adsabs/AstroCLIMB huggingface dataset:
Paper: Tracking Halo Orbits and Their Mass Evolution around Large-scale Filaments
Authors: Hannah Jhee, Hyunmi Song, Rory Smith, Jihye Shin, Inkyu Park, Clotilde Laigle
Figure caption: The fraction of massive halos within 2 Mpc h −1 from filaments (black circles) compared to its cosmic mean value (gray circles) at different redshifts. It is tested how the massive fraction near filaments changes when the mass evolution is switched off since z = 1 (brown dotted line) and when the inflow of halos to filaments is switched off (magenta dotted line).
Paper: Tracking Halo Orbits and Their Mass Evolution around Large-scale Filaments
Authors: Hannah Jhee, Hyunmi Song, Rory Smith, Jihye Shin, Inkyu Park, Clotilde Laigle
Figure caption: Number fraction of massive (M > 1012  M ⊙ h −1) halos as a function of distance to filaments at z = 0, which shows a clear mass segregation signal. The dashed line indicates the mean fraction of massive halos in the simulation at z = 0.
Paper: Numerical Research on the Effect of the Initial Parameters of CME Flux-rope Model on Simulation Results. III. Different Initial Energy of CMEs
Authors: Yousheng Liu, Fang Shen, Yi Yang, Mengxuan Ma
Figure caption: The schematic of the graduated cylindrical shell (GCS) models with a different half-angle from the cone. (a) α = 30° and δ = 10°; (b) α = 30° and δ = 20°; (c) α = 30° and δ = 30°. The angular width of the GCS model 2ω, the maximum height of the model H  front , and maximum radius of the front R  front  are marked in red in Figure 2(b).
Paper: Tracking Halo Orbits and Their Mass Evolution around Large-scale Filaments
Authors: Hannah Jhee, Hyunmi Song, Rory Smith, Jihye Shin, Inkyu Park, Clotilde Laigle
Figure caption: The distributions of the displacement (r perp(z = 0) − r FC) after the crossing (left), the maximum v perp (middle), and t FC (right) to confirm the contribution of dynamical friction to the mass segregation in Figure 12. The error bars are statistical errors.
Paper: Tracking Halo Orbits and Their Mass Evolution around Large-scale Filaments
Authors: Hannah Jhee, Hyunmi Song, Rory Smith, Jihye Shin, Inkyu Park, Clotilde Laigle
Figure caption: The distributions of excess time of massive halos (blue) and less massive halos (green). The excess time is defined by halo age subtracted by the required time to reach a 2 Mpc h −1 distance from filaments, assuming that halos travel at their initial velocity. Each arrow indicates the peak position.
Paper: Numerical Research on the Effect of the Initial Parameters of CME Flux-rope Model on Simulation Results. III. Different Initial Energy of CMEs
Authors: Yousheng Liu, Fang Shen, Yi Yang, Mengxuan Ma
Figure caption: 3D six-component grid in the spherical coordinate system (Feng et al. 2010).
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: Spectra collected with the Goodman spectrograph on the 4 m SOAR telescope (NOIRLab) for candidate DAWDs that were discarded from our Southern hemisphere sample. The first star is featureless and could be a DC WD, the second and third could be DB degenerates. The last three are magnetic WDs.
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: Single epoch minus the mean instrumental magnitude measurements for the Northern DAWD WDFS0103-00 as a function of observing epoch (black crosses). Averaged and binned relative magnitudes for a set of stable stars of comparable instrumental magnitude in the same FoV are overplotted as a red-shaded area. The variability index of the selected stars and the measurement dispersion are listed. Error bars are shown.
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: Single epoch minus the mean instrumental magnitude measurements for WD0554-165 as a function of observing epoch (black-filled dots). Averaged relative magnitudes for a set of stable stars of comparable instrumental magnitude in the same FoV are overplotted as cyan-filled dots. The 1σ dispersion of the measurements of the stable stars and the DAWD is labeled. Error bars are shown.
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: CALSPEC STIS spectrum of WDFS1514+00 (gray solid line) with overplotted photometric observations from GALEX, SDSS, APASS, Gaia, DECam, PS1, DENIS, UKIRT, 2MASS (black-filled dots). The WISE upper limit measurements are marked with downward-filled triangles.
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: IQR index compared to 1.34 × σ (top panel) and 1/eta index (bottom) vs. cyan average magnitudes from the ATLAS survey for WDFS1314-03 (red star symbol) and ≈100 stars of similar LCO instrumental g magnitude in the same FoV.
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: IQR index compared to 1.34 × σ (top panel) and 1/eta index (bottom) vs. the average g instrumental magnitudes for all the stars in the FoV observed toward WD0554-165. The DAWD is marked with a red star symbol.
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: Same as Figure 7 but for WDFS2351+37.
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption:  χ 2 index vs. instrumental average g magnitude for all stars observed in the FoV toward WD0554-165 (red star).
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: Same as Figure 12 but for star WDFS0228-08.
Paper: Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Annalisa Calamida, Thomas Matheson, Edward W. Olszewski, Abhijit Saha, Tim Axelrod, Clare Shanahan, Jay Holberg, Sean Points, Gautham Narayan, Konstantin Malanchev, Ryan Ridden-Harper, Nicola Gentile-Fusillo, Roberto Raddi, Ralph Bohlin, Armin Rest, Ivan Hubeny, Susana Deustua, John Mackenty, Elena Sabbi, Christopher W. Stubbs
Figure caption: Finding charts for 15 candidate DAWDs based on WFC3 drizzled F160W image cutouts centered on the star and covering an FoV of 26″ × 26″. Star Gaia DR3 magnitude and coordinates are labeled on the image. The yellow solid arrow points at the DAWD and the yellow line indicates 5″ on the image. The north and east directions are also shown.
Paper: The Metallicity and Distance of NGC 2403 from Blue Supergiants
Authors: Fabio Bresolin, Rolf-Peter Kudritzki, Miguel A. Urbaneja
Figure caption: Difference in the metallicities derived from blue supergiants and H II regions as a function of stellar metallicity for a galaxy sample drawn from the literature (after Bresolin et al. 2016) and NGC 2403. The nebular metallicities are increased by 0.1 dex, in order to account for oxygen depletion onto dust grains. The H II region chemical abundances are obtained either from collisionally excited lines (CELs) with the direct method (blue dots) or from O++ recombination lines (RLs, red squares).
Paper: The SDSS-Gaia View of the Color–Magnitude Relation for Blue Horizontal-branch Stars
Authors: Fabrícia O. Barbosa, Rafael M. Santucci, Silvia Rossi, Guilherme Limberg, Angeles Pérez-Villegas, Hélio D. Perottoni
Figure caption: Histograms of ﹩\mathrm{log}\,g﹩. Left column: log g adopted by the pipeline for stars with g 0 < 18 (top) and g 0 > 18 (bottom). Dashed lines are the Gaussian distributions defined by Santucci et al. (2015b). Right column: log g estimates provided by SSPP spectroscopically determined (top) and from ANNRR method (bottom) for all stars.
Paper: The Metallicity and Distance of NGC 2403 from Blue Supergiants
Authors: Fabio Bresolin, Rolf-Peter Kudritzki, Miguel A. Urbaneja
Figure caption: The stellar mass–metallicity relation of local galaxies based on abundance data derived from the analysis of stellar spectral features: blue supergiants (BSG), red supergiants (RSG), super star clusters (SSC), and SDSS galaxies. Predictions from the look-back models of Kudritzki et al. (2021) are included for comparison (green curve).
Paper: The Metallicity and Distance of NGC 2403 from Blue Supergiants
Authors: Fabio Bresolin, Rolf-Peter Kudritzki, Miguel A. Urbaneja
Figure caption: The galactocentric metallicity radial gradient of NGC 2403 from both blue supergiants and H II regions. Blue continuous line: regression determined using the 16 blue supergiants of Table 2, represented by closed (BA) and open (OB) circles. Red dashed line: regression determined using the oxygen abundances of the H II regions (Rogers et al. 2021), represented by small red dots. For the sake of clarity we omit the error bars of the H II region data points. The shaded areas represent the 95% confidence intervals of the fits.
Paper: The Metallicity and Distance of NGC 2403 from Blue Supergiants
Authors: Fabio Bresolin, Rolf-Peter Kudritzki, Miguel A. Urbaneja
Figure caption: Distance modulus offset between TRGB and FGLR determinations as a function of the FGLR distance modulus for 11 galaxies.
Paper: The SDSS-Gaia View of the Color–Magnitude Relation for Blue Horizontal-branch Stars
Authors: Fabrícia O. Barbosa, Rafael M. Santucci, Silvia Rossi, Guilherme Limberg, Angeles Pérez-Villegas, Hélio D. Perottoni
Figure caption: Distribution of classified stars with g 0 < 18 (left) and g 0 > 18 (right) in the surface gravity space. Median errors are indicated in the bottom right corner. Histograms show the distribution of log g from the respective axis for stars classified as BHB and BSS. Colors indicate the probability of being a BHB star.
Paper: The Metallicity and Distance of NGC 2403 from Blue Supergiants
Authors: Fabio Bresolin, Rolf-Peter Kudritzki, Miguel A. Urbaneja
Figure caption: The FGLR in NGC 2403. The data points (stars from Table 2, except for #47) are fitted with the fiducial relation (Equations (7)–(8)), vertically shifted by an amount equivalent to the distance modulus. The fitting relation is represented by the green line.
Paper: The SDSS-Gaia View of the Color–Magnitude Relation for Blue Horizontal-branch Stars
Authors: Fabrícia O. Barbosa, Rafael M. Santucci, Silvia Rossi, Guilherme Limberg, Angeles Pérez-Villegas, Hélio D. Perottoni
Figure caption: Error comparison between fits for colors (g − r)0, (u − g)0, and (u − r)0 from TuringBot.
Paper: Evolution, Structure, and Topology of Self-generated Turbulent Reconnection Layers
Authors: Raheem Beg, Alexander J. B. Russell, Gunnar Hornig
Figure caption: Evolution of the reconnection rate V rec over time. The three general stages are highlighted in different colors: (i) laminar 2.5D phase (blue); (ii) transition (red, striped); and (iii) SGTR (green). The vertical dotted lines mark additional times of interest: (a) 2.5D Sweet–Parker reconnection onset (t = 0.0); (b) 2.5D nonlinear tearing instability onset (t = 0.4); (c) Kink instability of central flux rope (CFR) and turbulent reconnection onset (t = 1.0); (d) CFR breaks down and reconnection layer becomes (almost) fully stochastic (t = 1.5); (e) CFR remnant ejected (t = 2.4); (f) CFR remnant fully absorbed at outflows and “pure” SGTR onset (t = 3.0).
Paper: Evolution, Structure, and Topology of Self-generated Turbulent Reconnection Layers
Authors: Raheem Beg, Alexander J. B. Russell, Gunnar Hornig
Figure caption: Current density strength ﹩j=\parallel {\rm{\nabla }}\times {\boldsymbol{B}}\parallel ﹩  over time. The left column is a cross section at z = 0.0 through the two large flux ropes; the middle column is a slice at y = 0.0 inside the reconnection layer; the right column is a slice at x = 0.0 through the current sheet along the guide-field direction. The top row (t = 1.0) shows three flux ropes on y = 0.0 formed by the tearing instability of the initial current layer. The second row (t = 1.4) is a snapshot during the transition phase while the 3D kink instability of the CFR is developing. The third row (t = 2.4) shows the highly nonuniform reconnection layer during the SGTR phase while the CFR reaches the left outflow. The bottom row (t = 4.5) shows how far the pair of initial large-scale flux ropes have merged at an advanced stage of the simulation during “pure” SGTR.
Paper: The Nonpotentiality of Steady-state Coronal Magnetic Field Derived with Time-relaxation Magnetohydrodynamics Simulations Using Helioseismic and Magnetic Imager Three-component Magnetic Field Data
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: Line-of-sight integration of the current density, viewed from 90° the Carrington longitude and 7° South (approximately corresponding to the Earth-Sun direction at 2011 February 9, 21UT). The brightness of these demonstration images is calculated as the fourth root of the integrated numbers in the unit of Gauss, ﹩{\left(\int | {\rm{\nabla }}\times \vec{B}| {dl}/4\pi \right)}^{1/4}﹩, truncated at 1.
Paper: The Nonpotentiality of Steady-state Coronal Magnetic Field Derived with Time-relaxation Magnetohydrodynamics Simulations Using Helioseismic and Magnetic Imager Three-component Magnetic Field Data
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: AIA synoptic map for CR 2106. The shown image is made by assigning the three primary colors, red, green, and blue, to the AIA 304 Å, 193 Å, and 171 Å data values, respectively, so that brighter parts will correspond to the solar active regions, and the solar filaments will be seen as dark-brown stretched structures surrounded by moderately bright regions that respond to the coronal streamers. The original synoptic map format data are taken from spaceweather.gmu.edu website.
Paper: Evolution, Structure, and Topology of Self-generated Turbulent Reconnection Layers
Authors: Raheem Beg, Alexander J. B. Russell, Gunnar Hornig
Figure caption: Three-dimensional diagram of the magnetic field at t = 0.0, illustrating the position and left-handed orientation of the two flux ropes. The pseudocolor plot on the midplane z = 0.0 indicates the strength of the guide-field B  z  > 0, which is initially invariant in the z-direction. Isosurfaces of B  z  at two different values are compared along with some sample magnetic field lines that lie on the corresponding flux surfaces.
Paper: The Nonpotentiality of Steady-state Coronal Magnetic Field Derived with Time-relaxation Magnetohydrodynamics Simulations Using Helioseismic and Magnetic Imager Three-component Magnetic Field Data
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: In the left column, (a) and (c), the relaxed states derived from the simulation with the boundary treatment BT2 are shown in the same formats as in Figures 1 and 6. These two plots are identical to Figure 1(c) and Figure 6(c), respectively. The time-relaxed state simulated with the initial radial field is shown in the right column (b) and (d).
Paper: The Nonpotentiality of Steady-state Coronal Magnetic Field Derived with Time-relaxation Magnetohydrodynamics Simulations Using Helioseismic and Magnetic Imager Three-component Magnetic Field Data
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: In the left column, (a) and (c), the relaxed states derived from the simulation with the boundary treatment BT2 are shown in the same formats as in Figures 1 and 6. These two plots are identical to Figure 1(c) and Figure 6(c), respectively. The time-relaxed state obtained with the boundary treatment BT2’ is shown in the right column (b) and (d).
Paper: The Nonpotentiality of Steady-state Coronal Magnetic Field Derived with Time-relaxation Magnetohydrodynamics Simulations Using Helioseismic and Magnetic Imager Three-component Magnetic Field Data
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: AIA images taken at the instant corresponding to the images in Figure 6. This is made by assigning the three primary colors, red, green, and blue, to the AIA 211 Å, 193 Å, and 171 Å, respectively.
Paper: The Thermonuclear X-Ray Bursts of 4U 1730–22
Authors: Peter Bult, Giulio C. Mancuso, Tod E. Strohmayer, Arianna C. Albayati, Diego Altamirano, Douglas J. K. Buisson, Jérôme Chenevez, Sebastien Guillot, Tolga Güver, Wataru Iwakiri, Gaurava K. Jaisawal, Mason Ng, Andrea Sanna, Jean H. Swank
Figure caption: Light-curve profiles of the 17 X-ray bursts observed from 4U 1730−22. The top panels show the individual bursts as labeled, with the black line showing the 0.5–10  keV count rate at 1/8 s time resolution and the gray area showing the 4–10  keV count rate (1/4 s resolution, multiplied by a factor of 4). The four panels in the bottom row show various groupings of bursts for comparison, with both labels and color coding ordered by increasing peak count rate. All curves are plotted relative to their respective burst onset time (Table 1) and with the preburst count rate subtracted. Additionally, a horizontal dotted line was added to each panel at 2000 counts s −1 to guide the eye.
Paper: The Thermonuclear X-Ray Bursts of 4U 1730–22
Authors: Peter Bult, Giulio C. Mancuso, Tod E. Strohmayer, Arianna C. Albayati, Diego Altamirano, Douglas J. K. Buisson, Jérôme Chenevez, Sebastien Guillot, Tolga Güver, Wataru Iwakiri, Gaurava K. Jaisawal, Mason Ng, Andrea Sanna, Jean H. Swank
Figure caption: Flux temperature diagram for the X-ray bursts of 4U 1730−22. The bolometric flux contributed by the blackbody component is shown in black, while the red points show the bolometric flux of the whole burst spectrum (blackbody plus the excess but not including the preburst contribution; see text). The horizontal dotted line indicates the PRE flux, while the three diagonal dashed lines show the constant radius contours as labeled, assuming a source distance of 6.9 kpc. These contours are for illustrative purposes only, as they do not take color corrections into account (see, e.g., Suleimanov et al. 2017). Error bars were omitted for clarity, but see the gray point in the legend for the average scale of the uncertainty.
Paper: Evolution, Structure, and Topology of Self-generated Turbulent Reconnection Layers
Authors: Raheem Beg, Alexander J. B. Russell, Gunnar Hornig
Figure caption: Comparison plots of parameters α* (pink) and ε* (red). Panel (a) shows the evolution of these parameters averaged over the CFR axis, denoted 〈α*〉axis and 〈ε*〉axis. The vertical dotted line labeled (c) denotes the turbulent reconnection onset at t = 1.0. Panel (b) is a sample plot comparing the field line averages of these parameters, denoted 〈α*〉 B  and 〈ε*〉 B , at the turbulent reconnection onset t = 1.0. The 1D slice is taken at z 0 = −0.5 over x = x axis. The y-coordinate of the CFR axis  x  axis is indicated by the vertical dotted line.
Paper: The Thermonuclear X-Ray Bursts of 4U 1730–22
Authors: Peter Bult, Giulio C. Mancuso, Tod E. Strohmayer, Arianna C. Albayati, Diego Altamirano, Douglas J. K. Buisson, Jérôme Chenevez, Sebastien Guillot, Tolga Güver, Wataru Iwakiri, Gaurava K. Jaisawal, Mason Ng, Andrea Sanna, Jean H. Swank
Figure caption: Time-resolved spectroscopy of bursts 5 (left, gray), 6 (left, orange), 15 (right, pink), 16 (right, green), and 17 (right, purple), using the same color coding as in Figure 2. Both panels show, from top to bottom, the bolometric burst flux, blackbody temperature, blackbody radius (at 6.9 kpc), f  a  factor, and reduced χ 2. We further highlighted the epoch of radius expansion for burst 5 in the left panel. The error bars show 1σ uncertainties, which for the bottom panels were calculated as ﹩\sqrt{2/{\rm{dof}}}﹩, with dof the degrees of freedom. The dashed line in the top panels indicates the PRE flux.
Paper: Evolution, Structure, and Topology of Self-generated Turbulent Reconnection Layers
Authors: Raheem Beg, Alexander J. B. Russell, Gunnar Hornig
Figure caption: Comparison plot of the mean open twist ﹩\langle \mathop{{ \mathcal T }}\limits^{\sim }\rangle ﹩ (pink), alternative twist ﹩{{ \mathcal T }}_{\mathrm{axis}}﹩ (purple), and open writhe ﹩{\mathop{{ \mathcal W }}\limits^{\sim }}_{\mathrm{axis}}﹩ (light blue) of/about the CFR axis over the interval t = 0.7−1.4 when the CFR axis can be detected. The vertical dotted line labeled (c) denotes the turbulent reconnection onset at t = 1.0.
Paper: The Thermonuclear X-Ray Bursts of 4U 1730–22
Authors: Peter Bult, Giulio C. Mancuso, Tod E. Strohmayer, Arianna C. Albayati, Diego Altamirano, Douglas J. K. Buisson, Jérôme Chenevez, Sebastien Guillot, Tolga Güver, Wataru Iwakiri, Gaurava K. Jaisawal, Mason Ng, Andrea Sanna, Jean H. Swank
Figure caption: Light curves in the 0.5–10  keV band (left and middle) and hardness intensity diagram (right) of 4U 1730−22, with each point representing a single NICER pointing. Those pointings containing an X-ray burst are marked in teal (weak) and red (bright).
Paper: The Thermonuclear X-Ray Bursts of 4U 1730–22
Authors: Peter Bult, Giulio C. Mancuso, Tod E. Strohmayer, Arianna C. Albayati, Diego Altamirano, Douglas J. K. Buisson, Jérôme Chenevez, Sebastien Guillot, Tolga Güver, Wataru Iwakiri, Gaurava K. Jaisawal, Mason Ng, Andrea Sanna, Jean H. Swank
Figure caption: Best-fit spectra of burst 5 at peak intensity, showing, in the top panel, the measured spectrum (black), the preburst model (red), a blackbody model (green), and the fa-model (blue). The bottom panel gives the ratio of the data over the respective models. Note that the spectral bin above 8 keV had an insufficient event count and was removed from the fit.