adsabs/AstroCLIMB huggingface dataset:
Paper: Mass Ratio Estimates for Overcontact Binaries Using the Derivatives of Light Curves
Authors: Shinjirou Kouzuma
Figure caption: View of a binary from an observer at ﹩t={t}_{32}^{{\prime} }=0.45﹩ day. The parameters of the binary are the same as those shown in Figure 1.
Paper: Mass Ratio Estimates for Overcontact Binaries Using the Derivatives of Light Curves
Authors: Shinjirou Kouzuma
Figure caption: Comparison between our photometric and the literature’s spectroscopic mass ratios. The red solid and broken lines show q ph = q sp and q ph = q sp ± 0.1, respectively.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Updated action plot as shown in Figure 1 and described in Section 1.2 with the Pleiades (pink), Pisces–Eridanus (orange), Praesepe (blue), Hyades (green), and Ruprecht 147 (red) overplotted. Vertical and horizontal slices chosen for P rot study are noted in black. As the clusters increase in age, so do their radial actions, motivating our choice for studying P rot and finding young stars at high J  R .
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Examples of quality flag designations. Light curves are on the left, the corresponding periodogram in the middle, and phase-folded light curves on the right. The position of the detected period is indicated by the orange line. First row: Q = 0. There is a clear 9 day periodic modulation in the light curve and a strong, sharp peak in the periodogram (literature P rot: 8.7 days). Second row: Q = 1. There is evidence of modulation measured at 8.3 days in the light curve, but it is weak due to instrument systematics and the data gap (literature P rot: 7.3 days). Third row: Q = 2. The light curve shows evidence for a long-term periodic trend likely due to systematics, which the periodogram chooses as the period instead of the masked and potentially astrophysically real period at 0.16 days (literature P rot: 0.32 days). Fourth row: Q = 3. Systematics completely dominate the light-curve structure, and no astrophysical periodicity appears to be present (literature P rot: 0.43 days).
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Example of the measurement and confirmation process for a star observed in sectors 42 (top row), 43 (middle row), and 44 (bottom row) that is detected in Pipelines I, II, and III. First column: star’s light curve for the sector. Second column: GLS periodogram with measured P rot associated with highest peak indicated in yellow, median power indicated in green, and calculated S/N of the highest peak. The S/Ns of the three sectors (21, 52, and 61) span our detection threshold of 40. Third column: phase-folded light curve with measured P rot. Fourth column: periodogram in frequency space with the primary peak fitted for width measurement (in black). This star has a strong S/N and small peak width in two of three sectors, which means its P rot is a Pipeline I detection that is automatically confirmed as part of Pipeline II and considered a Pipeline II/III detection.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: The figure shows L  z  vs. ﹩\sqrt{{J}_{R}}﹩ using updated kinematics from Gaia DR3, GALAH DR3, and APOGEE DR16. A larger L  z  is associated with a larger orbital size in the solar neighborhood, and a larger J  R  is associated with a more eccentric orbit.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Flowchart of the P rot pipelines. Starting with a star’s light curve(s), we check whether it is a candidate binary using ancillary data and discard if so. Next, we check for periodicity in the periodograms and identify stars with strong periodicity (Pipeline I detections). A Pipeline II detection is one in which a star has multiple sectors that have Pipeline I detections, where the same P rot is measured. A Pipeline III detection includes Pipeline II detections plus any additional Pipeline I detections that pass a by-eye inspection.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Literature P rot distributions for Pipeline III detections for Pleiades (pink), Pisces–Eridanus (orange), Praesepe (blue), Hyades (green), and MEarth (purple). The recovered P rot is noted by a dashed black line, and gray shaded regions indicate what we expect to detect with TESS (≤13 days).
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Literature vs. TESS P rot for Pipeline III for Pleiades (pink), Pisces–Eridanus (orange), Praesepe (blue), Hyades (green), and MEarth (purple). Pipeline III detections considered recovered are noted with black circles, and the detection limit is noted at 13 days with a vertical dashed line.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: TESS magnitude distributions for Pipeline III detections for Pleiades (pink), Pisces–Eridanus (orange), Praesepe (blue), Hyades (green), and MEarth (purple). Recovered stars are noted by a dashed black line, and gray shaded regions indicate what we expect to detect with TESS-SPOC (≤13.5 mag).
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Color–P rot distribution of likely single rotators for horizontal (filled stars) and vertical (open stars) sections of action space with benchmark clusters plotted for reference (120 Myr old Pleiades in pink, 670 Myr old Praesepe in blue, 1 Gyr old NGC 6811 in yellow, and 2.7 Gyr old Ruprecht 147 in red). The most robust region for gyrochronology (G dwarfs with reliable P rot measurements) is highlighted by the white region.
Paper: Relation between Latitude-dependent Sunspot Data and Near-Earth Solar Wind Speed
Authors: Qirong Jiao, Wenlong Liu, Dianjun Zhang, Jinbin Cao
Figure caption: Observation data of sunspot and solar wind speed from 1963 to 2018. (a) The daily latitude-dependent sunspot number. (b) The fitting result of daily sunspot number. (c) The daily solar wind speed. (d) Histogram of the annual average solar wind speed, and the solar cycle declining phase is represented in green.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Distribution of recovered sample stars from benchmark populations as a function of S/N (top left), input P rot (top right), magnitude (bottom left), and amplitude (bottom right) in red. The distribution of stars not recovered in S/N are shown with the blue dashed line. The distribution of the entire sample of stars used are shown with the black dashed line in input prot, magntidue, and amplitude.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Left: rotator distribution in the vertical slice of action space with benchmark clusters overplotted as shown in Figure 2. Bins from the right panel are indicated by dashed horizontal lines in the inset. Right: fraction of rotators vs. all stars found in bins of the square root of radial action.
Paper: Relation between Latitude-dependent Sunspot Data and Near-Earth Solar Wind Speed
Authors: Qirong Jiao, Wenlong Liu, Dianjun Zhang, Jinbin Cao
Figure caption: Results of Granger causality analysis of latitude-dependent sunspot data and annual average solar wind speed. The red dashed line indicates the confidence level p-value equal to 0.05.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Distribution of recovered stars with an injected P rot as a function of S/N (top left), input P rot (top right), magnitude (bottom left), and amplitude (bottom right) in red. The distribution of stars not recovered in S/N are shown with the blue dashed line. The distribution of the entire sample of stars used in the injection analysis are shown with the black dashed line in input prot, magntidue, and amplitude.
Paper: Wrinkles in Time. I. Rapid Rotators Found in High-eccentricity Orbits
Authors: Rayna Rampalli, Amy Smock, Elisabeth R. Newton, Kathryne J. Daniel, Jason L. Curtis
Figure caption: Left: rotator distribution in the horizontal slice of action space with benchmark clusters overplotted as shown in Figure 2. Bins from the right panel are indicated by dashed vertical lines in the inset. Right: fraction of rotators vs. all stars found in bins of angular momentum in the z-direction.
Paper: Relation between Latitude-dependent Sunspot Data and Near-Earth Solar Wind Speed
Authors: Qirong Jiao, Wenlong Liu, Dianjun Zhang, Jinbin Cao
Figure caption: Plot of the measured and predicted daily mean solar wind speed. The black line indicates the solar wind observation data; the blue line indicates the prediction result of solar wind speed as input; the red line indicates the result of adding sunspot data with latitudes less than 7.°2.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Bar properties and gas inflows in the S2BISO (left) and S2BSMU (right) models. First row: outer and inner bar amplitudes. The Fourier components A 2 and A 0 are measured in the radial range of 2.4–7.5 kpc for the outer bar and 0–0.75 kpc for the inner bar. Second row: enclosed mass of gas (S2BISO) and gas plus newly formed stars (S2BSMU) inside R inner and R outer. Third row: mass inflow rate obtained from the time derivative of the lines in the second row. Vertical gray solid and dashed lines indicate the moments when the two bars are aligned and perpendicular, respectively. Fourth row: enclosed SFR in S2BSMU. This quantity is calculated based on the total mass of new stars inside the given radius that are formed in the past 10 Myr.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Comparison of the inner gas surface density between S2BISO (top) and S2BSMU (bottom). The columns represent four different epochs when the two bars have different angles with respect to each other (indicated by the red and blue sticks in the bottom right corner of each panel in the top row). The snapshots are taken at t = 1.271, 1.287, 1.310, and 1.334 Gyr for S2BISO and t = 1.256, 1.272, 1.295, and 1.317 Gyr for S2BSMU. The dashed and dotted–dashed circles denote two characteristic cylindrical radii of R outer = 3.75 and R inner = 0.75 kpc. The gas disk rotates counterclockwise.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Initial gas surface density profiles used in our models. The solid curve shows the HOLE profile, with the two arrows denoting the inner and outer boundaries at R 1 = 3.75 and R 2 = 10.0 kpc; the dashed line shows the EXP profile with a central density Σ0 = 25 M ⊙ pc−2 and scale radius R  d  = 5 kpc.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Evolution of model S2BISO. Top: stellar surface density. Bottom: gas surface density. White lines represent the contours of the stellar surface density placed at 0.16, 0.54, 1.85, and 6.31 × 103 M ⊙ pc−2. The two stellar bars are clearly outlined by the contours. The first two columns show the early evolution when the two bars are misaligned, while they are parallel in the third column and perpendicular in the fourth column. The evolution time is given at the top. The disk rotates counterclockwise.
Paper: Relation between Latitude-dependent Sunspot Data and Near-Earth Solar Wind Speed
Authors: Qirong Jiao, Wenlong Liu, Dianjun Zhang, Jinbin Cao
Figure caption: Plot of daily solar wind speed prediction results. The blue point indicates the prediction result of solar wind speed as input; the red line indicates the result of including sunspot data with latitudes less than 7.°2.
Paper: Relation between Latitude-dependent Sunspot Data and Near-Earth Solar Wind Speed
Authors: Qirong Jiao, Wenlong Liu, Dianjun Zhang, Jinbin Cao
Figure caption: Plot of the measured and predicted 30 day average solar wind speeds. The black line indicates the solar wind observation data; the blue line indicates the prediction result of solar wind speed as input; the red line indicates the result of adding sunspot data with latitudes less than 7.°2.
Paper: Relation between Latitude-dependent Sunspot Data and Near-Earth Solar Wind Speed
Authors: Qirong Jiao, Wenlong Liu, Dianjun Zhang, Jinbin Cao
Figure caption: Plot of annual average solar wind speed and sunspot number linear correlation coefficients with time delay.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Similar to Figure 2 but for S2BSMU.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Comparison between an observed S2B galaxy, NGC 1433, and our S2BSMU model. We adopt a distance of 18.63 Mpc, a systemic velocity of 1057.4 km s−1, a disk position angle of 199.°7, and an inclination angle of 28.°6 for this galaxy (Buta et al. 2001; Lang et al. 2020). Top row, left to right: S4G 3.6 μm image (unit: L ⊙ pc−2), PHANGS-ALMA CO(2–1) integrated intensity map (moment 0; unit: K km s−1), intensity-weighted mean velocity map (moment 1; unit: km s−1), and residual velocity map obtained by subtracting circular motions (unit: km s−1). Note that the spatial scales are different for the S4G image and ALMA maps. Middle row, left to right: projected stellar surface density map (unit: M ⊙ pc−2), projected molecular gas surface density map (unit: M ⊙ pc−2), molecular gas LOS velocity map (unit: km s−1), and molecular gas residual velocity map (unit: km s−1) for the model at t = 818.2 Myr. Bottom row: same as the second row but at t = 892.7 Myr. The green plus sign marks the center of the image (x = 0, y = 0).
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Comparison of the enclosed mass (first row), mass inflow rate (second row), molecular gas fraction (third row), and SFR (fourth row) at two characteristic radii (R outer = 3.75 and R inner = 0.75 kpc) of models S2BSMU, S1BSMU, and S0BSMU. The molecular gas fraction is defined as the ratio of the molecular and total gas mass. Note that the range of the y-axis is not the same in the left and right columns.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: The KS relation in models S2BSMU, S1BSMU, and S0BSMU. Solid black curves are the contours of the scatter points. Only gas and newly formed stars in the disk region (﹩\left|z\right|\leqslant 2\,\mathrm{kpc}﹩) are considered in this plot. For each model, we include 11 snapshots separated by ∼100 Myr to increase the sample size. The black dashed line is the global fit from Querejeta et al. (2021) with a slope of 0.97. Two black dotted lines representing depletion times of 0.1 and 10 Gyr are included for comparison. The inset in the middle panel illustrates the placement of the hexagonal bins in our models. The bins are colored according to their galactocentric radius, and the underlying plot is the same gas surface density plot of S2BSMU shown in Figure 7.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Stellar and gas surface density comparison using S2BSMU, S1BSMU, and S0BSMU at t = 1.8 Gyr, from left to right as labeled. The top row is the stellar surface density, and the bottom row is the gas surface density. The outer bar is aligned with the x-axis for S2BSMU and S1BSMU. The dashed circles in the bottom row denote the two characteristic cylindrical radii, R outer = 3.75 and R inner = 0.75 kpc.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Kinematic maps of S2BEXP, viewed face-on. From left to right are four different epochs. The second (σ) and fourth (h 4) Gauss–Hermite moments of the vertical velocity v  z  distribution are shown in the top and bottom rows, respectively. White lines represent the contours of the stellar surface density. The outer bar is aligned with the x-axis.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Zoom-in view of Figure 6 to the central 2.5 kpc. The first and second columns are the stellar and gas surface densities. The third and fourth columns plot the metallicity (represented by [Fe/H]) and α abundance (represented by [Mg/Fe]) of the newly formed stars.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Evolution of A 2/A 0 (top) and pattern speed (bottom) in the inner bar region (R ≤ 0.75 kpc) of two models with different gas fractions. At t ≳ 1.7 Gyr in S2BEXP, the pattern speed calculated using the A 2 phase angle time derivatives may be less accurate due to the small A 2 amplitude.
Paper: How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Authors: Zhi Li, Min Du, Victor P. Debattista, Juntai Shen, Hui Li, Jie Liu, Mark Vogelsberger, Angus Beane, Federico Marinacci, Laura V. Sales
Figure caption: Solid lines: total SFR as a function of time in S2BSMU, S1BSMU, and S0BSMU. Dashed lines: SFR at R ≥ R outer = 3.75 kpc as a function of time in the models.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Cumulative distributions of the complexes per number of matched clumps (left panel, Section 4.2.1), clump filling factor (middle panel, Section 4.2.2), and clump-complex geometric center displacement (right panel, Section 5.1). Each quantity is computed for matched Hα-selected clumps (golden solid line) and UV-selected clumps (magenta dashed line). Furthermore, the displacement is computed considering separately UV-selected clumps in complexes with and without matched Hα clumps (the latter plotted as a gray dotted–dashed line). Median values are plotted as dark golden solid, dark magenta dashed, and when present, black dotted–dashed vertical lines. In the right panel, the gray dashed line shows our minimum resolvable resolution for the center displacement (∼0.055 kpc).
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Plots of the number of matched Hα-selected clumps (golden dots) and UV-selected clumps (magenta squares) as a function of area A compl (left), AR (middle), and radius of the largest matched resolved clump (right). Larger dark golden dots for Hα-selected clumps and dark magenta squares for UV-selected clumps show the median number of clumps per bin of the x-axis. The bins of the x-axis are equally spaced in linear or logarithmic scale according to the physical property. Error bars show the quartiles of the distribution in the bin. On the top right, we show the Pearson coefficient for each quantity and for Hα- and UV-matched clumps. For the sake of the clarity of the plots, we cut out one complex containing 21 clumps, which does not affect our interpretation of the plots.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Top panel: PSF-corrected core radius of the brightest Hα-resolved (golden dots) and UV-resolved (magenta squares) clump matched to the complex area. Median profiles are plotted as dark golden dots for Hα-selected clumps and dark magenta squares for UV-selected clumps. Error bars show the quartiles of the distribution in the bin. Bottom panel: same as the top panel, but for the number of matched Hα-selected clumps as a function of the Hα filling factor (golden dots) and the number of matched UV-selected clumps as a function of the UV filling factor (magenta squares).
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Color-composite images of JO201 (top), JO204 (left), and JW100 (right). The orange/yellow color traces the optical emission, and the blue one is the UV emission. The red color is associated with Hα emission. Zoomed-in images show typical examples of fireball configurations of the star-forming clumps in the tails of these galaxies. Credits for images: ESA/Hubble and NASA, M. Gullieuszik and the GASP team.