adsabs/AstroCLIMB huggingface dataset:
Paper: Spacecraft Charging Simulations of Probe B1 of Comet Interceptor during the Cometary Flyby
Authors: S. Bergman, Y. Miyake, S. Kasahara, F. L. Johansson, P. Henri
Figure caption: The resulting charge density of ions (panels (a)–(c)), warm electrons (panels (d)–(f)), and cold electrons (panels (g)–(i)) along the x-axis (panels (a), (d), and (g)), y-axis (panels (b), (e), and (h)) and z-axis (panels (c), (f), and (i)) when a Maxwell–Boltzmann approximation is used for the electrons (dark gray line) compared to a full PIC simulation, but with a smaller simulation volume (orange line). The plasma model for the case shown is the diamagnetic cavity case for a 67P-like comet and v  s/c  = 10 km s−1. Note that the ions are modeled as PIC in both simulations.
Paper: Spacecraft Charging Simulations of Probe B1 of Comet Interceptor during the Cometary Flyby
Authors: S. Bergman, Y. Miyake, S. Kasahara, F. L. Johansson, P. Henri
Figure caption: The resulting charge density of ions (panels (a)–(b)), warm electrons (panels (c)–(d)), and cold electrons (panels (e)–(f)) when a Maxwell–Boltzmann approximation is used for the electrons (panels (a), (c), and (e)) compared to a full PIC simulation, but with a smaller simulation volume (panels (b), (d) and (f)). The plasma model used is the diamagnetic cavity case for a 67P-like comet and v  s/c  = 10 km s−1. A cut in the x–z plane is shown. Note that the ions are modeled as PIC in both simulations.
Paper: Cosmological Tensions and the Transitional Planck Mass Model
Authors: Joshua A. Kable, Giampaolo Benevento, Graeme E. Addison, Charles L. Bennett
Figure caption: We include DES Y1 cosmic shear, galaxy–galaxy lensing, and galaxy clustering measurements, collectively referred to as the 3 × 2 point analysis in fits of the TPM model. In all cases, we use scale cuts on the DES data to remove nonlinear scales as we do not have a TPM model theory for the nonlinear collapse of dark matter. Additionally, we fix the TPM parameter c 0 = 0, which corresponds to the TPM f(R) case, as well as σ = 1 for numerical reasons. The inclusion of DES Y1 3 × 2 data do not significantly tighten the constraints on the TPM model parameters compared to the existing constraints from the CMB, BAO, and supernova data. Similar to the inclusion of the RSD data, the DES Y1 3 × 2 data restricts some of the non-Gaussian tail for S 8.
Paper: Spacecraft Charging Simulations of Probe B1 of Comet Interceptor during the Cometary Flyby
Authors: S. Bergman, Y. Miyake, S. Kasahara, F. L. Johansson, P. Henri
Figure caption: The resulting potential field around the spacecraft in the solar wind ion cavity (λ  D =1.0 m, U  s/c  = −4.7 V) and the diamagnetic cavity (λ  D =0.09 m, U  s/c  = −4.5 V) for a 67P-like comet at v  s/c  = 10 km s−1. The same potential surfaces are shown in both cases, corresponding to a potential of −4.0, −3.5, −3.0, −2.5, −2.0, −1.5, −1.0, and −0.5 V.
Paper: Spacecraft Charging Simulations of Probe B1 of Comet Interceptor during the Cometary Flyby
Authors: S. Bergman, Y. Miyake, S. Kasahara, F. L. Johansson, P. Henri
Figure caption: (a) The spacecraft model used for the SPIS simulations. (b) Illustration of the location of the spacecraft with respect to the comet and the Sun in the solar wind simulation. (c) Same as panel (b), but for the flyby simulations.
Paper: Spacecraft Charging Simulations of Probe B1 of Comet Interceptor during the Cometary Flyby
Authors: S. Bergman, Y. Miyake, S. Kasahara, F. L. Johansson, P. Henri
Figure caption: Balance of currents to and from the spacecraft surface for the solar wind simulation.
Paper: Spacecraft Charging Simulations of Probe B1 of Comet Interceptor during the Cometary Flyby
Authors: S. Bergman, Y. Miyake, S. Kasahara, F. L. Johansson, P. Henri
Figure caption: Balance of currents to and from the spacecraft surface for environments corresponding to (a) a 67P-like comet at the cometopause, (b) a 67P-like comet in the solar wind ion cavity, (c) a 67P-like comet in the diamagnetic cavity, (d) a Halley-like comet in the magnetic pile-up region, (e) a Halley-like comet at the exobase and (f) a Halley-like comet in the diamagnetic cavity. v  s/c  = 10 km s−1 in all cases.
Paper: Spacecraft Charging Simulations of Probe B1 of Comet Interceptor during the Cometary Flyby
Authors: S. Bergman, Y. Miyake, S. Kasahara, F. L. Johansson, P. Henri
Figure caption: Resulting potential profiles along the z-axis obtained with EMSES at a high flyby velocity. For the blue line only SEE is included, while the gray line shows the result when also SIE is included. The environment corresponds to a 67P-like comet in the solar wind ion cavity.
Paper: Spacecraft Charging Simulations of Probe B1 of Comet Interceptor during the Cometary Flyby
Authors: S. Bergman, Y. Miyake, S. Kasahara, F. L. Johansson, P. Henri
Figure caption: Same as Figure 6, but for v  s/c  = 70 km s−1.
Paper: Polarization of Intrabinary Shock Emission in Spider Pulsars
Authors: Andrew G. Sullivan, Roger W. Romani
Figure caption: 3D visualization of the IBS flow and magnetic structure we consider in this paper. Here the pulsar (red dot), in this case a redback, is wrapped by the IBS (fading gray surface). The IBS is viewed from an inclination i = 90° at the orbital phase Φ = 0.58. The blue arrows mark the bulk flow directions ﹩\hat{v}﹩, and the green arrows show the magnetic field vectors  b  for the shock-modified cylindrical model. For the flow model, the blue arrows also represent the magnetic field vectors. The green arrows with heads ending on the blue vectors are from the far side, viewed through the IBS. The lower right corner shows the preshock cylindrical field around the pulsar. The magenta rings denote the magnetic field lines, and the black arrow represents the orbital angular momentum axis; these strongly recycled spider pulsars are assumed to be spin-aligned.
Paper: Polarization of Intrabinary Shock Emission in Spider Pulsars
Authors: Andrew G. Sullivan, Roger W. Romani
Figure caption: IBS flux (top), polarization degree (middle), and polarization angle (bottom) for i = 40° (left), i = 60° (center), and i = 80° (right) for the cylindrical magnetic field model in the uncooled power-law part of the spectrum. The polarization angle 0° corresponds to the polarization vector  e  aligned with the orbital angular momentum vector of the binary projected onto the sky plane. The IBS model was computed with β = 5, f  v  = ∞, p = 1, Γ0 = 1.1, and k = 0.2.
Paper: Polarization of Intrabinary Shock Emission in Spider Pulsars
Authors: Andrew G. Sullivan, Roger W. Romani
Figure caption: IBS flux (top), polarization degree (middle), and polarization angle (bottom) for i = 40° (left), i = 60° (center), and i = 80° (right) for the flow model of the magnetic field. The conventions and model parameters are the same as in Figure 2.
Paper: Polarization of Intrabinary Shock Emission in Spider Pulsars
Authors: Andrew G. Sullivan, Roger W. Romani
Figure caption: The magnetic field flow model flux, polarization degree, and polarization angle as in Figure 3, zoomed in around the first peak. The dashed line in each panel marks the orbital phase of the flux peak.
Paper: Polarization of Intrabinary Shock Emission in Spider Pulsars
Authors: Andrew G. Sullivan, Roger W. Romani
Figure caption: Effects of synchrotron spectral features on the light curve (left), polarization degree (middle), and polarization angle (right), here for the cylindrical model at i = 60° with the same parameters as in Figure 2. The line types show the spectral bands that are dominated by three spectral regimes: the low-energy uncooled power law (PL), the intermediate range, in which a cooled power law (cPL) dominates, and a high-energy range that is sensitive to the exponential tail (ET) of the IBS spectrum. Note that the polarization degree grows as the spectrum steepens at high energy.
Paper: Polarization of Intrabinary Shock Emission in Spider Pulsars
Authors: Andrew G. Sullivan, Roger W. Romani
Figure caption: Sweepback-induced distortion of IBS light curves (left), polarization degree (middle), and polarization angle (right) with the same parameters (except f  v ) as in Figure 3. f  v  describes the speed of the companion wind and is hence inversely proportional to the sweepback distortion. The curves show the flow of the magnetic field model at i = 60°.
Paper: Intriguing Plasma Composition Pattern in a Solar Active Region: A Result of Nonresonant Alfvén Waves?
Authors: Teodora Mihailescu, David H. Brooks, J. Martin Laming, Deborah Baker, Lucie M. Green, Alexander W. James, David M. Long, Lidia van Driel-Gesztelyi, Marco Stangalini
Figure caption: Si X/S X results. From left to right: Hinode EIS Si X 258.38 Å intensity, Hinode EIS Si X 258.38 Å/S X 264.22 Å line ratio, SDO AIA DEM in the log(T/K) = 6.0–6.2 and the log(T/K) = 6.2–6.4 temperature bins (computed using the method developed by Hannah & Kontar 2012, 2013). The boxes indicate the locations of the macropixels for this diagnostic.
Paper: Intriguing Plasma Composition Pattern in a Solar Active Region: A Result of Nonresonant Alfvén Waves?
Authors: Teodora Mihailescu, David H. Brooks, J. Martin Laming, Deborah Baker, Lucie M. Green, Alexander W. James, David M. Long, Lidia van Driel-Gesztelyi, Marco Stangalini
Figure caption: SDO HMI continuum emission and photospheric magnetic field evolution of AR 12665, every 12 hours, prior to and during the Hinode/EIS scans. Red (blue) contours represent areas of HMI line-of-sight photospheric magnetic field strength above (below) 200 G (−200 G). Yellow contours represent values below 25,000 counts s−1 in the continuum emission, indicating the location of the sunspot umbrae.
Paper: Intriguing Plasma Composition Pattern in a Solar Active Region: A Result of Nonresonant Alfvén Waves?
Authors: Teodora Mihailescu, David H. Brooks, J. Martin Laming, Deborah Baker, Lucie M. Green, Alexander W. James, David M. Long, Lidia van Driel-Gesztelyi, Marco Stangalini
Figure caption: SDO AIA 193 Å passband images at the times matching the middle time of the EIS raster scans. Yellow contours represent values below 25,000 counts s−1 in the continuum emission, indicating the location of the sunspots. Black dotted (dashed) lines indicate representative examples of loops belonging to the new (preexisting) loop populations.
Paper: Intriguing Plasma Composition Pattern in a Solar Active Region: A Result of Nonresonant Alfvén Waves?
Authors: Teodora Mihailescu, David H. Brooks, J. Martin Laming, Deborah Baker, Lucie M. Green, Alexander W. James, David M. Long, Lidia van Driel-Gesztelyi, Marco Stangalini
Figure caption: SDO AIA 193 Å context image of target AR 12665 on 2017 July 9 at 03:59 UT.
Paper: Intriguing Plasma Composition Pattern in a Solar Active Region: A Result of Nonresonant Alfvén Waves?
Authors: Teodora Mihailescu, David H. Brooks, J. Martin Laming, Deborah Baker, Lucie M. Green, Alexander W. James, David M. Long, Lidia van Driel-Gesztelyi, Marco Stangalini
Figure caption: Predictions of the ponderomotive force model. The first row shows the variation with height of the following parameters: (a) electron temperature and density, (b) ionization fraction for low-FIP elements, and (c) ionization fraction for high-FIP elements. The second row shows the variation with height of (d) downward and upward fluxes of Alfvén wave energy for waves of assumed coronal origin, (e) ponderomotive acceleration, and (f) FIP bias relative to H in the case of resonant fractionation. The third row shows the variation with height of (g) fluxes of Alfvén wave energy—the downward and upward fluxes are identical, (h) ponderomotive acceleration, and (i) FIP bias relative to H in the case of nonresonant fractionation.
Paper: Intriguing Plasma Composition Pattern in a Solar Active Region: A Result of Nonresonant Alfvén Waves?
Authors: Teodora Mihailescu, David H. Brooks, J. Martin Laming, Deborah Baker, Lucie M. Green, Alexander W. James, David M. Long, Lidia van Driel-Gesztelyi, Marco Stangalini
Figure caption: Ca XIV/Ar XIV results. From left to right: Hinode EIS Ca XIV 193.87 Å intensity, Hinode EIS Ca XIV 193.87 Å/Ar XIV 194.40 Å line ratio, SDO AIA DEM in the log(T/K) = 6.4–6.6 and the log(T/K) = 6.6–6.8 temperature bins (computed using the method developed by Hannah & Kontar 2012, 2013). The boxes indicate the locations of the macropixels for this diagnostic.
Paper: On the Distances to the X-Ray Binaries Cygnus X-3 and GRS 1915+105
Authors: M. J. Reid, J. C. A. Miller-Jones
Figure caption: Plan-view model of the Milky Way after Reid et al. (2019), indicating the locations of Cyg X-3 (black dot) and four massive, young stars with water masers (red letters) associated with the Outer spiral arm (red lines) between Galactic longitudes 70° and 100° and with parallax distances from very long baseline interferometry astrometry. A is G097.53+3.18 (Hachisuka et al. 2015; Reid et al. 2019), B is G095.05+3.97 (Sakai et al. 2020), C is G075.30+1.32 (Sanna et al. 2012), and D is G073.65+0.19 (Reid et al. 2019). V LSR values in kilometers per second for the masers are indicated next to their positions; each is uncertain by about ±10 km s−1.
Paper: On the Distances to the X-Ray Binaries Cygnus X-3 and GRS 1915+105
Authors: M. J. Reid, J. C. A. Miller-Jones
Figure caption: Peculiar (noncircular) components of motion of Cyg X-3 as a function of its (unknown) line-of-sight velocity component (V LSR): U pec toward the Galactic center (red), V pec in the direction of Galactic rotation (blue), and W pec toward the north Galactic pole (green). The 3D magnitude of the peculiar motion is plotted in black and has a minimum of 8 km s−1 at V LSR = −64 km s−1. The V LSR range for the motion magnitude being >20 km s−1 is shown by dotted–dashed lines. Our parallax distance of 9.67 kpc is assumed.
Paper: On the Distances to the X-Ray Binaries Cygnus X-3 and GRS 1915+105
Authors: M. J. Reid, J. C. A. Miller-Jones
Figure caption: Likelihoods for three components of motion, V LSR in (blue), Galactic longitude (red solid line), and latitude (red dashed line), as a function of distance for Cyg X-3. The product of the three likelihoods is shown in black, indicating a distance of 8.95 ± 0.96 kpc. The parallax distance reported in this paper is indicated with the π symbol, and its 68% and 95% confidence ranges are indicated with solid and dotted lines above it. The distance range for the Outer spiral arm along the line of sight is indicated below the distance axis.
Paper: On the Distances to the X-Ray Binaries Cygnus X-3 and GRS 1915+105
Authors: M. J. Reid, J. C. A. Miller-Jones
Figure caption: Proper motions of four massive, young stars with water masers (red symbols) and Cyg X-3 (black symbols) as a function of Galactic longitude. Source names are given below their measurements along with letter codes used in Figure 5 (Sanna et al. 2012; Hachisuka et al. 2015; Reid et al. 2019; Sakai et al. 2020). Open circles indicate motions in the easterly direction, and filled squares indicate motions in the northerly direction. The young stars, which are associated with the Outer spiral arm of the Milky Way and straddle Cyg X-3 in Galactic longitude, have motions consistent with that of Cyg X-3.
Paper: On the Distances to the X-Ray Binaries Cygnus X-3 and GRS 1915+105
Authors: M. J. Reid, J. C. A. Miller-Jones
Figure caption: Likelihoods for three components of motion, V LSR in (blue), Galactic longitude (red solid line) and latitude (red dashed line), as a function of distance for GRS 1915+105. The product of the three likelihoods is shown in black, indicating a distance of 9.4 ± 0.6 (statistical) ± 0.8 (systematic) kpc. The parallax-based distance from Reid et al. (2014) is indicated with the π symbol, and its 68% confidence range is given above it. The range of distances for spiral arms along the line of sight is indicated below the distance axis.
Paper: On the Distances to the X-Ray Binaries Cygnus X-3 and GRS 1915+105
Authors: M. J. Reid, J. C. A. Miller-Jones
Figure caption: Parallax data and fits for Cyg X-3. Left panel: sky view with east and north offsets. Middle panel: east (data and fitted solid line) and north (data and fitted dashed line) positions vs. time. Right panel: same as middle panel, but with fitted proper motion removed to highlight the parallax effect. Error bars of 1σ include systematic uncertainty added in quadrature with the formal fitting uncertainties, yielding χ 2 per degree of freedom near unity in each coordinate.
Paper: On the Distances to the X-Ray Binaries Cygnus X-3 and GRS 1915+105
Authors: M. J. Reid, J. C. A. Miller-Jones
Figure caption: VLBA contour map of Cyg X-3 at 43 GHz on 2017 May 14 when the source was weakest. Contour levels are −0.5, 0.5, 1.0, 2.0, 3.0, 4.0, and 5.0 mJy. A 0.5 mas FWHM beam is shown as the shaded disk at the bottom left. The brightest component, near (0.2, −0.5) mas, was used for fitting the parallax.
Paper: Explaining the Chemical Inventory of Orion KL through Machine Learning
Authors: Haley N. Scolati, Anthony J. Remijan, Eric Herbst, Brett A. McGuire, Kin Long Kelvin Lee
Figure caption: Relative energies of sulfur (thiirane, thioacetaldehyde, syn-/anti-vinyl mercaptan) and oxygen (oxirane, acetaldehyde, syn-/anti-vinyl alcohol) isomeric families plotted with respect to their predicted column densities (annotated with each molecule). Detected optically thick molecules are indicated with crosses. The corresponding table (right) provides the structures for each molecule, as well as a visualization of the isomeric families and the isoelectronic pairs.
Paper: Explaining the Chemical Inventory of Orion KL through Machine Learning
Authors: Haley N. Scolati, Anthony J. Remijan, Eric Herbst, Brett A. McGuire, Kin Long Kelvin Lee
Figure caption: Workflow of the supervised machine learning methodology, beginning with molecular structures as SMILES string representations and ending with column density predictions. The strings are encoded into a vector chemical space using the VICGAE embedder. The vectors are then fed into a pretrained model where the target outputs (N col) are generated. String representations of counterfactual structures produced with the EXMOL package (Wellawatte et al. 2022) can also be transformed and provided as outputs.
Paper: Explaining the Chemical Inventory of Orion KL through Machine Learning
Authors: Haley N. Scolati, Anthony J. Remijan, Eric Herbst, Brett A. McGuire, Kin Long Kelvin Lee
Figure caption: Base molecules and corresponding counterfactual structures generated with our modified EXMOL procedure. From top to bottom, we provide two counterfactuals (center and right) for the base molecules silicon monosulfide (SiS), vinyl cyanide (CH2CHCN), and glycine (NH2CH2COOH). Additions or “swaps” within the molecule are highlighted in blue, while mutations via subtraction are indicated in red. The predicted column densities are reported in units of log10 cm−2. Cosine similarity scores are also provided for each counterfactual.
Paper: Explaining the Chemical Inventory of Orion KL through Machine Learning
Authors: Haley N. Scolati, Anthony J. Remijan, Eric Herbst, Brett A. McGuire, Kin Long Kelvin Lee
Figure caption: Model performance examined by observed column densities plotted against model predictions. The training and testing split of the data set is indicated by the light blue (training) and dark blue (testing) scatter points. For clarity of visualization, only the original data points have been plotted (i.e., bootstrapped data points were omitted from the plots).
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: Zero-point corrected parallax vs. total proper motion for 658 stars in our sample. The LMC is the obvious clump of stars in the lower left corner. We show the box used to select these stars in red.
Paper: Explaining the Chemical Inventory of Orion KL through Machine Learning
Authors: Haley N. Scolati, Anthony J. Remijan, Eric Herbst, Brett A. McGuire, Kin Long Kelvin Lee
Figure caption: Uncertainty estimations for gradient boosting and random forest regressions were calculated using an ensembling method to calculate the average predicted column density value for each molecule within the data set. The average predicted value is plotted against the reported observed value. Error bars reflect uncertainty within 1σ.
Paper: Explaining the Chemical Inventory of Orion KL through Machine Learning
Authors: Haley N. Scolati, Anthony J. Remijan, Eric Herbst, Brett A. McGuire, Kin Long Kelvin Lee
Figure caption: Observed column densities plotted against model predictions with respect to each environment within the Orion KL source (top). The individual regions (bottom) are plotted with the same slope = 1 line to indicate linearity in the model performance.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: Left: comparison between ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ values for Y21 stars derived in this work and ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ derived using J − K  S  photometry using the relations from N12 (blue points) and Britavskiy et al. (2019b; orange points, RSGs only). The one-to-one line is shown in black. The J − K  S  temperatures show significantly more scatter around ﹩\mathrm{log}{T}_{\mathrm{eff}}\approx 3.9\mbox{--}4.0﹩. Right: ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ values derived in this work as a function of J − K  S . Points are colored by 2MASS J-band magnitude. The sixth-order J − K  S –﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ relation from N12 is shown in blue. The scatter in the left panel at warmer temperatures is naturally explained between the steepness of the relation at higher effective temperatures and the overall faintness of these warmer stars in the near-infrared, resulting in noisier J − K  S  measurements.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: H-R diagram for the combined N12 (black points) and Y21 catalog (all others). Orange points fall outside of the temperature range of the training sample (OOB stars). Blue/green points are the stars whose luminosities are brighter/fainter than the minimum-luminosity training star in a narrow ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ bin. The black cross in the lower right indicates the typical uncertainties in the training set. We use vertical black lines to divide the H-R diagram into RSGs, YSGs, and BSGs based on effective temperature. Gray lines show nonrotating, Z = 0.006 evolutionary tracks for 7, 9, 12, 15, 20, 25, 32, and 40 M ⊙ stars from Eggenberger et al. (2021) for comparison.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: A breakdown of the luminosity functions of YSGs and BSGs, demonstrating the change in slope as a function of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ (normalized at ﹩\mathrm{log}L/{L}_{\odot }=4.5﹩). This sample excludes OOB and low-L stars. The black line is for all stars for reference, while the colored lines are for the stars in the temperature bins indicated in the legend (with the number of stars in each bin in parentheses), with the temperature of the bin increasing from yellow to blue.