adsabs/AstroCLIMB huggingface dataset:
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: [O II] kinematics for the three galaxies in our sample with the lowest velocity dispersion in our sample J1244 (top left-hand four panels), J1558 (top right-hand four panels), and J1713 (bottom four panels). In every four panels, we show in the top left-hand the [O II] central velocity (v 50); in the top right-hand the [O II] velocity dispersion (σ), in the bottom left-hand the [O II] maximum redshifted velocity (v 02); in the bottom right-hand [O II] maximum blueshifted velocity (v 98). All velocities of the ionized gas are relative to the systemic redshift of the source. The color bars show the velocity in km s−1. The axes are labeled in kpc from the brightest spaxel.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Velocity dispersion σ map of the [O II] emission for J0826, J1107, J1244, and J1341. Velocity profiles of representative spaxels are shown in the insets, highlighting areas with high and low velocity dispersion. In the velocity profiles and spectra, the black line is the continuum-subtracted spectrum, the red-solid line is the total emission-line model, and the blue-dashed lines are the [O II] emission-line models for the individual doublet components.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Velocity dispersion σ map of the [O II] emission for J1613 and J1622. See Figure 10 for more details. In addition, orange-dashed lines are the emission-line models for the broad kinematic components.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: —Same as in Figure A1
Paper: Radial Wave in the Galactic Disk: New Clues to Discriminate Different Perturbations
Authors: Chengye Cao, Zhao-Yu Li, Ralph Schönrich, Teresa Antoja
Figure caption: Shape and phase shift between particles of the L  Z  − 〈V  R 〉 wave with different orbit hotness in the Gaia DR3 data. The green line is the L  Z −〈V  R 〉 wave of the whole sample. The L  Z −〈V  R 〉 wave patterns composed of dynamically cold (J  Z  < 3 km s−1 kpc) and hot (J  Z  > 12 km s−1 kpc) populations are depicted in red and blue lines, respectively. The brown dashed line displays the phase shift amplitude (ΔL  Z , shown in the right axis) variation pattern, which peaks at around 2100 km s−1 kpc.
Paper: Radial Wave in the Galactic Disk: New Clues to Discriminate Different Perturbations
Authors: Chengye Cao, Zhao-Yu Li, Ralph Schönrich, Teresa Antoja
Figure caption: Temporal evolution of the modeled Galactic disk after the external satellite perturbation. The upper and lower rows are number density and the mean radial velocity 〈V  R 〉 map in the X–Y plane. The evolution times of the four snapshots are 1400, 1600, 2000, and 3400 Myr from left to right. The first and second pericenter passages are at around 1 and 3.1 Gyr, respectively. As phase mixing proceeds, the spiral arms become more tightly wound.
Paper: Radial Wave in the Galactic Disk: New Clues to Discriminate Different Perturbations
Authors: Chengye Cao, Zhao-Yu Li, Ralph Schönrich, Teresa Antoja
Figure caption: The orbit of the Sgr-like satellite in our test particle simulations, following the prescription in Section 3.1. The circles and crosses represent the orbits of the satellite before and after reducing its mass from 2.5 × 1010 M ⊙ to 1 × 1010 M ⊙. Each point is color coded with time at an interval of 50 Myr. The bold gray line represents the Milky Way disk.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: (a) Time–distance map of thread No.10. The blue pluses trace the local maximum of the thread, and the magenta line is the fitting result. The two blue dashed lines are parallel to the pluses with a fixed distance as the thread width of 1.1 Mm. (b) The black line represents the intensity curve integrated between the two dashed lines in panel (a). The green line corresponds to the smoothed intensity curve, obtained using a window size of 10 pixels. (c) The black line represents the original intensity curve subtracted from the smoothed component in panel (b). The magenta line is the fitting result using Equation (1).
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Oscillations at multiple positions of the thread enclosed by the cyan box in Figure 1. (a) Image of the thread at 06:48:39 UT. (b)–(e) Time–distance maps corresponding to different perpendicular slits, as marked by the solid cyan lines in (a). The vertical red line represents the thread time shown in (a). The distance between slits is about 1.8 Mm (15 pixels). The oscillation periods and phases are also given.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Similar to Figures 3(a), (c) but for thread No.9 (a), thread No.13 (b), thread No.15 (c), and thread No.24 (d) to show the displacement oscillation with the amplitude expansion.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Examples of the thread intensity PSD (blue) and best fit (red solid) of MCMC simulations. The red dashed lines are the 95% confidence level. Pink dashed–dotted lines mark the 200 s as the artificial lower limits. The Gaussian components indicate the intensity oscillation periods. Top panels show the fitting with M 0, and bottom panels show the fitting with M 1 of same thread. ﹩{\rm{\Delta }}{\mathrm{BIC}}_{{M}_{1}-{M}_{0}}﹩ are shown in the lower-left corner of bottom panels.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Scatter plots of correlation between the periods (a) and amplitudes (b) of seven threads exhibiting both the displacement and intensity oscillations. The Spearman’s rank coefficients (ρ) and p-value are given.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Similar to Figures 6(b), (c) but for all eight threads exhibiting intensity oscillations.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Histograms of the displacement oscillation periods (a), drifting velocities (b), and damping times (c). (d) Histogram of the intensity oscillation periods. The mean values are given.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Normalized intensity curves of 35 threads in Figure 2.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Similar to Figure 8 but for the other 30 threads, and only the preferable model fitting is shown.
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Schematic of (a) a Bonnor–Ebert (BE) sphere and (b) a turbulent equilibrium sphere (TES). The latter is a member of a family of exact equilibrium solutions to the angle-averaged equations of hydrodynamics, in which the velocity field is decomposed into bulk and turbulent motions, where the latter is assumed to be isotropic and obey a power-law linewidth–size relationship (see Sections 2 and 3). Both the BE sphere and TES solution families possess a critical radius r crit, such that for r > r crit the equilibrium is unstable to radial perturbations (Section 4). The widely used observational core radius R FWHM is comparable to r crit only when the underlying turbulence is very weak (i.e., close to the BE sphere), as will be shown in Figure 9. Vertical arrows represent line-of-sight projection, which shows that the observed linewidth may contain a nonthermal component even at the center of the core (discussed in Section 6.2).
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Density profiles of TESs with linewidth–size slope p = 0.5, for selected dimensionless sonic radii ξ  s  = ∞ (solid), 7 (dashed), and 3 (dotted–dashed). The profile with ξ  s  = ∞ is identical to the BE solution, while those with smaller ξ  s  correspond to turbulent equilibria (higher-amplitude turbulence for smaller ξ  s ). The density is normalized with respect to the central density ρ  c .
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: (a) Density profiles of the critical TESs with p = 0.5, for selected mass-weighted average velocity dispersions of σ 1D = 0 (brown; equivalent to the critical BE sphere), c  s  (yellow), and 2cs (cyan). The density is normalized to the density at the edge ﹩{\rho }_{e}=\left\langle \rho \right\rangle (r={r}_{\mathrm{crit}})﹩, and the radius is normalized to the gravitational radius defined in Equation (4), at the mean core density ﹩\overline{\rho }={M}_{\mathrm{crit}}/(4\pi {r}_{\mathrm{crit}}^{3}/3)﹩. (b) Density profiles of highly turbulent TESs with σ 1D = 10c  s , for selected linewidth–size index p = 0.3 (dashed), 0.5 (solid), and 0.7 (dotted). (c) The local power-law slope ﹩q\equiv -\partial \mathrm{ln}\rho /\partial \mathrm{ln}r﹩ for the curves shown in panels (a) and (b). The squares mark the point where q = 2p for each curve: the turbulent pressure gradient force is compressive (supportive) on the left (right) side of this marker. (d) The relative strength of the gravitational force compared to the thermal or turbulent pressure gradient force (the larger of the two). The maximum value ﹩{ \mathcal R }=2﹩ is reached when f thm = f trb. On the left and right sides of this peak, ∣f thm∣ > ∣f trb∣ and ∣f thm∣ < ∣f trb∣, respectively. The triangles mark the location of the sonic radius.
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Parametric dependence of the critical TES properties on the dimensionless sonic radius ξ  s , for p = 0.3 (dashed), 0.5 (solid), and 0.7 (dotted–dashed). (a) The dimensionless critical radius ξ crit. (b) The dimensionless critical mass m crit. (c) The critical density contrast u crit (left axis) and ﹩{({\rho }_{c}/{\rho }_{e})}_{\mathrm{crit}}\equiv \exp ({u}_{\mathrm{crit}})﹩ (right axis). (d) The mass-weighted average turbulent Mach number σ 1D/c  s . In panels (a)–(c), the corresponding critical values for the BE limit (i.e., ξ  s  → ∞ ) are plotted in dotted lines.
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Dependence of the physical properties of a critical TES on the internal turbulent Mach number σ 1D/c  s , for p = 0.3 (dashed), 0.5 (solid), and 0.7 (dotted–dashed). (a) The critical mass normalized by the gravitational mass M  G  (Equation (3)) evaluated at the mean core density ﹩\overline{\rho }={M}_{\mathrm{crit}}/(4\pi {r}_{\mathrm{crit}}^{3}/3)﹩. (b) The critical radius normalized by the gravitational radius R  G  (Equation (4)) evaluated at ﹩\bar{\rho }﹩. (c) The critical center-to-edge density contrast (black, left axis) and the ratio of the mean density to the edge density (red, right axis). (d) The ratio between the free-fall time to crossing time at the mean core density. The blue dashed lines in panels (a)–(c) plot analytic approximations given in Equations (58)–(60). The gray bands in panels (a) and (b) plot the BE mass and radius resulting from a naive substitution ﹩{c}_{s}\to {({c}_{s}^{2}+{\sigma }_{1{\rm{D}}}^{2})}^{1/2}﹩ in Equations (1)–(4).
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: (a) The ratio of the central free-fall time to the free-fall time defined at the average density ﹩\overline{\rho }\equiv 3{M}_{\mathrm{crit}}/(4\pi {r}_{\mathrm{crit}}^{3})﹩. The blue dashed line plots an analytic approximation provided in Equation (62). (b) The ratio of R FWHM computed from the column density profile to r crit. Both quantities are plotted against the internal turbulent Mach number σ 1D/c  s  of a critical TES for turbulent power-law index p = 0.5.
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: (a) The ratio of the critical radius to the gravitational length scale ﹩{R}_{G}={c}_{s}/({G}^{1/2}{\rho }_{c}^{1/2})﹩ (see Equation (4) for dimensional conversion) as a function of ﹩{\rho }_{c}/{\rho }_{c,\min }={({\xi }_{s}/{\xi }_{s,\min })}^{2}﹩, for a TES with turbulence index p = 0.5. (b) A similar ratio for the critical mass and the gravitational mass scale ﹩{M}_{G}={c}_{s}^{3}/({G}^{3/2}{\rho }_{c}^{1/2})﹩. The corresponding ratios for the critical BE sphere are shown as dashed lines in each panel. A core with ﹩{\rho }_{c}/{\rho }_{c,\min }\lt 1﹩ cannot collapse because the critical radius and mass for instability is undefined. When ﹩{\rho }_{c}/{\rho }_{c,\min }\gt 1﹩, a core may collapse, provided its outer radius and mass exceed r crit and M crit, respectively, as shown here.
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Schematic illustration of two alternative evolutionary scenarios for a nascent core. The first scenario leads to collapse/star formation (path A: (A1)→(A2)→(A3)); the second to dispersal (path B: (B1)→(B2)→(B3)). (A1) A core begins to form in the region where turbulent flows are locally converging. (A2) The forming core becomes dense enough and/or turbulence sufficiently dissipates such that r crit becomes smaller than the maximum radius r max of a core (beyond which gas belongs to other structures). (A3) The core undergoes outside-in collapse as the region near r crit becomes unstable. (B1) A core begins to form by weakly converging flows. (B2) The core approaches quasi-equilibrium, but its critical radius lies outside the maximum radius because of weak initial compression and/or strong local turbulence. (B3) The core is subsequently torn apart by turbulence rather than collapsing because the region inside r max is stable.
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Comparison of the internal structures of a critical BE sphere (gray dashed), critical logotrope (blue dotted–dashed), and critical TES with p = 0.5 (orange solid). (a) The radial density profile normalized to the edge density. Both the logotrope and TES have the mass-weighted average velocity dispersion σ 1D = c  s . The corresponding parameters are A = 0.337 for the logotrope and ξ  s  = 6.42 for the TES. (b) The turbulent Mach number vs. radius. The locations of critical radii are marked with circles. Panels (c) and (d) are similar to (a) and (b), respectively, but with higher velocity dispersion σ 1D = 2c  s ; the corresponding parameters for the logotrope and TES are A = 0.235 and ξ  s  = 3.42, respectively.
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Radial profiles of the angle-averaged density (blue solid line, left axis) for TES solutions with (a) ξ  s  = ∞ , i.e., zero turbulence, (b) ξ  s  = 7, i.e., low turbulence, and (c) ξ  s  = 3, i.e., higher turbulence. For all three panels, p = 0.5. Also shown is the dimensionless bulk modulus K (Equation (38); red line, right axis); positive values are shown solid and negative dotted. In each panel, the point at which K first becomes negative is marked with a blue circle. This is the critical solution; solutions with smaller radii are stable and those with larger radii are unstable.
Paper: Theory of Turbulent Equilibrium Spheres with Power-law Linewidth–Size Relation
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Column density profiles of the critical TESs with p = 0.5. Solid, dashed, and dotted lines correspond to internal turbulent Mach numbers σ 1D/c  s  = 0, 1, and 2, respectively. The column density Σ is normalized to its central value Σ c . The profiles extend to r crit, and the observational core radius R FWHM is marked with triangles.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Summary of process for data preparation. (A) Level 1 (L1) generated using SECCHI software. This data set includes a 2048 × 2048 pixel image, unpolarized and calibrated in units of average solar radiance along the x- and y-axes. Source: C. DeForest et al. (2018). (B) Illustration of coordinate resampling. The system of image coordinates is converted from Cartesian to polar coordinates, e.g., the conversion of L2 into L3. (C) Level 7 (L7) image, representing one of the final phases of the data preparation. The image shows the solar corona outflow in polar coordinates (ϕ, r), with radiance adjusted by r 3. Source: C. DeForest et al. (2018). (D) Representation of the coordinate transformation for J-maps. These maps were produced by selecting a thin sector or segment from a series of solar images and aligning these segments vertically in time order. J-maps serve to illustrate the kinematic progression of solar events across time and space. (E) STEREO-A/COR2 DT map. This map illustrates the temporal and spatial progression of features. The inclines on the map indicate the velocity of the features for that particular segment.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Analysis of a sinusoidal velocity profile. (a) Black dashes show the simulated velocity profile, characterized by a sinusoidal wave, which was used to produce SynCOM images; blue: the surfing velocity profile, which uses the surfing transform to integrate the DT plot along a dynamic spatiotemporal path encompassing various possible speeds (V. M. Uritsky et al. 2013); green: the correlation velocity profile, which determines a time delay to maximize the correlation peak; red: the interpolated correlation velocity profile, an enhanced version of the correlation method where the peak is derived from the second derivative of a third-order polynomial. (b) The differences between simulated and measured speeds. The speed difference for the TDC is highlighted in red, and the speed difference for the ST is shown in blue.
Paper: Embedded Young Stellar Objects near H72.97-69.39: A Forming Super Star Cluster in N79
Authors: Omnarayani Nayak, Conor Nally, Alec S. Hirschauer, Olivia C. Jones, Jeroen Jaspers, Laura Lenkić, Margaret Meixner, Nolan Habel, Megan Reiter, Laurie Chu, Patrick J. Kavanagh, Massimo Robberto, B. A. Sargent
Figure caption: YSO candidates in H72.97-69.39 colorized by mass overplotted on the F1000W filter. There are 13 YSOs with masses greater than 8 M ⊙ (pink circles), 27 with masses between 3 and 8 M ⊙ (green squares), 27 with masses between 2 and 3 M ⊙ (orange triangles), 31 with masses between 1 and 2 M ⊙ (cyan star shape), and four with masses less than 1 M ⊙ (red squares). The red-dashed line represents arc-like structures along which star formation is taking place.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Analysis of velocity measurement errors. (a) Probability distribution histograms for the velocity discrepancy using two approaches, the ST in blue and the TDC in red. The histograms highlight differences in peak shape and distribution characteristics, with calculations of mean, standard deviation, and median. (b) Semi-log graph showing log p vs. velocity discrepancy, showing that the TDC deviates more at the extremes, whereas both methods perform similarly near zero discrepancy.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Example of a SynCOM blob. This representation displays a sample Gaussian blob, designed to emphasize its shape and size. In this instance, the brighter blob stands out in the image, appearing to be centered at angle 301° and extending from 7.2 to 7.6 solar radii.
Paper: Embedded Young Stellar Objects near H72.97-69.39: A Forming Super Star Cluster in N79
Authors: Omnarayani Nayak, Conor Nally, Alec S. Hirschauer, Olivia C. Jones, Jeroen Jaspers, Laura Lenkić, Margaret Meixner, Nolan Habel, Megan Reiter, Laurie Chu, Patrick J. Kavanagh, Massimo Robberto, B. A. Sargent
Figure caption: Kroupa IMF fit to the mass distribution of the 102 YSO candidates. The total YSO mass is 1965 M ⊙. Assuming a typical formation time of 105 yr, the resulting SFR is 0.02 M ⊙ yr−1.