adsabs/AstroCLIMB huggingface dataset:
Paper: High-redshift Galaxy Candidates at z = 9–10 as Revealed by JWST Observations of WHL0137-08
Authors: Larry D. Bradley, Dan Coe, Gabriel Brammer, Lukas J. Furtak, Rebecca L. Larson, Vasily Kokorev, Felipe Andrade-Santos, Rachana Bhatawdekar, Maruša Bradač, Tom Broadhurst, Adam Carnall, Christopher J. Conselice, Jose M. Diego, Brenda Frye, Seiji Fujimoto, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Intae Jung, Guillaume Mahler, Stephan McCandliss, Masamune Oguri, Marc Postman, Keren Sharon, M. Trenti, Eros Vanzella, Brian Welch, Rogier A. Windhorst, Adi Zitrin
Figure caption: JWST NIRCam detection image, comprised of a weighted sum of all NIRCam LW images (F277W, F356W, F410M, F444W), of the WHL0137−08 cluster field. The field of view is ﹩\sim 2\buildrel{\,\prime}\over{.} 3\times 2\buildrel{\,\prime}\over{.} 3﹩, and the image is shown with north up and east left. The location of the strongly lensed z ∼ 9 high-redshift candidate in the WHL0137−08 cluster field is indicated with a red ellipse. The locations of the other high-redshift candidates are shown in Figure 2.
Paper: High-redshift Galaxy Candidates at z = 9–10 as Revealed by JWST Observations of WHL0137-08
Authors: Larry D. Bradley, Dan Coe, Gabriel Brammer, Lukas J. Furtak, Rebecca L. Larson, Vasily Kokorev, Felipe Andrade-Santos, Rachana Bhatawdekar, Maruša Bradač, Tom Broadhurst, Adam Carnall, Christopher J. Conselice, Jose M. Diego, Brenda Frye, Seiji Fujimoto, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Intae Jung, Guillaume Mahler, Stephan McCandliss, Masamune Oguri, Marc Postman, Keren Sharon, M. Trenti, Eros Vanzella, Brian Welch, Rogier A. Windhorst, Adi Zitrin
Figure caption: An 8.″5 × 5.″5 cutout image from the JWST NIRCam detection image showing the z ∼ 9 arc WHL0137–ID13362 (red outline), with a magnification of μ ∼ 8. The arc is 2.″4 long, has at least two bright star-forming knots, and is the most spatially resolved arc at z ∼ 9 known to date. A potential fainter counterimage of the arc, with a similar color and photometric redshift, is also shown outlined in blue.
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: Mean M/L s sampled by the hierarchical model for the Local Group galaxies. All galaxies have M/L of approximately 1 (﹩\mathrm{log}M/L\approx 0﹩), which is near what is expected based on Bell et al. (2003).
Paper: High-redshift Galaxy Candidates at z = 9–10 as Revealed by JWST Observations of WHL0137-08
Authors: Larry D. Bradley, Dan Coe, Gabriel Brammer, Lukas J. Furtak, Rebecca L. Larson, Vasily Kokorev, Felipe Andrade-Santos, Rachana Bhatawdekar, Maruša Bradač, Tom Broadhurst, Adam Carnall, Christopher J. Conselice, Jose M. Diego, Brenda Frye, Seiji Fujimoto, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Intae Jung, Guillaume Mahler, Stephan McCandliss, Masamune Oguri, Marc Postman, Keren Sharon, M. Trenti, Eros Vanzella, Brian Welch, Rogier A. Windhorst, Adi Zitrin
Figure caption: Same as Figure 3, but for the high-redshift galaxy candidates WHL0137–ID10060 and WHL0137–ID13362.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the time evolution of the main physical quantities at 1 au at Earth’s position for the propagation of the reference spheromak CME with positive handedness. The time is the number of physical days that lasted the simulation. The blue line shows the minimum of activity case, while the orange line shows the maximum of activity case. From top to bottom, we show the radial velocity (in kilometers per second), the proton number density (per cubic centimeter), the temperature (in units of 10,000 kelvin), the total magnetic field (in nanotesla), the z components of the magnetic field in HEEQ coordinates (in nanotesla) and the plasma beta parameter. The arrival of the shock is shown by a vertical line (light blue for the minimum of activity case, red for the maximum of activity case). The crossing of the ejecta is shown by a colored window (light purple for the minimum of activity, light red for the maximum of activity). We also show the vertical deviation at 5° and 10° north and south of the ecliptic plane as colored shaded areas around the curves.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the time evolution of the main physical quantities at 1 au at Earth’s position for the propagation of the cone CME. The time is the number of physical days that lasted the simulation. The blue line shows the minimum of activity case, while the orange line shows the maximum of activity case. From top to bottom, we show the radial velocity (in kilometers per second), the proton number density (per cubic centimeter), the temperature (in units of 10,000 kelvin), the total magnetic field (in nanotesla ), and the plasma beta parameter. The arrival of the shock is shown by a vertical line (light blue for the minimum of activity case, red for the maximum of activity case). The crossing of the ejecta is shown by a colored window (light purple for the minimum of activity, light red for the maximum of activity).
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the meridional view of the ICME at the minimum of activity depending on the input radial speed. Each panel shows the meridional cut passing across Earth in the simulation (in the x–z plane in HEEQ coordinates) when the ICME reaches Earth (blue point at 1 au). We show the density in order to visualize the magnetic ejecta as an under-density. The left panel shows the case for the median spheromak CME (Section 6.1), the middle panel the case for the reference spheromak CME (Section 5), and the right panel the case for the cone CME (Section 4.2). Each panel has the input CME speed at 0.1 au as a label. See Table 1 for a reminder of all the differences between the models. We see then that the faster the CME is, the more delay we observe between the equatorial and the polar parts of the ejecta, which means it is caused by the equatorial solar wind deceleration.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the time evolution of the background solar wind parameters at 0.11 au (left panel) and 1 au (right panel) along the Sun–Earth axis. The first row shows the total velocity in kilometers per second, the second row the number density per cubic centimeter, and the last row the radial magnetic field component in nanotesla. The curves for the minimum of activity are in blue, while the curves for the maximum of activity are in orange. Gray rectangles have been added to show the time intervals when the background solar wind is likely to interact with the ICME.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the 3D HCS structure for the selected minimum (left panel) and maximum of activity (right panel). The HCS contour is shown in dark blue. For context, the ecliptic plane with the radial velocity is shown in transparency. The position of Earth is indicated by a blue sphere. Both figures are in the HEEQ frame.
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: (a) Perspective rendering of field lines for an example timestep in the ξ = 0.4 model. The height of the TR is illustrated by the purple outline. (b) Cumulative probability distributions of ﹩\cos \alpha ﹩ for each of the 11 models. (c) Median (50% percentile) and ±1 standard deviation limits (16% and 84% percentiles) for the distributions of ﹩\cos \alpha ﹩ for each value of ξ. Curve colors in (b) agree with symbol colors in (c).
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: Ensemble-averaged reflection coefficients (dashed curves) and transmission coefficients (solid curves), with Alfvén-, fast-, and slow-wave properties shown in black, blue, and red, respectively. (a) Dependence on B 0 for ξ = 0.7 and Model I. (b) Dependence on ξ for B 0 = 10 G and Model I. Values of f (i.e., totals for all four non-Alfvénic components) are shown with purple symbols.
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: (a) Transmission (positive) and reflection (negative) coefficients for Alfvén waves produced at the TR for a Model I Monte Carlo ensemble with B 0 = 10 G and ξ = 0.7. (b) Same as panel (a), but for fast-mode MHD waves. (c) Same as panel (a), but for slow-mode MHD waves. Symbol color denotes ﹩\cos \alpha ﹩, as shown in the color bar.
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: (a) Radial dependence of characteristic velocities such as the sound speed c  s  (green dotted–dashed curve), Alfvén speed V A (black dashed curve), and angle-averaged group velocities for fast-mode (blue solid curve) and slow-mode (red solid curve) waves. (b) Radial dependence of flux-tube area A (black solid curve) and collisional damping rates for fast-mode (blue) and slow-mode (red) waves, with both total values computed with Pedersen conductivity (solid curves) as well as the fully ionized Braginskii limit (dashed curves).
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: (a) Radial dependence of wave velocity amplitudes for fast-mode waves (blue curves), slow-mode waves (red curves), and Alfvénic turbulence from the time-steady model (black dotted curve). For magnetosonic modes, both undamped (dashed) and damped (solid) amplitudes are shown. (b) Radial dependence of volumetric heating rates due to fast-mode waves (blue curves), slow-mode waves (red curves), and Alfvénic turbulence (black dotted curve).
Paper: Proton Synchrotron Origin of the Very-high-energy Emission of GRB 190114C
Authors: Hebzibha Isravel, Asaf Pe'er, Damien Bégué
Figure caption: Colors represent the value of the magnetization parameter ϵ  B  (in logarithmic scale) as a function of the ambient density, n 0, and total energy, E 53, from Equation (17) for the time bin centered at 90 s. In making the plot, we assumed ϵ  p  = 0.8 and display the results for three different values of ξ  p , namely, ξ  p  = 10−2, 10−1, and 1, respectively, presented from left to right. The thin black lines represent the combination of parameters that result in ϵ  B  = 10−1, 10−2, and 10−3.
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: Peak heating rates due to the damping of fast-mode waves (blue curve) and slow-mode waves (red curve), produced at the TR, as a function of B 0 for ξ = 0.7 and Model I. Vertical struts at B 0 = 10 G show how the peak heating rate changes when other wavenumber anisotropy models are applied (Models S or T). The typical heating rate due to incompressible Alfvénic turbulence at the TR is also shown (black dotted curve).
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: Ensemble-averaged reflection and transmission coefficients, with line styles and colors the same as in Figure 6. In order to illustrate the dependences on wavenumber anisotropy, we use dotted lines to connect identical parameters.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 340+0
Authors: Yash Bhargava, Sudip Bhattacharyya, Jeroen Homan, Mayukh Pahari
Figure caption: Plots involving fluxes of GX 340+0 as observed with AstroSat. Left panel: the ratio of the Comptonized flux to the blackbody flux in 6–20 keV as a function of the total flux in 3–20 keV. This panel reproduces the HB, the hard apex, and the NB of the observed Z track qualitatively (see Section 4.3). Right panel: evolution of bolometric flux (in 0.01–100 keV) values of blackbody and Comptonizing corona throughout HID zones. This panel shows that the blackbody becomes weaker and the corona becomes stronger from the hard apex to the HB (see Section 4.4).
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Flowchart of our visual classification process. The classification is based on four basic questions that can produce a simple disk/spheroid/peculiar/compact classification and additional flags regarding whether the source is smooth or structurally rich.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 340+0
Authors: Yash Bhargava, Sudip Bhattacharyya, Jeroen Homan, Mayukh Pahari
Figure caption: The power density spectrum for each HID zone with the same color scheme used in Figure 1. The excess power in the single bin at the 50 Hz is instrumental. HBOs and NBO are seen in zones 1–4 and zone 5, respectively (see Table 1).
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 340+0
Authors: Yash Bhargava, Sudip Bhattacharyya, Jeroen Homan, Mayukh Pahari
Figure caption: The QPO fractional rms amplitude vs. energy plot for all HID zones (HBOs for zones 1–4 and NBO for zone 5). QPOs are detected for all four energy bands in 3–20 keV only for zone 1.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Effective radius (R  n ) (top), axis ratio (b/a) (middle), and information entropy (bottom). We show key measurements that provide clues to differences most used by the classifiers for the spheroid and other classes. Spheroids are defined by their lack of structure, low elongation, and small sizes in general.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 340+0
Authors: Yash Bhargava, Sudip Bhattacharyya, Jeroen Homan, Mayukh Pahari
Figure caption: The frequency–time image of GX 340+0 with the colors indicating the variability of the source. The light curve of the source (same as in Figure 1) is shown in black points. The two deep HB excursions are clearly visible. The instrumental feature at 50 Hz is persistently present.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Rest-frame optical images for sources in our sample. The three panels show the three main classes disks, spheroids, and peculiars, respectively. Galaxies are ordered horizontally by redshift, from lowest on the left to highest on the right. Stamps are shown in square-root normalization. Redshifts are from Duncan et al. (2019) based on the CANDELS fields.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Redshift distribution of the sample (top). Numbers on top of each bar describe the galaxy counts in that redshift bin. Stellar mass–redshift distribution (bottom). The dashed line shows the stellar mass threshold at ﹩\mathrm{log}({M}_{\odot }/{M}_{* })=9﹩ used to divide the sample into two stellar mass bins. This threshold is close to the mean stellar mass of the whole distribution.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Example of the workflow outlined in Section 3.4, showing the last seven steps of the algorithm for one sample halo (Left). At each step, a rotation axis fit is determined for each snapshot grouping (represented by snapshot numbers 0–24, corresponding to TNG50 snapshots 75–99), and a fit ﹩{\chi }_{\nu }^{2}﹩ is measured using 16. The information criterion (IC) for all the snapshot groupings is measured using Equation (17), and the next level is formed by merging the snapshot groupings that least increase the new fit ﹩{\chi }_{\nu }^{2}﹩. The optimal snapshot groupings are selected as those with the minimum IC, which occurs in this example for n  c  = 3, implying that this halo has at most three coherent rotation epochs. The example halo shown here is the same halo used in Figure 3. It should be noted that the reduced ﹩{\chi }_{\nu }^{2}﹩ is undefined for snapshot groupings containing only two snapshots, because the degrees of freedom ν = 0. (Right) shows the evolution of the halo minor axis polar angle (θ) and azimuthal angle (ϕ) over time in the simulation box frame, colored by the rotation epochs found using our algorithm. The dashed lines show the angles predicted by the best-fit planes and pattern speeds. The different epochs of rotation found by our algorithm are visible in these panels as changes in slope that disrupt the otherwise approximately linear evolution.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Example of the single-axis fitting process described in Section 3.3. The plots to the left show the tracks traced out by each of the three principal axes during a stable rotation period as viewed from a position along the rotation axis shown in cyan (top left), from a position perpendicular to the rotation (bottom left), and from an arbitrary viewing angle (bottom middle). The motion of the principal axes are described well by three parallel planes, as discussed in Section 3.3. The figure to the right shows the localization of the rotation axis in the halo body frame (represented by an octant showing spherical-polar angles θ, ϕ) using Equation (16). The plot is colored by the change in the fit χ 2 as the rotation axis orientation deviates from the best-fit value. Δχ 2 = 1 corresponds approximately to a 1σ threshold on the orientation of the rotation axis. In this example, our methodology recovers the orientation of the rotation axis to within ∼5°.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Intermediate axis orientation uncertainties plotted against halo shape (left column) and number of particles (middle column) for a subsample of 10,000 random TNG50 DM-only, TNG50 with baryons, and randomly generated AGAMA halos. The right column shows the distributions of halos in the e–p shape parameter space, which are bounded by the triangle with sides e = 1 (fully flat halo), p = e (fully prolate halo), p = − e (fully oblate halo). Overplotted in the left and middle columns is the analytic error prescription defined in Equation (6), assuming an average number of halo particles (left column) and average halo shape (middle column). The errors for the DM-only and DM+B TNG50 runs appear functionally similar, while errors on the AGAMA halos show a similar overall trend with larger scatter. Errors for both TNG50 runs are determined using the jackknife sampling routine described in Section 3.2.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: (Top) Reverse-ordered cumulative histogram showing the fraction of halos whose longest-lived rotation is at least as large as a given duration. This fraction drops faster for halos in the DM+B run of TNG50, indicating a slightly reduced abundance of long-lived rotations compared to the DM-only case. (Bottom) histogram of the number of rotation epochs found for each TNG50 run. The number of found epochs is similar for both runs, suggesting that the differences in the top panel histograms cannot be explained by a difference in the number of rotation epochs.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Halo mass function of the selected halo catalog for the DM-only (blue) and DM+baryon (orange) TNG50 runs compared to the full DM+B TNG50 simulation mass function. Our selection criteria omit halos with large mass accretion rates, thereby preferentially selecting lower-mass halos.
Paper: The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies
Authors: Alessia Moretti, Paolo Serra, Cecilia Bacchini, Rosita Paladino, Mpati Ramatsoku, Bianca M. Poggianti, Benedetta Vulcani, Tirna Deb, Marco Gullieuszik, Jacopo Fritz, Anna Wolter
Figure caption: CO (2–1) spectra normalized to the peak temperature for the sources with an S/N > 3. The red Gaussian is the best fit. The blue solid line shows the optical velocity, while the orange dashed one shows the H I velocity. The gray shaded region is the rms of the observations in the plot range, after excluding the line emission.
Paper: The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies
Authors: Alessia Moretti, Paolo Serra, Cecilia Bacchini, Rosita Paladino, Mpati Ramatsoku, Bianca M. Poggianti, Benedetta Vulcani, Tirna Deb, Marco Gullieuszik, Jacopo Fritz, Anna Wolter
Figure caption: Optical maps from OmegaWINGS (Gullieuszik et al. 2015) for the galaxies that have been classified as having a star-forming tail. The red contours show the radio H I emission from MeerKAT corresponding to 1, 2, 4, 8×  the lowest column density level (in atoms cm−2) shown within each map. The red ellipse in the lower left corner is the MeerKAT beam. The grayscale insets show the UVIT data, when available. Black circles in each map and inset are the APEX pointings. Green contours show the ionized gas emission from MUSE, when available.
Paper: The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies
Authors: Alessia Moretti, Paolo Serra, Cecilia Bacchini, Rosita Paladino, Mpati Ramatsoku, Bianca M. Poggianti, Benedetta Vulcani, Tirna Deb, Marco Gullieuszik, Jacopo Fritz, Anna Wolter
Figure caption: Optical maps from OmegaWINGS (Gullieuszik et al. 2015) for the galaxies that have been classified as having no star formation in the tail. Colors and symbols are as in Figure 1.