adsabs/AstroCLIMB huggingface dataset:
Paper: White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System
Authors: Hua-Li Li, Jing Wang, Li-Ping Xin, Jian-Ying Bai, Xu-Hui Han, Hong-Bo Cai, Lei Huang, Xiao-Meng Lu, Yu-Lei Qiu, Chao Wu, Guang-Wei Li, Jing-Song Deng, Da-Wei Xu, Yuan-Gui Yang, Xiang-Gao Wang, En-Wei Liang, Jian-Yan Wei
Figure caption: Combined R-band light curve of the superflare triggered by the GWAC/FFoV in 2020 February 2. The green squares refer to the data obtained by the FFoV, and the red circles the data by F60A. The black curve shows the best fit to the light curve. The four components used to reproduce the light curve are shown separately by different colors in the insert subpanel.
Paper: White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System
Authors: Hua-Li Li, Jing Wang, Li-Ping Xin, Jian-Ying Bai, Xu-Hui Han, Hong-Bo Cai, Lei Huang, Xiao-Meng Lu, Yu-Lei Qiu, Chao Wu, Guang-Wei Li, Jing-Song Deng, Da-Wei Xu, Yuan-Gui Yang, Xiang-Gao Wang, En-Wei Liang, Jian-Yan Wei
Figure caption: The flare duration e-folding time τ vs. the bolometric flare energy. The red circles and black squares denote the flares detected in the M7 dwarf EI Cnc in this work and the superflares on G-type stars detected from the Kepler short cadence data by Maehara et al. (2015), respectively. The dashed line shows the best-fit τ–E relationship given in Maehara et al. (2015) when the superflares are considered. After including the flares in EI Cn, an updated τ–E relationship is overplotted by the solid line.
Paper: White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System
Authors: Hua-Li Li, Jing Wang, Li-Ping Xin, Jian-Ying Bai, Xu-Hui Han, Hong-Bo Cai, Lei Huang, Xiao-Meng Lu, Yu-Lei Qiu, Chao Wu, Guang-Wei Li, Jing-Song Deng, Da-Wei Xu, Yuan-Gui Yang, Xiang-Gao Wang, En-Wei Liang, Jian-Yan Wei
Figure caption: The 25 × 25 pixels R band images of the field of EI Cnc obtained by the F60A telescope on 2020 February 2 (the original size of the image is 19.5 ×19.5 arcmin2). The left and right columns correspond to the object and the comparison star, respectively. The upper row shows the first image obtained on 2020 February 2 UT 13:18:23.482, while the bottom row shows the last image at UT 18:57:20.759, about 5.5 hr later than the first one.
Paper: White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System
Authors: Hua-Li Li, Jing Wang, Li-Ping Xin, Jian-Ying Bai, Xu-Hui Han, Hong-Bo Cai, Lei Huang, Xiao-Meng Lu, Yu-Lei Qiu, Chao Wu, Guang-Wei Li, Jing-Song Deng, Da-Wei Xu, Yuan-Gui Yang, Xiang-Gao Wang, En-Wei Liang, Jian-Yan Wei
Figure caption: Images of the Superflare of EI Cnc obtained by the GWAC FFoV on 2020 February 2. The upper panel is the reference image, which was obtained about 15 s before the trigger of the flare (the lower panel). The observation times, direction, and spatial scale are labeled in both images.
Paper: White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System
Authors: Hua-Li Li, Jing Wang, Li-Ping Xin, Jian-Ying Bai, Xu-Hui Han, Hong-Bo Cai, Lei Huang, Xiao-Meng Lu, Yu-Lei Qiu, Chao Wu, Guang-Wei Li, Jing-Song Deng, Da-Wei Xu, Yuan-Gui Yang, Xiang-Gao Wang, En-Wei Liang, Jian-Yan Wei
Figure caption: The long-term light curve of EI Cnc obtained by GWAC JFoV after subtracting the quiescent flux level. The super flare on 2020 February 2 is marked by the magenta circles.
Paper: White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System
Authors: Hua-Li Li, Jing Wang, Li-Ping Xin, Jian-Ying Bai, Xu-Hui Han, Hong-Bo Cai, Lei Huang, Xiao-Meng Lu, Yu-Lei Qiu, Chao Wu, Guang-Wei Li, Jing-Song Deng, Da-Wei Xu, Yuan-Gui Yang, Xiang-Gao Wang, En-Wei Liang, Jian-Yan Wei
Figure caption: The R-band light curves of the 27 flares found by our off-line search in the GWAC JFoV achieved data obtained from 2018 October 1 to 2021 April 24. In order to display the main flare phase better, the tails of some of the flares are not shown due to a cutoff on the abscissa axis.
Paper: White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System
Authors: Hua-Li Li, Jing Wang, Li-Ping Xin, Jian-Ying Bai, Xu-Hui Han, Hong-Bo Cai, Lei Huang, Xiao-Meng Lu, Yu-Lei Qiu, Chao Wu, Guang-Wei Li, Jing-Song Deng, Da-Wei Xu, Yuan-Gui Yang, Xiang-Gao Wang, En-Wei Liang, Jian-Yan Wei
Figure caption: Continued from Figure 5.
Paper: Wobbling Jets in Common Envelope Evolution
Authors: Noam Dori, Ealeal Bear, Noam Soker
Figure caption: The ratio of the stochastic specific angular momentum of the accreted mass to the one that results from the orbital motion and density gradient in the envelope, j  R,d /j O, as a function of orbital separation, according to Equation (15) and for an NS companion of mass M 2 = 1.4M ⊙. Models are for a star with an initial mass of M ZAMS = 15M ⊙ that we evolved in Section 3. Upper panel: the ratio for the undisturbed star evolved up to R = 500R ⊙. At this point M 1 = 14.7M ⊙ and the envelope mass is M env = 11.4M ⊙. Lower panel: the same star, but after we removed mass at a high rate of ﹩\dot{M}﹩ to M env < 11.4M ⊙, for three cases as indicated in the inset.
Paper: Wobbling Jets in Common Envelope Evolution
Authors: Noam Dori, Ealeal Bear, Noam Soker
Figure caption: Similar to Figure 1, but we stop removing mass and start to inject energy once M env(0) = 5.9M ⊙ (rather than M env(0) = 1.9M ⊙).
Paper: Wobbling Jets in Common Envelope Evolution
Authors: Noam Dori, Ealeal Bear, Noam Soker
Figure caption: Similar to Figure 5 but after we deposited energy to the envelope following mass removal at a rate of ﹩\dot{E}﹩ and as in Figures 1 and 4. All panels are at t = 0.25 yr, i.e., we deposited energy for 0.25 yr. In all cases, the envelope mass is M env = 1.9M ⊙. The cases are for ﹩(\dot{M},\dot{E})﹩ values as given in the insets.
Paper: Wobbling Jets in Common Envelope Evolution
Authors: Noam Dori, Ealeal Bear, Noam Soker
Figure caption: Similar to Figure 6 but for the ratio j  R,2/j O as given by Equation (14), which is appropriate for a main-sequence companion. We take M 2 = 1.4M ⊙, but now representing a main-sequence star as in Figure 7.
Paper: Wobbling Jets in Common Envelope Evolution
Authors: Noam Dori, Ealeal Bear, Noam Soker
Figure caption: The ratio of the mixing length to the radius, λ(r)/r, as a function of radius inside the envelope for the same cases and times as in Figure 1.
Paper: Wobbling Jets in Common Envelope Evolution
Authors: Noam Dori, Ealeal Bear, Noam Soker
Figure caption: Similar to Figure 5 but for the ratio j  R,2/j O as given by Equation (14), which is appropriate for a main-sequence companion. We take M 2 = 1.4M ⊙, but now representing a main-sequence star.
Paper: Modeling the Central Supermassive Black Hole Mass of Quasars via the LSTM Approach
Authors: Seyed Sajad Tabasi, Reyhaneh Vojoudi Salmani, Pouriya Khaliliyan, Javad T. Firouzjaee
Figure caption: Panel (a) shows the examination of our model using multiple data sets in the redshift range of 0 < z < 7. An overview of the utilized data can be found in Tables 3 and 4. Panel (b) is also the model examination at 3 < z < 10 whose data are available in Tables 5 and 6.
Paper: Modeling the Central Supermassive Black Hole Mass of Quasars via the LSTM Approach
Authors: Seyed Sajad Tabasi, Reyhaneh Vojoudi Salmani, Pouriya Khaliliyan, Javad T. Firouzjaee
Figure caption: Panel (a) compares our model with the linear best fit. Blue dots indicate training data, the LSTM model prediction is shown in red, and the orange line is the linear best fit. Panel (b) illustrates our model and compares it with the linear best fit based on flux- and volume-limited samples. Training data are shown as blue dots, the LSTM model prediction is shown in red, and the linear best fit is shown as an orange line.
Paper: Modeling the Central Supermassive Black Hole Mass of Quasars via the LSTM Approach
Authors: Seyed Sajad Tabasi, Reyhaneh Vojoudi Salmani, Pouriya Khaliliyan, Javad T. Firouzjaee
Figure caption: Model built using flux- and volume-limited samples. Corrected QuasarNET+QUOTAS data are plotted with blue dots. The black line represents our LSTM model best fit. In addition, red dotted lines represent our models that include 95% of all data.
Paper: Modeling the Central Supermassive Black Hole Mass of Quasars via the LSTM Approach
Authors: Seyed Sajad Tabasi, Reyhaneh Vojoudi Salmani, Pouriya Khaliliyan, Javad T. Firouzjaee
Figure caption: Model evaluation for the (a) SGD, (b) RMSProp, (c) Adam, (d) Ftrl, and (e) AdaDelta optimization functions are illustrated. Optimization function loss is shown by the blue line and validation loss by the orange line.
Paper: Constraints on the Abundance of Primordial Black Holes from X-Ray Quasar Microlensing Observations: Substellar to Planetary Mass Range
Authors: A. Esteban-Gutiérrez, E. Mediavilla, J. Jiménez-Vicente, J. A. Muñoz
Figure caption: Probability  distributions of the fraction of total mass density in stars and BHs of three masses: M BH/M ⊙ = 0.0024, 0.013. and 0.082, plotted in yellow, turquoise, and orange, respectively. Bottom right: joint (2D) probability density function, ﹩{p}_{{ijkl}}({{\alpha }_{\mathrm{BH}}}_{k},{{\alpha }_{\mathrm{star}}}_{l}| \{{\rm{\Delta }}{m}_{{ij}}\})﹩. Contour levels in steps of 0.25σ with thicker lines for 1σ and 2σ. Straight black dashed lines represent constant α smooth for α smooth = 0.9, 0.8, 0.7, 0.6, 0.5 (bottom to top). Top right and bottom left: marginalized (1D) probability density functions, ﹩{p}_{k}({\alpha }_{{\mathrm{BH}}_{k}}| \{{\rm{\Delta }}{m}_{{ij}}\})﹩ and ﹩{p}_{l}({\alpha }_{{\mathrm{star}}_{l}}| \{{\rm{\Delta }}{m}_{{ij}}\})﹩, of the fraction of total mass density in BHs, α BH, and stars, α star, respectively. Upper limits at the 68% and 90% confidence levels for each BH mass are indicated as dotted and dashed–dotted lines, respectively.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: Results of the Lauer et al. (2007) bias simulation described in Section 4.1. Left: gray contours represent the underlying quasar sample, and the gray points are one realization of the mock sample at the i = 22 flux limit, after being perturbed with measurement uncertainties. The black solid line is the unbiased Kormendy & Ho (2013) relation. The colored lines indicate the results of the mock sample at different flux limits. Right: the best-fit M BH–M *,bulge parameters at each flux threshold and the best-fit M BH–M *,host parameters of our sample (plotted in red at i = 21.7). The dotted lines show the parameters and intrinsic scatter from the Kormendy & Ho (2013) relation.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: MCMC fitting for the M BH–M *,bulge relation when considering the selection bias. Left: the M BH–M *,bulge relation with the 1σ range drawn from the posterior (black dashed line and shaded area). The blue dashed lines and shaded area show the original best-fit relations from LINMIX_ERR (previously shown in Figure 5), and the red solid line is the local M BH–M *,bulge relation from Kormendy & Ho (2013). Right: the posterior distribution of the parameters a, b, and σ. The best-fit parameters from LINMIX_ERR and the MCMC fitting are indicated by the blue and white squares, respectively. The MCMC fitting recovers a similar BH–galaxy relation to the original linear regression, indicating that the selection effects are minimal.
Paper: Constraints on the Abundance of Primordial Black Holes from X-Ray Quasar Microlensing Observations: Substellar to Planetary Mass Range
Authors: A. Esteban-Gutiérrez, E. Mediavilla, J. Jiménez-Vicente, J. A. Muñoz
Figure caption: Upper limits of the contribution of PBHs to the fraction of dark matter from both X-rays (this study) and the optical (Esteban-Gutiérrez et al. 2022a), plus a new extra point at 3M ⊙. The gray band corresponds to the mass range for which quasar microlensing cannot distinguish between stars and BHs.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: The deviation of the measured BH masses from the expected BH masses estimated based on the local Kormendy & Ho (2013) M BH–M Bulge relation (﹩{\rm{\Delta }}\mathrm{log}({M}_{\mathrm{BH}})﹩), as a function of redshift. The top (bottom) panel shows the deviation estimated by the bulge (total) masses. There is no obvious trend in ﹩{\rm{\Delta }}\mathrm{log}({M}_{\mathrm{BH}})﹩ with redshift, indicating negligible redshift evolution in the BH–host relations. Our work is the only sample with RM-based BH masses beyond z > 0.3, and all other samples beyond z > 0.3 are based on SE BH masses. Vertical error bars are from uncertainties in BH mass only.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: Left: comparison of the derived host light fraction from this work and Shen et al. (2015b), both measured in the UVIS (F606W or F814W) bandpass. The black dashed line shows the 1:1 ratio line. Right: comparison of the total stellar masses derived from this work and Matsuoka et al. (2015) for overlapping objects.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: Same format as Figure 8, but for the M BH–M *,host relation.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: Color-composite images (F110W in red, F606W in blue, and the average of F110W and F606W in green) of the PSF-subtracted host galaxies. The RMIDs are labeled in the lower left corner of each panel, and the images are 7.″5 × 7.″5.
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: Indicative examples of weekly binned blazar gamma-ray light curves (black points) in the 0.1–316 GeV energy range. Gray triangles indicate 95% upper limits. The quiescent flux and flare threshold levels are plotted with dashed blue and red lines, respectively (for a definition of both flux thresholds, see Section 3.1). The Bayesian blocks’ representation of each light curve is overplotted with orange solid lines. The 1–316 GeV light curves of the same sources can be found in Appendix B.
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: Cumulative histograms (normalized to one) of the 0.1–316 GeV gamma-ray flare duty cycles (a) and flare energy fractions (b) of 145 blazars (black solid histogram), 106 FSRQs (blue solid histogram), and 31 BL Lac objects (orange solid histogram). In both panels, the vertical dashed line indicates the values for TXS 0506+056 .The dashed gray lines depict cumulative power-law functions (see text for more details).
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: Scatter diagram of the time-average gamma-ray energy flux and redshift for the 145 blazars in our sample (106 FSRQs in blue, 31 BL Lac objects in orange, and 8 BCUs in green). All blazars in the 4LAC are overlaid (gray markers) for comparison reasons. Side panels show the projected histograms on each axis. The energy fluxes are taken from 4LAC, and the redshifts are from 4LAC and SIMBAD (Oberto et al. 2019).
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: Cumulative histograms of the 0.1–316 GeV gamma-ray flare duty cycles (a) and flare energy fractions (b) of 145 blazars for different integer values of s ranging from 2 to 9. In the case of s = 6; cumulative histograms of p 0 = 0.01, 0.10 are also plotted.
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: Scatter plot of the 0.1–316 GeV gamma-ray flare duty cycles and flare energy fractions of 141 blazars (103 FSRQs in blue squares, 30 BL Lac objects in orange circles, and 8 BCUs in green triangles). Side panels show the projected histograms on each axis.
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: Scatter plot between 0.1–316 GeV gamma-ray flare duty cycle and quiescent gamma-ray luminosity for 137 blazars of 103 FSRQs (blue squares), 30 BL Lac objects (orange circles), and 4 BCUs (green triangles).
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: Top: recreation of the phase-space plots in the second and third panels of Figure 5. Here the color of each particle is based on the orbit family to which it belongs (as determined by the ratio of  Ω z  and  Ω R ). The bifurcations appear to have a different color than the main stream track in the top right panel (e.g., in stream 2, the bifurcation in the trailing arm is gray, whereas the rest of that arm is orange), indicating that these components belong to different orbit families. At the same time, the fans highlighted in the top left panel appear to mostly belong to the untrapped orbit family, suggesting that fans do not necessarily require particles from different orbit families in order to form. Bottom: same two plots but with the particle color determined by each particle’s libration time T  ℓ . The fans in the bottom left panel are accentuated by a noticeable gradient in the libration time. Similarly, the fanned-out debris structures between the main stream track and the bifurcations in the bottom right panel are characterized by long libration times (i.e., they are yellow) compared to the bifurcations themselves. The physical source of the fanned-out stream components is directly related to the large spread in these libration periods.
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: In the top panels, the solid green curve represents the percent of librating, or resonantly trapped, particles in mock stream simulations of M92 (left panel) and Phlegethon (right panel) as a function of the density ratio parameter (q = c/a) of the halo potential. In M92, the stream encounters the Ω z : Ω R  = 2: 3 resonance around q = 0.875. The shaded green regions represent the potentials in which the stream particles are split across two orbit families (with at least 5% of the particles in a different orbit family than the progenitor), suggesting that in these potentials, M92 could exhibit morphological deviations due to separatrix divergence. Phlegethon encounters a smaller resonantly trapped orbit family at the Ω z : Ω R  = 3: 4 resonance around q = 1.28. Because in this case, the stream occupies a greater volume in phase space than the resonance, at no orbit is the stream fully trapped. As a result, the single shaded green region extends across the entire range of potentials in which Phlegethon encounters the resonance. The blue line (and the associated secondary y-axis on the right of each panel) corresponds to the frequency ratio of the progenitor orbit as a function of q, demonstrating the range of potentials in which the progenitor encounters the resonance. Finally, the green dot marks the specific potential chosen for the visualizations in the bottom row. Bottom: mock stream simulations of M92 and Phlegethon in the two potentials marked by the green dots in the top row. Note that for M92, ﹩{Q}_{\mathrm{res}}=2/3﹩, while for Phlegethon, ﹩{Q}_{\mathrm{res}}=3/4﹩. Here M92 exhibits a fan, and Phlegethon develops a distinct bifurcation within the life span of the Galaxy.
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: Three snapshots of the phase-space positions of the five m = 105 M ⊙ streams introduced in Section 4.1, separated from each other along the z-axis (the streams are evolved from the same z-position in the halo and translated to higher/lower z-positions in these plots for visual clarity). The left panel demonstrates that initially, all of the streams appear to be evolving as thin stellar streams. In the middle panel, roughly 0.5 Gyr later, the trailing arms (in blue) of the three streams that were initiated near the separatrix fan out compared to the fully trapped and untrapped streams. The right panel shows that approximately 3 Gyr into their evolution, these three streams also develop bifurcations.
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: The five streams from Figure 5 plotted in SoS plots. The light gray contours and crosses are identical to those calculated for Figure 1 and correspond to the energy and angular momentum of the progenitors of all five streams. Each column corresponds to one of the snapshots in Figure 5, the bold black plus sign reflects the progenitor’s most recent consequent in the SoS before the time stamp of the snapshots in Figure 5, and the red and blue points reflect the consequents of the orbits of the leading and trailing arm particles of each stream, just like in Figure 5. The structure and evolution of each stream in the SoS plots can be related back to its morphology in Figure 5, as shown in the labels in this figure; the color-coding of the labels corresponds to whether the feature belongs to the leading (red) or trailing (blue) arm.
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: Snapshot of the leading arm of stream 3 from Figures 5–7 (a 105 M ⊙ stream initiated very close to the separatrix). The stream was evolved for approximately 5 Gyr, and only particles belonging to the leading arm that were stripped in the first 3 Gyr of the stream’s evolution are shown here. The morphology demonstrates how multiple components on distinct orbital tracks correspond to the different orbit families accessible to this stream.