adsabs/AstroCLIMB huggingface dataset:
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: The model correlation matrix with the color bar showing the Pearson correlation coefficient. The thick lines mark major model blocks explored in this work. Top left is the SFR–v Mpeak scaling relation; second to top left is the r  c  rank correlation between SFR and ﹩{\rm{\Delta }}({v}_{\max })﹩ at fixed halo mass; the single parameter T merge,300 is part of the orphan model; and bottom right is the new low-mass quenching model added in this work. All major blocks have negligible cross-correlations, although some parameters share degeneracies within each block diagonal.
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: Distribution of lookback times when the SAGA3-like satellites in c125-2048 formed 50% (t 50) and 90% (t 90) of their z = 0 stellar mass in the UM-SAGA model (this work) and the UM DR1 model. The solid curve shows the median, while the shaded region shows the [16%, 84%] distribution in each stellar mass bin. With the added low-mass quenching model, low-mass satellites systematically form stars and quench earlier in the new model compared to UM DR1 at M ⋆ ≲ 108 M ⊙. This also brings them closer to the observed LG dwarfs (≳70% satellites), which were not used as data constraints in this work (black plus signs; D. R. Weisz et al. 2014a).
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: The posterior distribution for the nine parameters from UM DR1 related to low-mass galaxies. Orange shows the original posteriors of these parameters in UM DR1, and turquoise shows reconstrained posteriors in UM-SAGA. The diagonal subplots show the marginalized distributions for each parameter, with the labeled values denoting the median and [16%, 84%] posterior. The off-diagonal subplots show the cross-correlations between each pair of parameters, with shaded contours marking out 68%, 95%, and 99% distributions. The orange dashed line in each panel marks the UM DR1 best-fit value, while the turquoise solid line indicates the UM-SAGA best-fit value. The posteriors of parameters from the UM DR1 model are much more tightened in UM-SAGA with the addition of the low-mass galaxy observational constraints from SAGA and SDSS.
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: The f  Q (v Mpeak) functions of the best-fit UM-SAGA (solid) and UM DR1 (dashed) models. The different colors represent the model relations at different redshifts. The new low-mass quenching mostly affects halos with v Mpeak ≲ 100 km s−1.
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: The posterior distribution for the six new low-mass quenching parameters added in this work. The legend is the same as in Figure A1.
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: Left panel: the v Mpeak–﹩{\rm{\Delta }}{v}_{\max }﹩ distribution of subhalos in c125-2048 that host SAGA-like satellites (green) or SDSS-like isolated field galaxies (blue). The side panels show the projected PDFs of v Mpeak or ﹩{\rm{\Delta }}{v}_{\max }﹩ for the two low-mass (sub)halo populations. There is a significant overlap between the SAGA-like subhalos and isolated field halos in ﹩{\rm{\Delta }}{v}_{\max }﹩ at fixed v Mpeak. Right panels: CDFs of ﹩{\rm{\Delta }}{v}_{\max }﹩ in two v Mpeak bins (marked by vertical dashed lines in the left panels) that roughly correspond to stellar mass ranges of M ⋆/M ⊙ ∈ [106, 107] and [107, 108.5]. The CDFs for the isolated field halos in both bins are much steeper than the SAGA-like satellites occupying a narrower range of ﹩{\rm{\Delta }}{v}_{\max }﹩ in the same v Mpeak bin. In the top right panel, we mark the ﹩{\rm{\Delta }}{v}_{\max }﹩ value at which the CDF of the SAGA-like subhalos reaches 90%. This corresponds to simultaneously quenching at least 60% of the isolated field galaxies in M ⋆/M ⊙ ∈ [106, 107] with r  c  → 1. In the bottom right panel, we mark the ﹩{\rm{\Delta }}{v}_{\max }﹩ value in the M ⋆/M ⊙ ∈ [107, 108.5] bin where the CDF of the SDSS-like isolated field halos reaches 2% and that yields a maximum quenching fraction of 65% for the SAGA satellites if r  c  = 1. The actual SAGA quenched fraction (Figure 2) is ≲60% in this mass range. Thus, the best-fit r  c  only needs to be ∼0.9 (Figure 7). We exclude the ~10% orphan galaxies from the CDFs presented in the two right panels.
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: Part one of the model predictions by the UM-SAGA model (solid) compared to the UM DR1 model (dashed) for observables used in P. Behroozi et al. (2019). First row left panel: SMFs at various redshifts. First row right panel: overall quenched fraction of galaxies at various redshifts. Second row left panel: mean specific SFR of galaxies at various redshifts. Second row right panel: cosmic SFR density history. Third row left panel: UV luminosity function at z ≥ 4. M 1500 is the rest-frame absolute UV magnitude at 1500 Å. Third row right panel: median stellar mass vs. M 1500 at z ≥ 4. Fourth row left panel: the average infrared excess (a probe of dust attenuation) at z ≥ 4. Fourth row right panel: the star-forming fraction of neighboring galaxies as a function of neighbor counts from 0.3 Mpc to 4 Mpc around the central galaxy. Central galaxies with stellar masses 1010 < M ⋆/M ⊙ < 1010.5 are considered. The UM-SAGA model predicts slightly higher f SF, neighbors at neighbor counts ≲10 than the UM DR1 model due to increased r  c .
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: Part two of model predictions by the UM-SAGA model (solid) and the UM DR1 model (dashed) for galaxy clustering observables used in P. Behroozi et al. (2019). The four panels in the first two rows show the projected autocorrelation functions for all galaxies (gray), quenched-only (red), and star-forming-only (blue) populations split into different stellar mass (M ⋆ > 1010.3 M ⊙) and redshift bins (z < 0.7). The bottom panel shows the cross-correlation between a lower and higher stellar mass bin for all galaxies at a mean redshift of z = 0.06.
Paper: The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UNIVERSEMACHINE 
Authors: Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Risa H. Wechsler, Tom Abel, Peter Behroozi, Marla Geha, Yasmeen Asali, Mithi A. C. de los Reyes, Erin Kado-Fong, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner, John F. Wu
Figure caption: The SFHs of four example low-mass galaxies at M ⋆ ∼ 107.5 M ⊙. The green are two SAGA-like satellites, and the blue are two SDSS-like isolated galaxies. The top panel shows their SFHs, and the bottom panel shows their stellar mass evolution. The green triangles indicate the two SAGA-like satellites’ most recent accretion time. The stellar mass history takes into account the mass loss from the death of massive stars over time (Equation (21) of P. Behroozi et al. 2019).
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Schematic diagram of observer and star’s coordinates with the light-traveling time correction. The black axis of (x, y, z) with its spherical coordinate of (r, β, ϕ) is for the star’s frame. The blue axis of (﹩x{\rm{^{\prime} }},y{\rm{^{\prime} }},z{\rm{^{\prime} }}﹩) with its spherical coordinate of ﹩(r{\rm{^{\prime} }},\beta {\rm{^{\prime} }},\phi {\rm{^{\prime} }})﹩ is for the observer’s viewing frame obtained by the rotating star’s frame along the x-axis by θ. The red square in the direction of ﹩{\boldsymbol{r}}﹩ represents the emitting surface elements on the sphere of collecting radius, r  s . The angle between  r  and the viewing direction of ﹩{\hat{{\boldsymbol{r}}}}_{\mathrm{RO}}﹩ or ﹩z{\rm{^{\prime} }}﹩ is ﹩\beta {\rm{^{\prime} }}﹩. The distance difference from the observer between the elements at polar angles of 0 and ﹩\beta {\rm{^{\prime} }}﹩ is ﹩{\rm{\Delta }}d(\beta {\rm{^{\prime} }})=2\,{r}_{s}{\sin }^{2}(\beta {\rm{^{\prime} }}/2)﹩ and the corresponding light-traveling time difference is ﹩{\rm{\Delta }}t(\beta {\rm{^{\prime} }})={\rm{\Delta }}d(\beta {\rm{^{\prime} }})/c﹩.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: LCs from simulations with different resolution. Left: LCs from Model N with the following resolutions:4096 for N 1, 10,240 for N 2, and 102,400 for N 3. The 1D LC duration is ∼0.2–0.3 hr, with a peak luminosity of ∼1045–1046 erg s−1 Right: LCs from Model R with resolutions at different viewing angles: 20482 (green), 10242 (red), and 5122 (blue). The 2D LC duration is ∼2–3 hr, with a peak luminosity of ∼(2–4) × 1046 erg s−1. Although the LC duration and peak luminosity from current resolutions are similar, the results from 5122 deviate more from those of 20482 to 10242, indicating that insufficient resolution can affect the shock breakout emissions.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: 1D density and opacity profiles for Model T when the shock is about to break out. Profiles show various opacity components from the scattering opacity, the absorption opacity from OPAL for band VIII, and the electron scattering. The OPAL opacity in the region within a stellar radius, r = 3.2 × 1012 cm, is higher than electron scattering. The overlapping lines are slightly shifted for legibility.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: LC peak and duration of band VIII plot with different perturbation strengths (P; s = 1%, 3%, 5%, 10%, 15%, 20%, 25%, and 30%). Models of different perturbation strengths show a roughly consistent peak luminosity of (5–6) × 1046 erg s−1 and LC duration of 1.2–1.5 hr. In general, the higher peak luminosity corresponds to the shorter duration.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Resolution comparison of Model R. Left: resolution of 5122. Middle: resolution of 10242. Right: resolution of 20482. After the shock breakout, the shocked SN ejecta and CSM deviate from the spherical symmetry. The filaments and layers of the shock front are reasonably resolved. The difference between 5122 and 10242 is in the more detailed filamentary structures. Although 20482 resolves the details of fine filamentary structures, it looks similar to 10242. These tests suggest that the optimal resolution is close to 10242.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Zoom-in of gas density structures. Panels from left to right show the gas density for models with perturbation strengths of s = 3%, 10%, and 20%, respectively. All panels clearly show the development of Rayleigh–Taylor instabilities, which are less sensitive to the strengths of perturbations.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The 1D radial profile of Model T when the shock travels to 3 × 1013 cm (yellow dotted line). The background grayscale color map shows the optical depth (τ) as a function of r, and the green dotted line shows the position where τ = 1. We show the radiation-to-gas-pressure ratio and gas density. The radiation pressure largely exceeds the gas pressure throughout the simulation regions.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The evolution of the radiation temperature profile for Model T. The shock is located at a turning point from flat to decay of the profile. As the shock propagates from ∼2 × 1013 cm to ∼6 × 1013 cm, the CSM gas beyond the shock front is heated up by the radiation precursor.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Comparison of LCs in Model T with different methods: VO (black), uncorrected RO (orange), and RO (blue) for the viewing angles of 45° and 60°. The RO LCs are smoother compared to VO and the uncorrected RO and have lower peak luminosities; the LCs for viewing angles of 45° and 60° are very similar. The angle-averaged LC durations for them are 1.34, 1.33, and 1.50 hr, respectively. The corresponding peak luminosities are (4.5, 4.6, 3.8) × 1046 erg s−1.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The density and velocity evolution of Model P. Panels show the evolution of SN and CSM mixing as the shock propagates outward. The shock velocity reaches >1010 cm s−1, and the post-shock region becomes highly turbulent.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Comparison of LCs in Model B with different methods: VO (black), uncorrected RO (orange), and RO (blue) for the viewing angles of 45° and 60°. The RO LCs are smoother compared to VO and projection and have lower peak luminosities. The angle-averaged LC durations for them are 0.57, 0.70, and 0.83 hr, respectively. The corresponding peak luminosities are (3.0, 2.1, 1.3) × 1046 erg s−1.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The LCs calculated with VO at different distances r = 7 × 1013, r = 8 × 1013, and r = 9 × 1013 for Model P. The peak luminosities are (4.1, 4.5, 4.1) × 1046erg s−1 with durations of 1.4, 1.3, and 1.4 hr, respectively. These angle-averaged LCs of different photon-collecting radius show minor differences.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: 1D velocity and density profiles at three different viewing angles for Model P. The shock front is shown as the velocity jumps at ∼5.3 × 1013 cm. The density profiles vary across different viewing angles owing to the mixing. Small fluctuations of density and velocity in regions >5.3 × 1013 cm are caused by the radiation precursor.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The density and velocity evolution of Model T. The left panel is plotted without velocity contours to show the density structure clearly. The density and velocity distribution remains spherical around the shock front; however, the post-shock CSM becomes much more turbulent.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: RO LCs for Model T with different viewing angles. The dotted lines are for 0° and 90° for differentiating from other angles, and their peak luminosities are lower.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The distribution of radiation flux vectors of band VIII in Model P. The flux magnitude is maximum at the emitting region between the shock and the photosphere. Due to mixing, the radiation flux vectors are misaligned with radial directions, and their magnitude is also nonuniform.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: LCs from different viewing angles for band VIII in Model P. The LCs show small deviations during the rising phase, and the deviations slightly increase around the peak.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Color LCs of Model R; the dotted curves are smoothed LCs by data binning to better locate the peak. Before the luminosity peaks, the radiation precursor gradually heats the ring and creates small bumps from band I at 0.7 hr to around 1.1 hr for bands IV, V, and VI. During the breakout phase, the ring absorbs the short-wavelength radiation and reemits it into longer wavelengths. The dominant band of emission transits from VIII to VII after ∼3 hr of the shock breakout.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The density and velocity evolution of Model R. The middle panel reveals strong mixing around the reverse shock and shock front layer around the collision site of r ∼ (4–7) × 1013 cm. Finally, the ringlike CSM is completely destroyed by the shock, as shown in the right panel.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The peak luminosity and LC duration as a function of the mass-loss rate parameter (P; α = 0.1, 0.2, 0.5, 1.0, 2.0, 5.0, and 10). The dashed fitting curves are for the correlation between α and LC duration (pink) and peak luminosity (cyan). Higher values of α correspond to denser CSM profiles. We find that LC duration positively correlates with α: ﹩{\tau }_{\mathrm{shock}}\,=\,0.17\,\mathrm{log}\alpha +1.48﹩ hr. A dilute CSM tends to produce a higher peak luminosity with a shorter duration.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The density and velocity evolution of Model B. The companion star can hinder the shock and drive the turbulence through KH instabilities when the SN ejecta and shocked CSM pass.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Color LCs of Model P at a viewing angle of 45°; the dotted curves are smoothed by data binning to better identify the peak for longer wavelengths. The peak luminosity for band VIII is 4 × 1046 erg s−1, and the corresponding duration is 1.4 hr. The dominant band VIII transits to lower frequency bands VII and VI at ∼3 hr owing to the cooling of the photosphere. Larger fluctuations appear around the peak, followed by bumpy features at lower wavelengths.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The velocity and density profile from three different viewing angles in Model R. The velocity jumps at distances around 8.7 × 1013 cm and 8 × 1013 cm are the shock fronts. For the velocity profile of 45°, a reverse shock forms at 7.5 × 1013 cm from the collision of the ring.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Density snapshots from Model P with α = 0.1, 1.0, and 10. These snapshots are taken when the shock front arrives at ∼6 × 1013 cm. Higher α models form denser CSM profiles, and their breakout emission is delayed, but the shock front can still propagate to a comparable distance regardless of α values.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: LCs of band VIII in Model R. The LC duration is ∼1.45 hr, with peak luminosity at ∼3.5 × 1046 erg s−1. The LCs fluctuate owing to radiation precursor interaction with the ring.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The velocity and density profiles of Model B at ∼1890 s. At this time, the shock reaches 2.1 × 1013 cm, and the collision between the shock and the companion forms a strong reverse shock along 45° at 1.8 × 1013.
Paper: Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Authors: Haoyang Liu, Cuihua Du, Dashuang Ye, Jian Zhang, Mingji Deng
Figure caption: Thirty groups generated by HDBSCAN are divided into substructures in the E−L  z  plane, the L ⊥−L  z  plane, and in the Toomre diagram (from left to right), including previously known and unknown substructures: GSE (medium aquamarine), Helmi streams (pink), Arjuna (orange), I'itoi+Sequoia (navy), Thamnos (light blue), and the hot thick disk (magenta), as well as the three unknown debris PG1 (light coral), PG2 (light green),and Low Energy Group (yellow). The red dashed line indicates ∣V−V LSR∣ = 210 km s−1.
Paper: Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Authors: Haoyang Liu, Cuihua Du, Dashuang Ye, Jian Zhang, Mingji Deng
Figure caption: Top row: the velocity distributions in the V  R −V  ϕ , V  R −V  x , and V  x −V  y  spaces, where the sausage shape is visible in the V  R −v  ϕ  space. Bottom row: the eccentricity distribution along the galactocentric distance r gal and metallicity distribution of GSE with two noticeable peaks that peak around −1.25 and −0.7, respectively, where the latter peak is related to eccentric Splash stars. The chevron-like shape in the V  r −r gal space is shown and color-coded by energy.