adsabs/AstroCLIMB huggingface dataset:
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: Detection sensitivity curves from speckle imaging and joint RV+astrometry in terms of Jupiter masses as a function of the separation from the central star. The purple sensitivity curve for speckle imaging is an upper limit, while the blue curve is a measurement for joint RV and astrometry constraint. The RV observational baseline is indicated by the vertical green dashed line. Any potential companion is likely to be either a high-mass giant planet, a brown dwarf, or a very-low-mass star.
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: GLS periodogram of activity indicators for HARPS and UCLES data. Window functions for each are in black. The horizontal dashed lines are 0.1% FAP and vertical solid lines represent period locations for the five planet candidates. No peaks in this periodogram coincide with any of the candidates’ periods.
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: RV completeness contour of HD 134606 from the injection–recovery tests. Tests conducted with only HARPS1 are shown in the left panel and those carried out with all the RV data are in the right panel. Blue dots are injected signals that were successfully recovered, whereas red dots were not. The black line represents the 50% detection probability, with the redder color showing a lower probability.
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: Speckle imaging detection limit in terms of instrumental magnitude difference as a function of the separation from the primary star. No bright companion was detected. Only the red channel was used for observation as the blue channel suffered an instrument alignment issue.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Top: overview of the Cygnus X region in the MWISP 13CO observations (Zhang et al. 2024), which is integrated over the velocity range of [−100, 40] km s−1. Bottom: three-color image of the 12CO (blue), 13CO (green), and C18O (red) emission toward the L914 cloud. The integral velocity intervals for the individual lines are the same as in Figure 3.
Paper: Magnetic Fields in the Southern Coalsack and Beyond
Authors: M. J. F. Versteeg, Y. Angarita, A. M. Magalhães, M. Haverkorn, C. V. Rodrigues, R. Santos-Lima, Koji S. Kawabata
Figure caption: Top right: locations of the five fields analyzed in this work. Gray rectangles represent the data; black markers indicate mean position of all stars in the field. Background contours show the total intensity in CO (Nyman et al. 1989) at the 2 and 6 K km s−1 levels. The surrounding histograms show the polarization angle distributions for each of the fields, including a Gaussian fit to the distribution (see also Section 3.1). Field C11, indicated with a circle, lies outside the area observed by Nyman et al. (1989).
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: PV maps along striations S5 and S6. The grayscale background shows the 12CO emission, and the blue contours are at 0.5 and 1.5 K (σ 12 ∼ 0.2 K). The overlapped lime and magenta contours show the 13CO and C18O emission, respectively. The lime contours start at 0.5 K and increase with steps of 1 K (σ 13 ∼ 0.15 K). The magenta contours start at 0.5 K and increase with steps of 0.5 K (σ 18 ∼ 0.15 K). The orange solid line represents the dense ridge and the blue shadow region shows its width. The red solid curve is the fitted velocity profile for a free-falling particle under the gravity of a cylinder with a line mass of 80 M ⊙ pc−1 (see Section 4.1 for more details). The two dashed lines display the expected velocity profiles by changing the line masses to 60 (yellow) and 100 M ⊙ pc−1 (orange). The scaling is shown with the vertical arrow line and the resolution is marked with the pink rectangle.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Power spectra of column density cuts (blue lines) perpendicular to striations in subregion R2 and velocity centroid power spectra (red dashed lines). The column density is derived from the 12CO emission with the equation of ﹩{N}_{{{\rm{H}}}_{2}}=X\int {T}_{\mathrm{MB},{\ }^{12}\mathrm{CO}}{dV}﹩, where X = 2.0 × 1020 cm−2 K−1 km−1 s (Bolatto et al. 2013).
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Statistics of polarization PAs (red step line). The blue dashed line shows the fitting result with a multicomponent Gaussian function. The green, orange, and blue shadow areas represent the angle ranges of the three components, respectively.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Relative angles between B-fields and filamentary structures. The colorful dots show the relative orientations of segments and large-scale B-fields, while the distribution of striations is represented by the colorful squares. The blue and orange shadow areas represent the regions that are within 30° from parallelism and perpendicularity, respectively.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Left: the same as Figure 15, but for subregion R3. Right: the distribution of the parameter Γ as a function of wavenumber for the peaks in the power spectra shown in the left panel. The red dashed line shows the fitting result obtained with the orthogonal distance regression method, and the shaded region shows the 1σ error of the fit.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Measured distance of L914. The middle panel shows the selected region used for distance estimation. The colorful background represents the MWISP 12CO emission, and the gray contour shows the edge of the cloud (∼3σ ). The cyan and pink dots represent the on- and off-cloud Gaia DR3 stars, respectively. The corner plots of the Markov Chain Monte Carlo sampling (distance and the extinction values and uncertainties of foreground and background stars) are shown in the left panel, where the mean values of the samples are shown with solid vertical lines. In the right panels, the dots show the Gaia stars as illustrated in the legend of each panel. The orange solid line in the upper right panel represents the result of monotonic regression fitting, while the dashed green lines in the bottom right panel are the modeled extinction A G.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Distribution of the one-dimensional velocity dispersion in the three subregions.
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Restoring single-epoch Cepheid photometry at one band, using a time-averaged PL relation, constructed at a different wavelength. In this case the V-band data at the top of the plot (for which there are many observations contributing to high-precision, time-averaged magnitudes) are used to predict the amount and the sign of amplitude-induced scatter contained in the single-epoch B-band PL relation (shown in the second plot down from the top). See Section 1.4 for a full description of the process and a detailed discussion of the remaining two PL relations at the bottom of the panel. Dashed lines are fits to the mean PL relations; solid lines are 2σ boundaries.
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Tight correlation of interband period–luminosity residuals (derived from Figure 2). This example shows the detailed scaling of B-band residuals as a function of I-band residuals. The slope is well defined and the scatter is very low. Here the slope is DB/DI = 1.89 mag/mag, and the residual scatter around the fit is only ± 0.061 mag. The slope defines the expansion/compression factor in using either one of these PL relations to predict the width of the other and the relative placement of points therein.
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Residual scatter in the predicted B-band PL relation after random-phase corrections to mean light have been applied. For our sample the residual scatter is σ = ±0.061 mag. Dashed lines, on either side of zero, indicate 1σ deviations.
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Period–amplitude distribution for Milky Way Cepheids. The range of Cepheid periods generally encountered in extragalactic studies (1.0 < log P < 1.8) is indicated by the two vertical red lines. The dashed red line marks a representative B-band amplitude of 1.6 mag for that restricted period range. (Diagram from data provided in Klagyivik & Szabados 2009).
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Same as Figure 7, except that the I-band data, shown at the top of the panel, are being used to predict the corrections needed to bring the single-epoch B-band data back to their time-averaged positions.
Paper: Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31
Authors: Denis A. Leahy, Jakob Hansen, Andrew M. Hopkins
Figure caption: Top panel: line extinction (E_BV_lines) vs. distance of each region. The red lines show the best-fit functions, with parameters given in Table 2. Middle panel: dust.umin and 〈U〉 vs. distance. The blue line is an exponential with a scale length of 12 kpc. Bottom panel: dust.luminosity per area vs. distance.
Paper: Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31
Authors: Denis A. Leahy, Jakob Hansen, Andrew M. Hopkins
Figure caption: Top panel: age_burst (young stellar population) vs. deprojected distance of each region from the center of M31. Middle panel: tau_burst (young stellar population) vs. distance. Bottom panel: f_burst (stellar mass in the young population divided by mass in the old population) vs. age_burst.
Paper: Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31
Authors: Denis A. Leahy, Jakob Hansen, Andrew M. Hopkins
Figure caption: UVIT F148W (150 nm) mosaic image of M31 in gray scale (Leahy et al. 2023b). This image is ≃115′ E–W by ≃140′ N–S. N is up, and E is left. Overlaid on the image in green are the regions used in this study. The field labels F1–F19 are in blue, and the subregions are the smaller numbers in blue (e.g., 1–10 for F1, 1–2 for F19). The number of subregions is 73.
Paper: Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31
Authors: Denis A. Leahy, Jakob Hansen, Andrew M. Hopkins
Figure caption: Mass per unit area vs. age for the old stellar population (red) and for the young population (blue).
Paper: Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31
Authors: Denis A. Leahy, Jakob Hansen, Andrew M. Hopkins
Figure caption: Cigale best-fit model for region F4_1 (top plot) and residuals between model and data (bottom plot). The legend shows the symbols for the data and model and the different contributions to the model fluxes.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Membership probability distribution for each membership assessment technique shown for stars from the YSOC catalog (left) and the Gaia query (right). The top three panels show the contributions from the astrometric, photometric isochronal, and light-curve variability assessments, with the combined final result in the bottom panels. We consider all stars with P > 50% in the combined histogram (red vertical line) to be likely members of Mon R2.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Isochrones compared to RP absolute magnitude and G-RP color for all stars in the initial Gaia query. Stars are colored by their location relative to the isochrones, with green points representing stars above the 106 yr isochrone, cyan between 106 and 107 yr, red between 107 and 108 yr, and blue points stars below the 108 yr isochrone.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Top: distribution of proper motion in R.A. (left) and proper motion in decl. (middle) for YSOC catalog stars. Gaussian fits to the distributions are overplotted in red, with ±3σ values marked with orange lines. The vector point diagram (right) shows the proper motion distribution, with an ellipse indicating the 3σ contour. Bottom: same plot as above but zoomed in around the main distribution.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Distribution of the total membership probability P total, as given by the color bar, across proper motion and parallax space for the 2551 Gaia stars with P astro > 0.25. Given the weighting of the membership selection criteria, most of the highly probable members lie close to the estimated median kinematic parameters for the cluster. However, the additional criteria based on photometry relative to isochrones, and photometric variability, mean that some stars identified as candidate cluster members are further away from the kinematic centers.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Left: Gaussian fit to parallax values of YSOC catalog stars with parallax error over parallax larger than the 90th percentile value (0.375). Right: parallax vs. inverse signal-to-noise ratio in the parallax measurements. The boxed region shows data within 3σ of the Gaussian mean. Bottom: same plot as above but zoomed in around the main distribution.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Sloan filter i vs. i − z, i vs. r − i, and i vs. g − i absolute magnitude–color diagrams for YSOC stars. Isochrones are from MIST (Paxton et al. 2011; Choi et al. 2016; Dotter 2016) with parameters [Fe/H] = 0, v/v critical = 0.4, and Av = 0. The Red dashed line on the g − i diagram shows a cutoff for stars we deem to be likely background due to high reddening.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Left: vector point diagram of proper motion distributions among all Gaia DR3 stars over the 2.5 × 2.5 deg2 query area centered on Mon R2. The color bar indicates the astrometric membership probability (P astrom) as described in the text. Middle: stars with astrometric membership probability P astrom > 0.25. Right: field stars excluded from the candidate member sample as a result of low astrometric membership probability.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Same as Figure 1, but now showing only the 921 Gaia-selected sources that have membership probability P total > 0.5. Blue points are members already suspected as such from the literature while red points are members of Mon R2 identified from Gaia.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Gaussian fits (red lines) and 3σ limits (orange lines) for proper motion in R.A. (left), proper motion in decl. (middle), and parallax (right) for the final catalog of highly probable literature plus newly identified member stars.
Paper: Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph
Authors: Satoshi Itoh, Taro Matsuo, Motohide Tamura
Figure caption: The vertical and horizontal axes mean the planetary throughput (including fiber-coupling efficiency) and the azimuthal angles of the planetary separation, respectively. (Left) The dashed, solid, and dotted curves correspond to the cases of 1.000, 1.352 (the radius of the maximum throughputs), and 1.600 λ  c /D of the radius of the planetary separation, respectively. (Right) The red solid curve indicates the same curve as the solid curve in the left panel. The green dashed, blue dotted, and orange dashed–dotted curves show the same ones shifted (rotated) along the horizontal axis by 45°, 90°, and 135°, respectively. The gray solid curve denotes the sum of all four curves.
Paper: Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph
Authors: Satoshi Itoh, Taro Matsuo, Motohide Tamura
Figure caption: A schematic showing which terms of ﹩\left\{{g}_{K;N-K}(\alpha ,\beta )| K,N\in {\mathbb{Z}}\right\}﹩ can transmit the optical system of the new method. The horizontal and vertical axis indicates the values of K and N − K, respectively. Every lattice point on the figure corresponds to a pair of integers K and N − K. The diagonal dashed lines connect the lattice points belonging to the same values of N. The red prohibited symbols mean that the associated terms fail to transmit the single-mode fiber. The blue-filled squares denote the terms to be erased by the coronagraph system perfectly in the case of the zero spectral bandwidth.
Paper: Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph
Authors: Satoshi Itoh, Taro Matsuo, Motohide Tamura
Figure caption: The markers in the left panel are the same as the ones in Figure 5. The curves in the left panel show the fitted function for the different spectral bandwidths. The fitting assumes the functional form of Equation (33). The legend in the left panel includes the fitting results of the fitting parameters c 2 and c 6. The vertical axis of the right panel means the fitting results of the fitting parameters c 2 (red markers) and c 6 (black markers), and the horizontal axis denotes the spectral bandwidth. The dashed straight lines connect the markers as interpolation.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Top left panel: periodic orbits associated with Kozai resonance in the system of β = 168 of the full octupole Hamiltonian (colored curve), and fixed points defined in Equation (4) in Hansen & Naoz (2020) under the quadrupole-order Hamiltonian (black curve, for which e 2 is set at 0.3). The last three panels: Poincaré sections defined by g 2 = 90° at different levels of the  Hamiltonian. The resonant centers are marked by red asterisks with letters from “A” to “D.”
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Dynamical structures associated with Kozai resonance under different mass ratios. The regions denoted by different colors stand for orbits inside Kozai resonance, and the color bars represent different values of the Hamiltonian. The pure blue regions stand for orbits outside Kozai resonance. The black dots represent stable periodic orbits associated with Kozai resonance. Forbidden regions are shown in white. The initial angles are fixed at g 1 = π/2 and g 2 = π/2.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Characteristic curves of stable and unstable periodic orbits corresponding to the octupole-order resonance centered at σ = π under different mass ratios. The initial angles are set at g 1 = 0, g 2 = π. The stable ones are denoted by the colors shown in the legends, and the unstable periodic ones are all denoted by red dots.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Characteristic curves of stable and unstable periodic orbits corresponding to the octupole-order resonance centered at σ = 0 under different mass ratios. The initial angles are set at g 1 = 0, g 2 = 0. The stable orbits are denoted by the colors shown in the legends, and the unstable periodic ones are all denoted by red dots.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Characteristic curves of stable periodic orbits associated with Kozai resonance under different mass ratios in the i tot–e 1 plane. The initial angles are fixed at g 1 = π/2 and g 2 = π/2.