adsabs/AstroCLIMB huggingface dataset:
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: The location of wavelength-dependent flux-ratio measurements with respect to the stellar rotational phase (P rot = 5.7 days). Dashed lines mark the rotational phase of the eight SALT–HRS spectra with well-separated velocity components. The rotational-phase-folded TESS light curves from Sectors 5, 6, and 32 are shown in blue. The spot-modulation model is over-plotted in orange. Eclipse events in the TESS light curve are visible by eye. The dotted line shows the rotational phase of the eclipse observed with LCO, eclipse 9.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Combined broadening function for two epochs of SALT–HRS spectra. These highlight a typical epoch that is well separated (top) and blended (bottom). The orbital phase of each epoch is provided in the top-right panel.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption:  A(Li)Coord−DenseNet of LAMOST LRS DR8 predicted by Coord-DenseNet vs. ﹩{\rm{A}}{(\mathrm{Li})}_{{\rm{H}}.\mathrm{Res}.}﹩ of the high-resolution literature. The solid line represents the diagonal line, while the black dotted line is the overall shift of 0.27 dex.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: The A(Li) vs. (a) T eff, (b) ﹩\mathrm{log}\,g﹩, and (c) [Fe/H]. The bin sizes are 50 K, 0.1 dex, and 0.1 dex, respectively. In panel (a), there is a clear peak at 4850 K. When T eff > 5300 K, the number of Li-rich giants shows an increasing trend with increasing temperature. In panel (b), there is a peak at ﹩\mathrm{log}\,g﹩ of 2.5 and 3.5 dex, respectively. In panel (c), [Fe/H] has a clear peak near −0.3 dex.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: TESS light curve of TOI 450. The top panel displays Sectors 5 and 6, with data from Sector 32 in the bottom panel. The Gaussian process variability model is shown in the orange.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: Distribution of A(Li) for 7768 Li-rich giants predicted by the model. The bin size is 0.1 dex. As A(Li) increases, the number of Li-rich giants in each bin decreases, except for the first few bins.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: The Li abundance distribution of 2323 RC stars (blue) and 1029 RGB stars (green) obtained by crossing our predicted Li-rich giants with Table 1 of Ting et al. (2018). The bin size is 0.1 dex. The distribution trends of RC and RGB stars in different A(Li) ranges are consistent.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Detection limits (5σ) for companions to TOI 450 as observed by the SOAR HRCam speckle imager. The reconstructed image is presented in the inset panel. No companions are detected.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Phase-folded eclipse light curves in the ﹩r^{\prime} ﹩ (blue diamonds), TESS (orange circles), and I (red squares) bandpasses. The best-fitting eclipse model from our combined fit is over-plotted in each filter in its associated color. Horizontal lines at the right of the plot highlight the eclipse depth in each filter. A strong color dependence is observed due to wavelength-dependent limb-darkening.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption:  FriendFinder results for TOI 450, which recovers the Columba association. In each panel, TOI 450 is labeled with a red ×. “Friends” are plotted by a circle if their Gaia RUWE is less than 1.2 (presumed single) and by a square if their Gaia RUWE is greater than 1.2 (presumed binary). The size of the point encodes its 3D distance from TOI 450 (larger is closer). The color encodes the tangential velocity difference from TOI 450 as shown in the color bars. Left: sky map of TOI 450 friends. Right: XYZ spatial distributions of TOI 450 friends.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Wavelength-dependent flux ratios from eight SALT–HRS epochs. Decreased measurement precision at short wavelengths is due to decreasing signal-to-noise at short wavelengths. Scatter in orders near ∼8000 Å probes temperature-sensitive TiO features where spot variability has the largest impact. Filter curves from the photometric filters used to observe eclipses are provided in the bottom panel.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: RV orbital solution for TOI 450. The top panel set presents the RVs for the primary (blue) and secondary (red). The bottom panel set presents the RV difference. In each panel set, SALT–HRS and HARPS data are shown with circles and diamonds, respectively. The best-fitting orbital solution from our combined fit is shown as the solid lines. The bottom panels in each set present the fit residuals in kilometers per second and in units of their measurement error (σ). The gray vertical line marks the phase of the primary eclipse. Phase ϕ = 0 corresponds to periastron passage.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Gaia color–magnitude diagram (CMD) of TOI 450 friends. The CMD distribution is broadly consistent the with Tuc–Hor empirical sequence at ∼40 Myr. The shape, size, and color coding scheme are described in Figure 8.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Example of our spectral energy distribution (SED)-fitting procedure. The top subpanel shows an example template (black) and BT-SETTL model (blue) along the synthetic photometry (green). The observed photometry is colored by the source, with vertical errors indicating measurement errors and horizontal errors indicating the filter width. The bottom panel shows the residuals in units of standard deviations. The final residuals include errors from filter zero-points and hence do not perfectly match the comparison in the top panel.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Radius ratio and surface-brightness ratio posterior for the TESS bandpass from our fit to the SALT–HRS flux ratios and broadband spectral energy distribution. The top panel presents the 68% contours for the eight individual epochs. The bottom panel is the joint posterior with contours enclosing the 50th, 68th, 95th, and 99.7th percentiles.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Hα line profiles for select SALT–HRS epochs. Spectra have been shifted to the system’s center-of-mass velocity. Blue and red dashes mark the primary and secondary velocities, respectively. The orbital phase of each observation is provided to the right of each spectrum.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: RV difference friends from TOI 450 as a function of the absolute G magnitude. Velocities compiled from Gaia EDR3 and the literature. The shape, size, and color coding scheme are described in Figure 8.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Comparison of fits including spots. The top row presents a possible realization of the stellar surfaces at first contact of the primary eclipse, with the derived radii labeled for each star. The associated spot-covering fraction (f s) and spot-covering fraction of the eclipsed area (f s,ecl) are provided below. The second and third rows present the eclipse models without and with the effect of spots included for each filter, respectively. Horizontal dotted lines in these rows represent the best-fit eclipse depth from the fiducial fit (i.e., the observed eclipse depth; Figure 13). The last row presents the limb-darkening profiles for each filter. The leftmost column is the fiducial fit (Section 5.2). The middle two columns are a subset of the “eclipsing ambient” models (Section 6.2.1). The third column is the “eclipsing spots” model (Section 6.2.2), which can be ruled out based on its poor match to the filter-dependent eclipse depths and its reversal of the expected filter-dependent limb-darkening trend. The secondary appears completely spotted, but instead has a lower surface brightness than the primary, which is favored in this fit. The rightmost column is the fit spot model (Section 6.2.3), from which we adopt our definitive measurements. Diverse spot configurations and derived radii can reproduce the observed eclipse depths.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Filter-dependent radial brightness profiles from our individual filter (left) and combined fits (right). The top panels present the surface brightness with respect to μ. The bottom panels are with respect to the normalized radius coordinate. The median profile for each filter is shown with a thick line, and 50 random draws from the limb-darkening coefficient posteriors are shown in thin lines of the associated color. In the right panels, dashed lines with black backgrounds represent the theoretical predictions. The vertical gray lines mark the maximal radius occulted by the eclipse (solid) and its uncertainty (dashed), and arrows indicate the portion of the plot that correspond to eclipsed area.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Quantitative comparison of TOI 450 measurements with various model suites. In each panel, model suites correspond to rows of measurements. Measurements that are made in the mass–radius plane are depicted as circles. Measurements from the HR diagram are shown as diamonds and triangles representing empirical and synthetic measurement approaches, respectively. Top left: isochronal age measurements. The literature Columba age, ∼40 Myr, is shown as the vertical shaded region. Measurements from different approaches are slightly offset vertically for clarity. Top right: fractional difference between the HR diagram mass measurement and the dynamical mass. Bottom left: fractional difference between the model radii given the dynamical mass and the derived radii from the EB fit. The comparison is made at three discrete ages. Bottom right: absolute difference in T eff given the dynamical mass. Comparison is made at three discrete ages for each T eff measurement approach (empirical, synthetic).
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Comparison of TOI 450 to isochrones from various stellar evolution model suits in the HR Diagram. See the text for model descriptions. Colored lines represent isochrones at specific ages provided in the legend. The literature age of Columba (40 Myr) is shown with a solid line. Gray lines mark mass sequences, which are labeled in solar masses at the 20 Myr isochrone. The blue and red points are the T eff and luminosity for the primary and secondary, respectively, from the fit of synthetic templates described in Section 5.1. The black point is a fit using empirical stellar templates (Section 3.8), where we assume both stars have the same T eff and radius.
Paper: A Low-mass, Pre-main-sequence Eclipsing Binary in the 40 Myr Columba Association—Fundamental Stellar Parameters and Modeling the Effect of Star Spots
Authors: Benjamin M. Tofflemire, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Michael A. Gully-Santiago, Andrew Vanderburg, William C. Waalkes, Zachory K. Berta-Thompson, Kevin I. Collins, Karen A. Collins, Louise D. Nielsen, François Bouchy, Carl Ziegler, César Briceño, Nicholas M. Law
Figure caption: Comparison of the TOI 450 masses and radii to isochrones from various stellar evolution model suites. See the text for model descriptions. Colored lines represent isochrones at specific ages provided in the legend. The literature age of Columba (40 Myr) is shown with a solid line. The TOI 450 primary and secondary are overlapping.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets
Authors: Jéa I. Adams Redai, Katherine B. Follette, Jason Wang, 劲飞 王, Clare Leonard, William Balmer, Laird M. Close, Beck Dacus, Jared R. Males, Katie M. Morzinski, Joseph Palmo, Laurent Pueyo, Elijah Spiro, Helena Treiber, Kimberly Ward-Duong, Alex Watson
Figure caption: Optimization results for six HD 142527 data sets in which the companion is recovered. The top panel shows S/N maps of KLIP reductions using a single set of fixed KLIP parameters for all data sets: annuli = 5, movement = 2, KL = 10. Panels 2, 3, and 4 show S/N maps of Hα KLIP reductions with optimal parameters identified for injected continuum planets under the pyKLIP-PE image quality metrics peak S/N (panel 2), average S/N (panel 3), and contrast (panel 4) individually. Panel 5 shows the optimal parameters selected by the combination of these three metrics. Panel 6 shows the peak S/N, average S/N, contrast combination, along with the false-positive pixel and neighbor quality metrics. Note that the best parameters based on false-positive pixels are not shown individually because they are nearly degenerate for most data sets. In each of the six epochs, pyKLIP-PE was able to recover the real planet at a higher S/N than the generic reductions under each individual metric in 22/30 cases. A Gaussian smoothing was applied to these data with a standard deviation of 1 before computing the S/N maps.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets
Authors: Jéa I. Adams Redai, Katherine B. Follette, Jason Wang, 劲飞 王, Clare Leonard, William Balmer, Laird M. Close, Beck Dacus, Jared R. Males, Katie M. Morzinski, Joseph Palmo, Laurent Pueyo, Elijah Spiro, Helena Treiber, Kimberly Ward-Duong, Alex Watson
Figure caption: A depiction of pyKLIP output demonstrating the variation in the quality of recovery for a true companion (HD 142527 B) across a range of KLIP movement and annuli parameters. Each pixel in the central heat map represents a separate, independent KLIP reduction with the movement and annuli values depicted on the x- and y-axes, respectively. The color of that pixel reflects the highest single-pixel S/N value at the location of the companion in the S/N map. Inset images depict the S/N maps for a representative sample of individual reductions. While much of this parameter space yields recovery of the companion at >5σ, there is intense variation in the quality of the extraction, and even some parameters for which the signal from the bright companion is nearly absent. For this data set, an optimal combination of parameters to maximize the S/N of the companion for 10 KL modes is a movement value of 1 pixel and 3 annuli. An in-depth explanation of this grid search technique is provided in Section 4.2.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets
Authors: Jéa I. Adams Redai, Katherine B. Follette, Jason Wang, 劲飞 王, Clare Leonard, William Balmer, Laird M. Close, Beck Dacus, Jared R. Males, Katie M. Morzinski, Joseph Palmo, Laurent Pueyo, Elijah Spiro, Helena Treiber, Kimberly Ward-Duong, Alex Watson
Figure caption: Maps of pyKLIP-PE output for continuum injected (CF) planets (first column) and the Hα real (HR) companion (second column), for each HD 142527 B data set, normalized so that the 10th–90th percentiles in the ADQ metric span the range 0–1. The difference between the two normalized maps is shown in the third column, where red values indicate parameter combinations that are more strongly favored for false planets and blue indicates the opposite. Shown in the rightmost column are histograms of the difference maps. The highest relative parameter quality annuli/movement combinations are highlighted in red in the two leftmost columns.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets
Authors: Jéa I. Adams Redai, Katherine B. Follette, Jason Wang, 劲飞 王, Clare Leonard, William Balmer, Laird M. Close, Beck Dacus, Jared R. Males, Katie M. Morzinski, Joseph Palmo, Laurent Pueyo, Elijah Spiro, Helena Treiber, Kimberly Ward-Duong, Alex Watson
Figure caption: Histograms of summary statistics for continuum injected planet—real Hα companion difference maps. These maps are generated for each of 32,768 possible combinations of image quality metric and KL mode from the pyKLIP-PE output. For each map, the sum of the difference map (top left), standard deviation of the difference map (top right), median of the difference map (bottom left), and difference in the ADQ metric score between the injected and true companions at the location of the peak (bottom right) is computed. These quantities are averaged across the six HD 142527 B detections, and these averaged quantities are depicted in the histograms. The red vertical lines indicate the value of these statistics for our choice of “best” collapse method.