adsabs/AstroCLIMB huggingface dataset:
Paper: Calibration of Complementary Metal-oxide-semiconductor Sensor–based Photometry to a Few-millimagnitude Precision: The Case of the Mini-SiTian Array
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Zhirui Li, Yongkang Sun, Timothy C. Beers, Min He, Jifeng Liu, Hong Wu, Yongna Mao, Bowen Huang, Mingyang Ma, Chuanjie Zheng, Hongrui Gu, Beichuan Wang, Lin Yang, Shuai Xu
Figure caption: The MST2 image of the test sky field, f02, has a center located approximately at R.A. = 73° and decl. = 41°. The field contains roughly 50,000 stars.
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: Exploring the eccentricity distribution beyond Gaia binaries. The left panel plots the mean eccentricity as a function of orbital periods for stellar and planetary companions. RV data are combined from S. Udry et al. (1998), D. Raghavan et al. (2010), R. F. Griffin (2012); visual binary data are from A. Tokovinin & O. Kiyaeva (2016); planet data are taken from exoplanetarchive.ipac.caltech.edu and are split into light and heavy Jovian companions. Stellar binaries beyond 103 days exhibit rising mean eccentricities. The right panel compares these long-period binaries against some models.
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: We use the Sun-like sample in Table 1 to explore the effects of detection bias. The left panel shows that the mean eccentricity (〈e〉) gradually declines with distance. The brown line is ﹩\langle e\rangle /\sqrt{\pi /2}﹩, a proxy for the Rayleigh mode. Using Equation (B1) to describe how distance affects the mode, we find an an intrinsic Rayleigh mode of σe0 ≈ 0.30, and that systems inward of d0 ∼ 150 pc should be free of detection bias. The blue curve on the left (﹩{\bar{\epsilon }}_{e}﹩) denotes the mean measurement error in eccentricity.
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: Correction for detection bias. The left panel repeats that in Figure 1. The middle panel shows the completeness as a function of binary eccentricity, obtained from the mock astrometry pipeline (K. El-Badry et al. 2024). The right panel shows the corrected values. Correction brings the different distributions into better agreements with each other, though some differences still exist. Measurement errors, not included here, may help resolve some of these differences.
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: A possible dependence of the Rayleigh mode on binary mass ratios is seen, in the Gaia Sun-like sample. The left panel shows the number of systems with reported mass ratios, divided by distances. The drop-off beyond mass ratio 0.6 may be explained by astrometric bias against detecting equal brightness pairs. The right panel shows the proxy for the Rayleigh mode, ﹩\langle e\rangle /\sqrt{\pi /2}﹩. A possible reduction toward equal mass is seen, but we remain suspicious.
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: Distribution in the sky-projected displacement-velocity angle γ for resolved binaries. The observed values (thick histograms for different values of projected separation s) are adopted from Figure 6 of H.-C. Hwang et al. (2022), and different models are in thin lines, with our best-fit mixture model (Appendix I) in red. Wide binaries (102 < s < 103 au) are best described by a thermal distribution, but close binaries (101 < s < 102 au) can be described equally well by a uniform distribution (﹩dN/de={\rm{const}}﹩) or by our mixture model.
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: Results of scattering experiments. We populate binary systems (primary 0.7M⊙, secondary M* = 0.3M⊙) with brown dwarfs that have the same total mass but different individual masses. The final binary e-distributions are Rayleigh in form (left panel, 100 cases each), with modes that depend only on the individual brown dwarf mass (Equation (4)). The right panel shows an example case with the orbits of the brown dwarfs as colored curves, and the secondary as heavy black curves. The vertical axis is the distance to the binary center of mass. All brown dwarfs are promptly ejected except for one that becomes bound to the primary.
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: Mass functions in the low-mass end, in differential (left panel) and cumulative forms (right panel, cumulative number). The two determinations are from young clusters and from microlensing of bulge stars. For both cases, the number ratio between brown dwarfs (taken to be below 0.05M⊙) and stars is ∼1/4, enough to excite Solar-type close binaries but not enough to harden them.
Paper: Density Fluctuation–Mach Number Scaling in Compressible, High Plasma Beta Turbulence: In Situ Space Observations and High-Reynolds Number Simulations
Authors: Riddhi Bandyopadhyay, James R. Beattie, Amitava Bhattacharjee
Figure caption: A two-dimensional slice of the logarithmic mass density fluctuations, ﹩\mathrm{ln}(\rho /{\rho }_{0})﹩, where ρ0 is the volume average, overlaid with in-plane magnetic field streamlines shown in white. The mean density ρ = ρ0 is shown in black, overdensities ρ > ρ0 in yellow, and underdensities ρ < ρ0 in green. Due to the strong ρ/ρ0 contrasts and the coherent, overdense filamentary structures and deep underdense voids, the mass-density (and magnetic field) is highly inhomogeneous. More details of the 10,0803 simulation are shown in J. R. Beattie et al. (2024).
Paper: Density Fluctuation–Mach Number Scaling in Compressible, High Plasma Beta Turbulence: In Situ Space Observations and High-Reynolds Number Simulations
Authors: Riddhi Bandyopadhyay, James R. Beattie, Amitava Bhattacharjee
Figure caption: An example of the MMS data in Earth’s turbulent magnetosheath. The data shown are from the FGM and FPI instruments onboard the MMS1 spacecraft. The top panel shows the magnetic field measurements in GSE coordinates; the second panel shows the electron density; the third panel shows the ion temperature; and the bottom panel shows the ion velocity in GSE coordinates. Each panel shows significant temporal turbulent fluctuations, which, under the assumption of Taylor’s frozen-in hypothesis, we can equate to sampling the spatial turbulent fluctuations.
Paper: Fast Transients from Magnetic Disks around Nonspinning Collapsar Black Holes
Authors: Justin Bopp, Ore Gottlieb
Figure caption: The time-averaged outflow efficiency in simulations with strong magnetic fields and rapid rotation (red dots) follows Equation (5) (blue curve) for a ≳ 0.3. For a ≲ 0.3, the outflow efficiency is dominated by disk outflows rather than the BH. BHs with weak magnetic fields (green square) or without accretion disks (turquoise diamonds) exhibit a low launching efficiency.
Paper: Fast Transients from Magnetic Disks around Nonspinning Collapsar Black Holes
Authors: Justin Bopp, Ore Gottlieb
Figure caption: Smoothed time evolution at the horizon for models with fast rotation that form accretion disks. Magnetic disks eject outflows more efficiently than hydrodynamic disks (model α9ω). Higher BH spins increase the launching efficiency (panel (a)), resulting in more powerful outflows (panel (c)). Consequently, higher spins exert stronger feedback on accretion, moderately reducing the mass accretion onto the BH (panel (b)).
Paper: Fast Transients from Magnetic Disks around Nonspinning Collapsar Black Holes
Authors: Justin Bopp, Ore Gottlieb
Figure caption: Vertical cut of the logarithmic mass density map of model a9σ shows that in the absence of an accretion disk, the jets become misaligned, resulting in an intermittent jittering behavior. The lighter blue regions are indicative of previous jittering jet episodes that have mixed with the infalling gas.
Paper: Spectral Diversity of DiSCo’s TNOs Revealed by JWST: Early Sculpting and Late Irradiation
Authors: R. Brunetto, E. Hénault, S. Cryan, N. Pinilla-Alonso, J. P. Emery, A. Guilbert-Lepoutre, B. J. Holler, L. T. McClure, T. G. Müller, Y. Pendleton, A. C. de Souza-Feliciano, J. Stansberry, W. Grundy, N. Peixinho, G. Strazzulla, M. T. Bannister, D. Cruikshank, B. Harvison, J. Licandro, V. Lorenzi, M. N. de Prá, C. Schambeau
Figure caption: (a) The 2.27 μm band area (CH3OH and other organics) and (b) 2.7 μm band area (CO2) as a function of eccentricity. (c) The 2.27 μm/2.7 μm band area ratio as a function of eccentricity. (d) The CO2 band area as a function of perihelion distance. A vertical dashed line is drawn at 31.3 au to guide the eye. Panels (a), (b), and (c) include an asymptotic exponential fit for Cliff1-TNOs to guide the eye.
Paper: Spectral Diversity of DiSCo’s TNOs Revealed by JWST: Early Sculpting and Late Irradiation
Authors: R. Brunetto, E. Hénault, S. Cryan, N. Pinilla-Alonso, J. P. Emery, A. Guilbert-Lepoutre, B. J. Holler, L. T. McClure, T. G. Müller, Y. Pendleton, A. C. de Souza-Feliciano, J. Stansberry, W. Grundy, N. Peixinho, G. Strazzulla, M. T. Bannister, D. Cruikshank, B. Harvison, J. Licandro, V. Lorenzi, M. N. de Prá, C. Schambeau
Figure caption: (a) PCA performed in the 0.78–4.45 μm range (the original spectra covered 0.6–5.3 μm; here we focus on the range of higher signal-to-noise ratio) on the complete DiSCo data set, including Bowl-types. (b) The SIR2 spectral slope (1.15–2.42 μm range) vs. the SIR1 spectral slope (0.7–1.2 μm range), including Bowl-types. This panel also includes ID49 2001 QY297, as its slopes indicate it as a Cliff2-TNO, like the other cold classicals. (c, d) SIR1 slope vs. the 2.27 μm band (CH3OH and other organics) and the 3 μm band (O–H, N–H). (e, f) Same as panels (c) and (d), but for SIR2. TNOs are labeled by their ObsID (Table A1). Slopes are measured in %/1000 Å. Note that these plots cannot discriminate between Cliff2-Eccentric and Cliff2-ColdCl.
Paper: Spectral Diversity of DiSCo’s TNOs Revealed by JWST: Early Sculpting and Late Irradiation
Authors: R. Brunetto, E. Hénault, S. Cryan, N. Pinilla-Alonso, J. P. Emery, A. Guilbert-Lepoutre, B. J. Holler, L. T. McClure, T. G. Müller, Y. Pendleton, A. C. de Souza-Feliciano, J. Stansberry, W. Grundy, N. Peixinho, G. Strazzulla, M. T. Bannister, D. Cruikshank, B. Harvison, J. Licandro, V. Lorenzi, M. N. de Prá, C. Schambeau
Figure caption: The 2.27 μm band area (methanol and organics) as a function of (a) semimajor axis and (b) aphelion. (c, d) Same as panels (a) and (b), but for CO2.
Paper: Spectral Diversity of DiSCo’s TNOs Revealed by JWST: Early Sculpting and Late Irradiation
Authors: R. Brunetto, E. Hénault, S. Cryan, N. Pinilla-Alonso, J. P. Emery, A. Guilbert-Lepoutre, B. J. Holler, L. T. McClure, T. G. Müller, Y. Pendleton, A. C. de Souza-Feliciano, J. Stansberry, W. Grundy, N. Peixinho, G. Strazzulla, M. T. Bannister, D. Cruikshank, B. Harvison, J. Licandro, V. Lorenzi, M. N. de Prá, C. Schambeau
Figure caption: Histogram of the DiSCo spectral groups split by dynamical classes. Scat: scattering disk objects. Resonant: see Table A1 for the resonances. HC: hot classical TNOs. CC: cold classical TNOs.
Paper: Spectral Diversity of DiSCo’s TNOs Revealed by JWST: Early Sculpting and Late Irradiation
Authors: R. Brunetto, E. Hénault, S. Cryan, N. Pinilla-Alonso, J. P. Emery, A. Guilbert-Lepoutre, B. J. Holler, L. T. McClure, T. G. Müller, Y. Pendleton, A. C. de Souza-Feliciano, J. Stansberry, W. Grundy, N. Peixinho, G. Strazzulla, M. T. Bannister, D. Cruikshank, B. Harvison, J. Licandro, V. Lorenzi, M. N. de Prá, C. Schambeau
Figure caption: The PCC (−1≤ r ≤1) between the 2.27, 2.5, 2.7, 3, 3.36–3.56, and 4.68 μm band areas, as well as SIR1 and SIR2, only for Cliff1-TNOs.
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: Eccentricity distribution for the Gaia Sun-like sample (Table 1), split by distances, shown in differential (left panel) and cumulative (right panel) forms. The gold sample (<150 pc, thick black lines) is least affected by selection bias in eccentricity and is well described by a Rayleigh distribution with a mode σe = 0.30 (gray-shaded areas). E-distributions for binaries at larger distances gradually shift to the left, reflecting the increasing severity of selection bias (not corrected here). They also suffer larger measurement uncertainties (﹩{\bar{\epsilon }}_{e}﹩, also not corrected here). The right panel also presents the N = 110 spectroscopic binaries within the same period range from S. Udry et al. (1998). The Gaia gold sample is statistically consistent with this set; both firmly reject the uniform hypothesis (dN/de ∝ e0).
Paper: Eccentricities of Close Stellar Binaries
Authors: Yanqin Wu, Sam Hadden, Janosz Dewberry, Kareem El-Badry, Christopher D. Matzner
Figure caption: Properties of the full sample from Table 1, split by primary radii (rows) and orbital periods (x-axis). The left panels show the period distributions, indicating different detection methods. The right panels show kernel density estimation in the ﹩e-\mathrm{log}P﹩ plane. The effects of tidal circularization are seen for binaries shortward of ∼20 days. But beyond that, all bins reach the same mean eccentricity (〈e〉, green curves), corresponding to a Rayleigh mode of ﹩{\sigma }_{e}=\langle e\rangle /\sqrt{\pi /2}=0.25﹩. The low-lying blue curves are the mean eccentricity errors (﹩{\bar{\epsilon }}_{e}﹩), with individual uncertainties ranging typically from 0.02 to 0.05.
Paper: A Recent Supermassive Black Hole Binary in the Galactic Center Unveiled by the Hypervelocity Stars
Authors: Chunyang Cao, F. K. Liu, Shuo Li, Xian Chen, Ke Wang
Figure caption: Cumulative distribution functions of velocity (left panel) and Galactocentric distance (right panel) of the HVSs of mass ≥2.5 M⊙ from our model after propagation through the Galactic potential to the distance between 50 and 120 kpc. The results (back hatched green and hatched blue) are obtained with the best-fitting parameters of our SMBHB model in the empty-loss-cone regime to the observational data of the late B-type halo HVSs without (W. R. Brown et al. 2018; black) and with (S. Kreuzer et al. 2020; gray) the corrections of the Gaia proper motions. To illustrate the uniqueness and advantage of our model, we also give the distributions obtained with binary tidal separation by the SMBH Sgr A* (pink) and the SMBHB slingshot in the full-loss-cone regime (purple).
Paper: A Recent Supermassive Black Hole Binary in the Galactic Center Unveiled by the Hypervelocity Stars
Authors: Chunyang Cao, F. K. Liu, Shuo Li, Xian Chen, Ke Wang
Figure caption: Semimajor axis distribution of the captured stars after the tidal separations of binaries predicted by our SMBHB model (green), compared to the observed distribution of the semimajor axis of the S-stars with the selection-effect truncation at 0.04 pc (gray arrow) from S. Gillessen et al. (2017) and F. Peißker et al. (2020; black). The captured stars expected by our SMBHB model consist of two populations: S-NSC population (blue back hatched) with progenitor binaries from the NSC and captured before the SMBHB coalescence, and the S-CWD population (orange hatched) with progenitor binaries from the CWD and predominantly captured after the SMBHB coalescence.
Paper: A Recent Supermassive Black Hole Binary in the Galactic Center Unveiled by the Hypervelocity Stars
Authors: Chunyang Cao, F. K. Liu, Shuo Li, Xian Chen, Ke Wang
Figure caption: All-sky detection probability map of the HVSs of mass ≥1.5 M⊙ and Galactocentric distance ≥1 kpc predicted for the S5 survey. The contours are labeled with the HVS number per unit logarithmic area, i.e., ﹩{d}^{2}N/d\mathrm{log}(R)d\mathrm{log}(v)﹩. The detection probability for the expected HVSs with progenitors from the CWD is in orange, and that from the young stellar population of the NSC is in blue. The HVS S5-HVS 1 is marked with a green “⋆,” which is located close to the peak detection probability of the HVSs originating from the CWD.
Paper: A Recent Supermassive Black Hole Binary in the Galactic Center Unveiled by the Hypervelocity Stars
Authors: Chunyang Cao, F. K. Liu, Shuo Li, Xian Chen, Ke Wang
Figure caption: The evolution of the semimajor axis (aMBHB) and eccentricity (eMBHB) of the SMBHB from the hardening radius ah (upper panel) and the production rate of HVSs of mass ≥2.5 M⊙ (lower panel) as functions of lookback time in our model with best-fitting parameters. The solid purple and dashed brown curves are, respectively, the production rate of HVSs through the slingshot effect (Γss) and the binary tidal separation (Γbt). The dashed–dotted pink curve (ΓCWD) shows the HVS production rate by the tidal separations of stellar binaries from the CWD. The vertical green dotted line marks the beginning of the formation of the 500 Myr population in the NSC. The cyan shadow region shows the time window when the halo HVSs observed in the MMT survey are ejected.
Paper: A Recent Supermassive Black Hole Binary in the Galactic Center Unveiled by the Hypervelocity Stars
Authors: Chunyang Cao, F. K. Liu, Shuo Li, Xian Chen, Ke Wang
Figure caption: Mean energy exchange fraction 〈C〉 as a function of the diffusion step length the angular momentum Ld in a unit of ﹩{L}_{2}={({T}_{{\rm{d}}}/{T}_{{\rm{r}}})}^{1/2}{L}_{{\rm{c}}}﹩. The orange vertical line marks the boundary between the full and empty-loss-cone regimes.
Paper: The Red Supergiant Progenitor of the Type II Supernova 2024abfl
Authors: Jingxiao Luo, Lifu Zhang, Bing-Qiu Chen, Qiyuan Cheng, Boyang Guo, Jiao Li, Yanjun Guo, Jianping Xiong, Xiangcun Meng, Xuefei Chen, Zhengwei Liu, Zhanwen Han
Figure caption: MIST evolution tracks of a massive star with initial mass range of 9 to 20 M⊙. The red box shows the luminosity of the SN 2024abfl progenitor at a distance of D = 15.6 Mpc; the error bar shows the luminosity range corresponding to ﹩15.{6}_{-3.0}^{+6.1}\,{\rm{Mpc}}﹩. The black star-shaped marks are the positions when carbon in the core is exhausted.
Paper: The Red Supergiant Progenitor of the Type II Supernova 2024abfl
Authors: Jingxiao Luo, Lifu Zhang, Bing-Qiu Chen, Qiyuan Cheng, Boyang Guo, Jiao Li, Yanjun Guo, Jianping Xiong, Xiangcun Meng, Xuefei Chen, Zhengwei Liu, Zhanwen Han
Figure caption: Spectra of LMC 002 with a different amount of extinction, normalized to have the same F814W as the SN 2024abfl progenitor. The F606W and F555W magnitudes of the progenitor are also marked. The central wavelength of each filter is placed at the pivot wavelength given by the HST FITS header.
Paper: Lyman Continuum Leakers at z  > 3 in the GOODS-S Field: Mergers Dominated
Authors: Shuairu Zhu, 帅儒 朱, Zhen-Ya Zheng, Fang-Ting Yuan, Chunyan Jiang, Ruqiu Lin
Figure caption: ΣSFR as a function of redshift. Red circles represent our sample of LyC leakers at 3 < z < 4.5 in the GOODS-S field, while gray squares indicate LyC leakers at z ∼ 0.3 (Y. I. Izotov et al. 2016a, 2016b, 2018a, 2018b; B. Wang et al. 2019; S. R. Flury et al. 2022). Star-forming galaxies at z > 5, including those at 5.0 < z < 7.2 (F070W dropouts), 7.2 < z < 9.7 (F090W dropouts), and 9.7 < z < 13.0 (F115W dropouts) from T. Morishita et al. (2024), are shown as gold diamonds. The filled and open red circles represent the high-confidence LyC leakers and the other LyC leakers in our sample, respectively. We also highlight sources of comparable size and MUV (0.5 kpc  < r50 < 1.2 kpc and −21.5 < MUV < −18) to LyC leakers in our sample using filled symbols. The filled and open large symbols represent the mean values of the comparison samples and the whole samples, respectively, and the error bars represent 1σ distributions for the comparison samples. The blue dashed line shows the ΣSFR evolution calculated from the size evolution given by T. Shibuya et al. (2015), assuming an SFR of 10 M⊙ yr−1. We use a red-shaded region to highlight the range of 1σ around the mean of our sample.
Paper: Lyman Continuum Leakers at z  > 3 in the GOODS-S Field: Mergers Dominated
Authors: Shuairu Zhu, 帅儒 朱, Zhen-Ya Zheng, Fang-Ting Yuan, Chunyan Jiang, Ruqiu Lin
Figure caption: Half-light radius (r50) vs. UV absolute magnitude MUV for high-z (3 < z < 4.5) LyC leakers (circles) in the GOODS-S. The sizes (r50) are derived from the ACS/F814W image. The high-confidence LyC leakers are represented by filled circles, and open circles represent the others. We also mark high-confidence LyC leakers by their names. We highlight LyC leakers where the LyC signal is not offset from the nonionizing emission using larger circles. The shaded region shows the size range of the sample that we use to select the comparison samples at other redshifts. For comparison, low-z LyC leakers (Y. I. Izotov et al. 2016a, 2016b, 2018a, 2018b; B. Wang et al. 2019; S. R. Flury et al. 2022). The color bar encodes the fesc values of high-z and low-z LyC leakers. The size–MUV relation for LBGs at z ∼ 4 is also displayed by blue lines (T. Shibuya et al. 2015). Arrows denote r50 of the PSF for ACS/WFC F814W, COS/NUV, and JWST/NIRCam F150W, and the values are 0.56 kpc at z = 3.5, 0.19 kpc at z = 0.3, and 0.19 kpc at z = 7, respectively.
Paper: On the Anisotropic Velocity Distribution of Newborn Pickup Ions in the Heliosheath
Authors: Senbei Du, Merav Opher, Marc Kornbleuth
Figure caption: The common logarithm of initial velocity distribution (unnormalized) of newborn pickups at vy ≃ 0. The left panel is the initial distribution and the right panel is taken at time Ωcit ≃ 1600.
Paper: On the Anisotropic Velocity Distribution of Newborn Pickup Ions in the Heliosheath
Authors: Senbei Du, Merav Opher, Marc Kornbleuth
Figure caption: The radial velocity distribution function of ISNs and the NSW. The distributions are mirrored with respect to the bulk flow velocity of 150 km s−1, plotted as the dashed lines of the corresponding colors.
Paper: On the Anisotropic Velocity Distribution of Newborn Pickup Ions in the Heliosheath
Authors: Senbei Du, Merav Opher, Marc Kornbleuth
Figure caption: Left: unnormalized pitch angle (cosine) distribution for selected particles at several times of the simulation. Top right: evolution of the width of the pitch angle distribution. Bottom right: enhancement of the phase-space density near μ = 0 over an isotropic distribution.
Paper: Lyman Continuum Leakers at z  > 3 in the GOODS-S Field: Mergers Dominated
Authors: Shuairu Zhu, 帅儒 朱, Zhen-Ya Zheng, Fang-Ting Yuan, Chunyan Jiang, Ruqiu Lin
Figure caption: High-resolution 2″ × 2″ cutouts for the LyC leakers. The cutouts are arranged in order of increasing fesc. In the top-left corner of each cutout, we show the source ID, the type of image used, and the criteria for identifying mergers. High-confidence LyC leakers are marked with a star next to their IDs. The redshift is indicated in the bottom-left corner and the star formation activity is shown in the bottom-right corner (MS for the star-forming main sequence and SB for starbursts).
Paper: On the Anisotropic Velocity Distribution of Newborn Pickup Ions in the Heliosheath
Authors: Senbei Du, Merav Opher, Marc Kornbleuth
Figure caption: Snapshots of magnetic field component Bx (left panel) and ion density ni (middle panel) at Ωcit = 200 from the simulation. Right: frequency spectra of δBx at several selected wavevectors.
Paper: On the Anisotropic Velocity Distribution of Newborn Pickup Ions in the Heliosheath
Authors: Senbei Du, Merav Opher, Marc Kornbleuth
Figure caption: The inverse maximum growth rates for the mirror mode ﹩{\gamma }_{\mathrm{mirror}}^{-1}﹩ (orange) and the charge-exchange timescale τ as functions of the newborn pickup ion fraction nn/ni. Both quantities are normalized by ﹩{\Omega }_{\mathrm{ci}}^{-1}﹩.