adsabs/AstroCLIMB huggingface dataset:
Paper: Binary Yellow Supergiants in the Magellanic Clouds. I. Photometric Candidate Identification
Authors: Anna J. G. O'Grady, Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig, Ylva Götberg, B. M. Gaensler
Figure caption: YSG T eff vs. minimum OB star mass. Each line shows, as a function of YSG temperature, the minimum mass of OB companion star required for the binary to be discernible from a single YSG at the same temperature, specifically requiring the binary model to be 0.15 mag bluer in U – B or W1 − U. Optical colors are solid green lines, and UV colors are dashed violet lines. YSG luminosities of log(L/L ⊙) = 4.2, 4.5, and 5.1 are shown as lines of increasing thickness.
Paper: Binary Yellow Supergiants in the Magellanic Clouds. I. Photometric Candidate Identification
Authors: Anna J. G. O'Grady, Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig, Ylva Götberg, B. M. Gaensler
Figure caption: Top: Hertzsprung–Russell diagram showing the Geneva stellar evolutionary models (T. Lejeune & D. Schaerer 2001) at metallicity Z = 0.008 for the LMC. A range of colors denotes mass. Black solid lines denote the region of interest (log(L/L ⊙) ≥ 4.0 and 4000 ≤ T eff ≤ 9000 K). Middle: Effective temperature vs. J − K color for the same models. Solid vertical lines denote the same temperature range as above, and a dashed orange line shows the fitted relationship. Bottom: Same as the middle panel, but for effective temperature vs. K-band bolometric correction.
Paper: Binary Yellow Supergiants in the Magellanic Clouds. I. Photometric Candidate Identification
Authors: Anna J. G. O'Grady, Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig, Ylva Götberg, B. M. Gaensler
Figure caption: Top: Hertzsprung–Russell diagrams for the SMC (left) and LMC (right), showing the final YSG candidate sample as gold circles. The limits of log(L/L ⊙)≥4.0 and 4000 ≤ T eff ≤ 9000 K are shown as gray dotted lines. As well, the Geneva stellar evolutionary models (T. Lejeune & D. Schaerer 2001) at metallicities Z = 0.004/0.008 for the SMC/LMC are plotted, with masses indicated. Finally, examples of partially stripped-envelope progenitors from J. J. Eldridge et al. (2013) are shown as light blue crosses.
Paper: Binary Yellow Supergiants in the Magellanic Clouds. I. Photometric Candidate Identification
Authors: Anna J. G. O'Grady, Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig, Ylva Götberg, B. M. Gaensler
Figure caption: The percentage that the OB-type MS star contributes toward the total flux in the YSG+OB binary system. Each column shows the results for a filter (from left to right, W1 (Swift), U, B, and V (MCPS), and J (2MASS)), and each row shows the results for a given YSG luminosity (from top to bottom, log(L/L ⊙) = 4.0, 4.5, 5.0). Within the panels, each box represents a combined model for a given YSG spectral type and OB-star mass.
Paper: A Potential Dynamical Origin of the Galactic Disk Warp: The Gaia–Sausage–Enceladus Major Merger
Authors: Mingji Deng, Cuihua Du, Yanbin Yang, Jiwei Liao, Dashuang Ye
Figure caption: Three velocities vary with time in different panels. The precession rate is retrograde relative to the disk. The spin velocity is along the body-fixed z-axis. The nutation velocity is along the x-axis after the first rotating with the ϕ angle.
Paper: Lensing Point-spread Function of Coherent Astrophysical Sources and Nontrivial Wave Effects
Authors: Xun Shi
Figure caption: Regimes of wave effects in lensing. The parameter space is spanned by the lens amplitude κ and the reduced frequency ν. Between the geometric optics regime at high frequencies ν ≳ 10 (blue) and the low-frequency perturbative wave optics regime where lensing effects are heavily suppressed (red), there is a range of intermediate frequencies where nontrivial wave effects are observable (white). The lower limit of the regime of nontrivial wave effects can be determined by the maximum difference ﹩{\rm{\Delta }}{I}_{\max }﹩ between the LPSF and the smoothed unlensed field. The dotted and dashed–dotted lines show the limits defined using different threshold values of ﹩{\rm{\Delta }}{I}_{\max }﹩. They both follow κ ν = const. at large κ. A 1D rational lens at β = 0 and a smoothing kernel of width 0.1 are used for computing the LPSFs.
Paper: Are There Local Dynamos Acting in Sunspot Regions?
Authors: Chunlan Jin, Guiping Zhou, Haisheng Ji, Jingxiu Wang
Figure caption: The identification of BMEs around the mature sunspot. Five BMEs around AR 12158 are identified in 16 hr observations, which are framed by the blue bold ellipses for initial identification and by the blue thin ellipses for subsequential evolution. One of them consists of two sub-bipoles, which are outlined by the black dashed lines and enlarged in the same panels (b) and (c). The two sub-bipoles merge around 14:48 UT and compose one BME. The magnetic field saturates at ±500 G in these magnetograms. These red (green) arrows represent the horizontal field corresponding to the vertical field with the positive (negative) polarity. The field of view for the top two rows is framed in the bottom left panel by the purple lines. The corresponding UV images at 160 and 170 nm wave bands are also shown in the bottom panels, and the domains framed by the white lines and yellow lines in the bottom panels represent the umbrae.
Paper: Lensing Point-spread Function of Coherent Astrophysical Sources and Nontrivial Wave Effects
Authors: Xun Shi
Figure caption: The same as Figure 2, but for a diverging rational lens that mimics an overdense plasma lens. This axisymmetric lens with κ = 10, β = 2 is a generalization of the lens in panel (c) of Figure 1 to 2D. It creates the same images, i.e., one real image and two imaginary images along the complexified x-axis. Note that the two discrete patches of the LPSF at ν = 10 (upper right panel) include one corresponding to an imaginary image (the one to the right).
Paper: Are There Local Dynamos Acting in Sunspot Regions?
Authors: Chunlan Jin, Guiping Zhou, Haisheng Ji, Jingxiu Wang
Figure caption: The regular distributed BMEs around the isolated smaller-scale sunspots in NOAA 12673 and 13078, as well as the magnetic flux changes in the two ARs. These BMEs in the two ARs are identified and framed by the blue ellipses. With the evolution of these BMEs, the magnetic flux increases from 5.1e21 Mx to 5.2e22 Mx for AR 12673 and from 5.1e21 Mx to 2.0e22 Mx for AR 13078, which are shown in the bottom panel. These red (green) arrows represent the horizontal field corresponding to the vertical field with the positive (negative) polarity. The magnetic field saturates at ±500 G.
Paper: Are There Local Dynamos Acting in Sunspot Regions?
Authors: Chunlan Jin, Guiping Zhou, Haisheng Ji, Jingxiu Wang
Figure caption: The polarity distribution of BMEs in the ARs NOAA 8375, 11515, and 12158. For NOAA 8375 shown in panels ((a1)–(a3)), the vertical magnetograms are adopted from the observations of SOHO/MDI, and the horizontal fields are observed by HSOS. These red (green) arrows represent the horizontal field corresponding to the vertical field with the positive (negative) polarity, and the length of 2500 G for horizontal field is shown by the red line in panel (b1). The magnetic field saturates at ±500 G in these magnetograms.
Paper: Are There Local Dynamos Acting in Sunspot Regions?
Authors: Chunlan Jin, Guiping Zhou, Haisheng Ji, Jingxiu Wang
Figure caption: The polarity distribution of BMEs around NOAA 10930. These red (green) arrows represent the horizontal field corresponding to the vertical field with the positive (negative) polarity. The magnetic field saturates at ±1000 G.
Paper: Lensing Point-spread Function of Coherent Astrophysical Sources and Nontrivial Wave Effects
Authors: Xun Shi
Figure caption: Lefschetz thimbles (red) and flow lines (white) for 1D rational lenses ψ = 1/(1 + x 2). The images are marked with pink crosses, and the poles are marked with gray crosses. Contours of the H function are shown in the background. The four subplots correspond to the four lensing configurations in Figure 1.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: MRCOLA_CNM density slice plots for the collision midplane. It corresponds to the x = 0 plane in Figure 1 and faces the positive x-direction. The linear color scale shows the total gas density in units of n H,tot. The magenta filled circles show the sinks. The circle size is proportional to the sink mass. The time step is shown at the top right in each panel. The arrows show the velocity vectors. The arrow color scales with the velocity magnitude (the bottom color bar).
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: Zoom-in views of the central 2 pc region of the 250 μm emission at t = 5 Myr. Again, each panel shows a random viewing angle of the filament (not a slice plot). The images are smoothed to a spatial resolution of 10″, corresponding to 0.02 pc at a distance of 400 pc. The lower left black filled circle shows the 10″ beam. The color bar has units of MJy sr−1. The magenta filled circles are the sinks. Their sizes are proportional to the mass. The red cross marks the location of sink 31. The lower right legend represents an 8 M ⊙ sink.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: CO(1-0) channel maps from RT modeling of Figure 9(g). The color scale shows the emission intensity in K. To match Figure 9, the channel maps are smoothed to a Gaussian beam with an FWHM of 10″, which is shown in the lower left corner in each panel. The channel width is 0.05 km s−1, and the channel velocity is shown in the lower right corner. The magenta filled circles are the same as those in Figure 9(g). The red cross marks the location of sink 31. The red plus marks the location of no sink 1.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: MRCOLA_CNM sonic Mach number ﹩{ \mathcal M }﹩ for the collision midplane (x = 0). This is the same slice as Figure 3. The color scheme diverges at ﹩{ \mathcal M }=1﹩. The velocity direction can be depicted from Figure 3.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: MRCOLA_CNM molecular abundance [CO] slice plots for the collision midplane (x = 0). This is the same slice as Figure 3. The logarithmic color scale shows [CO] from 3 × 10−10 to 3 × 10−6. The time step is shown at the top right.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: Left: linear polarization P  l  overlaid on the Stokes I intensity at 214 μm. The white segments are oriented along the plane-of-sky fields. Their lengths are proportional to P  l  (5% P  l  labeled at the top right). The line of sight follows Figure 1(a) except that the cube is rotated by 30° about the y-axis. Right: a zoom-in model of the left panel. The color map shows P  l . The black contours show the Stokes I intensity. The map has a beam size of 10″.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: MRCOLA_CNM molecular fraction [H2] slice plots for the collision midplane (x = 0). This is the same slice as Figure 3. The linear color scale shows [H2] from 0 to 0.5 (fully molecular). The magenta filled circles show the sinks. The circle size is proportional to the sink mass. The time step is shown at the top right.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: MRCOLA_CNM synthetic observations of dust emission at 250 μm at t = 5 Myr. In each panel, we view the entire filament (∼20 pc) at a random orientation (not a slice plot). The pixel scale is 0.02 pc, corresponding to 10″ at a distance of 400 pc. The color bar has units of MJy sr−1.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: MRCOLA_CNM density slice plots for the y = 0 plane (compared to Figure 1(b)). The linear color scale shows the total gas density in units of n H,tot. The vector stream lines show the field lines in the plane. Note how the reconnected lines encircle the high-density pancake at x = 0. The time step is shown at the top right. This slice corresponds to Figure 1(b).
Paper: The BANANA Project. VII. High Eccentricity Predicts Spin–Orbit Misalignment in Binaries
Authors: Marcus L. Marcussen, Simon H. Albrecht, Joshua N. Winn, Yubo Su, Mia S. Lundkvist, Kevin C. Schlaufman
Figure caption: Observed differences in vbroad between face-on and edge-on binaries. First panel: Smoothed and normalized histograms of the Gaia line-broadening parameter vbroad for all binaries in the sample, as well as for the edge-on or face-on subsamples. Second panel:  Fraction of systems for which vbroad exceeds 5 km s−1, or more literally, the fraction for which vbroad was reported in Gaia DR3. This fraction is shown for the edge-on systems, face-on systems, and the full sample separately, and was split into temperature bins of 100 K. Third panel:  vbroad as a function of T eff. The mean vbroad values of stars in 100 K bins are also shown. Across all temperatures, the edge-on sample shows systematically higher values of vbroad, and vice versa for the face-on sample, indicative of spin–orbit alignment. Bottom panel: The mean value of ﹩\widehat{{\mathtt{vbroad}}}﹩, the factor by which vbroad exceeds the mean value of all stars of the same effective temperature. This is shown as a function of orbital eccentricity. Horizontal lines indicate the width of the eccentricity bins, and vertical lines indicate the uncertainty. Evidently, nearly circular binaries exhibit stronger spin–orbit alignment than highly eccentric binaries.
Paper: The BANANA Project. VII. High Eccentricity Predicts Spin–Orbit Misalignment in Binaries
Authors: Marcus L. Marcussen, Simon H. Albrecht, Joshua N. Winn, Yubo Su, Mia S. Lundkvist, Kevin C. Schlaufman
Figure caption: Empirical calibration of rotation speed and vbroad. This 4 × 3 grid of panels illustrates the steps in our model relating v, vbroad, and effective temperature. The first row shows simulated rotation speeds v, with the first column displaying the distribution of values, and the second and third columns showing histograms on linear and logarithmic scales. Also shown are the best-fit functions for v min and v scat. The second row shows simulated ﹩v\,\sin \,i﹩ values, assuming isotropic orientations. The third row shows the corresponding values of vbroad using our conversion formulas. The fourth row shows simulated measurements of vbroad, taking the statistical uncertainties and the floor of 5 km s−1 into account. The black points in the lower left panel are the real values of vbroad in the sample. Different colors are used for different temperature ranges, as indicated in the legend.
Paper: The BANANA Project. VII. High Eccentricity Predicts Spin–Orbit Misalignment in Binaries
Authors: Marcus L. Marcussen, Simon H. Albrecht, Joshua N. Winn, Yubo Su, Mia S. Lundkvist, Kevin C. Schlaufman
Figure caption: Relationship between vbroad and ﹩v\,\sin \,i﹩, based on our FIES calibration sample. The top panel shows vbroad and ﹩v\sin i﹩ for 203 stars. The dashed black line is the identity line. The red curve shows a simple fit to the data, and the blue curve is our adopted relationship (see Equation (1)). The black histogram in the bottom panel shows the fraction of all the stars we observed with the Nordic Optical Telescope for which vbroad was reported in Gaia DR3 (and therefore exceeds 5 km s−1). The red and blue histograms are based on simulations employing the red and blue calibration curves depicted in the top panel.
Paper: The BANANA Project. VII. High Eccentricity Predicts Spin–Orbit Misalignment in Binaries
Authors: Marcus L. Marcussen, Simon H. Albrecht, Joshua N. Winn, Yubo Su, Mia S. Lundkvist, Kevin C. Schlaufman
Figure caption: Orbital inclinations i  o  of binaries in the sample. Top: Values and uncertainties of i  o  from Gaia DR3. We classified the binaries as “edge-on” (pink points), “face-on” (green points), or intermediate (white points). Bottom: Distribution of ﹩\cos {i}_{o}﹩ of stars for which SB1 solutions are available in addition to astrometry (AstroSpectroSB1) and stars for which only astrometric data are available (Orbital). An isotropic distribution of orientations would lead to a uniform distribution in ﹩\cos {i}_{o}﹩.
Paper: The BANANA Project. VII. High Eccentricity Predicts Spin–Orbit Misalignment in Binaries
Authors: Marcus L. Marcussen, Simon H. Albrecht, Joshua N. Winn, Yubo Su, Mia S. Lundkvist, Kevin C. Schlaufman
Figure caption: Physical parameters of the binary sample. A selection of relevant parameters and their correlations are shown for the full sample of binary systems (black) and for the face-on and edge-on subsets (green and pink). The p-values printed above the histograms come from KS tests comparing the edge-on and face-on samples.
Paper: Heavy Ion Escape at Mars during the Disappearing Solar Wind Event in 2022 December
Authors: Han-Wen Shen, Jasper S. Halekas, James P. McFadden, Jacob R. Gruesbeck, Neesha R. Schnepf
Figure caption: Variations in the flux difference between tailward and planetward ions in the tail region. The flux difference in each orbit is calculated by subtracting the median flux (blue diamond symbol) of planetward ions shown in Figure 5 from that of tailward ions shown in the four bottom panels of Figure 2.
Paper: Binary Disruption and Ejected Stars from Hierarchical Star Cluster Assembly
Authors: Claude Cournoyer-Cloutier, Jeremy Karam, Alison Sills, Simon Portegies Zwart, Maite J. C. Wilhelm
Figure caption: Initial conditions from the full TORCH run, zoomed in to show the merging clusters. The full domain width is 17.5 pc, and the central 7 pc are shown. The surface density shown is calculated using the resolution of the gas cells, 0.136 pc.
Paper: A Model of the C IV λ λ1548, 1550 Doublet Line in T Tauri Stars
Authors: Thanawuth Thanathibodee, Connor E. Robinson, Nuria Calvet, Catherine C. Espaillat, Caeley V. Pittman, Nicole Arulanantham, Kevin France, Hans Moritz Günther, Seok-Jun Chang, P. Christian Schneider
Figure caption: The contribution to the line profiles of an example model with f = 0.01 for all three values of ﹩{ \mathcal F }﹩, i = 60°, ﹩{v}_{t,{\rm{pre}}/{\rm{post}}}=50\,{\rm{km}}\,{{\rm{s}}}^{-1}﹩, [C/H]= −1, and distance of 360 pc. The dotted lines mark the rest-frame line centers. Left: the contribution to the flux from each ϕ. The solid lines are from the preshock, and the dashed lines are from the postshock. Note that the observer is at ϕ = π/2. Center: the contribution of the postshock and preshock for ﹩{ \mathcal F }={10}^{11}\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}﹩. The dashed lines show the individual emission and their sum, ignoring the attenuation effect of the preshock on the postshock. The spectra plotted with the dotted lines take into account the attenuation of the postshock and the opacity of the preshock. Right: the contribution to the overall line profiles from each energy flux.
Paper: A Model of the C IV λ λ1548, 1550 Doublet Line in T Tauri Stars
Authors: Thanawuth Thanathibodee, Connor E. Robinson, Nuria Calvet, Catherine C. Espaillat, Caeley V. Pittman, Nicole Arulanantham, Kevin France, Hans Moritz Günther, Seok-Jun Chang, P. Christian Schneider
Figure caption: Left: the total line profile for an example model as seen at different inclinations (left) while other parameters are the same as in the right panel of Figure 8. Right: an example of a model profile calculated at different magnetospheric truncation radii and otherwise the same accretion/geometric parameters. The dotted lines mark the rest-frame line centers.
Paper: A Model of the C IV λ λ1548, 1550 Doublet Line in T Tauri Stars
Authors: Thanawuth Thanathibodee, Connor E. Robinson, Nuria Calvet, Catherine C. Espaillat, Caeley V. Pittman, Nicole Arulanantham, Kevin France, Hans Moritz Günther, Seok-Jun Chang, P. Christian Schneider
Figure caption: The distributions of fitting parameters from the top 100 best fits of CVSO 176, CVSO 109A, CVSO 107, and CVSO 104. The vertical lines mark the median of the distribution.
Paper: A Model of the C IV λ λ1548, 1550 Doublet Line in T Tauri Stars
Authors: Thanawuth Thanathibodee, Connor E. Robinson, Nuria Calvet, Catherine C. Espaillat, Caeley V. Pittman, Nicole Arulanantham, Kevin France, Hans Moritz Günther, Seok-Jun Chang, P. Christian Schneider
Figure caption: The top 100 best fits. The blue lines are the observations. The red dashed lines are the Gaussian representation of the H2 feature. The black lines are the reddened C IV models plus the Gaussian. The continua have been subtracted for the models and the observations. The models fit the observations well for stars in the top rows (CVSO 176, CVSO 109A, CVSO 107, and CVSO 104).
Paper: A Model of the C IV λ λ1548, 1550 Doublet Line in T Tauri Stars
Authors: Thanawuth Thanathibodee, Connor E. Robinson, Nuria Calvet, Catherine C. Espaillat, Caeley V. Pittman, Nicole Arulanantham, Kevin France, Hans Moritz Günther, Seok-Jun Chang, P. Christian Schneider
Figure caption: The change in radiative properties of the flow due to different carbon abundance. The solid lines are the properties with the abundance as an input in Cloudy. The dashed lines are the values computed by scaling the level population from the results of the [C/H] = 0 calculation, demonstrating the nonlinear relationship between emissivity and abundance. The units are the same as in Figure 4.
Paper: A Model of the C IV λ λ1548, 1550 Doublet Line in T Tauri Stars
Authors: Thanawuth Thanathibodee, Connor E. Robinson, Nuria Calvet, Catherine C. Espaillat, Caeley V. Pittman, Nicole Arulanantham, Kevin France, Hans Moritz Günther, Seok-Jun Chang, P. Christian Schneider
Figure caption: The best-fits inclination and A V compared to the values from the literature and accretion modeling. The error bars are the standard deviations from the top 100 best fits. The green shades mark stars that have good fits. The model inclinations are constrained to be between those from ﹩v\sin i﹩ (C. V. Pittman et al. 2022) and from accretion flow modeling (Section 4.1). The ranges of A V are from C. F. Manara et al. (2021) and the shock modeling (Section 4.2), plus 0.1 mag for uncertainty.
Paper: A Model of the C IV λ λ1548, 1550 Doublet Line in T Tauri Stars
Authors: Thanawuth Thanathibodee, Connor E. Robinson, Nuria Calvet, Catherine C. Espaillat, Caeley V. Pittman, Nicole Arulanantham, Kevin France, Hans Moritz Günther, Seok-Jun Chang, P. Christian Schneider
Figure caption: The magnetospheric accretion flow model fits to individual Balmer lines. The blue lines are the observations, the gray lines are the 100 best fits, and the black lines are the average of the model profiles. The vertical/horizontal dotted lines mark the line center and the continuum, respectively. The corresponding fit parameters are shown in Table A1.
Paper: A Model of the C IV λ λ1548, 1550 Doublet Line in T Tauri Stars
Authors: Thanawuth Thanathibodee, Connor E. Robinson, Nuria Calvet, Catherine C. Espaillat, Caeley V. Pittman, Nicole Arulanantham, Kevin France, Hans Moritz Günther, Seok-Jun Chang, P. Christian Schneider
Figure caption: Same as Figure A1.