adsabs/AstroCLIMB huggingface dataset:
Paper: Photometric Mapping of Carbonaceous/Siliceous Dust and Water Ice in the ISM with JWST: Applications to the Dense Sightlines
Authors: Burcu Günay, Karl D. Gordon, Joshua E. G. Peek, Marjorie Decleir, Dries Van De Putte, Kirill Tchernyshyov, Michael G. Burton
Figure caption: The maps illustrate the spatial gradient distribution of optical depths for water ice, aliphatic hydrocarbons, and silicates across the modeled FOV. The first row shows spectroscopic optical depths (τs), the second row presents photometric optical depths (τp), and the third row displays calibrated photometric optical depths (τc). The fourth row is constructed using reference optical depths (τr) from the literature (E. L. Gibb et al. 2004).
Paper: Photometric Mapping of Carbonaceous/Siliceous Dust and Water Ice in the ISM with JWST: Applications to the Dense Sightlines
Authors: Burcu Günay, Karl D. Gordon, Joshua E. G. Peek, Marjorie Decleir, Dries Van De Putte, Kirill Tchernyshyov, Michael G. Burton
Figure caption: The photometric fluxes are illustrated, as an example, on the spectrum of the Galactic Center source Sgr A* (E. L. Gibb et al. 2004), with colored dots indicating the JWST filters used. The half-power passband wavelengths of the filters are also illustrated in the background using filled areas with matching colors. The gray line represents the general continuum fit using photometric flux measurements from the selected continuum filters.
Paper: Photometric Mapping of Carbonaceous/Siliceous Dust and Water Ice in the ISM with JWST: Applications to the Dense Sightlines
Authors: Burcu Günay, Karl D. Gordon, Joshua E. G. Peek, Marjorie Decleir, Dries Van De Putte, Kirill Tchernyshyov, Michael G. Burton
Figure caption: Local linear continuum fitting (dashed lines) examples with Set 1 for the NIR region (left panel) and Set 1 for the MIR region (right panel) of the spectrum of Sgr A* (E. L. Gibb et al. 2004). The photometric fluxes measured at continuum and absorptions are indicated with filled circles, and the corresponding continuum flux estimations are indicated with unfilled circles. The half-power passband wavelengths of the filters are also illustrated in the background using filled areas.
Paper: Photometric Mapping of Carbonaceous/Siliceous Dust and Water Ice in the ISM with JWST: Applications to the Dense Sightlines
Authors: Burcu Günay, Karl D. Gordon, Joshua E. G. Peek, Marjorie Decleir, Dries Van De Putte, Kirill Tchernyshyov, Michael G. Burton
Figure caption: The photometric optical depths compared with the spectroscopic optical depths. In this comparison, calibrated optical depths are represented by filled dots, while uncalibrated optical depths are shown with unfilled dots. The polynomial fits show the trend between τp and τs values, and the dotted line indicates equal τp and τs values.
Paper: Binary Analysis and Period Study of the Long-period, High-mass-ratio Contact Binary KIC 7766185
Authors: Conor M. Larsen, Andrej Prša
Figure caption: ETV curve for Kepler 7766185. The red and orange points are the Kepler and TESS ETVs determined through the phase method. The green points are the averages and standard deviations of the individual measurements over each TESS sector. The black curve is a third-body fit with an eccentricity of e3 ∼ 0.95 and a period of P3 ∼ 6000 days.
Paper: Binary Analysis and Period Study of the Long-period, High-mass-ratio Contact Binary KIC 7766185
Authors: Conor M. Larsen, Andrej Prša
Figure caption: (a) Luminosity vs. Mass for detached EBs, W UMa primaries and the primary of KIC 7766185. (b) Luminosity vs. Mass for detached EBs, W UMa secondaries and the secondary of KIC 7766185.
Paper: Binary Analysis and Period Study of the Long-period, High-mass-ratio Contact Binary KIC 7766185
Authors: Conor M. Larsen, Andrej Prša
Figure caption: (a) The mass vs. period relationship for both the primary and secondary stars. (b) The mass ratio vs. period relationship. (c) The radius vs. period relationship for both the primary and secondary stars. (d) The radius vs. mass relationship for both the primary and secondary stars.
Paper: easyspec: An Open-source Python Package for Long-slit Spectroscopy
Authors: Raniere de Menezes, Francesco Massaro, Michela Negro, Claudia M. Raiteri, Harold Peña-Herazo, Jose A. Acosta-Pulido
Figure caption: Raw spectrum of G4Jy 1709 for an exposure of 1800 s. The spectrum of our target is the dim horizontal line near the y-axis pixel 1000. In the edges of the image, we can see the dark patches in the light sensor where the light coming from the aperture does not arrive.
Paper: easyspec: An Open-source Python Package for Long-slit Spectroscopy
Authors: Raniere de Menezes, Francesco Massaro, Michela Negro, Claudia M. Raiteri, Harold Peña-Herazo, Jose A. Acosta-Pulido
Figure caption: Trimmed raw spectrum (top), median bias (middle), and normalized median flat-field (bottom) for our observations.
Paper: easyspec: An Open-source Python Package for Long-slit Spectroscopy
Authors: Raniere de Menezes, Francesco Massaro, Michela Negro, Claudia M. Raiteri, Harold Peña-Herazo, Jose A. Acosta-Pulido
Figure caption: Spectral trace found with easyspec (blue line). The orange band around the trace is the region at which the spectrum will be extracted with a Gaussian.
Paper: easyspec: An Open-source Python Package for Long-slit Spectroscopy
Authors: Raniere de Menezes, Francesco Massaro, Michela Negro, Claudia M. Raiteri, Harold Peña-Herazo, Jose A. Acosta-Pulido
Figure caption: Cosmic-ray corrected and stacked 2D spectrum for G4Jy 1709. We can see the stacked spectrum as the horizontal line just above the y-axis pixel 600. The vertical lines are all sky lines, produced by excited molecules in Earth’s atmosphere.
Paper: Binary Analysis and Period Study of the Long-period, High-mass-ratio Contact Binary KIC 7766185
Authors: Conor M. Larsen, Andrej Prša
Figure caption: Period histogram for the systems in the WUMaCat database. The red line denotes the period of KIC 7766185.
Paper: Investigating the Binary Source Degeneracy for Wide-orbit Planets
Authors: Parisa Sangtarash, Jennifer C. Yee
Figure caption: Scatter plots of simulated wide planetary microlensing parameters for different values of ρ, q, s, and u0 across varying trajectories of the source. Each panel (total of nine panels) corresponds to a specific trajectory(traj 1, traj 2, and traj 3) and ρ value (ρ = {0.01, 0.001, 0.0001}). The horizontal axis represents ﹩{{\rm{log}}}\,_{10}(q)+0.1s﹩ where ﹩{\rm{log}}\,q=\{-6,-5.5,-5,-4.5,-4\}﹩ and s = [1.5, 2, 2.5, 3, 3.5] while the vertical axis shows ﹩{{\rm{log}}}\,_{10}({\mathrm{Number\, of\, Data\, Points}})+0.37{u}_{0}﹩ where Npts = {1000, 2000, 5000, 20,000, 40,000, 80,000} and u0 = {0.3, 0.5, 0.7}. In each panel, there are 30 groups of points, with each group containing 15 points. These points correspond to combinations of three values of u0 and five values of s (3 × 5 = 15). The value of Δχ2 represents a measure of the deviation of the binary-source model from the wide-orbit planet model under our assumption of 1% photometric errors. The data behind this figure is available in machine readable format. The same data set can be used for Figure 7. These figures are generated using the input parameters (u0, q, s) from parameters.txt and the (fitted chi2s, Npts) from *k-points.txt by matching the files on the model identifier (k).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Investigating the Binary Source Degeneracy for Wide-orbit Planets
Authors: Parisa Sangtarash, Jennifer C. Yee
Figure caption: Light curves for the parameters t0 = 0, u0 = 0.5, s = 2.5, and ﹩{\rm{log}}\,(q)=-5﹩, calculated for three different values of ρ = 0.01, 0.001, and 0.0001, and for three different trajectories traj 1, traj 2, and traj 3 (3 × 3 = 9 cases in total). The top panel shows the full simulated light curves, but the magnification is displayed only up to 3. The bottom-left panel zooms in on all 9 planetary perturbations. The bottom-right panel focuses on the smallest bump. In these panels, the data points correspond to a case with 20,000 data points, and these points are overlaid on the different models. Additionally, the point-source point-lens model is represented by a dashed gray line. In these light curves, error bars and fitted binary-source models are not displayed.
Paper: Investigating the Binary Source Degeneracy for Wide-orbit Planets
Authors: Parisa Sangtarash, Jennifer C. Yee
Figure caption: Different trajectories of the source with respect to the planetary caustic for three distinct cases. traj1 represents the case where the source passes through the caustic. traj2 corresponds to the case where the source passes tangentially to the upper cusp of the caustic. traj3 depicts the case where the source passes outside but near the upper cusp of the caustic. The right panel is a zoomed-in view of the left panel around the planetary caustic region. In the bottom-left corner of this panel, the size of the source star is shown. In this configuration, the parameters are as follows: s = 2.5, ﹩{\rm{log}}\,(q)=-5﹩, u0 = 0.5, tE = 20, and ρ = 0.001.
Paper: Investigating the Binary Source Degeneracy for Wide-orbit Planets
Authors: Parisa Sangtarash, Jennifer C. Yee
Figure caption: Top: distributions of the logarithms of the source flux ratio for the best-fitting binary-source models. Bottom: logarithms of the source flux ratio compared to the best-fitting source size for the second source compared to the true value from the planetary model. Cases where the binary-source light curve model is degenerate with the planet at Δχ2 = 15, 50 are shown in red, gold. The left panels show the results for Npts = 2000 while the right panels show our fiducial case with Npts = 20,000. The figure can be reproduced with the contents of the data behind the figure file associated with Figure 3 by crossmatching 2k-points.txt and 20k-points.txt (rho2, flux ratio, Npts) to parameters.txt (rho_true) on the model identifier (k).
Paper: Investigating the Binary Source Degeneracy for Wide-orbit Planets
Authors: Parisa Sangtarash, Jennifer C. Yee
Figure caption: This figure is identical to Figure 3, except that here the photometric precision is set to 5% by dividing Δχ2 by 25. The figure can be reproduced with the contents of the data behind the figure file associated with Figure 3. These figures are generated using the input parameters (u0, q, s) from parameters.txt and the (fitted chi2s, Npts) from *k-points.txt by matching the files on the model identifier (k).
Paper: Investigating the Binary Source Degeneracy for Wide-orbit Planets
Authors: Parisa Sangtarash, Jennifer C. Yee
Figure caption: Examples of simulated light curves of wide-orbit planetary microlensing events (blue points; underlying model shown as the violet line) and the corresponding binary-source models fitted to them (red line). Each subpanel corresponds to a planetary event with s = 2.5 and u0 = 0.5, and the residuals between the simulated planetary model and the fitted binary-source model are shown below each light curve. The point-source point-lens model is shown with a gray dashed line. The left subpanels correspond to resolved degeneracies (Δχ2 > 50), while the right subpanels represent unresolved degeneracies (Δχ2 < 15). Additional details are given in the legends.
Paper: Investigating the Binary Source Degeneracy for Wide-orbit Planets
Authors: Parisa Sangtarash, Jennifer C. Yee
Figure caption: Radius of the secondary relative to the radius of the primary for binary sources with various flux ratios (see legend) in I (left) and H bands (M. J. Pecaut & E. E. Mamajek 2013).
Paper: The HUSTLE Program: The UV to Near-IR Transmission Spectrum of the Hot Jupiter KELT-7b
Authors: C. Gascón, M. López-Morales, R. J. MacDonald, J. K. Barstow, V. A. Boehm, H. R. Wakeford, M. K. Alam, L. Alderson, N. E. Batalha, C. E. Fairman, D. Grant, N. K. Lewis, M. S. Marley, S. E. Moran, K. Ohno, G. Anglada-Escudé, I. Ribas
Figure caption: Top: HST WFC3/UVIS G280 exposure showing the order zero image, and the spectra corresponding to positive and negative orders. Two background stars are highlighted by purple circles. The dashed rectangles in the image corners indicate the region used to estimate background on each image. Middle: raw +1 (left) and −1 (right) order white-light curve obtained with lluvia. Bottom: systematics corrected +1 (left) and −1 (right) order white-light curve. The narrow panel below shows the transit fit residuals, with the dashed lines indicating the corresponding standard deviation of the residuals.
Paper: The HUSTLE Program: The UV to Near-IR Transmission Spectrum of the Hot Jupiter KELT-7b
Authors: C. Gascón, M. López-Morales, R. J. MacDonald, J. K. Barstow, V. A. Boehm, H. R. Wakeford, M. K. Alam, L. Alderson, N. E. Batalha, C. E. Fairman, D. Grant, N. K. Lewis, M. S. Marley, S. E. Moran, K. Ohno, G. Anglada-Escudé, I. Ribas
Figure caption: Results from the KELT-7b light-curve fitting. Top: +1 (blue) and −1 (red) order transmission spectra obtained with the lluvia pipeline (left), and the Hazelnut pipeline (right). Bottom: combined transmission spectrum obtained with lluvia (purple), and the Hazelnut (gray). The narrow panels below each plot show the differences between the corresponding transmission spectra in units of σ, with the dashed lines and the shaded regions indicating the corresponding ±1σ and ±3σ limits.
Paper: The HUSTLE Program: The UV to Near-IR Transmission Spectrum of the Hot Jupiter KELT-7b
Authors: C. Gascón, M. López-Morales, R. J. MacDonald, J. K. Barstow, V. A. Boehm, H. R. Wakeford, M. K. Alam, L. Alderson, N. E. Batalha, C. E. Fairman, D. Grant, N. K. Lewis, M. S. Marley, S. E. Moran, K. Ohno, G. Anglada-Escudé, I. Ribas
Figure caption: Displacements in the X (left) and Y (right) detector directions, measured by cross correlation of the spectral trace (red triangles and purple circles) and by tracking the centroid position of several background stars (blue squares).
Paper: The HUSTLE Program: The UV to Near-IR Transmission Spectrum of the Hot Jupiter KELT-7b
Authors: C. Gascón, M. López-Morales, R. J. MacDonald, J. K. Barstow, V. A. Boehm, H. R. Wakeford, M. K. Alam, L. Alderson, N. E. Batalha, C. E. Fairman, D. Grant, N. K. Lewis, M. S. Marley, S. E. Moran, K. Ohno, G. Anglada-Escudé, I. Ribas
Figure caption: Atmospheric retrievals of KELT-7b’s transmission spectrum conducted with POSEIDON (left panel, purple) and NEMESIS (right panel, blue). Each panel shows the median retrieved spectrum (solid lines), together with the 1σ (dark shading) and 2σ (light shading) regions.
Paper: Detecting Asteroids in TESS Full-frame Images Using a Gradient-based Iterative Algorithm
Authors: Peilin Zhang, Rui Luo, Man Chen
Figure caption: Two examples of velocity hypothesis diagrams and the corresponding stacked images with and without bright asteroid reduction. Upper-left subplot: the velocity hypothesis diagram of the unprocessed image stack. Upper-right subplot: the velocity hypothesis diagram with bright asteroid signal reduction. Lower-left subplot: the shift-stacking image with the velocity of vx = 43﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 hr−1 and vy = −11﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 hr−1 (according to the peak in the upper-left velocity hypothesis diagram). Lower-right subplot: shift-stacking image with the velocities of vx = 34﹩\mathop{.}\limits^{\unicode{x02033}}﹩9 hr−1 and vy = 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩8 hr−1 (according to the newly emerged peak in the upper-right velocity hypothesis diagram).
Paper: Detecting Asteroids in TESS Full-frame Images Using a Gradient-based Iterative Algorithm
Authors: Peilin Zhang, Rui Luo, Man Chen
Figure caption: Velocity hypothesis diagram (left panel) and shift-stacking images of corresponding velocities (right panel). The axes of the velocity hypothesis diagram represent velocities in x (along the ecliptic plane) and y (along the normal of the ecliptic plane) direction, respectively. The color in this diagram denotes the maximum pixel value in the stacked image. The subplot (a) and (b) in the right panel represent shift-stacking image using corresponding velocity hypotheses marked with two asterisks in the left panel. In the subplot (a), the asteroid with well-matched velocity hypotheses appears as a point-like signal. In the subplot (b), the asteroid signal is prolonged as a streak when velocity hypotheses are slightly mismatched.
Paper: Detecting Asteroids in TESS Full-frame Images Using a Gradient-based Iterative Algorithm
Authors: Peilin Zhang, Rui Luo, Man Chen
Figure caption: An example of pixel value time series around a star in the original TESS FFIs and the processed images. The upper-left panel shows a star in the raw TESS FFI, and the lower-left panel shows the same region in the DVA removed image. In the right panels, the red and blue curves corresponds to the pixels marked by the red and blue crosses, respectively, in the left panels. The spike in the blue curves indicates an asteroid passing over this pixel. Note that the maximum pixel value in the upper-left image is 49,613 electrons per second, and the maximum pixel value in the lower-left image is 80 electrons per second.
Paper: Detecting Asteroids in TESS Full-frame Images Using a Gradient-based Iterative Algorithm
Authors: Peilin Zhang, Rui Luo, Man Chen
Figure caption: A demonstration of the flat-field correction and destrapping. The left panel is the image cropped from a TESS FFI. The scattered light brightens the lower-right part of the image. The middle panel is the flat-field corrected image. The right panel is the image after destrapping.
Paper: Detecting Asteroids in TESS Full-frame Images Using a Gradient-based Iterative Algorithm
Authors: Peilin Zhang, Rui Luo, Man Chen
Figure caption: Left panel: the precision (the blue line) against threshold and the numbers (the red line) of detections above the threshold. Right panel: the completeness (the blue line) of three different thresholds and numbers (the red line) of known asteroids in visual magnitude bins. The points of magnitude of 16 include all asteroids brighter or equal to magnitude of 16 in this data.
Paper: Detecting Asteroids in TESS Full-frame Images Using a Gradient-based Iterative Algorithm
Authors: Peilin Zhang, Rui Luo, Man Chen
Figure caption: Velocity hypothesis diagrams (the first row) and accordingly shift-stacked images (the second row) of three detections that the iterative algorithm returned but failed to pass the filtering process. Note that the velocities used to shift-stack the images correspond to central points of the velocity hypothesis diagrams.
Paper: Detecting Asteroids in TESS Full-frame Images Using a Gradient-based Iterative Algorithm
Authors: Peilin Zhang, Rui Luo, Man Chen
Figure caption: Velocity hypothesis diagrams and shift-stacked images of three known asteroids that our pipeline detected. Note that the velocity hypothesis diagram for 2020 BM63 shows a fuzzy pattern. This is due to an nearby asteroid, which is fainter than 2020 BM63, according to the Horizons ephemeris data.
Paper: Delayed and Displaced: The Impact of Binary Interactions on Core-collapse SN Feedback
Authors: Tom Wagg, Julianne J. Dalcanton, Mathieu Renzo, Katelyn Breivik, Matthew E. Orr, Adrian M. Price-Whelan, Akaxia Cruz, Alyson Brooks, Ulrich P. Steinwandel, Eric C. Bellm
Figure caption: The type of mass transfer that a primary star first initiates prior to its core collapse is a function of its initial mass. The transition at ∼10 M⊙ leads to the knee in the distribution in the top-left panel of Figure 1. Mass transfer initiated on the donor star’s main-sequence is case A, while case B corresponds to expansion during the Hertzsprung gap, and case C occurs after the onset of core helium burning. Primary stars below ∼10 M⊙ mostly initiate case C mass transfer, while more-massive stars initiate case A or B mass transfer. The top axis shows the main-sequence lifetime corresponding to the initial primary mass for the average metallicity of m11h as calculated by COSMIC.
Paper: A Massive Yellow Supergiant in the Far Outer Disk of M31: Evidence for in Situ Massive Star Formation beyond the Optical Radius
Authors: Pinjian Chen, Bingqiu Chen, Haibo Yuan, Xuan Fang, Xiaodian Chen, Chao-Wei Tsai, Kai Zhang, Xiaowei Liu
Figure caption: Normalized spectra of J0048+4154 compared to template supergiants. (a) Blue spectra showing J0048+4154 (top three) alongside two UVES-POP spectra of Galactic F-type supergiants. Key absorption features are labeled, and radial velocity corrections have been applied. (b) Same as (a), but for the red spectra. Telluric features, which remain uncorrected in both the DBSP and UVES-POP spectra, are indicated by gray shading. (c) Comparison of the normalized DBSP spectrum of J0048+4154 (black) with a velocity-shifted template spectrum of HD 74180 (red). (d) Zoom-in on the Hα region for J0048+4154. The color scheme matches panel (a), and no velocity corrections were applied.
Paper: A Massive Yellow Supergiant in the Far Outer Disk of M31: Evidence for in Situ Massive Star Formation beyond the Optical Radius
Authors: Pinjian Chen, Bingqiu Chen, Haibo Yuan, Xuan Fang, Xiaodian Chen, Chao-Wei Tsai, Kai Zhang, Xiaowei Liu
Figure caption: Location of J0048+4154 in M31. (a) Herschel SPIRE 250 μm image displayed on a logarithmic scale. Green triangles mark supergiant candidates identified from LAMOST, selected based on the sample of P. Chen et al. (2025) with PM31 > 0.8 and PMW < 0.1, where PM31 and PMW refer to the probability that the star belongs to M31 and the Milky Way, respectively. Blue circles indicate spectroscopically confirmed massive stars compiled from the literature (G. Maravelias et al. 2022). The dotted–dashed ellipses correspond to galactocentric radii of RGC = R25 and 1.5R25. The black cross denotes a physical scale of 5 kpc in both the x- and y-directions. (b) Same image as (a), but with the y-axis deprojected assuming a fixed inclination angle of 77﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Non-LTE abundance corrections (in dex) for various atomic species in the five program stars. The vertical axis lists the elements and their ionization states, and the horizontal axis shows the stellar identifiers. The color indicates the magnitude of the non-LTE correction, which is defined as the abundance difference between the non-LTE and LTE calculations for each element. Corrections were computed using the available literature grids. Positive values indicate an increase in the inferred abundance when non-LTE effects are considered.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Corner plot displaying the posterior probability distributions for HD 122956 and HD 189349, with confidence levels marked at 68%, 90%, and 95%. The 1D marginal distributions indicate the median values, along with the 16th and 84th percentiles. The right side of each panel shows the corresponding positions of the stars on the Kiel diagram. Corner plots for the remaining three stars (HD 2665, HD 5916, and HD 218857) are provided in Appendix Figure A2.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: An example for the determination of atmospheric parameters Teff and ξ using abundance (﹩{\mathrm{log}}\,\epsilon ﹩) as a function of both LEP (panels (a) and (b)) and reduced EW (REW; log (EW/λ), panel (c)) for HD 189349 and HD 122956. The solid line in each panel is the least-squares fit to the data.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: A small region of the spectrum for five HPM sample stars. Identified lines are also indicated.