adsabs/AstroCLIMB huggingface dataset:
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Interdependence of Paloma’s spin and orbital profiles across the beat cycle (relative to T 0, beat[BJD] = 2,458,836.1495). Panels (a)–(c) share the same x-axis (spin phase relative to T 0, spin[BJD] = 2,458,836.9065), while panels (d) and (e) show the orbital phase on a common x-axis. Panels (a) and (d) present six-harmonic Fourier-series representations of the average spin and orbital profiles across the entire TESS observation. Horizontal slices through panels (b) and (c) yield the spin profile that would be observed if the beat and orbital phases, respectively, could be held constant, and panel (c) shows that the secondary spin maximum disappears at inferior conjunction. Similarly, panel (e) shows the evolution of the orbital profile across the beat cycle. Panel (c) establishes that the spin profile changes significantly near inferior conjunction.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Top panel: representative ∼4-day segment of the K2 light curve of J0846. Each datum is a 30-minute integration, and consecutive measurements have been joined with dotted line segments to guide the eye. Flux uncertainties are negligibly small at this scale. BKJD is defined as JD −2,454,833. Middle and bottom panels: Lomb–Scargle power spectrum of the K2 light curve of J0846, split into two panels to improve the visibility of major frequencies. ω is the WD’s spin frequency and Ω is the binary orbital frequency.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Average of three SDSS spectra of J0846, including one obtained during the K2 observation, showing very strong He II λ4686 emission and single-peaked emission lines. Both are commonly observed features in spectra of polars. Overall, this spectrum is similar to the one reported in Szkody et al. (2006), except that He I emission is more pronounced here. The absorption feature near 5200 Å is attributable to MgH from the secondary. As discussed in Section 3.5, we estimate the secondary’s spectral type to be between K5 and M0, with K7 being the most likely classification.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Light curve and 2D power spectra for J0846. BKJD is defined as BJD –2,454,833. The middle and bottom panels use different color maps to reflect that they have different intensity cuts. The size of the sliding window is 0.5 days.
Paper: Searching for Barium Stars from the LAMOST Spectra Using the Machine-learning Method: I
Authors: Fengyue Guo, Zhongding Cheng, Xiaoming Kong, Yatao Zhang, Yude Bu, Zhenping Yi, Bing Du, Jingchang Pan
Figure caption: Comparisons of the Ba abundances calculated by our work ([Ba/Fe]LGBM) and values determined from N19 ([Ba/Fe]N19). The yellow line signifies that the predicted value is equal to the target value. The yellow dot represents the point at which ∣[Ba/Fe]4554 Å − [Ba/Fe]4934 Å∣ ≥ 0.5 in N19. The left shows the differences between [Ba/Fe]LGBM and [Ba/Fe]N19 in the prediction of 4554 Å (Ba II), and the right shows these differences in the prediction of 4934 Å (Ba II).
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Top: the TESS light curve of Paloma. BTJD is defined as BJD –2,457,000. Middle: 2D power spectrum with a 0.25-day sliding window, with linear intensity scaling. Across the 0.7-day beat cycle, the light curve alternates between a single- and double-humped profile, causing power to shift cyclically between ω and 2ω. Bottom: 2D power spectrum with a 2-day sliding window and logarithmic scaling. The larger window size offers improved frequency resolution at the expense of completely concealing the changes evident in the middle panel.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Lomb–Scargle power spectrum of the TESS light curve of Paloma, with the two sets of frequency identifications proposed by Schwarz et al. (2007). The usage of “Case A” and “Case B” matches that of Schwarz et al. (2007). For the Case A identifications, there would be no appreciable signal at either ω or ω − Ω. For reasons discussed in the text, we prefer the “Case B” identifications.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: 2D light curves of J0846 phased to the sideband, spin, and orbital periods. Phase 0.0 is arbitrary in all panels.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Top: continuum-subtracted, 2D spectra of He II λ4686 and Hβ. There is no evidence of an eclipse at inferior conjunction. The two panels use different intensity cuts. Bottom: Radial-velocity curve of the Ca II triplet, showing a semiamplitude of 220 km s−1 with a systemic velocity of 60 km s−1. The blue-to-red crossing establishes the epoch of inferior conjunction. The Ca II line fluxes near the time of inferior conjunction have been excluded because they are very low. This suggests that the secondary’s inner hemisphere is occluded by the rest of the star near inferior conjunction, consistent with a moderate-to-high orbital inclination.
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Diagnostic plots for membership determination. Red circles indicate clear Ret II members, orange squares are candidate Ret II members (with star ID labeled), cyan crosses are nonmember stars with radial velocities similar to Ret II, small blue dots indicate spectroscopic targets with velocities far from Ret II, and small gray points indicate DES stars within five elliptical half-light radii. Top left: color–magnitude diagram with dereddened DES photometry. The solid magenta line is a Dartmouth 13 Gyr, [Fe/H] = −2.5 isochrone. The dashed magenta lines are more metal-rich 13 Gyr isochrones with metallicities [Fe/H] = −2.0 and −1.5. The dashed blue line is a 10 Gyr isochrone with [Fe/H] = −2.5 to show where potential younger member stars or blue stragglers could lie. The dotted black lines show the region for membership, though individual stars outside this range were also considered. Top right: spatial position of stars around the Ret II center, only including stars within five elliptical half-light radii. The dotted black line shows two half-light radii, which is used as the main membership cut, although stars at larger radii were also considered. Bottom left: radial velocity of spectroscopically observed stars vs. elliptical half-light radius. Binaries are indicated as open circles, with the error bar spanning the range of observed velocities. There is no significant radial velocity gradient. The dotted black lines show the range of velocities allowed for membership. Bottom right: Gaia EDR3 proper motions. All our spectroscopic targets are bright enough to have EDR3 proper motions. Stars 14, 16, 97, 142, and 154 are located at the center and thus not labeled. Note that the bulk of field stars are beyond the plot limits. The dashed black lines indicate the mean Ret II proper motion.
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: [Ba/H] and [Ba/Fe] vs. [Fe/H] as measured by VLT/GIRAFFE. Red points indicate clear Ret II members and orange points indicate candidate Ret II members. Large symbols are stars with S/N > 25, while small symbols are stars with S/N < 25. 1σ error bars are shown for all detected abundances, with arrows drawn to indicate upper/lower limits. Open circles indicate stars with at least one upper limit, and stars are colored gray if they have no detection of either Ba or Fe. Considering only the clear members with high S/N (large red points), there is no apparent scatter in Ba but significant spread in Fe.
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: VLT spectra with best-fit models of the Ba line. From low to high wavelength the primary absorption features are due to Ca, Fe, and Ba. The Ba abundance measurement or limit is indicated. Stars are sorted by S/N, membership, and effective temperature. Top section: stars with S/N > 25. Bottom section: stars with S/N < 25. The sky residuals are clearly substantial for the lower S/N stars. The black line shows the data, while the gray shaded region indicates the 1σ spectrum noise. Best-fit models are shown in red and orange for clear and candidate members, respectively. The solid colored lines are the model including the sky line, while the dashed colored lines are the model fit in the absence of the fitted sky line residual. In some cases (e.g., stars 020, 134, 157) the Ba line is completely degenerate with the sky emission line, so no useful constraint is obtained. The shaded colored regions indicate the 16–84th percentile range of model parameters. Note that we have not explicitly plotted the upper limit model.
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Barium measurements/upper limits and best-fit models for stars with S/N > 25. The left panel shows our fiducial result only including clear members (16 stars), while the right panel also includes candidate members (three more stars). Detections are shown as points with 1σ error bars, stacked within bins of 0.5 dex like a histogram. Stars with larger uncertainties are placed toward the bottom of each bin. Upper limits are shown as leftward-pointing arrows. Red and orange symbols indicate definite and candidate members, respectively. The shaded regions show the best-fit two-Gaussian model normalized to the number of stars on each panel. The width of both distributions (σ Ba) is unresolved, so we plot the width using the 95% upper limit. Note that the model including candidates is wider primarily to accommodate Star 14.
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption:  α-element abundances in Ret II. Symbols are the same as those in Figure 5, with large red solid points indicating abundances of confident members, large orange points indicating abundances of candidate members, open red points indicating stars with one upper limit, and open gray points indicating stars with two upper limits. Note that two stars have Mg and Ca measurements but only Fe upper limits. Left: [Mg/Fe] vs. [Fe/H]. Middle: [Ca/Fe] vs. [Fe/H]. Right: [Mg/Ca] vs. [Fe/H].
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Individual radial velocity measurements for all stars from this study and the literature. No systematic velocity corrections have been applied in this figure. The left panel shows red giant branch stars previously marked as confirmed or candidate members, while the right panel shows other stars. Along the bottom axis, red bars indicate stars that are certain members, while orange lines indicate candidate members. Along the top axis, gray lines indicate binary stars.
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Histogram of measured velocities (blue), with definite (candidate) Ret II members in red (orange). For comparison, velocities from the Besançon model are shown as a gray histogram, normalized to match the observed sky area of 490 sq arcmin. The solid (dotted) purple histograms indicate subtracting the definite, red (candidate, orange) members from the full blue histogram. The nonmembers are overall consistent with the Besançon background model, though there is still a small excess above background near the velocity of Ret II.
Paper: Astrophysical Properties of 600 Bona Fide Single Stars in the Hyades Open Cluster
Authors: Wolfgang Brandner, Per Calissendorff, Taisiya Kopytova
Figure caption: Color–color–magnitude diagram of the Hyades open cluster based on Gaia DR3 photometry. Bluish-purple cross symbols mark sources with valid photometry in all three Gaia photometric bands. The circles mark stars with potentially unreliable photometry in at least one of the photometric bands as identified by sigma clipping.
Paper: Astrophysical Properties of 600 Bona Fide Single Stars in the Hyades Open Cluster
Authors: Wolfgang Brandner, Per Calissendorff, Taisiya Kopytova
Figure caption: Minimum distance in color–magnitude space of each single star from the best-fitting isochrone, plotted against the absolute magnitude (lower abscissa) and color (upper abscissa) on the isochrone. A positive residual corresponds to stars that are brighter (redder) than predicted by the isochrone. A negative residual corresponds to stars that are fainter (bluer) than the isochrone. The uncertainties for each source in Gabs correspond to the Gaia uncertainties in absolute G magnitude, and the uncertainties in the residuals correspond to the quadratically added uncertainties in absolute G magnitude and BP-RP color.
Paper: Astrophysical Properties of 600 Bona Fide Single Stars in the Hyades Open Cluster
Authors: Wolfgang Brandner, Per Calissendorff, Taisiya Kopytova
Figure caption: Color-absolute–magnitude diagram of ≈600 bona fide single-star candidate members of the Hyades open cluster based on Gaia DR3. Overall, the family of PARSEC isochrones for [M/H] = +0.18 ± 0.03, age = 775 ± 20 Myr, and A V = 3.1 mmag provides a very good fit to the observed main sequence. In the color range 2.4 mag ≤ BP-RP ≤3.2 mag (≈0.22 to 0.40 M ⊙), stars are systematically brighter (respectively redder) than predicted by the isochrones.
Paper: Astrophysical Properties of 600 Bona Fide Single Stars in the Hyades Open Cluster
Authors: Wolfgang Brandner, Per Calissendorff, Taisiya Kopytova
Figure caption: Color-absolute–magnitude diagram of candidate members of the Hyades open cluster based on GAIA DR3, showing the results of our classification into bona fide single main-sequence stars (and white dwarfs), likely binary and multiple systems, and stars with problematic photometry in at least one of the Gaia bands.
Paper: Astrophysical Properties of 600 Bona Fide Single Stars in the Hyades Open Cluster
Authors: Wolfgang Brandner, Per Calissendorff, Taisiya Kopytova
Figure caption: RUWE as a function of G. The dashed line marks the canonical border line between likely binary and multiple systems with RUWE >1.4 and bona fide single stars. For comparison the dotted blue line marks the sliding window median and dashed–dotted red lines marks the 1.2 times sliding window median RUWE values.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: The left two columns show the radial velocity (black dashed lines L  Z  = 1750, 2160, 2600 kpc km s−1) and vertical velocity (L  Z  is 2160 kpc km s−1) difference distributions of the north minus south sides. There are still three ridges in the same location as Figure 3. The amplitude of the south and north ridges is different, which is showing the clear asymmetries, especially for the vertical nonnull values. The right two columns show the velocity differences at different age populations for velocity (L  Z  is 2220 kpc km s−1 for V  R  , 1900, 2160, and 2450 kpc km s−1 for V  Z ), which are showing there are remaining one and three time-evolving ridges, respectively.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: The left column shows the star counts distribution in log scale, the middle column shows the radial velocity V  R  distribution, and the right column shows the vertical velocity V  Z  distribution in different age populations. The black dashed lines in the radial velocity diagram represent the constant angular momentum L  Z  = (1570, 1750, 2160, 2320, 2600) kpc km s−1.The black dashed lines in the right vertical velocity diagram represent the constant angular momentum L  Z  = (2320, 2600, 2920) kpc km s−1.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: The radial velocity distribution of RGB stars used in this paper are shown in the L  Z  and V  ϕ  plane. The five vertical fuchsia lines in the figure represent constant angular momentum L  Z  = (1570, 1750, 2160, 2320, 2600) kpc km s−1. We can see that the third ridge (R3 in the context) changes with age or has an offset, and others are relatively stable in the left column. The middle and right columns show the distribution of sample on the north and south sides, which are similar to the left one, but the north–south differences are detected.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: Similar to Figure 5 it shows the chemical difference in the north and south sides (left two columns), and meanwhile, the difference at different age populations (right two columns). Three ridges signals are detected in the [Fe/H] and [α/Fe] in the left two columns. Three ridges signals are detected in the right two columns, as shown the dashed lines, which are slightly different from the velocity analysis. It is also clearly shown that north–south has chemical difference for ridges.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: The left and middle columns show the metallicity and chemical abundance distribution corresponding to the vertical height of [−1.5, 1.5]  kpc respectively. The right one shows the vertical velocity distribution but with vertical height of [−0.2, 0.2]  kpc. Obviously the ridge signals are detected in all three panels, although it is not as clear as the kinematic space, the number of ridge here is also less than that in the kinematic space.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: Three-dimensional velocity distributions of the final sample in the R–Z plane, the top three are V  R , V  ϕ  and V  Z  velocity and the error is determined by bootstrap method in the bottom three. R and Z are limited to [8,15]  kpc and [−1.5,1.5]  kpc, respectively.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: The left two columns show the radial velocity distribution on the north and south sides of the Galactic disk, and the right two columns show the vertical velocity features. The north and south sides of the Galactic disk have obvious ridge pattern and there are clear asymmetries indicated by the different color distributions.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: Distribution of 3D angular momentum component in the R–V  ϕ  plane: angular momentum in the x direction (left), y direction (middle), and z direction (right). The only one dashed line represents the constant angular momentum curve implying there might be a ridge corresponding to the previous R6 = 2920 kpc km s−1.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: Similar to Figure 8 for the chemical analysis but the sample is divided into north and south sides.