adsabs/AstroCLIMB huggingface dataset:
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: SED fitting of G6084 (top panel), G6081 (middle panel), and G6405 (bottom panel). The photometric data used for fitting (violet circles) are from Gaia DR2 (G, G BP, and G RP), 2MASS (J, H, and K S), APASS (B, V, g, r, and i), and WISE (W1 and W2). The black line represents the best-fit model.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Hertzsprung–Russell diagram of G6084 (blue asterisk), G6081 (green square), and G6405 (red triangle). The gray points are the stars from Gaia eDR3 with distances d < 150 pc, G mag between 4 and 18 mag, and Galactic latitude ∣b∣ > 10. No extinction was corrected for these stars.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Summary flowchart of the source selection process in this paper.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Lomb–Scargle periodograms of G6084 (top panel), G6081 (middle panel), and G6405 (bottom panel) from ZTF g -band observations. Red vertical line is the frequency with the maximum power. Black horizontal dashed line represents the 5% false alarm probability.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Folded multiband light curves of G6084.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Folded multiband light curves of G6405.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Folded multiband light curves of G6081.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Low-resolution spectra of G6084 (top panel), G6081 (middle panel), and G6405 (bottom panel) from LAMOST observations.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Phase-folded RV data (blue dots) and the best-fit RV curves (black lines) of G6084 (top panel), G6081 (middle panel), and G6405 (bottom panel).
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Left panel: spectral disentangling of G6084 with q = 0.8. Right Panel: spectral disentangling of G6084 with q = 1.2. The vertical panels show spectra in different phases (close to the minimum or maximum RV phase of the visible star). The blue lines represent the reconstructed spectra of the visible star in those three systems, and the red lines represent the second component in each spectra. The green lines are the sum of the two components, and the black lines mark the observed spectra.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Corner plot showing the distribution of observed and physical parameters of G6084, derived from the isochrones code. The parameters are labeled as effective temperature (T eff, in K), surface gravity (logg, in dex), metallicity ([Fe/H], in dex), mass (M, in M ⊙), radius (R, in R ⊙), and bolometric luminosity (logL, in L ⊙).
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Corner plot showing distribution of orbital parameters of G6084, derived from the Joker. The parameters are labeled as orbital period (P, in days), eccentricity of the system (e), argument of pericenter (ω, in radians), mean anomaly at reference time (M 0, in radians), RV semiamplitude of the star (K, in km s−1), and the center of mass velocity (ν0, in km s−1).
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Left panel: spectral disentangling of G6405 with q = 0.8. Right panel: spectral disentangling of G6405 with q = 1.2. Symbols are as in Figure 10.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Corner plot showing the distribution of observed and physical parameters of G6405, derived from the isochrones code, as an example. The parameters are as in Figure B1.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Corner plot showing the distribution of observed and physical parameters of G6081, derived from the isochrones code. The parameters are as in Figure B1.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Corner plot showing distribution of orbital parameters of G6405, derived from the Joker. The parameters are as in Figure C1.
Paper: Binaries with Possible Compact Components Discovered from the LAMOST Time-domain Survey of Four K2 Plates
Authors: Xue Li, Song Wang, Xinlin Zhao, Zhongrui Bai, Hailong Yuan, Haotong Zhang, Jifeng Liu
Figure caption: Corner plot showing distribution of orbital parameters of G6081, derived from the Joker. The parameters are as in Figure C1.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Behavior of lensing observables θ ∞ (left), s (right) as a function of parameter b in strong field limit by considering that the spacetime around the compact objects at the centers of nearby galaxies is REC spacetime. The vertical black line corresponds to the extremal black hole for b = b  E  ≈ 0.226. For no-horizon spacetime (b > b  E ), separation s increases with b to reach a maximum and then decreases. On the other hand, for REC black holes (0 < b < b  E ), it has an increasing behavior.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: (a) (left) Variation of the effective potential V eff, for REC black holes as a function of radial coordinate x. The photons with critical impact parameter (u ps) (black solid curve) make unstable circular orbits. (b) (right) Trajectories of photons for REC black holes with different impact parameters u. A photon with impact parameter u > u ps (red curves) is scattered to infinity, while the photon impacted by parameter u < u ps (green and blue curves) is absorbed in the black hole. A photon with an impact parameter almost close to the critical impact parameter u ≈ u ps (black curve) makes several loops around the black hole before being scattered to infinity.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: (a) (left) Variation of the effective potential V eff for REC black holes as a function of radial coordinate x. The photons with critical impact parameter (u ps) (black solid curve) make unstable circular orbits. (b) (right) Trajectories of photons for REC black holes with different impact parameters u. Photons having impact parameter u > u ps (red curves) are scattered to infinity, while photons impacted by parameter u < u ps (green and blue curves) are absorbed in the black hole. Photons with an impact parameter almost close to the critical impact parameter u ≈ u ps (black curve) make several loops around the black hole before being scattered to infinity.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: (a) (left) Variation of the deflection angle for REC black hole spacetime as a function of the impact parameter u for different values of parameter b. Dots on the horizontal axis represent the values of the impact parameter u = u ps at which the deflection angle diverges. (b) (right) Deflection angles for REC black hole spacetime evaluated at u = u ps + 0.001 as a function of parameter b.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Behavior of the photon sphere radius x ps (left) and the critical impact parameter u ps (right) for REC black hole spacetime as a function of parameter b. As b → 0, the values x ps → 1.5 and u ps → 2.598 correspond to a Schwarzschild black hole (Bozza 2002).
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Behavior of strong lensing coefficients ﹩\bar{a}﹩ and ﹩\bar{b}﹩ for REC black hole spacetime as a function of parameter b. ﹩\bar{a}=1﹩ and ﹩\bar{b}=-0.4002﹩ at b = 0 correspond to the values of a Schwarzschild black hole.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Plot showing A(x) vs. x; for 0 < b ≤ b  E  one has a black hole with two horizons while b > b  E  corresponds to no-horizon spacetime. Case b = 0 corresponds to the Schwarzschild black hole.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Einstein rings for different compact objects at the centers of nearby galaxies by considering them to be REC black holes. Black, blue, orange, and red rings correspond to Sgr A*, M87*, NGC 4649, and NGC 1332.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Locations of event horizon x + (solid line) and Cauchy horizon x − (dashed line) for REC black holes.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: (a) (left) V eff for REC no-horizon spacetime (b = 0.23). x ps and x aps are the locations of the photon sphere and anti-photon sphere, respectively. For a photon that has the impact parameter u < u ps, the closest approach distance x 0 is close to x  c , where x  c  is the smaller positive root of V eff for u = u ps. (b) (right) Trajectories of photons for REC no-horizon spacetime with different impact parameters u. Photons with impact parameter u > u ps (red curves) are scattered to infinity after reaching the closest approach distance x 0, which is greater than x ps. At the same time, the photons with impact parameter u < u ps (green and blue curves) enter inside the photon sphere and are scattered to infinity after reaching the closest approach distance x 0, which is close to x  c . A photon with an impact parameter almost close to the critical impact parameter u ≈ u ps (black curve) makes several loops around the center before being scattered to infinity. The inner black circular curve shows the location of the anti-photon sphere.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Deflection angle for REC no-horizon spacetime as a function of the impact parameter u. Dots on the horizontal axis represent the values of the critical impact parameter u ps at which the deflection angle diverges. The curves on the left of the dots represent strong lensing from the inside of the photon sphere (u < u ps), while the curves on the right represent strong lensing from the outside of the photon sphere (u > u ps).
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Behavior of strong lensing observable r mag for REC black hole spacetime as a function of parameter b. It is independent of the black hole’s mass or distance from the observer.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Shadow angular diameter θ sh( = 2θ ∞) as a function of b, when M87* is modeled as REC spacetimes: (a) black hole (left) (b) no-horizon spacetime (right). The dark black line corresponds to calculated values of 2θ ∞ as a function of b. The white/red regions represent areas that are 1σ consistent/inconsistent with the 2017 EHT observations, indicating that the latter imposed constraints on parameter b.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Shadow angular diameter θ sh( = 2θ ∞) as a function of b, when Sgr A* is modeled as REC spacetimes: (a) black hole (left) (b) no-horizon spacetime (right). The dark black line corresponds to calculated values of 2θ ∞ as a function of b. The white/red regions represent areas that are 1σ consistent/inconsistent with the 2017 EHT observations, indicating that the latter imposed constraints on parameter b.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Locations of photon sphere x ps (black solid line), anti-photon sphere x aps (black dashed line), event horizon x + (blue solid line), Cauchy horizon x − (blue dashed line), and smaller positive root of V eff for u = u ps (red solid curve) for REC no-horizon spacetime.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Behavior of lensing observables S 1, S −1, S −2, and S −3, for REC no-horizon spacetime as a function of parameter b.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Behavior of strong lensing observables ﹩{{ \mathcal R }}_{1}﹩, ﹩{{ \mathcal R }}_{-1}﹩, ﹩{{ \mathcal R }}_{-2}﹩, and ﹩{{ \mathcal R }}_{-3}﹩ for REC no-horizon spacetime as a function of parameter b.
Paper: Testing Strong Gravitational Lensing Effects of Supermassive Compact Objects with Regular Spacetimes
Authors: Jitendra Kumar, Shafqat Ul Islam, Sushant G. Ghosh
Figure caption: Behavior of lensing observable θ ∞ for REC no-horizon spacetime as a function of parameter b.
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: (a) MCMC estimates of the ISM density surrounding SNR 0509−67.5 (for γ eff = 5/3) as a function of PA. The blue points are the density values obtained when age (T) and distance (D) and density (ρ  i ) are all allowed to vary, while the orange points are when T and D are fixed at their estimated values. The black curve shows the harmonic fit to the blue data points (see Section 6.3). (b) A schematic visualization of the density map of SNR 0509−67.5 obtained from the harmonic fit shown in panel (a) (see Section 6.3).
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: (a) Corner plot showing the posterior distributions of the age (T), distance (D), and two of the 144 densities (ρ  i ) constrained by the MCMC analysis with SNR 0509−67.5’s center fixed. The densities correspond to PAs 0.°34 and 10.°32. (b) Corner plot for the case where we fit for the center, given by the two additional parameters RA_cen and DEC_cen (equivalent to α dyn and δ dyn).
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: Velocity and radius of the FS of SNR 0509−67.5 as a function of PA around the rim. The shock velocities and radii for all the 231 regions are shown in green in the top and bottom panel respectively, with the golden sample (see Section 3.2) overplotted in orange. In the top panel, we also show the shock-velocity results from Hovey et al. (2015) (plotted in gray), measured over a 1 yr baseline. The longer baseline by almost a factor of 10 for our data allows us to measure the PM of the rim to higher precision, while also showing the variability over small spatial scales. The middle panel shows an image of SNR 0509−67.5’s shock front region in polar coordinates (radius vs. azimuthal PA) aligned with the other panels along the PA axis.
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: Center: SNR 0509−67.5 Hα image showing the two types of apertures used for the PM analysis. Left: zoomed images showing a 1° wide aperture (top) used for bright portions of the rim and a 5° wide aperture (bottom) used for faint regions. Right: difference image of SNR 0509−67.5 from observations separated by 10 yr, clearly showing the remnant’s expansion (white shows regions where intensity increased, black shows where it decreased).
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: Radial density profiles for γ eff = 5/3 (solid curve) and γ eff = 4/3 (dotted curve) reflecting the compression factors for the two cases. The profiles are shown for the age, density, and energy values corresponding to rows 1 and 3 of Table 3 for a fixed mass of M ej = 1.4M ⊙.
Paper: 2D and Slab Turbulent Cascade Rates in the Inner Heliosphere
Authors: L. Adhikari, G. P. Zank, L.-L. Zhao, D. Telloni
Figure caption: Comparison of the theoretical and observed 2D and 2D+slab turbulence cascade rate (solid curve), and the slab and 2D+slab turbulence cascade rate (dashed curve) ratios as a function of heliocentric distance—correspond to Panels (a)–(e) of Figure 3. Red and blue circles are the ratios observed by SolO between the 2D and 2D+slab turbulence cascade rates, and the slab and 2D+slab turbulence cascade rates, respectively.
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: Left: sample of a 1° wide aperture used to extract a brightness profile. Right: brightness profiles of the extracted region; black shows the brightness profile from the 2006 observation, red from the 2016 observation, and blue shows the best-fit shifted profile.
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: The measured values (red points) and best-fit results (blue points) from our MCMC run with a fixed explosion center for the FS velocity (top two panels) and radius (bottom two panels) along with residual plots.
Paper: Large Sunspot Groups and Great Magnetic Storms: Magnetic Suppression of CMEs
Authors: Edward W. Cliver, Werner Pötzi, Astrid M. Veronig
Figure caption: Longitudes of source flares for the principal components of great storms from 1932–2014 with minimum Dst (or Dxt) values ≤−300 nT.
Paper: Large Sunspot Groups and Great Magnetic Storms: Magnetic Suppression of CMEs
Authors: Edward W. Cliver, Werner Pötzi, Astrid M. Veronig
Figure caption: Comparison of the geomagnetic activity associated with two large area sunspot groups—16763 in 1951 May (largest daily spot area during disk passage = 4865 μsh) and 12192 in 2014 October (4419 μsh)—in the top and middle panels, respectively, with the extensive magnetic activity observed during 1957 September, the most magnetically active month of the modern era. The three great storms in 1957 September (as well as the −246 nT storm on the 29th) are associated with spot groups significantly smaller than groups 16763 and 12192 (Table 1; Lefèvre et al. 2016). The largest daily area recorded for any spot group in 1957 September was 2214 μsh.
Paper: Large Sunspot Groups and Great Magnetic Storms: Magnetic Suppression of CMEs
Authors: Edward W. Cliver, Werner Pötzi, Astrid M. Veronig
Figure caption: Scatter plot of peak solar wind speed following an SC (V SW(max)) vs. CME-driven shock average transit speed (V SH). Black circle data points and linear fit are for a sample of high-confidence flare-SC associations for 1979–1983 from Cane (1985) and the light blue circle points are post-1962 events from Table 1. The black open circle data point was excluded from the reduced major axis curve fit and a similar outlier can be seen from the Table 1 events. The square black data point in 1972 August had the shortest Sun–Earth CME transit time yet observed (adapted from Cliver et al. 1990).
Paper: Large Sunspot Groups and Great Magnetic Storms: Magnetic Suppression of CMEs
Authors: Edward W. Cliver, Werner Pötzi, Astrid M. Veronig
Figure caption: The probability of great storm occurrence for a spot group of a given area.
Paper: Large Sunspot Groups and Great Magnetic Storms: Magnetic Suppression of CMEs
Authors: Edward W. Cliver, Werner Pötzi, Astrid M. Veronig
Figure caption: Histogram of the numbers of great magnetic storms originating in spot groups of increasing area. The numbers at the bottom of each bin give the number of daily observations of a spot group of a given size.
Paper: Large Sunspot Groups and Great Magnetic Storms: Magnetic Suppression of CMEs
Authors: Edward W. Cliver, Werner Pötzi, Astrid M. Veronig
Figure caption: Distribution of principal source flare onset to SC delay times (inferred CME transit times) for great magnetic storms from 1932–2014.