adsabs/AstroCLIMB huggingface dataset:
Paper: First Detections of PN, PO, and PO+ toward a Shocked Low-mass Starless Core
Authors: Samantha Scibelli, Andrés Megías, Izaskun Jiménez-Serra, Yancy Shirley, Jennifer Bergner, Judit Ferrer Asensio, Robin T. Garrod, Mélisse Bonfand, Anissa Pokorny-Yadav
Figure caption: PO emission observed toward Pers326 with the IRAM 30 m using both the 3 mm and 2 mm receivers. In solid red are the Gaussian fits to the detected (>3σ) lines, and in dotted red are LTE fits at Tex = 4.6 K. The vertical dashed line shows the consistent vlsr of 7.6 km s−1, and the horizontal gray line shows the 1σ noise level. Spectra are offset by 80 mK for easier viewing. Full quantum numbers for each transition are given in Table 1.
Paper: First Detection of Low-frequency Striae in Interplanetary Type III Radio Bursts
Authors: Vratislav Krupar, Eduard P. Kontar, Jan Soucek, Lynn B. Wilson, Adam Szabo, Oksana Kruparova, Hamish A. S. Reid, Mychajlo Hajos, David Pisa, Ondrej Santolik, Milan Maksimovic, Jolene S. Pickett
Figure caption: Solar wind plasma parameters recorded by Wind from 2010 March 13 to 2010 March 18. (a) Electron density (red). (b) Bulk speed (green) and estimated propagation of the source region (magenta). (c) Electron thermal speed (blue). (d) Magnetic field magnitude (cyan). The dashed line marks the type III burst onset on March 13, while the orange rectangle highlights the plasma parcel’s arrival time at 1 au (approximately 3 days later).
Paper: First Detection of Low-frequency Striae in Interplanetary Type III Radio Bursts
Authors: Vratislav Krupar, Eduard P. Kontar, Jan Soucek, Lynn B. Wilson, Adam Szabo, Oksana Kruparova, Hamish A. S. Reid, Mychajlo Hajos, David Pisa, Ondrej Santolik, Milan Maksimovic, Jolene S. Pickett
Figure caption: The 2010 March 13 type III radio burst as observed by the Wind and Cluster-4 spacecraft. (a) Dynamic spectrum from Wind, illustrating the burst onset at frequencies below 1 MHz. (b) Cluster’s WBD data in the 30–80 kHz range, highlighting the detected striae (zebra-like thin bands). Shaded intervals in (a) and (b) indicate the time–frequency ranges investigated more closely in Figure 3.
Paper: First Detections of PN, PO, and PO+ toward a Shocked Low-mass Starless Core
Authors: Samantha Scibelli, Andrés Megías, Izaskun Jiménez-Serra, Yancy Shirley, Jennifer Bergner, Judit Ferrer Asensio, Robin T. Garrod, Mélisse Bonfand, Anissa Pokorny-Yadav
Figure caption: PN emission centered on the F = 2–1 hyperfine component for each of the J transitions observed toward Pers326 with both the Yebes 40 m and IRAM 30 m. The solid blue and red curves are the Gaussian fits to the lines, the vertical dashed line shows a vlsr of 7.6 km s−1, and the horizontal gray line shows the 1σ noise level. Spectra are offset by 100 mK for easier viewing. Annotated on the spectra are also the locations of the weaker and blended hyperfine components.
Paper: First Detections of PN, PO, and PO+ toward a Shocked Low-mass Starless Core
Authors: Samantha Scibelli, Andrés Megías, Izaskun Jiménez-Serra, Yancy Shirley, Jennifer Bergner, Judit Ferrer Asensio, Robin T. Garrod, Mélisse Bonfand, Anissa Pokorny-Yadav
Figure caption: Rotation diagram for PN (red circle points) for the three observed J transitions as well as PO (blue square points) for the two observed J transitions. From the Monte Carlo simulations, the best fit is shown as the solid line, and the samples are shown as faded lines. The calculated column densities (Ntot) and excitation temperatures (Tex) are in the bottom left corner.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Evolutions of the mass-averaged out-of-weak-equilibrium potentials ﹩{\langle {\mu }_{{\rm{\Delta }}}\rangle }_{xy}﹩ for the 3-ν (dashed lines) and 5-ν (solid lines) scenarios when employing the SFHo EOS (top panel) or the DD2 EOS (bottom panel). Both npeν and npμν equilibria with asymptotic values ﹩{\mu }_{{\rm{\Delta }}}^{npe\nu }\approx {\mu }_{{\rm{\Delta }}}^{np\mu \nu }\approx 0﹩ in the gray shaded regions are also reported in Figures 1 and 9. Note that μν for calculating ﹩{\mu }_{{\rm{\Delta }}}^{npl\nu }﹩ is most accurate in regions with ρ > 1012 g cm−3 (P. L. Espino et al. 2024a), where the neutrinos are equilibrated thermally with the matter, and the mass-averaged values of ﹩{\langle {\mu }_{\Delta }^{npl\nu }\rangle }_{xy}﹩ are determined mainly in the high-density regions.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Columns, left to right: equatorial snapshots of the 5-ν scenarios for the SFHo (top) and DD2 (bottom) at the inspiral, merger, and postmerger phases, where the left (right) portion of each panel is associated with T (Yμ). The dotted, dashed–dotted, dashed, and solid lines show rest-mass density contours at 1011, 1012, 1013, and 1014 g cm−3, respectively, highlighting the dependence of muonization on high density and temperature.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: The same as Figure 1 but for the DD2 EOS.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Evolution of the conserved muon number Nμ(t) normalized to the initial value Nμ(0) for the two EOSs considered.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: The same as Figure 4 but for the DD2 EOS. Note that unlike SFHo cases, red lines are the total distributions, while green and blue lines refer respectively to ﹩\bar{t}\leqslant 6.5\,{\rm{ms}}﹩ and ﹩\bar{t}\geqslant 6.5\,{\rm{ms}}﹩. Similar to SFHo cases, Yμ is negligible, and Yp ≈ Ye.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: The same as Figure 5 but for the DD2 EOS.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: The same as Figure 3 but for the DD2 EOS. Note that the five-neutrino-species scenario shows a smaller decrease in Yp when compared to the SFHo EOS.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Comparison of the accumulated ejecta mass for the 5-ν and 3-ν scenarios and for the DD2 and SFHo EOSs. Here we find that 5-ν consistently results in lower postmerger ejecta for both EOSs.
Paper: Reconnection Nanojets in an Erupting Solar Filament with Unprecedented High Speeds
Authors: Yuhang Gao, Hui Tian, David Berghmans, Yadan Duan, Tom Van Doorsselaere, Hechao Chen, Emil Kraaikamp
Figure caption: Snapshots of the erupting filament and location of the Solar Orbiter. (a) EUI/HRI 174 Å  observation, with time calibrated to Earth time. (b) AIA 171 Å  observation. The red boxes in (a) and (b) indicate the same region. (c) Positions of Solar Orbiter and Earth at 23:50 UT on 2024 September 30.
Paper: Reconnection Nanojets in an Erupting Solar Filament with Unprecedented High Speeds
Authors: Yuhang Gao, Hui Tian, David Berghmans, Yadan Duan, Tom Van Doorsselaere, Hechao Chen, Emil Kraaikamp
Figure caption: Histograms of nanojet properties including durations, (maximum) length, width, speed, and kinetic energy.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: Total dust-to-stellar mass ratio as a function of redshift with dust masses predicted from AV following C. M. Casey et al. (2024a). We overlay the models of R. Schneider & R. Maiolino (2024) for SNe with (purple) and without (blue) reverse shock processing, as well as for AGB stars (orange hatched). The left and right panels show SN and AGB yields when the initial metallicity at z = 20 is above or below 0.1 Z⊙, respectively. In the upper right corner, we illustrate the change in ﹩{\mathrm{log}}\,{M}_{{\rm{dust}}}/{M}_{* }﹩ that would arise from factors of 2 in radius. The predicted dust-to-stellar mass ratios are largely within the range of SN yields with 60% favoring reverse shock processing and the remaining 40% requiring high yields with no destruction during the reverse shock. We emphasize that accurate dust masses are needed to validate the adoption of pure SN dust attenuation laws; however, the dust-to-stellar mass ratios we infer from the modeled AV are to first order self-consistent with SN yields assuming that the dust fully covers the extent of the rest-frame optical-emitting regions and that the dust is optically thin.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: (a) Grain size distribution normalized at 0.1 μm for standard dust (solid; J. S. Mathis et al. 1977) and SNe dust (dashed; T. Nozawa et al. 2003) with a break below ≈0.02 μm. (b) The rest-frame wavelength corresponding to the average extinction efficiency Qext for a grain of size a, based on the Astrodust model (B. T. Draine & B. S. Hensley 2021; B. S. Hensley & B. T. Draine 2023). Below a ≈ 0.016 μm, Qext converges to the Lyman limit, which is also the wavelength limit of Astrodust. Grains with a ≲ 0.2 μm contribute to UV attenuation, but the total UV attenuation is dominated by very small grains with a ≲ 0.01 μm that are ∼104×  more numerous because of the steep power-law grain size distribution. (c) The fraction of mass in dust grains with size < a. In all cases, 90% of the total dust mass is accounted for by grains with a > 0.1 μm that contribute negligibly to the total UV attenuation.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: Change in stellar mass and AV when assuming SN vs. SMC dust attenuation. Black circles show fits that converge to similar star formation histories under both attenuation law assumptions, whereas gray circles have divergent star formation histories. The solid black line shows the best-fit ﹩{\rm{\Delta }}\,{\mathrm{log}}\,{M}_{* }=0.6{\rm{\Delta }}{A}_{V}﹩ to fits with convergent star formation histories. We find that modeling SN dust with flat attenuation leads to higher stellar mass estimates by up to ∼0.8 dex and AV by up to ∼1 mag.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: Star formation history consistency between fits with SN and SMC dust using the 10 Myr burst fraction fb and ﹩{\chi }_{{\rm{SFH}}}^{2}﹩ as defined in Equation (3). We consider star formation histories between these two runs to be consistent (black) when the burst fractions agree within 20% or ﹩{\chi }_{{\rm{SFH}}}^{2}\lt 0.25﹩. A total of 96/138 (70%) fits are consistent, and the remaining 30% prefer different star formation histories when changing just the attenuation law.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: Empirical UV slopes β vs. the observed UV magnitudes taken from the best-fit models (black circles). The red diamonds show the weighted average of β in bins of ΔMUV = 2. The gray region encases the trends from M. W. Topping et al. (2024) for sources with z ∼ 6−9. The red line shows a linear fit to the binned average. Our results are generally consistent with the β−MUV trends of prior studies even with different dust prescriptions.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: Example SED fits to the JWST/NIRCam photometry of spectroscopically confirmed z > 8 galaxies from D. J. Eisenstein et al. (2023a), A. J. Bunker et al. (2024), and F. D'Eugenio et al. (2025). Photometry shown with filled (open) circles has SNR > 5 (SNR < 5). Red and blue SEDs show the maximum-likelihood models when assuming flat attenuation for SN dust and SMC dust attenuation, respectively.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: Stacked histograms of stellar mass, AV, UV slope β, and total UV magnitude MUV for our sample subdivided into three redshift bins: z < 7 with mean z = 6.6 (black), 7 < z < 8 with mean z = 7.3 (blue), and z > 8 with mean z = 9.1 (red). We report the 16th, 50th, and 84th percentiles in each redshift bin at the top of each panel.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: Reduced χ2 from model fits using SN vs. SMC dust attenuation calculated in the rest-frame UV. The one-to-one relation is shown with the dashed black line, and black (gray) circles have consistent (inconsistent) star formation histories as defined in Section 5.2. Fairly flat dust attenuation laws find better fits to the rest-frame UV data of z = 6−12 galaxies.
Paper: Modeling Galaxies in the Early Universe with Supernova Dust Attenuation
Authors: Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides, Arianna S. Long
Figure caption: Stacked histogram showing the change in MUV measured from the model SEDs assuming SN vs. SMC dust attenuation. The dark (light) gray histogram corresponds to sources with convergent (divergent) star formation histories between the two fitting assumptions. Fairly flat attenuation leads to fainter observed MUV by ﹩0.2{3}_{-0.16}^{+0.18}﹩ mag.
Paper: XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stéphane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Andrew Fabian, Dylan Nelson, Nobuhiro Okabe, Annalisa Pillepich, Cicely Potter, Manon Regamey, Kosei Sakai, Mona Shishido, Nhut Truong, Daniel R. Wik, John ZuHone
Figure caption: A histogram of velocities of cluster member galaxies within ﹩r\lt 2{0}^{{\prime} }﹩ from the Coma X-ray center, retrieved from Sloan Digital Sky Survey, DESI, and NASA/IPAC Extragalactic Database (NED; 2019) archival data. The gas velocities measured with XRISM for the Center and South fields (marked C and S, respectively) are offset from the cluster galaxy mean. The two main BCGs are marked; NGC 4874 is located near the Center field.
Paper: On the Orbital Effects of Stellar Collisions in Galactic Nuclei: Tidal Disruption Events and Ejected Stars
Authors: Sanaea C. Rose, Brenna Mockler
Figure caption: Left column: we show the final masses of our sample stars vs. their final distances from the SMBH for four select simulations without relaxation, allowing us to isolate the effect of collisions. The final mass and distance are the star's properties either when it evolved off the main sequence or at the end of the 10 Gyr integration time, whichever is shorter. The gray points are the initial conditions, while red circles are the final sample stars that remained in the cluster. Blue diamonds denote stars that escaped from the cluster, and black and lime stars represent TDEs from different types of collisions, mergers and high-speed collision deflections, respectively. In the upper right corner, we indicate the percentage of stars that became unbound orbits. Since unbound orbits have a negative semimajor axis, here we plot the absolute value for their final orbits. Right column: we show the orbital period of the stars when they become TDEs vs. β, the ratio of the tidal radius to the orbit’s periapsis. The gray dashed horizontal line marks 30 yr, approximately the threshold below which we could conceivably observe multiple passages. Rows: each row corresponds to different initial conditions or collision treatment. The first row uses the Rauch99 prescription for mergers and mass loss. The second row is identical to the above except we always reduce the postcollision speed in the center-of-mass frame by 10% for high-speed collisions. The third and fourth rows use Rauch99 and Lai+93 fitting formulae, respectively. These are higher-resolution “zoom-in” simulations where the stars have been sampled on a cusp from 0.001 to 0.1 pc. In this radius range, the collision timescale becomes comparable to the lifetime of a solar mass star, and increasing our resolution in this range allows us to follow rarer events, such as merger TDEs.
Paper: On the Orbital Effects of Stellar Collisions in Galactic Nuclei: Tidal Disruption Events and Ejected Stars
Authors: Sanaea C. Rose, Brenna Mockler
Figure caption: Upper panel: we plot the relevant timescales as a function of distance from the SMBH for a range of stellar density profiles, α = 1.25 (dashed line) to α = 1.75 (solid line). The collision and relaxation timescales are in red and blue, respectively, while the gray line marks the total simulation time of 10 Gyr. The vertical red line emphasizes the radius at which the collision timescale equals the simulation time; within this radius, collisions are common and shape the evolution of the stars and cluster. We also mark the radius at which the velocity dispersion is approximately the escape speed from the surface of a Sun-like star using the green vertical line. External to this radius, we expect collisions to result in mergers. Lower panel: we consider a hyperbolic encounter between two stars in the cluster. This plot shows the impact parameter in solar radii for a 90∘ deflection as a function of the relative speed between the stars. Note that the x-axis is inverted to reflect the dependence of velocity dispersion on distance from the SMBH; it parallels the x-axis of the plot above, with the largest velocities occurring near the SMBH and decreasing further out. We have marked the speeds that correspond to the inner and outer allowed initial semimajor axes of the stars in our sample, 0.001 and 1 pc, respectively. Additionally, we mark where b90 becomes equal to the star’s radius. This point coincides well with the speed at which we would expect the collision outcome to transition from mergers to the sorts of high-speed encounters that might strip or destroy stars but leave them unbound from each other.
Paper: On the Orbital Effects of Stellar Collisions in Galactic Nuclei: Tidal Disruption Events and Ejected Stars
Authors: Sanaea C. Rose, Brenna Mockler
Figure caption: We plot the final vs. initial eccentricities for the stars on unbound orbits for the first and second rows in Figure 2. Both the initial and final eccentricities are clustered near 1, with the initial eccentricities slightly under this value and the final eccentricities above. The diamonds are color coded by the speed at infinity of the unbound stars, whose distributions are shown in the histograms. We note that this calculation does not take into account any additional contribution to the potential, such as the stellar cluster, beyond the mass of the SMBH. Typical ﹩{v}_{\inf }﹩ are of order 100 km s−1.
Paper: On the Orbital Effects of Stellar Collisions in Galactic Nuclei: Tidal Disruption Events and Ejected Stars
Authors: Sanaea C. Rose, Brenna Mockler
Figure caption: This figure shows semimajor axis vs. 1 − e, a quantity proportional to the periapsis distance, of the sample stars from the first three rows of Figure 2. Systems with ef > 1 (unbound orbits) are omitted, as are uncollided stars, whose properties cannot change without two-body relaxation. In the bottom panel of each plot, gray dots represent the initial population. Stars with M > 1 M⊙, represented by green circles, must have experienced a merger. Orange dots are stripped stars (0.08 M⊙ < M < 1 M⊙), indicative of a high-speed collision. Destroyed stars (M < 0.08 M⊙) are marked with pink crosses. TDEs are marked using the same conventions as in Figure 2 and lie on nearly radial orbits with extreme eccentricity values. To guide the eye, we plot the full (partial) disruption radii for a 1 M⊙ star in dashed (dotted) black lines. The upper panel of each plot shows a histogram of the spatial distribution of these subpopulations in the same color scheme as the scatter plot.