normalization. Second panel: light curve, divided by the best-fit model for the systematics. Third panel: residuals for the best-fit model. Fourth panel: autocorrelation function of the residuals. Bottom: spectral light curves fitted with Iraclis for the same observation, where, for clarity, an offset has been applied. Left panel: the detrended spectral light curves with the best-fit model plotted. Right panel: fitting residuals with values for the χ 2, the standard deviation of the residuals with respect to the photon noise (﹩\bar{\sigma }﹩), and the autocorrelation (AC) of the residuals.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Top: white light curve for the HST/STIS G430L transmission observation taken on 2012 June 8 of WASP-17 b. First panel: raw light curve, after normalization. Second panel: light curve, divided by the best-fit model for the systematics. Third panel: residuals for the best-fit model. Fourth panel: autocorrelation function of the residuals. Bottom: spectral light curves fitted with Iraclis for the same observation, where, for clarity, an offset has been applied. Left panel: the detrended spectral light curves with the best-fit model plotted. Right panel: fitting residuals with values for the χ 2, the standard deviation of the residuals with respect to the photon noise (﹩\bar{\sigma }﹩), and the autocorrelation (AC) of the residuals.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Top: white light curve for the HST/WFC3 G102 transmission observations of WASP-17 b. First panel: raw light curve, after normalization. Second panel: light curve, divided by the best-fit model for the systematics. Third panel: residuals for the best-fit model. Fourth panel: autocorrelation function of the residuals. Bottom: spectral light curves fitted with Iraclis for the HST/WFC3 G102 transmission spectra, where, for clarity, an offset has been applied. Left panel: the detrended spectral light curves with the best-fit model plotted. Right panel: fitting residuals with values for the χ 2, the standard deviation of the residuals with respect to the photon noise (﹩\bar{\sigma }﹩), and the autocorrelation (AC) of the residuals.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Top: white light curve for the HST/WFC3 G141 transmission observations of WASP-17 b. First panel: raw light curve, after normalization. Second panel: light curve, divided by the best-fit model for the systematics. Third panel: residuals for the best-fit model. Fourth panel: autocorrelation function of the residuals. Bottom: spectral light curves fitted with Iraclis for the HST/WFC3 G141 transmission spectra, where, for clarity, an offset has been applied. Left panel: the detrended spectral light curves with the best-fit model plotted. Right panel: fitting residuals with values for the χ 2, the standard deviation of the residuals with respect to the photon noise (﹩\bar{\sigma }﹩), and the autocorrelation (AC) of the residuals.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: Raw light curves (first panel), detrended light curves (second panel), and residuals (third panel) for IRAC observations of WASP-17 b with channel 1 (top) and channel 2 (bottom).
Paper: Atmospheric Characterization of Hot Jupiter CoRoT-1 b Using the Wide Field Camera 3 on the Hubble Space Telescope
Authors: Kayli Glidic, Everett Schlawin, Lindsey Wiser, Yifan Zhou, Drake Deming, Michael Line
Figure caption: Secondary eclipse light curves of CoRoT-1 b, Visit 2. The first (leftmost) panel displays the raw light curves (the eclipse, baseline, and ramp profile) for the ten wavelength channels. One hundred randomly sampled light curves are drawn from the posterior distribution and overlaid with the median model shown as a solid black line. The second (middle) panel displays the astrophysical signal (the eclipse) with the ramp profile and baseline divided out of both the data and the randomly sampled light curves. The third (rightmost) panel displays the residuals from the median model. The residuals in any wavelength channel maximally varied by ∼1001 ppm from the median model. Additionally, Table 4 notes the correlation coefficients between wavelengths. All panels display an applied flux offset in between wavelength channels for clarity. Notice here that the traditionally discarded first orbit remains included within these model fits.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Evolution of the g − r color with time, based on the photometric predictions of E-MILES SEDs. The SSP models assume a Kroupa-like IMF and make use of the Padova 2000 isochrones. Four evolutionary tracks with metallicities ﹩{\mathrm{log}}_{10}(Z/{Z}_{\odot })=-1.3﹩, −0.7, −0.4, and 0.0 in the age range of 0–14 Gyr, with ages starting at 0.063 Gyr and increasing by ∼12% between successive age steps, are shown as thick color-coded lines. We also superimpose the average g − r colors of the diffuse and substructure components of our Fornax dwarf ETG sample in red and blue colors, respectively. Left panel: average g − r colors of the diffuse and substructure components of the subsample of disky dwarf ETGs. Right panel: average g − r colors of the diffuse and substructure components of the subsample of clumpy dwarf ETGs. The median value of the color measurements within one effective radius is shown by a dashed line, while the median value within two effective radii is shown by a continuous line. The shaded regions correspond to the 16th and 84th percentiles of the distributions.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: (a) Surface brightness and g − r color profiles of the diffuse component (red points) and substructure component (blue points) of our Fornax dwarf ETG sample. Left panels: surface brightness profiles in the g and r bands. The bright-red and bright-blue points correspond to the r-band profile, while the faint-red and faint-blue points correspond to the g-band profile. Right panels: g − r color profiles. The measurements are performed in elliptical annuli of constant width that match the geometry of the isophotes of the diffuse component of the galaxies out to two effective radii. The central region is excluded due to the effects of the PSF, and disregards an amount equal to 1.5 times the PSF FWHM. The gray-shaded area indicates the extension of the PSF FWHM. (b) Surface brightness and g − r color profiles of the diffuse and substructure components of our Fornax dwarf ETG sample.
Paper: Atmospheric Characterization of Hot Jupiter CoRoT-1 b Using the Wide Field Camera 3 on the Hubble Space Telescope
Authors: Kayli Glidic, Everett Schlawin, Lindsey Wiser, Yifan Zhou, Drake Deming, Michael Line
Figure caption: Secondary eclipse light curves of CoRoT-1 b, Visit 3. The residuals in any wavelength channel maximally varied by ∼924 ppm from the median model. Additionally, Table 4 notes the correlation coefficients between wavelengths. Other comments are the same as for Figure 2.
Paper: Atmospheric Characterization of Hot Jupiter CoRoT-1 b Using the Wide Field Camera 3 on the Hubble Space Telescope
Authors: Kayli Glidic, Everett Schlawin, Lindsey Wiser, Yifan Zhou, Drake Deming, Michael Line
Figure caption: Image of CoRoT-1 b, Visit 2, displayed in relation to its location on the instrument detector (in pixels). The color bar depicts the count value at each pixel. The red rectangle outlining the source, CoRoT-1 b, represents the source aperture, the spectral extraction area. The shaded red rectangular regions represent the areas for background subtraction. The varying widths for the background subtraction regions are to avoid neighboring sources of flux.
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Heliocentric velocity relative to M31's systemic velocity vs. projected M31-centric radius for M31 RGB stars (Section 5.1) along the line of sight to the GSS (green open squares; Gilbert et al. 2009), the NE (red filled triangles; this work), W (outlined magenta circles; F12), and SE (blue open diamonds) shelves, and the region of M31's northeastern disk surveyed by SPLASH (black points; Dorman et al. 2012, 2015). We also show PNs that are possibly GSS-related (blue open inverted triangles; Merrett et al. 2003, 2006). Each RGB sample contains stars belonging to the phase-mixed stellar halo in addition to substructure (i.e., the disk and/or tidal debris). Left panel: the NE shelf compared to the GSS and the disk region. The secondary kinematical component along the GSS known as the KCC (Kalirai et al. 2006; Gilbert et al. 2009) is located at v helio–v M31 > −150 km s−1 and R proj < 25 kpc, overlapping with the lower envelope of the NE shelf. We do not find clear evidence for a continuation of the NE shelf in the disk region or an intact progenitor core based on its predicted velocity range (Section 4.2; Fardal et al. 2013). Right panel: the shell patterns for the NE, W, and SE shelves, which are predicted to correspond to successive orbital wraps of GSS-related tidal debris. We show the projected radial range of the NE shelf edge inferred from imaging by F07 for reference.