adsabs/AstroCLIMB huggingface dataset:
Paper: CHIMERA Occultation Constraints on the Abundance of Kilometer-scale Kuiper Belt Objects
Authors: Qicheng Zhang, Gregg W. Hallinan, Navtej S. Saini, Hilke E. Schlichting, Leon K. Harding, Jennifer W. Milburn
Figure caption: Cumulative distribution of stars by effective S/N measured per correlated length of light curve (light blue) and per 30.39 ms exposure frame (dark blue). The distributions roughly follow a truncated power law, with the mean number of stars per frame above a given S/N scaling approximately with (S/N)−1.6 at between 100 and 1000 stars.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Left: absolute H vs. J − K  S  CMD of all available 2MASS photometry for our full sample. Here, dark blue points indicate sources with high-quality 2MASS photometry in all bands (Qflg=AAA) and light blue indicates nonoptimal quality flags in one or more bands. Center: the same CMD for our synthetic photometry suite. Blue points indicate spectra with no data caveats. Orange indicates CALSPEC library stars that were observed only with STIS, where the spectra are filled in outside the STIS wavelength range (≳1 μm) using theoretical spectra. Green indicates XSL spectra that were corrected for slit loss via spline fitting (Verro et al. 2022b), and red indicates XSL spectra uncorrected for slit loss. Right: the same in J − H vs. J − K  S  color–color space.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Schematic comparison of NIR stellar spectra (black lines; Verro et al. 2022a) and their integrated flux densities (colored points, plotted at respective effective wavelengths) for three broad classes of cool and luminous giants. These include nonpulsating AGB and upper RGB stars (upper three), and TP carbon-rich (center) and oxygen-rich (lower) AGB stars, respectively. Transmission curves for the 2MASS JHK  S  and HST F110W and F160W bandpasses are shown as filled curves at the bottom, and regions with significant atmospheric telluric absorption are marked by gray vertical bands.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Differences between observed and synthetic magnitudes in Gaia (E)DR3 BP, G, and RP (left) and 2MASS JHK  S  (right) as functions of observed magnitude for select CALSPEC stars. Blue points indicate empirical spectrophotometry (available for effectively all CALSPEC stars in the optical), and orange indicates spectra extrapolated from theoretical models (e.g. missing WFC3/IR and/or NICMOS data), which we exclude from calculations and show only for reference. Blue dashed lines and solid bands show the weighted means and standard deviations of the photometric offsets, as reported in Table 2.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Summary stellar properties (effective temperature T eff, metallicity [Fe/H], and surface gravity ﹩\mathrm{log}(g)﹩) of the merged spectral libraries. We note that these literature measurements are extremely heterogeneous, and these data are used primarily to understand the ranges of stellar properties over which our library can provide insight. Stars with known photometric variability are plotted in orange, whereas stars not known to be variable are shown in blue.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Filter transformation fits to F110W – J (top row), F125W – J (center row), and F160W – H (bottom row) as functions of J − K  S , J − H, F110W – F160W, and F125W – F160W color from left to right. Points used in the fitting are shown in dark blue with light blue covariance ellipses. Solid black lines show the resulting piecewise linear transformations with 68% confidence intervals in gray, and dashed black lines mark the break-point locations.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Fractional distance uncertainties as a function of distance (linear on the lower axis, modulus on the upper) for all library stars. Colors and symbols correspond to host objects, which are Galactic field or bulge stars, open and globular clusters, and the Magellanic Clouds. Note that many of the distance uncertainties are asymmetric; we show the mean values here.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Sky maps of our final cross-library sample, color coded by adopted E(B − V) values. We show all-sky maps in Galactic coordinates for Milky Way stars in three distance bins of 0–0.1 kpc, 0.1–1 kpc, and 1–20 kpc. Magellanic Cloud stars are shown in separate insets in the lower right in equatorial coordinates.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: CMDs of our final fitting sample (left) and stars excluded from fitting (right), color mapped by literature effective temperature.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: Schematic diagram of the pillar system as viewed from the southwest, so that the observer’s line of sight runs horizontally across the figure. The green lines mark molecular gas structures, and the yellow highlight marks atomic gas structure, which forms an envelope around the molecular gas (Section 4.1.1). The gold rays originating from the top of the figure mark the direction of illumination, with the solid central line marking the “perpendicular” ray and the assumed line-of-sight position of the stars. P1a and P1b are both collections of features. The Shared Base and P1b overlap in definition, and the distinction between them is not particularly relevant because they are both approximate labels for (sets of) observed features. We estimate that the heads of P1a and P2 are separated by ∼1 pc along the line of sight; see Section 3.8 for more details.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: The top-left, top-right, and bottom-left panels show hydrogen column densities N H derived from C+, CO(J=1-0), and FIR dust emission. The bottom-right panel shows the JWST F335M image in grayscale as a reference. All four plots are on the same size scale, and the gray grid lines are in the same place. On the bottom-right panel, blue boxes show the integration areas for the pillar masses in Table 4, and red boxes show the same for Table 6. Orange squares mark the locations from which column densities are sampled in Table 3. In Table 3, from P1a-edge to Shared-Base-Mid, locations are listed in order of decreasing decl. along P1. The P2 locations are also in order of decreasing decl. along P2.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: (Left) The [C II] integrated intensity between V LSR = 18 and 27 km s−1, the same interval shown earlier in Figure 2, is shown in color. The four northern background regions (numbered) and the single southern background region are outlined. (Right) The mean spectrum from within each individual background region on the left panel, labeled accordingly. The “Average” background spectrum drawn in the bold, solid line is the average across all pixels in the numbered northern regions and does not include the southern region. Vertical lines mark every 1 km s−1 between 20 and 30 km s−1.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: Spectra observed toward the pillars in several lines. All data are convolved to the [C II] resolution, except CO(J = 3-2), which is shown at its native resolution. Locations are those shown in the leftmost panel of Figure 12 and listed by name in Tables 3 and 8. The [C II] line spectra are shown with a dotted line before and a solid line after subtracting out the background as described in Appendix B; the second column in Table 3 lists whether the northern or southern background was subtracted. Vertical lines mark every 1 km s−1 between 20 and 28 km s−1. Several lines/locations show additional components separated from the peak emission, such as CO at V LSR ∼ 29 km s−1 toward multiple positions or [C II] at V LSR ∼ 20–23 km s−1 toward the Ridge; all such components originate from background features identified in channel maps.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: R.A.–velocity projections of the one-, two-, and three-component line center solutions. Four-component model results are not shown here but are not significantly different than the three-component results.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: (Top row) Overlay plots made using pdrtpy, which show observed line ratios toward 4 locations that are labeled in the top-left corner of each plot. The black cross shows the automatically fitted solution and associated uncertainty; these values are listed in Table 2. (Bottom row) The reduced χ 2 associated with the automatic fit, with overlaid labeled contours. Radiation field values estimated via stellar catalog and FIR emission are plotted as horizontal dashed lines in each figure.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: Same as Figure 13 showing different species. All data except 13CO(J = 3-2) are convolved to the [C II] resolution. The line intensity axis spans a smaller range here. Multiple satellite lines appear in the HCN spectra. The N2H+ line is the satellite line (J, F1, F)=(1–0, 0–1, 1–2). The CO emission around V LSR ∼ 29 km s−1 is from a background feature.
Paper: CHIMERA Occultation Constraints on the Abundance of Kilometer-scale Kuiper Belt Objects
Authors: Qicheng Zhang, Gregg W. Hallinan, Navtej S. Saini, Hilke E. Schlichting, Leon K. Harding, Jennifer W. Milburn
Figure caption: Two examples of limiting events showing occultation-like signatures in ﹩i^{\prime} ﹩ light curves, setting the upper limits on the total 33–52 au KBO sky density for D > 0.9 km (upper row) and D > 0.65 km (lower row) shown in Figure 6. The left column shows the searched ﹩i^{\prime} ﹩ and simultaneously observed ﹩g^{\prime} ﹩ light curves for each star with the corresponding templates in black, while the bolded points indicate the corresponding ﹩i^{\prime} ﹩ and ﹩g^{\prime} ﹩ inset frames centered on the respective stars shown to the right (1 px = 0.″6). Templates are well-matched to the actually fitted ﹩i^{\prime} ﹩ light curves as expected, but are not as well-matched to the simultaneous ﹩g^{\prime} ﹩ light curves, while the star-centered insets do not obviously show changes in the brightness of those stars (although we caution even real fluctuations with similar ∼10%–20% amplitude may be only marginally discernible visually), suggesting these events in the ﹩i^{\prime} ﹩ light curve likely represent artifacts of dense-field photometry rather than true occultations.
Paper: Machine-learning Morphological Classification of TESS Light Curves of T Tauri Stars
Authors: Astaroth Elizabethson, Javier Serna, Alejandro García-Varela, Jesús Hernández, Juan F. Cabrera-García
Figure caption: Comparison of the recall estimations for each final classifier. The dotted line represents the identity. The x-axis shows the recall estimation done by the classifiers using cross-validation over the training sample. The y-axis shows the recall estimated using as an evaluation set the complete testing sample (All), the LCs in the testing sample with only one final class verified by visual inspection (Sum-1), and those with two final verified classes (Sum-2). Since each class has the same recall from cross-validation using different sets, they are located in the same position on the x-axis.
Paper: Machine-learning Morphological Classification of TESS Light Curves of T Tauri Stars
Authors: Astaroth Elizabethson, Javier Serna, Alejandro García-Varela, Jesús Hernández, Juan F. Cabrera-García
Figure caption: Morphological variability classes. We include some examples of stars representing the classes described in Section 2. (P) The star TIC 50657928 shows a periodic LC. (Pn) The star TIC 11296154 shows a periodic LC with significant noise. (N) The star TIC 249040852 exhibits a noisy LC, in which brightness variability is not detected. (Pi) The star TIC 50792805 exhibits a periodic LC with an overall increase in brightness. (Pd) The star TIC 249070479 shows a periodic LC with an overall decrease in brightness. (L) The star TIC 436013242 has a long-term variability. (MP) The star TIC 50748110 shows an LC with at least two periodic signals. (Pia) The star TIC 50622261 shows a periodic LC in which the variability amplitude increases with time. (Pda) The star TIC 4352899 shows a periodic LC in which the variability amplitude decreases with time. (EB) The star TIC 72829000 exhibits a typical Algol eclipsing binary LC. (D) The star TIC 11453668 shows an LC with sudden decreases (dips) in brightness, and (B) the star TIC 11296297 shows an LC with sudden increases (bursts) in brightness. Since we expect asymmetries in the brightness distribution in both dippers and bursters, we have joined them in a single class called the DB class.
Paper: Machine-learning Morphological Classification of TESS Light Curves of T Tauri Stars
Authors: Astaroth Elizabethson, Javier Serna, Alejandro García-Varela, Jesús Hernández, Juan F. Cabrera-García
Figure caption: Normalized distributions of χ 2 for our study samples. The left panel shows comparative histograms of χ 2 for the training and testing samples. The dotted vertical line shows the quality cut χ 2 = 0.006, defined as 3σ levels from the minor distribution peak. The right panel shows the cumulative plot of χ 2 per stellar region in the testing sample. The γ Velorum LCs could be more affected by systematic effects than other stellar regions. For example, the quality cut indicates that 30% of γ Velorum LCs are strongly dominated by systematics, while 10% of the LCs in other regions have this problem.
Paper: Machine-learning Morphological Classification of TESS Light Curves of T Tauri Stars
Authors: Astaroth Elizabethson, Javier Serna, Alejandro García-Varela, Jesús Hernández, Juan F. Cabrera-García
Figure caption: Recall values of multiclass (left panel) models as a function of the feature space’s dimension, for DB, N, and P classes. The order in which the features are decreased is given by the importance in Table 3. Recall values of SVM binary models (right panel) in function of the feature space’s dimension. For each class, the order in which the features are decreased is given by the importance in Table 2.
Paper: Machine-learning Morphological Classification of TESS Light Curves of T Tauri Stars
Authors: Astaroth Elizabethson, Javier Serna, Alejandro García-Varela, Jesús Hernández, Juan F. Cabrera-García
Figure caption: Correlation matrix of the initial 28 features calculated over all of our data (training and testing samples). Since there are few NAs values in DeltaM, those correlations are calculated over slightly less data.
Paper: Machine-learning Morphological Classification of TESS Light Curves of T Tauri Stars
Authors: Astaroth Elizabethson, Javier Serna, Alejandro García-Varela, Jesús Hernández, Juan F. Cabrera-García
Figure caption: Distribution of 706 candidates to P or DB classes proposed by the algorithm. In the upper panel we have a density histogram of the color of both classes giving an estimation of their probability densities. In the bottom panel we show a color–magnitude diagram using K and W3 bands obtained from the AllWISE catalog (Cutri et al. 2021), and selected to have a profile-fit flux signal-to-noise ratio over 2, and discarding those with possible contamination or bias due to proximity to an image artifact. The number of members in each star-forming region is distributed as follows: 457 stars in OSFC, 112 in Upper Scorpius, 60 in γ Velorum, 49 in IC 348, 19 in Corona Australis, and nine in Perseus OB2. The color–magnitude diagram shows that the behavior of the infrared excess of both classes occurs among all regions we studied.
Paper: Machine-learning Morphological Classification of TESS Light Curves of T Tauri Stars
Authors: Astaroth Elizabethson, Javier Serna, Alejandro García-Varela, Jesús Hernández, Juan F. Cabrera-García
Figure caption: Selected LCs of single-classed stars in the testing sample. The proposed morphology class is made by the final algorithm and confirmed by the visual revision. For each plot from left to right at the top: (A) Light curve in TESS magnitudes with a representative error bar. The legend at the top refers to the star identification, the mean TESS magnitude, and the uncertainty. (B) Field of view (210 ×  210 arcsec2) corresponding to a TESS image of 10 × 10 pixels. The white circle shows the photometric aperture, and the orange circles the sky annulus. The red dot marks the centroid of the star. In the bottom panels from left to right: (C) Phase-folded light curve to the estimated best period. ΔM shows the amplitude. (D) Lomb-Scargle periodogram, with the estimated period. (E) 210 ×  210 pixels Digital Sky Survey (DSS2) thumbnail, same field of view as (B). ﹩\tfrac{{F}_{{in}}}{{F}_{* }}﹩ shows the contamination level estimator (CLE).
Paper: Machine-learning Morphological Classification of TESS Light Curves of T Tauri Stars
Authors: Astaroth Elizabethson, Javier Serna, Alejandro García-Varela, Jesús Hernández, Juan F. Cabrera-García
Figure caption: Correction process done to star TIC 279581307. The top-left panel shows the original LC and its linear fit. The top-right panel shows the corrected LC, where the fit is subtracted. The middle panels show their phased curves using the proposed periods found by the LSP, which are shown in the bottom panels.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Orbits of 14 KBOs of the Sedna family projected onto the ecliptic plane. The blue line is parallel to the projection of ﹩{\hat{{\boldsymbol{n}}}}_{G}﹩ onto the ecliptic plane; it points toward the center of the Galaxy. The orbits of the six KBOs that are stable are shown in purple; these are the same orbits plotted in Figure 3. Eight additional KBOs with metastable orbits are shown in green. These 14 KBOs are the ones considered in support of the Planet Nine hypothesis in the review by Batygin et al. (2019). The orbital elements are from the Minor Planet Database and are given in Table 1.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Plot of ﹩({e}_{K}^{2},{\omega }_{K}^{2})﹩ for all 22 KBOs of the Sedna family listed in Table 1 (purple points for the six KBOs known to have stable orbits, green points for those with metastable orbits, and pink points for the eight added to the Minor Planet Database since the publication of the review by Batygin et al. 2019). Also shown is the location of the corresponding fixed point of the MOND orbital dynamics in the quadrupole approximation (red points). The clustering shown in Figure 4 for the six KBOs with known stable orbits is seen to persist for all 22 KBOs.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Same as Figure 8 with eight additional KBO orbits plotted (pink curves). These are the KBOs that have been added to the Minor Planet Database since the publication of the review by Batygin et al. (2019). The 14 objects plotted in Figure 8 are shown in purple (stable orbits) and green (metastable orbits).
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Plot of the C(u) staircase (blue) for all 22 KBOs listed in Table 1. These objects meet the criteria used in the review article by Batygin et al. (2019) to identify potential members of the Sedna family (a ≥ 250 au, q ≥ 30 au and i < 40°). Also shown is K(u), the cumulative distribution function for the null hypothesis (red dashed line).
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Plot of the C(u) staircase (blue) for the six KBOs of the Sedna family that are known to have stable orbits. Also shown is K(u), the cumulative distribution function for the null hypothesis (red dashed line).
Paper: Uncorrelated Amplitude and Frequency Variations of the Harmonics in SX Phoenicis Star XX Cygni
Authors: Jia-Shu Niu, 家树 牛, Yue Liu, 越 刘, Hui-Fang Xue, 会芳 薛
Figure caption: Light curves of XX Cyg observed by TESS.
Paper: Uncorrelated Amplitude and Frequency Variations of the Harmonics in SX Phoenicis Star XX Cygni
Authors: Jia-Shu Niu, 家树 牛, Yue Liu, 越 刘, Hui-Fang Xue, 会芳 薛
Figure caption: Periodogram of XX Cyg based on DS2. The fundamental frequency and its 						harmonics are marked as the red dots.
Paper: Uncorrelated Amplitude and Frequency Variations of the Harmonics in SX Phoenicis Star XX Cygni
Authors: Jia-Shu Niu, 家树 牛, Yue Liu, 越 刘, Hui-Fang Xue, 会芳 薛
Figure caption: Variations of the frequencies of F0 to F19. The blue dots with errorbars 						present the frequencies in moving windows, and the red dashed lines present 						the time-averaged frequencies.
Paper: Uncorrelated Amplitude and Frequency Variations of the Harmonics in SX Phoenicis Star XX Cygni
Authors: Jia-Shu Niu, 家树 牛, Yue Liu, 越 刘, Hui-Fang Xue, 会芳 薛
Figure caption: Variations of the amplitudes of F0 to F19. The red dots with errorbars 						present the amplitudes in moving windows, and the blue dashed lines present 						the time-averaged amplitudes.