adsabs/AstroCLIMB huggingface dataset:
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Schematic diagram for the varying branches of merger trees constructed between snapshots n − 1, n, and n + 1. The gray shades are self-bound structures, the diamonds present the MBPs in the self-bound structures, and the colored ellipses are galaxies in them. The black solid arrows indicate main progenitor/descendant relations, dotted arrows mark the mass transfers between the structures with no main progenitor/descendant relations, and the dashed lines indicate mergers along the main descendant branches. The green solid arrows show the backtracking of the MBPs to repair the branches broken by structure misidentification, and the red solid arrow marks the main progenitor‒descendant branch repaired by the MBP backtracking scheme.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Same as in Figure 3, but for galaxies at z = 5. Only half the sample in x < 0.5L box, where L box is the side length of the HR5 volume, is plotted here to make the figure less saturated.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Flowchart showing the morphology classification scheme. We first classify galaxies into symmetric and asymmetric ones using the asymmetry parameter and divide the symmetric galaxies into disks, spheroids, and irregulars based on their radial stellar-mass-density profile parameterized by the Sérsic index ﹩{n}_{{\rm{S}}\acute{{\rm{e}}}\mathrm{rsic}}﹩. Galaxies that are not fitted to the Sérsic profile are classified as irregulars together with the asymmetric ones.
Paper: Magnetohydrodynamic Waves in an Asymmetric Magnetic Slab with Different External Flows
Authors: Noémi Kinga Zsámberger, Carmen M. Sánchez Montoya, Róbert Erdélyi
Figure caption: Phase speed of waves in a symmetric magnetic slab with no flows in any region, prepared using background parameter values of c 0 = 11 km s−1, v A = 12 km s−1, c  e  = 8 km s−1, ρ  e /ρ 0 = 2.41. The real (imaginary) parts of the solutions are plotted in blue (red).
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Overview of A2744 showing the HST F606W image of the cluster, with the MUSE footprint shown by the black square. Locations of the different cluster regions as defined in Owers et al. (2011) are overlaid as colored circles, the RPS and PSB galaxies are shown by the black and red diamonds, respectively. The arrow marks the BCG used as the center for this analysis and the black X marks the X-ray surface-brightness peak measured by Owers et al. (2011).
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Overview of A370 showing the HST F606W image of the cluster, with the MUSE footprint shown by the black square. RPS and PSB galaxies are shown by the black and red diamonds, respectively. The arrow marks the point between the two BCGs used as the center for this analysis.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Plot of the outer and full centroid covariance parameters for galaxies within A2744 and A370 combined, derived as described in the text. The median and the standard deviation of the centroid covariance within each category are shown as error bars marked with the relevant color or symbol. Galaxies are colored accordingly as described in the color–magnitude diagrams, Figure 1, and marked as described in Figure 8.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Values of precision and recall calculated across the range of selection thresholds for PC1. The selected value of 4.3, chosen in the analysis, is close to the crossover between the two diagnostics as well as the peak in the precision.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Variance of the top five principal components yielded by the PCA. The horizontal dashed line shows the cutoff of 11.1%, below which a principal component was not used, as described in Section 5.2.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Example morphology diagnostics and segmentation maps, showing some cases where a galaxy has a close neighbor and some deblending has been required to produce the segmentation map.
Paper: Magnetohydrodynamic Waves in an Asymmetric Magnetic Slab with Different External Flows
Authors: Noémi Kinga Zsámberger, Carmen M. Sánchez Montoya, Róbert Erdélyi
Figure caption: Changes in the phase speed of trapped oscillations in a slab of intermediate width (kx 0 = 1) caused by changing the flow speed on one side of the slab (M  A2 = u 2/v A) while keeping the flow speed on the other side fixed. The real part of the phase speed values is displayed in blue, while the imaginary part is shown in red. The Alfvén Mach numbers used to obtain these solutions were M A0 = 0, M A1 = −0.1, while M A2 changed from −1.5 to 1.5, representing both up- and downflows on the right-hand side of the slab.
Paper: Magnetohydrodynamic Waves in an Asymmetric Magnetic Slab with Different External Flows
Authors: Noémi Kinga Zsámberger, Carmen M. Sánchez Montoya, Róbert Erdélyi
Figure caption: Dispersion diagrams, where green (blue) lines show the real part of the quasi-kink (quasi-sausage) mode phase speeds, and red lines display their imaginary parts. The slab and its environment have background flows of Alfvén Mach numbers (a) M A0 = 0, M A1 = 0.15, and M A2 = 0.65 and (b) M A0 = 0, M A1 = −0.1, and M A2 = −0.35. The hatched areas represent regions where there are no trapped solutions.
Paper: Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra
Authors: Nickolay Y. Gnedin
Figure caption: Example of a synthetic line of sight containing a dark gap of length 192h −1cMpc. The bottom panel shows the profiles of the total baryon number density (blue) and neutral hydrogen number density (red). This line of sight crosses a DLA system at x ≈ 70h −1cMpc. The middle panel shows the slice through the computational volume at a random orientation perpendicular to the synthetic line of sight. The slice shows the gas density with the logarithmic stretch between 1 + δ = 0.1 (blue) and 1 + δ = 10 (red) and with higher/lower values capped to the values at the bounds (10/0.1 respectively). The line of sight mostly goes along the filaments, avoiding large voids (blue colors), except a part of the void just next to the DLA. The top panel shows the synthetic spectrum without noise in red and the same spectrum with the Gaussian noise added. The noise level in the data is low enough to avoid noise spikes breaking the dark gap artificially.
Paper: Magnetohydrodynamic Waves in an Asymmetric Magnetic Slab with Different External Flows
Authors: Noémi Kinga Zsámberger, Carmen M. Sánchez Montoya, Róbert Erdélyi
Figure caption: Equilibrium configuration of the slab. Red arrows indicate the external flows, while blue arrows show the internal magnetic field.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Phase-space diagram for the cluster member galaxies in the MUSE FoV of A2744 (left) and A370 (right). Galaxies within the color–magnitude red sequence are shown as red points. Galaxies below the red sequence are shown in blue, with galaxies bluer than 0.6 on the color–magnitude diagram highlighted as larger circles. The KDEs of the red and blue galaxy distributions are shown in respectively colored contours. Our sample of RPS galaxies is shown as black stars, while the PSB galaxies are shown as black squares. The vertical gray dashed line denotes the 100% completeness radius described in the text. The vertical histograms show the velocity distributions of each cluster, with the same vertical axis as the phase-space diagrams. The blue and red histograms show the blue and red populations accordingly, with the light gray histogram showing the combined total. A2744, left: marked as dashed black lines are the reference velocities of the X-ray gas (v gas), the SMRC (v SMRC), and the velocity of both the NC and CTD (v NC,CTD), from Owers et al. (2011). A2744_01 and A2744_07 are marked as both RPS and PSB, for the reasons described in Section 2.4. The cluster is clearly bimodal in velocity distribution from the histogram, and the majority of blue galaxies and RPS galaxies are located in the blueshifted component. A370, right: black dashed lines indicate the reference velocities of the northern and southern BCGs, from (Lagattuta et al. 2019), as explained in the text. From the velocity histogram, the cluster appears to have a comparably singular velocity distribution in contrast to A2744 and the two merging components do not appear to be significantly separated. Furthermore, the blue galaxies are distributed across a wider range of velocities compared with the red galaxies. The RPS galaxies, PSB galaxies, and the majority of the bluest galaxies with F606W-F814W > 0.6 are generally situated at extremes in velocity with respect to the observed component of the cluster.
Paper: Radio Jet Proper-motion Analysis of Nine Distant Quasars above Redshift 3.5
Authors: Yingkang Zhang, Tao An, Sándor Frey, Krisztina Éva Gabányi, Yulia Sotnikova
Figure caption: Naturally weighted images of the nine high-redshift sources after deep cleaning, derived from our VLBA observations at 8.4 GHz in 2017. The lowest contours represent ±4 times of the rms noise, and the positive contour levels increase by a factor of 2. The image parameters are listed in Table B2. The green crosses mark the optical positions detected by Gaia, and the bar length is three times the Gaia positional errors reported in https://gea.esac.esa.int/archive.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Color–magnitude diagrams for A2744 (left) and A370 (right), showing all cluster members within the central regions of each cluster covered by the observations. Red galaxies are classified as described in the text (Section 2.3) and marked as red squares. Other galaxies are divided into those with F606W-F814W > 0.6, marked as light blue diamonds, and those with F606W-F814W < 0.6, marked as blue circles. The red dashed line denotes the linear regression fitted to the red sequence galaxies. The gray shaded region indicates the magnitude limit of 25.5 applied in both the F606W and F814W bands.
Paper: Radio Jet Proper-motion Analysis of Nine Distant Quasars above Redshift 3.5
Authors: Yingkang Zhang, Tao An, Sándor Frey, Krisztina Éva Gabányi, Yulia Sotnikova
Figure caption: The apparent proper-motion–redshift (μ–z) diagram based on the latest VLBI observations of radio jets. Downward-pointing triangles: this work; upward-pointing triangles: from the literature, see Table 3; circles: Piner et al. (2012) measured at 8.4 GHz; squares: Britzen et al. (2008) measured at 5 GHz; plus signs: Lister et al. (2021) measured at 15 GHz. The solid lines represent the maximum apparent speed ﹩{\beta }_{\mathrm{app},\max }﹩ with the given bulk Lorentz factors Γ = 20 and 40.
Paper: Radio Jet Proper-motion Analysis of Nine Distant Quasars above Redshift 3.5
Authors: Yingkang Zhang, Tao An, Sándor Frey, Krisztina Éva Gabányi, Yulia Sotnikova
Figure caption: Spectral index maps of our sample, based on simultaneous 2.3 and 8.4 GHz observations. In each map, the background contours represent the 2.3 GHz image. They start from three times its rms noise and increase by a factor of 2. The bottom-left ellipses are the restored beams of the 2.3 GHz map and the epochs used for the imaging are shown at the bottom right.
Paper: Radio Jet Proper-motion Analysis of Nine Distant Quasars above Redshift 3.5
Authors: Yingkang Zhang, Tao An, Sándor Frey, Krisztina Éva Gabányi, Yulia Sotnikova
Figure caption: (a) Proper motions of the fitted jet components. For each line, the left panel is a sketch map of the component motions with respect to the core component (marked with a star). The middle panel represents the change of the relative radial distances of the components. The right panel is the corresponding position angle change. (b) Jet proper motions. (c) Jet proper motions.
Paper: A Mass Model for the Lensing Cluster SDSS J1004+4112: Constraints from the Third Time Delay
Authors: R. Forés-Toribio, J. A. Muñoz, C. S. Kochanek, E. Mediavilla
Figure caption:  χ 2 contours and profiles for the virial mass, concentration, and inner slope parameters of the generalized NFW model (Equation (1)). Red lines and points mark the values for which the χ 2 is minimized, orange lines delimiter the 1σ contours, and green lines the 2σ contours. The black (gray) shadow is the 1σ (2σ) region.
Paper: A Mass Model for the Lensing Cluster SDSS J1004+4112: Constraints from the Third Time Delay
Authors: R. Forés-Toribio, J. A. Muñoz, C. S. Kochanek, E. Mediavilla
Figure caption: Critical curves and images positions for the four background sources. The green dots mark the observed positions of the images. Circles denote the quasar, A1, B1, and C1 images, squares represent the images of A2, B2, and C2, and lastly the triangles mark the A3 images. Additionally, images are color coded depending on their flux, from the brightest in red to the dimmest in yellow.
Paper: A Mass Model for the Lensing Cluster SDSS J1004+4112: Constraints from the Third Time Delay
Authors: R. Forés-Toribio, J. A. Muñoz, C. S. Kochanek, E. Mediavilla
Figure caption: The left panel shows the Hubble Space Telescope Advanced Camera for Surveys (ACS)/WFC (GO-9744, PI: C. Kochanek) images of the lens. The right panel shows the reconstructed mass distribution on a logarithmic scale along with the images positions: quasar in white, galaxy group A in lime-green, B in blue, and C in turquoise. The orientation for both figures is north up, west right.
Paper: Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra
Authors: Nickolay Y. Gnedin
Figure caption: Probability distribution function for gaps of different lengths per unit redshift for the DC = −1 and DC = 0 CROC simulations (as in Figure 3 but without noise). For each simulation I show a distribution ﹩L/{L}_{0}{e}^{-L/{L}_{0}}﹩ of line segments that can be placed in between randomly distributed hard spheres, with two different values of L 0 for each run that correspond to two commonly used variations of the void abundance model, as described in the text.
Paper: Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra
Authors: Nickolay Y. Gnedin
Figure caption: Distributions of mean opacities in 50h −1cMpc skewers (left) and probability distribution functions for gaps of different lengths (right) for per-unit redshift for gaps whose central redshifts fall in the redshift bin [5.9, 6.1]. Blue and red lines show the DC = −1 and DC = 0 CROC simulations, respectively, as in the previous figures. The purple line (shown in the right panel only) is for the DC = −1 run with Voigt profiles replaced by Doppler profiles in synthetic spectra. Orange and green lines are for the two artificial fixes for the DC = −1 run described in the text.
Paper: Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra
Authors: Nickolay Y. Gnedin
Figure caption: Top: sketch of the possible “fixes” for reconciling the DC = −1 run with the observed distribution of mean opacities. Black bars sketch a piece of the spectrum in the original DC = −1 run. Red lines show a “fix A,” with more transmitted flux at high gas densities, below the gap detection threshold (so that the gap distribution is unaffected but the mean opacity is). Blue lines are for deeper, more transparent voids, with more transmitted flux in already existing spikes that also does not affect the gap distribution. Bottom: the actual spectrum from the DC = −1 run shown in black, with colored spectra implementing fixes A and B sketched above.
Paper: Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra
Authors: Nickolay Y. Gnedin
Figure caption: Left: cumulative distributions for observational signal-to-noise ratios for the Zhu et al. (2021) sample at different redshifts. These distributions need to sampled properly in order to compare simulation results with the data. Right: dark gap distributions for the DC = −1 run with and without Gaussian noise at z = 6. The noise level in the observational data is low enough not to affect the dark gap distribution appreciably.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Fraction of age that galaxies spend their lives as spheroids (top), fraction of stellar mass increased during mergers (middle), and rotational velocity to velocity dispersion ratio at z = 6 (bottom) as a function of the height ν pk of the initial dark-matter overdensity peak matched to galaxies. Density peaks are defined on the “galaxy” scale of R  G  = 0.35 cMpc. The blue and red dots in the top and middle panels are the fractions integrated through z = 6 and 4, respectively, after their stellar mass reaches 2 × 109 M ⊙. The left panels are for the galaxies with M ⋆ = 5−6 × 109 M ⊙, and the right panels for those with M ⋆ > 6 × 109 M ⊙ at z = 6. Median curves and their uncertainty limits are given.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Alignment between the initial angular momentum and angular momentum of the total mass (top panels), angular momentum of stellar particles (middle) and the minor axis of the moment of inertia of the stellar-mass distribution (bottom) as functions of the magnitude of the initial angular momentum (left column) and spin parameter ﹩\lambda ^{\prime} ﹩ (middle column). Histograms are shown on the right. Galaxies with M ⋆ > 2 × 109 M ⊙ at z = 6 are used. The initial angular momentum is strongly aligned with the total angular momentum of galaxies.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Fraction of age that galaxies spend their lives as spheroids (top), stellar-mass fraction increased during mergers (middle), and rotational velocity to velocity dispersion ratio of stars at z = 6 (bottom) as a function of the initial angular momentum (in arbitrary units). Blue and red points in the top and middle panels are the fractions integrated through z = 6 and 4, respectively, after their stellar mass reaches 2 × 109 M ⊙. The left panels are for the galaxies with M ⋆ = 5−6 × 109 M ⊙, and the right panels for those with M ⋆ > 6 × 109 M ⊙ at z = 6.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Fraction of age that galaxies have spent their lives as spheroids by z = 6 (top) and 4 (bottom) after their stellar mass reaches M ⋆ = 2 × 109 M ⊙. The abscissa is the fraction of stellar mass increased through mass jumps typically accompanied by mergers (see the text). The blue and red dots indicate galaxies having M ⋆ = 5 − 6 × 109 M ⊙ and M ⋆ > 6 × 109 M ⊙ at z = 6, respectively. There are 44 (20) blue and 38 (18) red points at the origin out of a total 278 (146) points in the upper (lower) panel. The dashed curves present the medians at given f mass,merger, and error bars are the uncertainties of the medians.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: An 1.5 cMpc-thick slice of a relatively high-density region in HR5 showing gas density and stars (left) and dark matter (right) from z = 10 to 4. Gas density is higher in redder shades. Whitish gray dots in the left illustrate stellar-mass distribution. The white arrows show the velocity field of gas in dense areas. The black arrows at dense cores mark the spin direction of galaxy stellar-mass projected on the slice. The spin direction perpendicular to the slice (clockwise or counterclockwise rotation) is also shown on top of the spin arrows. Numbers are logarithmic stellar mass (left) and dark-matter halo mass (right) in M ⊙ units. The areas where dark-matter velocity field is shown are the same as in the gas-density plot.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Fraction of age that galaxies spend their lives as spheroids (top) and stellar-mass fraction increased during mergers (bottom) integrated through z = 6 (blue) and 4 (red) because galaxy mass reaches M ⋆ = 2 × 109 M ⊙. The abscissa is the initial background overdensity contrast (﹩{\delta }_{\mathrm{initial},\mathrm{bg}}\,\equiv ({\rho }_{\mathrm{DM}}/{\bar{\rho }}_{\mathrm{DM}}-1)/{\sigma }_{{DM}}﹩) smoothed with a top-hat filter over the “protocluster” scale of R TH = 4 cMpc.