adsabs/AstroCLIMB huggingface dataset:
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: Estimation of the ISP toward SN 2021rhu based on the observations on days −7 (left column) and +0 (right column). The top row gives the flux spectra normalized to the maximum value within the range. The middle row presents the degree of linear polarization for the given epochs. The red long-dashed curve indicates the best fit using a Serkowski law. The fitted parameters are labeled in each panel. The data have been rebinned to 40 Å. Data points plotted in gray were excluded from the fitting since they cover broad and polarized features or major telluric lines. The bottom row shows the residuals from the fit.
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: Same as Figure 2, but for day +79. The red histograms in panel (e) display the ISP-corrected PA across Ca II H and K and Ca II NIR3 after correction for the ISP.
Paper: Determining the Core Structure and Nuclear Equation of State of Rotating Core-collapse Supernovae with Gravitational Waves by Convolutional Neural Networks
Authors: Yang-Sheng Chao, 仰生 趙, Chen-Zhi Su, 晨知 蘇, Ting-Yuan Chen, 莛元 陳, Daw-Wei Wang, 道維 王, Kuo-Chuan Pan, 國全 潘
Figure caption: The predicted values of ω 0 using two different models: our CNN model without TL (green circles), and a TL model trained by using additional waveforms from Pan (blue triangles). Filled symbols represent results for HI ω 0, and open symbols indicate results for NHI ω 0. The diagonal dashed line indicates the correct results.
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: Same as Figure 2, but for day +36. The red histograms in panel (e) display the ISP-corrected PA across Ca II H and K and Ca II NIR3 after correction for the ISP.
Paper: A Semianalytical Line Transfer Model. III. Galactic Inflows
Authors: C. Carr, C. Scarlata
Figure caption: Orientation effects on galactic systems with inflows and outflows. All diagrams are to be viewed from the right. Inflowing gas is shown in light blue while outflowing gas is shown in salmon. The would-be spectrum for each flow is shaded in matching colors. The composite spectrum is shown at a resolution of 50 km s−1 (black) and 120 km s−1 (dark gray). Upper left: looking down the line of sight into an outflow with inflows moving perpendicular to the line of sight. Upper right: looking down the line of sight of an inflow with an outflow occurring perpendicular to the line of sight. Bottom middle: both inflow and outflow are observed edge-on. The remaining parameters for these profiles are as follows. Outflows: γ = 1.0, δ = 3.0, ﹩\mathrm{log}(N\ [{\mathrm{cm}}^{-2}])=15﹩, v 0 = 25 kms−1, v  w  = 500 kms−1, R AP > R  W , κ = 0, and f  c  = 1.0. Inflows: γ = 0.5, δ = 1.5, ﹩\mathrm{log}(N\ [{\mathrm{cm}}^{-2}])=15﹩, v 0 = 15 kms−1, v  w  = 200 kms−1, R AP > R  W , κ = 0, and f  c  = 1.0.
Paper: A Semianalytical Line Transfer Model. III. Galactic Inflows
Authors: C. Carr, C. Scarlata
Figure caption: Galactic fountains with inflows represented by streams observed in the Fe II 2343 Å line viewed at different orientations and geometries. The Fe II 2343 Å line has a strong fluorescent component (not shown) and therefore has reduced resonant emission. All diagrams are to be viewed from the right. Inflowing gas is shown in light blue, outflowing gas is shown in salmon, and regions of overlap are shown in violet. The resulting spectra for each type of flow is shaded in the matching color. The composite spectrum is shown at a resolution of 50 km s−1 (black) and 120 km s−1 (dark gray). Top left: a spherical fountain. Top right: a biconical fountain observed parallel to the line of sight. Bottom left: a biconical fountain oriented perpendicular to the line of sight. Bottom right: a biconical fountain observed edge-on. The remaining parameters are as follows. Outflows: v 0 = 25 [km s−1], v ∞ = 500 [km s−1], R AP > R  W , ﹩\mathrm{log}(N\ [{\mathrm{cm}}^{-2}])=15﹩, κ = 0, δ = 3.0, and γ = 1.0. Inflows: v 0 = 15 [km s−1], v ∞ = 200 [km s−1], R AP > R  W , ﹩\mathrm{log}(N\ [{\mathrm{cm}}^{-2}])=15﹩, κ = 0, δ = 1.5, and γ = 0.5.
Paper: A Semianalytical Line Transfer Model. III. Galactic Inflows
Authors: C. Carr, C. Scarlata
Figure caption: Left: cross-sectional view of a spherical inflow. Continuum rays are drawn in purple and are shown passing through a surface of constant observed velocity whose curve of constant observed velocity, Γ x , is shown in blue. Note that the rays can either intersect Γ x  once, twice, or zero times. For the continuum ray that intersects Γ x  twice, the shells of intrinsic velocities ﹩{y}_{{h}_{1}}﹩ and ﹩{y}_{{h}_{2}}﹩ that pass through the intersections are shown in black. A shell of intrinsic velocity, y max, intersecting the maximum of Γ x , is shown in red. Right: a close-up view of the intersections. The maximum of Γ x  as well as the points of intersection with the continuum rays provide enough information to compute the absorption profile as described in the text.
Paper: A Semianalytical Line Transfer Model. III. Galactic Inflows
Authors: C. Carr, C. Scarlata
Figure caption: Left panel: line profiles for biconical inflows of various opening angles oriented along the line of sight (i.e., ψ = 0°). Right panel: line profiles for biconical inflows with opening angle, α = 30°, oriented at various angles with respect to the line of sight. The remaining parameters for these profiles are γ = 0.5, δ = 1.5, ﹩\mathrm{log}(N\ [{\mathrm{cm}}^{-2}])=15﹩, v 0 = 15 kms−1, v  w  = 200 kms−1, R AP > R  W , κ = 0, and f  c  = 1.0.
Paper: A Semianalytical Line Transfer Model. III. Galactic Inflows
Authors: C. Carr, C. Scarlata
Figure caption: Left column: the absorption profile (top), emission profile (middle), and inverse P Cygni profile (bottom) of a spherical inflow for various values of δ with γ = 0.5. Right column: the same as the left column except γ varies and δ = 1.5. The remaining parameters for these profiles are α = 90°, ψ = 0°, ﹩\mathrm{log}(N\ [{\mathrm{cm}}^{-2}])=15﹩, v 0 = 15 kms−1, v  w  = 200 kms−1, R AP > R  W , κ = 0, and f  c  = 1.0.
Paper: A Semianalytical Line Transfer Model. III. Galactic Inflows
Authors: C. Carr, C. Scarlata
Figure caption: Left: the absorption profile, middle emission profile, and right inverse P Cygni profile for a spherical inflow. The asymmetry in the emission profile reflects the occultation effect where photons emitted from behind the source are blocked by the source from the observer’s field of view. The parameters for this inflow are listed on the left most panel.
Paper: A Semianalytical Line Transfer Model. III. Galactic Inflows
Authors: C. Carr, C. Scarlata
Figure caption: Various curves of constant observed velocity for inflowing velocity fields. The curves drawn with the darkest, middle, and lightest shades correspond to velocity fields with γ = 2.0, 1.0, and 0.5, respectively. The different colors represent different observed velocities.
Paper: A Semianalytical Line Transfer Model. III. Galactic Inflows
Authors: C. Carr, C. Scarlata
Figure caption: Envelope of material (shown in blue) of radius R  W  surrounding a galaxy (shown in green) of radius R  SF . The ξ- and s-axes are written in normalized units (r/R SF). The envelope represents a flow characterized by a density and velocity field.
Paper: Millimeter Dust Emission and Planetary Dynamics in the HD 106906 System
Authors: Anna J. Fehr, A. Meredith Hughes, Rebekah I. Dawson, Rachel E. Marino, Matan Ackelsberg, Jamar Kittling, Kevin M. Flaherty, Erika Nesvold, John Carpenter, Sean M. Andrews, Brenda Matthews, Katie Crotts, Paul Kalas
Figure caption: Naturally weighted ALMA image of the 1.3 mm continuum emission from the disk around HD 106906. The star symbol denotes the expected location of the central stellar binary, while the blue dot denotes the expected location of the planetary companion HD 106906b. There is no continuum emission visible at the location of the planet. Twenty-five orbit tracks sampled randomly from the posterior distribution of orbital elements obtained in Nguyen et al. (2021) are projected onto the sky plane and represented by the white ellipses. A zoomed-in image of the disk emission is inset, with contour levels at [−2,2,4,6,8] × σ, where σ is the rms noise in the image, 6.2 μJy beam−1. The hatched ellipse represents the size and orientation of the synthesized beam, 0.″38 × 0.″31. The size of Neptune’s orbit is displayed beneath the scale bar for visual comparison.
Paper: Millimeter Dust Emission and Planetary Dynamics in the HD 106906 System
Authors: Anna J. Fehr, A. Meredith Hughes, Rebekah I. Dawson, Rachel E. Marino, Matan Ackelsberg, Jamar Kittling, Kevin M. Flaherty, Erika Nesvold, John Carpenter, Sean M. Andrews, Brenda Matthews, Katie Crotts, Paul Kalas
Figure caption: Interpolated model of accreting circumplanetary disks from Zhu et al. (2018) with the viscosity parameter α on the x-axis, outer radius on the y-axis, and flux density in μ Jy as color, adjusted to a distance of 140 pc. The dashed contour line represents the upper limit of 11 μ Jy beam−1 within a radius of 1/3 R Hill, while the solid line represents the upper limit of 33 μ Jy beam−1 within a radius of 1 R Hill.
Paper: Millimeter Dust Emission and Planetary Dynamics in the HD 106906 System
Authors: Anna J. Fehr, A. Meredith Hughes, Rebekah I. Dawson, Rachel E. Marino, Matan Ackelsberg, Jamar Kittling, Kevin M. Flaherty, Erika Nesvold, John Carpenter, Sean M. Andrews, Brenda Matthews, Katie Crotts, Paul Kalas
Figure caption: (Left column) Naturally weighted ALMA image of the 1.3 mm continuum emission from the HD 106906 system. (Center column) Best-fit models for each functional form sampled at the same baseline lengths and orientations as the ALMA data. (Right column) Residual images after subtracting the models from the data in the visibility domain. The top row shows the narrow Gaussian ring model, the middle row shows the broad Gaussian ring model, and the bottom row shows the similarity solution model. Contour levels and symbols are as in Figure 1.
Paper: Millimeter Dust Emission and Planetary Dynamics in the HD 106906 System
Authors: Anna J. Fehr, A. Meredith Hughes, Rebekah I. Dawson, Rachel E. Marino, Matan Ackelsberg, Jamar Kittling, Kevin M. Flaherty, Erika Nesvold, John Carpenter, Sean M. Andrews, Brenda Matthews, Katie Crotts, Paul Kalas
Figure caption: Histograms of the posterior probability distributions for the similarity solution model. The central line designates the median of each distribution while the outer dashed lines mark the 16th and 84th percentiles.
Paper: Millimeter Dust Emission and Planetary Dynamics in the HD 106906 System
Authors: Anna J. Fehr, A. Meredith Hughes, Rebekah I. Dawson, Rachel E. Marino, Matan Ackelsberg, Jamar Kittling, Kevin M. Flaherty, Erika Nesvold, John Carpenter, Sean M. Andrews, Brenda Matthews, Katie Crotts, Paul Kalas
Figure caption: Histograms of the posterior probability distributions for the Gaussian ring model. The central line designates the median of each distribution while the outer dashed lines mark the 16th and 84th percentiles.
Paper: Millimeter Dust Emission and Planetary Dynamics in the HD 106906 System
Authors: Anna J. Fehr, A. Meredith Hughes, Rebekah I. Dawson, Rachel E. Marino, Matan Ackelsberg, Jamar Kittling, Kevin M. Flaherty, Erika Nesvold, John Carpenter, Sean M. Andrews, Brenda Matthews, Katie Crotts, Paul Kalas
Figure caption: Histograms of the posterior probability distributions for the narrow ring model. The central line designates the median of each distribution while the outer dashed lines mark the 16th and 84th percentiles.
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Same as Figure 7, except the data correspond to X Per, and the theoretical spectra were computed based on the model 2 parameters listed in Table 1. The data were reported by Delgado-Marti et al. (2001; circles and crosses). This case also includes interstellar absorption with hydrogen column density N H = 3.0 × 1021 cm−2.
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Vacuum-modified electron scattering cross sections, ﹩{\sigma }_{{}_{V1}}﹩ and ﹩{\sigma }_{{}_{V2}}﹩, plotted as functions of the propagation angle θ relative to the Thomson value ﹩{\sigma }_{{}_{{\rm{T}}}}﹩ for extraordinary mode (solid lines) and ordinary mode (dashed lines) photons using Equations (14) and (15) for n  e  = 1.89 × 1021 cm−3 and B = 4.41 × 1012  G, which are the values used in Figure 4 from Meszaros & Ventura (1979). The value of the photon energy ratio ϵ/ϵ  c  is indicated. For comparison, the plasma-only cross sections are also plotted for the extraordinary mode (dotted–dashed lines) and ordinary mode (dotted lines) using Equations (6) and (7).
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Theoretical column-integrated count-rate spectrum F  ϵ (ϵ) computed using Equation (182) based on the model 1 parameters listed in Table 1, compared with the deconvolved (incident) X-ray spectrum for Her X-1 reported by Wolff et al. (2016; magenta and cyan points and lines). The plot includes the total theoretical spectrum as well as the individual spectral components due to the column-wall and column-top emission of Comptonized bremsstrahlung, cyclotron, and blackbody seed radiation, as indicated. An additional iron emission line feature is also included. Note that the total spectrum is dominated by the bremsstrahlung component emitted through the column walls.
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Model velocity profile υ for X Per (blue line), computed using Equation (45) with k 0 = 0.3 and k ∞ = 0.244. The gas impacts the stellar surface with speed 0.19c, and the flow satisfies the jump conditions for a strong shock at the top of the accretion column.
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Electron scattering cross sections in a magnetized plasma, ﹩{\sigma }_{{}_{P1}}﹩ and ﹩{\sigma }_{{}_{P2}}﹩, plotted as functions of the energy ratio ϵ/ϵ  c  relative to the Thomson value ﹩{\sigma }_{{}_{{\rm{T}}}}﹩ for extraordinary mode (solid lines) and ordinary mode (dashed lines) using Equations (6) and (7). The value of the propagation angle θ is indicated. Note the strong resonance at the cyclotron energy for the extraordinary mode. These results are consistent with Figure 2 from Ventura (1979).
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Model velocity profile υ for Her X-1 (blue line), computed using Equation (45) with k 0 = 0 and k ∞ = 1. The flow settles onto the star with zero velocity at the surface, and approaches Newtonian freefall far from the star.
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Vacuum-modified electron scattering cross sections, ﹩{\sigma }_{{}_{V1}}﹩ (solid lines) and ﹩{\sigma }_{{}_{V2}}﹩ (dashed lines), plotted as functions of the photon energy ratio ϵ/ϵ  c  relative to the Thomson value ﹩{\sigma }_{{}_{{\rm{T}}}}﹩ using Equations (14) and (15) for n  e  = 1.89 × 1021 cm−3 and B = 4.41 × 1012  G. The value of the propagation angle θ is indicated. Note that in the angular range considered here, ﹩{\sigma }_{{}_{V1}}﹩ is independent of θ.
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Various examples of the dimensionless flow velocity profile, u, for gas accreting in a conical accretion column, plotted as a function of y = R/R * using Equation (45), for the indicated values of the impact velocity parameter, k 0. The cases with k ∞ = 1 (blue lines) merge with the freefall profile as y → ∞ , and the cases with k ∞ = 0.25 (green lines) approximate the velocity profile below a shock at the top of the column. We have also included the BW07 velocity profile (cyan line), and the Newtonian freefall profile (red line). The yellow region on the left-hand side represents the interior of the neutron star.
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Variation of the electron scattering optical depth, τ, measured upwards from the bottom of the accretion column, for photons propagating in the radial direction, computed using Equation (52). The four examples plotted correspond to α = 0.3, k 0 = 0, (blue line); α = 0.3, k 0 = 0.4, (red line); α = 0.2, k 0 = 0, (green line); and α = 0.2, k 0 = 0.4 (cyan line). In each case, we set k ∞ = 1 so that the accretion velocity approaches Newtonian freefall as R → ∞.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: (Left) Bardeen black hole shadow angular diameter θ sh, in units of μas, as a function of (a, g). Black lines are for 46.9 and 50μas corresponding to the Sgr A* black hole shadow bounds. Bardeen black holes with parameter region between these two black lines cast shadows that are consistent with the Sgr A* shadow size. (Right) Bardeen no-horizon spacetime shadow angular diameter θ sh, in units of μas, as a function of (a, g). The black line is for 41.7 μas, corresponding to the Sgr A* black hole shadow 1σ bounds, such that the region under the black line satisfies the Sgr A* shadow 1σ bound.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: A comparison of the silhouettes of regular black holes and no-horizon spacetime shadows with varying charge g. The black curve represents the black hole case g ≤ g  E , whereas the red and green curves are for the no-horizon spacetime g ≥ g  E . Interestingly, the no-horizon spacetime with g  E  ≤ g ≤ g  p  casts a closed shadow boundary, as shown with the red curve.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Parameter space (a, g) corresponding to a black hole and no-horizon spacetime. Parameters in the gray regions define a black hole such that regions outside the red line represent no-horizon spacetime. No-horizon spacetime with parameters only in the black shaded region leads to the closed photon ring structure
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: (Left) Angular diameters, θ sh, of Hayward black hole shadows, in μas, as a function of (a, g). The black line is for θ sh = 50 μas, corresponding to the Sgr A* black hole shadow. Hayward black holes that have parameters outside of the black line produce a shadow that is consistent with the Sgr A* shadow size. (Right) Angular diameter, θ sh, of Hayward no-horizon spacetime shadows, in units of μas, as a function of (a, g). The black line is for θ sh = 46.9 μas, corresponding to the Sgr A* black hole shadow, such that the region under the black line satisfies the Sgr A* shadow size.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Shadow silhouette for a Kerr black hole (left) and the Kerr naked singularity (right) for an inclination angle θ 0 = 50°. The Kerr naked singularity (a > M) always casts an open arc shadow.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Regular black hole shadow silhouettes with varying charge g.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Deviations of the angular diameters of Bardeen black hole (left) and no-horizon spacetime (right) shadows from that of a Schwarzschild black hole as a function of (a, g). The black and green lines are, respectively, for values of δ = −0.04 (Keck) and δ = −0.08 (VLTI), corresponding to the Sgr A* black hole shadow bounds.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Bardeen black hole (left) and no-horizon spacetime (right) shadows' circularity deviation observables ΔC as a function of (a, g).
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius 141 members compared with the Ursa Major core and the various Kounkel & Covey (2019) Theia groups tentatively identified as possible tidal tails around Ursa Major (Gagné et al. 2020b). Crius 141 may be associated with the missing part of the tidal tails not recovered by Kounkel & Covey (2019) due to projection effects, and is likely associated with the Ursa Major stream (or the “Sirius supercluster”) of Eggen (1992). We identify stars with known 3D UVW-space velocities within 6 km s−1 of the Ursa Major core stars with a distinct color; we allow for a larger space velocity difference in this case because Crius 141 (and the other structures possibly associated with the Ursa Major core) display a large spread in UVW velocities.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Median UV-space velocities of all Crius groups (open red stars), and new candidate associations presented here (filled red stars) compared with other known young associations in the literature (blue circles) and field stars within 100 pc of the Sun in Gaia EDR3 (gray circles). Open blue circles indicate “candidate” associations that have not yet been fully characterized, such as most of the Kounkel & Covey (2019) Theia groups, and we indicate the velocity regions introduced by Eggen (1958) and Eggen (1971). We have excluded Crius groups within the Hercules regions as well as the higher-velocity groups at V > 40 km s−1 or U < −60 km s−1 from this study (Gaia Collaboration et al. 2021).