adsabs/AstroCLIMB huggingface dataset:
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: Keck HIRES [S II] 6731 Å spectral image and derived densities along the minor axis (PA = +347°). (a), (b), and (c) [S II] 6731 Å logarithmic-scale flux of the S-SE rim, CSPN, and N-NW rim spectral images (see slit positions in Figure 1). The slit lengths are 10″, 14″, and 10″ (2.6 pixels arcsec–1), respectively. (d)–(f) Derived electron density P-V maps. The minimum flux cuts are 1.5% for (d), 4% for (e), and 2% for (f), with respect to the absolute maximum fluxes. False dark colors indicate regions with no [S II] flux (that is, those that are very noisy or below the level of the flux minimum or log N e = 2.5 dex), while the false white color on the color bar indicates values exceeding the maximum value (4.6 dex) of the density (but no region exists exceeding this limit) in the P-V maps. The white vertical line is the position of the radial velocity of −48.91 km s−1, determined by the flux median position. The sky blue vertical line is the newly estimated kinematic centroid (see Section 3.2). See the text and Table 3.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Evolution of a typical PIC simulation of the pair-plasma MRI in a small 2D box (﹩2\times 2{\lambda }_{\mathrm{MRI}}^{2}﹩). Left column: spatial distribution of the out-of-plane magnetic field B  y  and of the in-plane field strength ﹩{B}_{\mathrm{pol}}=\sqrt{{B}_{x}^{2}+{B}_{z}^{2}}﹩ at subsequent times during the simulation. Right column: evolution of the change in magnetic energy in all three components of  B  (top) and evolution of the volume-averaged β ∥ = p ∥/[B 2/(8π)] and β ⊥ = p ⊥/[B 2/(8π)] (bottom). The beginnings of different phases characterizing the system evolution (described in the text) are marked with vertical black lines.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: As in Figure 2, but for a large 2D box (﹩32\times 32{\lambda }_{\mathrm{MRI}}^{2}﹩).
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Representation of the hierarchy from microscopic (kinetic) to macroscopic (fluid) length scales that are relevant for kinetic shearing-box simulations of the MRI.
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: Keck HIRES [S II] 6731 Å spectral image and derived densities: (a) 25 minute and (b) 30 minute exposures. The minimum flux cuts with respect to the maximum fluxes are 1.5% for (a) and 2% for (b). See Figure 6 caption and the text.
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: [S II] 6716 Å vs. [S II] 6731 Å flux intensities along a fixed spatial component, i.e., a 4″ sky (see Figure 6(e)). The [S II] 6716 Å (dotted) and [S II] 6731 Å (solid) flux intensities (10−16 erg−1 cm−2 s−1 pixel−1) have been both continuum level and interstellar extinction corrected. The x-axis is the pixel corresponding to the wavelength. See the text and Table 2.
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: A plot of density as a function of slit position. The x-axis indicates the slit position along the slit length (Figure 6(e)), while the y-axis shows the mean density value from the slit position. The mean densities derived along the slit length are 3.69 to 4.09 (±0.14) cm−3, which are much lower than the local density maxima in Figure 6. See the text.
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: The Hubble-type expansion velocities of the main (M) and outer (O) shells along the minor axis with two trend lines, refined from Hyung et al. (2014). When drawing trend and regression lines, He and H data were excluded. See Table 4 and the text.
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Relative variations in ﹩{\dot{M}}_{\mathrm{acc}}﹩, computed from results based on X-Shooter data of this work and Manara et al. (2022), on timescales from hours to 3–4 yr. The different colors represent different timescale variations, as described in the legend. The black crosses show the mean value for each timescale subsample.
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Top: smoothed flux-calibrated spectra of all the epochs. Bottom: smoothed flux-calibrated spectra of all the epochs. All the spectra are normalized and suitably shifted in flux for clarity.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Left: observed 0.3–7.0 keV data with one-eighth binning. Right: the 0.3–7.0 keV radial surface brightness profile centered on the position of the hard 3.0–7.0 keV nuclear source (see the text), compared with that of the Chandra point response function (PSF) in the 0.3–7.0 keV band (red points) for the full 360° sector.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Gas distribution and kinematics as seen in simulations of a tilted (45°) 1044 erg s−1 jet interacting with a gas-rich galactic disk. The jet lies in the X–Z plane. The 2D maps show projections along a line of sight at a 45° angle to the galactic disks (rotation around the Y-axis). Top left: column density map. Top middle: mass-weighted velocity dispersion. Top right: mass-weighted velocity dispersion. Bottom left: a 3D volume rendering of the density of the simulated gas disk (with n > 1 cm−3). Colder gas with T < 5000 K is shown in blue. Hotter gas with T > 5000 K, shown in red, represents dense gas shocked to high temperatures by the jet (in green). Bottom middle: the same as in the left panel but at an orientation closer to an edge-on view. Bottom right: a surface brightness map of the thermal X-ray emission in the energy range 0.1–2 keV from shocks in the dense clouds.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Corner plot illustrating the posterior distribution for our variability model of RR Lyrae And XII - V004614, one of the sparsest sampled light curves in our data set. In addition to the period (P), the light curve is parameterized through a phase (Φ), an amplitude (A), and an intensity-averaged magnitude (M), in each filter. The vertical dashed lines and the plot headers report the 50th, 15.9th, and 84.1th percentiles of the PPD. This is a prototypical example of our posteriors, illustrating that variability parameters are generally well constrained (except for the phase parameters, which we consider nuisance parameters to be marginalized over) even for our more sparsely sampled data.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: RR Lyrae period–amplitude diagrams for our entire sample, ordered by decreasing galaxy luminosity. Galaxy labels are color-coded by whether the amplitude refers to the F475W (blue) or F606W (black) magnitude variation. The purple and cyan points indicate RRab (fundamental mode) and RRc (first-overtone). This homogeneous compilation of period–amplitude diagrams illustrates the diversity of RR Lyrae populations in our galaxy sample, which, in turn, is indicative of a variety of formation histories.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Observed light curves (black points) of three RR Lyrae stars within our sample of 4694 variables, demonstrating representative time-series samplings for our data set. The best-fit template (red line) is overlaid on the observed light curves. The gray lines show 100 random samplings from our MCMC chains, providing an illustration of our model uncertainties. The models are well matched to the data in all cases. The titles and insets list the constraints on the period, amplitude, and mean magnitude of the RR Lyrae star, marginalized over all other model parameters.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Fraction of solutions affected by period aliases, as a function of the number of time-series photometric epochs per filter, at the end of step (iii) (circles), step (iv) (squares), and step (v) (triangles) of our pipeline. Results are shown for the simulated light curves of a long-period RRab star (top panel), a short-period high-amplitude RRab star (middle panel), and an RRc star (bottom panel).