adsabs/AstroCLIMB huggingface dataset:
Paper: Shadow Implications: What Does Measuring the Photon Ring Imply for Gravity?
Authors: Avery E. Broderick, Kiana Salehi, Boris Georgiev
Figure caption: Constraints on N″(r  γ )/B 2(r  γ ) arising from a 10% measurement of γ. For reference, the curves associated with parameterized metrics (left) and alternative theories (right) are shown. Line types and points are the same as in Figure 1 (left) and Figure 2 (right).
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: A correlation wheel plot for the PC1 and PC2. The right panel shows a zoomed-in view for detail and the numbers in blue refer to the COM number identified in Table A1.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: Pearson correlation coefficients (ρ) between the eigencube of PC1 and the spectral cube data for each isolated strong line. The black dashed line indicates ρ = 0.7.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: The moment 0 and channel maps of the eigencube of PC1 (T PC1) (upper) and observed lines (lower). In the upper panels, the white circles mark a radius of 0.″3, within which most of the emission features arise. On the moment 0 map of PC1, the white-filled ellipse at the left bottom represents the beam shape, and the magenta dashed line indicates a cut for the PV diagram, Figure B1, along the semimajor axis of the protoplanetary disk. The blue ellipse represents the radial distance of 0.″15, along which the aligned spectra for the line selection were extracted, on the de-projected image of V883 Ori. The lower-left panel shows the mean moment 0 map of the isolated strong lines, while the lower-right small panels present the channel maps for the CH3OH line at 261.8057 GHz (Line 1; see Table A1).
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: The spectra for the second SPW of the first science goal (covering 221.63–222.54 GHz). The spectra are divided into three panels for better visibility. The aperture-averaged and PC1-filtered spectra are presented in black and red, respectively. The black and red horizontal dashed lines represent 3σ uncertainties in the aperture-averaged and PC1-filtered spectra, respectively. The blue shading indicates a member of the 34 isolated strong lines (see Table A1), and the orange shading indicates the spectral ranges selected for checking the conservation of total intensity (see Section 5.1). The red triangles indicate some of the additional emission lines identified above the 3σ level in the PC1-filtered spectrum.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: Left: correction of the line profile of PC1 using the PC1-filtering method. The black solid line represents a spectrum extracted from the PC1 eigencube with an aperture of r = 0.″3. Note that the y-axis is normalized by the maximum value of the average spectrum. The PC1-filtered spectrum is presented as the red solid line. The gray dashed vertical line denotes the system velocity of 4.3 km s−1. Right: the PC1-filtered spectrum and its Gaussian fitting result (blue). The blue dashed and dotted lines represent the central velocity (v  c ) and FWHM of the Gaussian profile, respectively.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: The integrated intensities for 34 isolated strong lines (left) and 109 selected frequency ranges (right). The top panels show a comparison between the integrated intensities measured from the aperture-averaged and PC1-filtered spectra. The bottom panels show the difference in integrated intensity (residuals). The error bars in both panels represent the 3σ uncertainty of the measured integrated intensities.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: Comparison of spectra produced by the PC1-filtering (red), aligned (blue), and matched-filtering methods (green). Note that the matched-filtering method provides the filter response values instead of the intensities. The red bars indicate two tentatively identified COM lines that are detected in the PC1-filtered spectrum over the 1σ level, which are not visible in the matched-filtered spectrum.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: An example of the selected frequency ranges and their PC1-filtered spectra. Each panel shows the aperture-averaged (black) and PC1-filtered spectra (red) within the selected frequency ranges (the orange-filled regions); they are one of the (1) Gaussian-like emission lines with high peak intensities, (2) Gaussian-like lines but with low intensities, (3) blended broad emission lines, (4) deep absorption features, and (5) emission-free-regions. As presented in the upper-right panel, if two adjacent lines are intrinsically blended because of thermal and nonthermal effects or a low spectral resolution, those lines cannot be completely decoupled even with the PC1-filtering method.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: Line profile corrections for the isolated strong lines. The four left panels show the aperture-averaged (black) and PC1-filtered (red) spectra for Lines 1, 2, 33, and 34. Lines 1 and 2 have the strongest correlation with PC1, while Lines 33 and 34 have the weakest correlations. The right panel shows the mean spectra of 34 isolated strong lines.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: The same as the right panel of Figure 7 but for a comparison between the PC1-filtered spectra and the average spectra over the 1″ × 1″ area centered on V883 Ori. The gray dashed line shows y = ax, where a is the area ratio between the circular aperture of r = 0.″3 and the boxy aperture of 1″ × 1″.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: Moment 1 (top) and moment 2 (bottom) maps for the eigencube of PC1. The black contours in both panels show the moment 0 map of PC1 (presented in the upper-left panel of Figure 3.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: The PV diagrams extracted along the semimajor axis of the V883 Ori disk (the magenta dashed line in Figure 3). The left panel shows the PV diagram for T PC1, and the right panel shows that for Line 1. In each panel, the contour levels start from 5 times the noise level of the data and are spaced by a factor of 2. The red solid lines on the left panel depict the Keplerian rotation profile of the V883 Ori disk.
Paper: The Principal Component Analysis Filtering Method for an Unbiased Spectral Survey of Complex Organic Molecules
Authors: Hyeong-Sik Yun, Jeong-Eun Lee
Figure caption: Moment 0 maps for the 34 isolated strong lines. The lines are referred to by the numbers listed in Table A1. The bottom-right panel presents a mean moment 0 map of the 34 lines. The white dashed box in the mean moment 0 map represents 1″ × 1″ area centered on V883 Ori.
Paper: High-angular-resolution Imaging of the V892 Tau Binary System: A New Circumprimary Disk Detection and Updated Orbital Constraints
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: SQUEEZE images reconstructed with a binary model from the ﹩L^{\prime} ﹩-band (left) and ﹩K^{\prime} ﹩-band (right) observables. The central stars and companions are represented with δ functions equal to their fractional fluxes and the images are normalized appropriately. Changes in the separations and position angles of the δ functions show the orbital motion of the stellar companion between the two epochs. The fractional fluxes of the central stars are 0.51 and 0.62 at ﹩L^{\prime} ﹩ band and ﹩K^{\prime} ﹩ band, respectively. The fractional fluxes of the secondary components are 0.28 and 0.25 at ﹩L^{\prime} ﹩ band and ﹩K^{\prime} ﹩ band, respectively.
Paper: High-angular-resolution Imaging of the V892 Tau Binary System: A New Circumprimary Disk Detection and Updated Orbital Constraints
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Left: the best-fit geometric model at ﹩L^{\prime} ﹩ band. The FWHM of the CB disk is ﹩189.9{\pm }_{19.7}^{16.5}﹩  mas and the separation of the stellar companion is 26.84 + 0.75/−0.64 mas at 146.°6 + 1.°35/−1.°32 measured east of north. The image has been cropped and smoothed with a Gaussian to make the δ functions visible. Right: the best-fit geometric model at ﹩K^{\prime} ﹩ band. The circumprimary disk has an FWHM of ﹩15.7{\pm }_{2.0}^{2.3}﹩  mas and a separation of ﹩42.1{\pm }_{0.6}^{0.7}﹩  mas located ﹩238^\circ .51{\pm }_{{0}^{^\circ }\,.83}^{{0}^{^\circ }\,.98}﹩ measured east of north. The image has been cropped and smoothed with a Gaussian to make the δ functions visible. Changes in the separations and position angles of the companions between the two epochs show the orbital motion of the stellar companion. The locations of the companion in both panels are similar to those in Figure 4; however their appearances are stretched here due to differences in the images’ fields of view.
Paper: High-angular-resolution Imaging of the V892 Tau Binary System: A New Circumprimary Disk Detection and Updated Orbital Constraints
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: SQUEEZE images reconstructed from the disk-plus-companion model closure phases and squared visibilities at ﹩L^{\prime} ﹩ band (left) and ﹩K^{\prime} ﹩ band (right) using a binary model. The fractional fluxes of the central stars are 0.57 at ﹩L^{\prime} ﹩ band and 0.65 at ﹩K^{\prime} ﹩ band. The fractional fluxes of the companion are 0.31 at ﹩L^{\prime} ﹩ band and 0.27 at ﹩K^{\prime} ﹩ band. This approximately matches the fractional fluxes in the SQUEEZE reconstructions of the data.
Paper: High-angular-resolution Imaging of the V892 Tau Binary System: A New Circumprimary Disk Detection and Updated Orbital Constraints
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: SQUEEZE images reconstructed from the ﹩L^{\prime} ﹩-band (left) and ﹩K^{\prime} ﹩-band (right) observables. The central stars are represented with δ functions occupying fractional fluxes of 0.71 and 0.50 at ﹩L^{\prime} ﹩ band and ﹩K^{\prime} ﹩ band, respectively. These fractional fluxes differ significantly from those estimated by the geometric models. This is not a physical feature of V892 Tau, but rather a bias in the SQUEEZE algorithm that we quantify using simulations (Sections 4.1 and 4.3).
Paper: High-angular-resolution Imaging of the V892 Tau Binary System: A New Circumprimary Disk Detection and Updated Orbital Constraints
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: V892 Tau Fourier observables. Left panels show closure phases for ﹩L^{\prime} ﹩ band (top) and ﹩K^{\prime} ﹩ band (bottom). The red points with error bars show the closure phases calculated from the data as described in Section 2.3. Hollow black circles show the closure phases calculated from the best-fit geometric model as described in Section 3.2. Right panels show the squared visibilities at ﹩L^{\prime} ﹩ band (top) and ﹩K^{\prime} ﹩ band (bottom). The red points with error bars show the squared visibilities calculated from the data as described in Section 2.3. Hollow black circles show the squared visibilities calculated from the the best-fit geometric model as described in Section 3.2.
Paper: High-angular-resolution Imaging of the V892 Tau Binary System: A New Circumprimary Disk Detection and Updated Orbital Constraints
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Top left: scattered points with error bars in the left panels show the correlation between the closure phase data and the best-fit model closure phases at L′ (top) and K′ (bottom). Scattered points with error bars in the right panels show the correlation between the squared visibility data and the best-fit model squared visibilities at L′ (top) and K′ (bottom). In all panels the orange solid line represents a 1:1 correlation.
Paper: High-angular-resolution Imaging of the V892 Tau Binary System: A New Circumprimary Disk Detection and Updated Orbital Constraints
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: SQUEEZE images reconstructed from the disk-plus-companion model closure phases and squared visibilities at ﹩L^{\prime} ﹩ band (left) and ﹩K^{\prime} ﹩ band (right) using a single point-source model. The fractional fluxes of the central stars are 0.79 at ﹩L^{\prime} ﹩ band and 0.51 at ﹩K^{\prime} ﹩ band. This approximately matches the fractional fluxes in the SQUEEZE reconstructions of the data.
Paper: High-angular-resolution Imaging of the V892 Tau Binary System: A New Circumprimary Disk Detection and Updated Orbital Constraints
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Scattered points show the uv coverage (the rotation of each baseline with parallactic angle) at ﹩L^{\prime} ﹩ band (left) and ﹩K^{\prime} ﹩ band (right). We obtained ∼64° and ∼108° of sky rotation at ﹩L^{\prime} ﹩ and ﹩K^{\prime} ﹩, respectively.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: Snapshots of pressure profiles along the subsolar line during the solar wind pressure pulse event. Pressure profiles of thermal pressure (red), dynamic pressure (green), magnetic pressure (blue), and total pressure (black) are plotted in each panel.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: Fluid speed and density as a function of radial distance at four different times from a one-dimensional, spherically symmetric hydrodynamic simulation of a fast disturbance overtaking a preexisting density enhancement. The times associated with each curve are indicated in the legend in the upper panel. See the main text and the Appendix for more details.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: The distributions of the density of O2 + in logarithmic scale and the velocity with θ at altitudes of 200 km and 350 km in the x–y plane, respectively. θ is the angle with the subsolar line with a positive degree for the +y hemisphere and a negative degree for the −y hemisphere. The red, green, and blue lines represent the simulation results at 1 hr, 1 hr 1 minute 19 s, and 2 hr, respectively.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: Solar wind velocity used in the simulation.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: Orbit of VEX on 2006 June 1 with the spacecraft position in the x–y–z coordinate.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: Comparison of simulation results with the VEX observations along the trajectory.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: Same as Figure 9, except that these are profiles as a function of time seen by three different radial distances (observation locations), as indicated by the legend in the bottom panel. See the main text for more details.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: Contour plots of average ion velocity and magnetic field strength in the x–z and x–y planes. The dashed black curves show the average bow-shock location from Zhang et al. (1990).
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an in-plane recoil kick. The line-of-sight velocity maps in the frame comoving with the recoiling black hole (“o” marker) in the x–y (top), x–z (center), and y–z (bottom) planes at t = 0 (left), t = 0.1 Myr (center), and t = 0.35 Myr (right). In each orientation, the color bar is adjusted such that approaching velocities are blue and receding velocities are red. The recoil kick direction is marked and labeled as v kick for each row. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. In the x–z plane, there appears a cluster of stars with high line-of-sight velocities immediately behind the recoiling black hole. In the y–z plane, different radial regions become coherently blueshifted over time as both the prograde and retrograde populations evolve along their orbits.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an in-plane recoil kick. The face-on, postkick distribution of stars at t = 0 (top left), t = 0.15 Myr (top right), and t = 0.75 Myr (bottom). Bound stars are separated into prograde (blue triangle markers) and retrograde (orange “+” markers). The unbound stars are marked with green dots. The “x” marker shows the center of the galaxy and the “o” marker shows the recoiling black hole. The arrow labeled v kick indicates the recoil direction. Positions are computed in the galactic center frame of reference. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The prograde and retrograde populations are nearly mirror images of each other about the x-axis. Prograde stars are aligned in one direction and retrograde stars are antialigned with the prograde orbits.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Parameter study with disks of varying initial inclination distributions. Top: the average y-component of the eccentricity vector, 〈e  y 〉, for an in-plane kick. Bottom: the average first component of the tilt vector, 〈t 1〉, for an out-of-plane kick, as a function of the initial eccentricity, with different lines showing different inclination distributions taken from a suite array of numerical simulations. Apsidal alignment becomes weaker with increased disk thickness, but tilt alignment is expected regardless of the inclination distribution.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an out-of-plane recoil kick. Top: the postkick eccentricity distribution as a function of semimajor axis with the inclination on the color bar. Bottom: the postkick mean first component of the tilt vector, 〈t 1〉, which measures roll, as a function of semimajor axis. The shaded noise floor shows the maximum expected deviation from 0 (at the 3σ level) if the distribution were isotropic. The eccentricity gradient, de/da, is negative inward of a ∼ 2 and positive outward, with most stars taking on a high inclination ∼90°. The tilt alignment is statistically significant at most semimajor axis ranges.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an out-of-plane recoil kick. The line-of-sight velocity maps in the frame comoving with the recoiling black hole in the face-on (top) and edge-on (bottom) orientations at t = 0 (left), t = 0.1 Myr (center), and t = 0.35 Myr (right). In each orientation, the color bar is adjusted such that approaching velocities are blue and receding velocities are red. The recoil kick direction is marked and labeled as v kick for each row. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The face-on orientation shows circular patterns where the edges of the distribution become more blueshifted over time. The edge-on orientation demonstrates that the elongated ball structure maintains coherent rotation as it evolves.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an out-of-plane recoil kick. The edge-on, postkick distribution of stars at t = 0 (top left), t = 0.15 Myr (bottom left), and t = 0.75 Myr (right). Bound and unbound stars are shown with blue triangle markers and green dots, respectively. The “x” marker shows the center of the galaxy and the “o” marker shows the recoiling black hole. The arrow labeled v kick indicates the recoil kick direction. Positions are computed in the galactic center frame of reference. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. Both bound and unbound stars form an elongated ball around the recoiling black hole.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an out-of-plane recoil kick. The postkick surface density distribution of bound stars in the face-on (top) and edge-on (bottom) orientations at t = 0 (left), t = 0.01 Myr (center), and t = 0.04 Myr (right). The “o” marker shows the recoiling black hole, and the contours are computed in the frame comoving with the black hole. In each orientation, the recoil kick direction is marked and labeled as v kick. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The edge-on orientation reveals an overdensity behind the recoiling black hole.