adsabs/AstroCLIMB huggingface dataset:
Paper: Three-dimensional Global Hybrid Simulation of Magnetosheath Jets at Mercury
Authors: Jin Guo, San Lu, Quanming Lu, Junyi Ren, Jiuqi Ma, James A. Slavin, Weijie Sun, Jun Zhong, Xinliang Gao, Rajkumar Hajra, Rongsheng Wang
Figure caption: Plasma jets and cavities in Mercury’s magnetosheath under a radial IMF at t = 117 s. (a) Dynamic pressure (﹩{P}_{d}﹩) near the noon–midnight meridian plane. The gray 3D surface, identified by the boundary of the open–closed field lines, represents the magnetopause. The black dashed line indicates the bow shock, and the violet contour indicates ﹩{P}_{d}﹩ that is two times the background dynamic pressure (﹩{P}_{d0}﹩) in the magnetosheath. ﹩{P}_{d0}﹩ is obtained by smoothing the magnetosheath dynamic pressure with a 3D window of 0.21 RM × 0.21 RM × 0.21 RM. (b) The ratio of Pd and Pd0 downstream of the bow shock.
Paper: Longitudinal Dependence of Heavy Ion Composition in the 2021 October 28 Ground Level Enhancement Event
Authors: C. M. S. Cohen, G. M. Mason, E. R. Christian, A. C. Cummings, G. A. de Nolfo, M. I. Desai, J. Giacalone, M. E. Hill, A. W. Labrador, R. A. Leske, D. J. McComas, R. L. McNutt Jr, D. G. Mitchell, J. G. Mitchell, G. D. Muro, J. S. Rankin, N. A. Schwadron, M. M. Shen, M. E. Wiedenbeck, Z. G. Xu, G. C. Ho, R. F. Wimmer-Schweingrüber
Figure caption: Upper left: difference image of LASCO/C2 showing the CME (from CACTus; E. Robbrecht & D. Berghmans 2004). Upper right: SDO/AIA 171 Å image of the erupting active region (from SolarSoft, https://www.lmsal.com/solarsoft/latest_events_archive.html). Lower left: difference image of AIA 193 Å showing the EUV wave. Lower right: positions of the relevant spacecraft at the time of the event from Solar-MACH (J. Gieseler et al. 2023); the black arrow shows the longitude of the source active region. Colored lines correspond to nominal Parker spirals for 400 km s−1 solar wind at each spacecraft and for the active region (dashed black line).
Paper: Longitudinal Dependence of Heavy Ion Composition in the 2021 October 28 Ground Level Enhancement Event
Authors: C. M. S. Cohen, G. M. Mason, E. R. Christian, A. C. Cummings, G. A. de Nolfo, M. I. Desai, J. Giacalone, M. E. Hill, A. W. Labrador, R. A. Leske, D. J. McComas, R. L. McNutt Jr, D. G. Mitchell, J. G. Mitchell, G. D. Muro, J. S. Rankin, N. A. Schwadron, M. M. Shen, M. E. Wiedenbeck, Z. G. Xu, G. C. Ho, R. F. Wimmer-Schweingrüber
Figure caption: Upper left: O and Fe event-integrated fluence spectra from PSP, ACE, and STA as a function of energy. Upper right: the same data replotted with O fluences indicated by the left y-axis and Fe fluences on the right y-axis. The right y-axis has been shifted to align the STA O and Fe spectra (corresponding to an Fe/O ratio of 0.39). A power law with index of −1.7 is shown for reference. Lower left: Fe/O abundance ratios vs. energy calculated from the data plotted in the upper panels. A value of Fe/O = 0.39 is indicated by the horizontal line. Lower right: similar spectra plot as the upper right but for the two sensors on SolO.
Paper: Longitudinal Dependence of Heavy Ion Composition in the 2021 October 28 Ground Level Enhancement Event
Authors: C. M. S. Cohen, G. M. Mason, E. R. Christian, A. C. Cummings, G. A. de Nolfo, M. I. Desai, J. Giacalone, M. E. Hill, A. W. Labrador, R. A. Leske, D. J. McComas, R. L. McNutt Jr, D. G. Mitchell, J. G. Mitchell, G. D. Muro, J. S. Rankin, N. A. Schwadron, M. M. Shen, M. E. Wiedenbeck, Z. G. Xu, G. C. Ho, R. F. Wimmer-Schweingrüber
Figure caption: Fe/O at 10 MeV nuc−1 from STA vs. that from STB for several multispacecraft events where the two spacecraft were separated by <60° (circles). The box represents the 2021 October 28 event where the Fe/O value of 0.39 is consistent with all three spacecraft observations. Equality is indicated by the black diagonal line.
Paper: Longitudinal Dependence of Heavy Ion Composition in the 2021 October 28 Ground Level Enhancement Event
Authors: C. M. S. Cohen, G. M. Mason, E. R. Christian, A. C. Cummings, G. A. de Nolfo, M. I. Desai, J. Giacalone, M. E. Hill, A. W. Labrador, R. A. Leske, D. J. McComas, R. L. McNutt Jr, D. G. Mitchell, J. G. Mitchell, G. D. Muro, J. S. Rankin, N. A. Schwadron, M. M. Shen, M. E. Wiedenbeck, Z. G. Xu, G. C. Ho, R. F. Wimmer-Schweingrüber
Figure caption: H and He intensity time profiles at ∼4 MeV nuc−1 for the event from PSP/LET, STA/LET, ACE/SIS (which does not measure protons), and SolO/SIS (He is calculated by scaling the measured 1.3 MeV nuc−1 He intensities).
Paper: Gamma-Ray Bursts and Kilonovae from the Accretion-induced Collapse of White Dwarfs
Authors: Patrick Chi-Kit Cheong, 志杰 張, Tetyana Pitik, Luís Felipe Longo Micchi, David Radice
Figure caption: GRB 211211A and GRB 230307A data (dots with error bars and upper limits marked by triangles) compared with SNEC AB apparent magnitudes in Gemini J and Ks filters, with offsets applied for readability. The displayed data correspond to the model with Bpol = 1012 G (see Table 1 for ejecta properties). The bands account for uncertainties in ejecta velocity, total mass, and maximum opacity. We find that our model, with the strongest magnetic field and neutron-rich ejecta, is in good agreement with the observational data. Assumed distances are 350 Mpc for GRB 211211A and 291 Mpc for GRB 230307A.
Paper: Gamma-Ray Bursts and Kilonovae from the Accretion-induced Collapse of White Dwarfs
Authors: Patrick Chi-Kit Cheong, 志杰 張, Tetyana Pitik, Luís Felipe Longo Micchi, David Radice
Figure caption: Magnetization βmag := Pgas/Pmag profiles (color map) at different times (from left to right columns) of different models (from top to bottom rows). The blue regions show the matter-dominating regions (βmag > 1), while the red regions represent the magnetic-dominating ones (βmag < 1). For the Bpol = 1012 G case, significant parts of the shown regions are magnetic dominated, and a strongly magnetized jetlike structure is formed at the polar region. The corresponding magnetization βmag can decrease below 10−4.
Paper: Gamma-Ray Bursts and Kilonovae from the Accretion-induced Collapse of White Dwarfs
Authors: Patrick Chi-Kit Cheong, 志杰 張, Tetyana Pitik, Luís Felipe Longo Micchi, David Radice
Figure caption: Electron fraction Ye profiles (color map) and the magnetic field lines (blue streamlines) at different times (from left to right columns) for different models (from top to bottom rows). The Bpol = 109 G case is not shown, as it looks identical to the Bpol = 1010 G case. Neutron-rich outflow is found when the materials are accelerated out due to strong magnetically driven wind before reaching β-equilibrium. As shown in the figure, when the magnetic field is sufficiently strong (see also Figure 1), low-Ye materials can be accelerated and escape the disk region. It is clearly visible that the pattern of the electron fraction profile follows the magnetic fields lines.
Paper: Gamma-Ray Bursts and Kilonovae from the Accretion-induced Collapse of White Dwarfs
Authors: Patrick Chi-Kit Cheong, 志杰 張, Tetyana Pitik, Luís Felipe Longo Micchi, David Radice
Figure caption: The total ejected mass and energy (left and middle panels), and the jet energy (right panel) of accretion-induced collapse WDs as functions of time. Strong magnetically driven winds enhance the total amount of mass and energies. The jet energy counts the energy carried away via magnetically dominated collimated outflow that is leaving along the z-direction in the region where θ ≤ 10°. Solid, dashed, and dotted lines show the same diagnostic energy and with extra constraints on the magnetization: βmag ≤ 1, 0.1, 0.01, respectively.
Paper: Gamma-Ray Bursts and Kilonovae from the Accretion-induced Collapse of White Dwarfs
Authors: Patrick Chi-Kit Cheong, 志杰 張, Tetyana Pitik, Luís Felipe Longo Micchi, David Radice
Figure caption: 1D histograms of the ejecta of an accretion-induced collapse WD up to 1.3 s after bounce. These plots compare the distribution of the ejected mass as functions of electron fraction Ye, entropy per baryon s, asymptotic velocity v∞, and angle (﹩\theta \in \left[0^\circ ,90^\circ \right]﹩ from pole to equatorial plane) with different initial magnetic fields. The stronger the magnetic fields, the more neutron-rich the ejecta are. Notably, there is a significant amount of very neutron-rich ejecta (i.e., 0.133 M⊙ for Ye ≤ 0.25) in the case of Bpol = 1012 G.
Paper: Gamma-Ray Bursts and Kilonovae from the Accretion-induced Collapse of White Dwarfs
Authors: Patrick Chi-Kit Cheong, 志杰 張, Tetyana Pitik, Luís Felipe Longo Micchi, David Radice
Figure caption: Evolution of the rest-mass density-averaged magnetic fields 〈B〉PNS (left panel), angular momentum JPNS (middle panel), and rest-mass MPNS (right panel) of the proto-neutron stars.
Paper: Evaluating the Potential to Constrain Dark Matter Annihilation with Fermi-LAT Observations of Ultrafaint Compact Stellar Systems
Authors: Antonio Circiello, Alex McDaniel, Alex Drlica-Wagner, Christopher Karwin, Marco Ajello, Mattia Di Mauro, Miguel Á. Sánchez-Conde
Figure caption: Top: sensitivity of Fermi-LAT observations of UFCSs to DM annihilation via the ﹩b\mathop{b}\limits^{\unicode{x00304}}﹩ (left) and τ+τ− (right) channels. The solid black lines represent the constraints obtained from the combined analysis of the UFCSs in the nominal sample. The pink lines are constraints obtained excluding UMa III from this selection. The dotted–dashed purple lines are the constraints obtained from the combined analysis of UFCSs in the inclusive sample. The yellow and green regions are, respectively, the 95% and 68% containment bands for the inclusive sample obtained from the combined analysis of random subsets of 26 of the 1000 blank fields. The dotted line is the thermal relic cross section from G. Steigman et al. (2012). The dashed blue lines are constraints from A. McDaniel et al. (2024) for the measured sample of dSphs. The light blue profile represents the DM interpretation of the GCE from F. Calore et al. (2015), while the red point with error bars is the GCE measurement from M. Di Mauro & M. W. Winkler (2021). Center: sensitivity of Fermi-LAT observations to DM annihilation via the ﹩b\mathop{b}\limits^{\unicode{x00304}}﹩ (left) and τ+τ− (right) channels derived by randomly selecting half of the UFCSs in the inclusive sample. The green band represents the selections that do not include UMa III, while the pink band represents the selections that include this source. The solid lines represent the average constraint from the respective band of the same color. The solid black line represents the constraints from the nominal sample of UFCSs. We also include results from previous analyses on the dSphs (A. McDaniel et al. 2024) and GCE (F. Calore et al. 2015; M. Di Mauro & M. W. Winkler 2021). Bottom: sensitivity of Fermi-LAT observations to DM annihilation via the ﹩b\mathop{b}\limits^{\unicode{x00304}}﹩ (left) and τ+τ− (right) channels derived for different sizes of the random subsamples.
Paper: Resolving Turbulence Drivers in Two Luminous Obscured Quasars with JWST/NIRSpec Integral Field Unit
Authors: Mandy C. Chen, Hsiao-Wen Chen, Michael Rauch, Andrey Vayner, Weizhe Liu, David S. N. Rupke, Jenny E. Greene, Nadia L. Zakamska, Dominika Wylezalek, Guilin Liu, Sylvain Veilleux, Nicole P. H. Nesvadba, Caroline Bertemes
Figure caption: The second-order VSF, ﹩{S}_{2}^{{\prime} }(r)﹩. The top panel presents measurements constructed from the directly measured line-of-sight velocity maps of XID2028 and J1652, whereas the bottom panel shows the results with the velocity gradient subtracted maps (see columns (2)–(4) of Figure 1). Vertical dashed lines indicate the FWHM of the PSF for the two fields. The gray dotted–dashed curve represents ﹩{S}_{2}^{{\prime} }(r)﹩ with a Kolmogorov slope of 2/3, convolved with a mean PSF of the two fields. Gray-shaded regions represent previous measurements for a sample of eight extended nebulae around UV-luminous quasars at z ≈0.5–1 (M. C. Chen et al. 2023b; M. C. Chen et al. 2024). Within the overlapping scales of approximately 10–20 kpc, the measurements from XID2028 and the systemic gas of J1652 display a higher amplitude in contrast to the UV quasar sample. Conversely, the VSF of the tidally stripped gas in J1652 is  ~ 10 times lower in amplitude, in good agreement with the lower-redshift UV sample.
Paper: Resolving Turbulence Drivers in Two Luminous Obscured Quasars with JWST/NIRSpec Integral Field Unit
Authors: Mandy C. Chen, Hsiao-Wen Chen, Michael Rauch, Andrey Vayner, Weizhe Liu, David S. N. Rupke, Jenny E. Greene, Nadia L. Zakamska, Dominika Wylezalek, Guilin Liu, Sylvain Veilleux, Nicole P. H. Nesvadba, Caroline Bertemes
Figure caption: Top panel: turbulent heating rate per volume, Qturb, across various scales and systems. The blue-shaded region represents Qturb for the cool phase gas in XID2028 and the systemic component of J1652 with a density range of 10–500 cm−3. The green-shaded region shows the Qturb measured for the tidal gas of J1652. The red and red-hatched regions indicate the estimated Qturb for quasar nebulae at z ≈0.5–1, as presented in M. C. Chen et al. (2023b) and M. C. Chen et al. (2024), assuming gas densities of 0.01–1 cm−3 for the hot phase and 1–40 cm−3 for the cool phase. The gray-shaded region, showing measurements from S. Ganguly et al. (2023) for the ICM, represents an upper limit due to potential contributions from bulk motions in the utilized velocity maps. The brown-shaded region shows results for star-forming molecular clouds as presented in P. Hennebelle & E. Falgarone (2012). A. Marchal et al. (2021) measurements of Qturb for a bright concentration location in the HVC Complex C are shown by the green data points. Gray points display the results for CGM cool clumps based on absorption line measurements presented in H.-W. Chen et al. (2023a). The fields XID2028 and J1652 exhibit the highest Qturb among the systems presented here. Bottom panel: the eddy turnover time, teddy, for different systems.
Paper: Resolving Turbulence Drivers in Two Luminous Obscured Quasars with JWST/NIRSpec Integral Field Unit
Authors: Mandy C. Chen, Hsiao-Wen Chen, Michael Rauch, Andrey Vayner, Weizhe Liu, David S. N. Rupke, Jenny E. Greene, Nadia L. Zakamska, Dominika Wylezalek, Guilin Liu, Sylvain Veilleux, Nicole P. H. Nesvadba, Caroline Bertemes
Figure caption: The second-order VSF, ﹩{S}_{2}^{{\prime} }(r)﹩, measured for the inner and outer regions of the extended nebulae (see dashed circles in the second column of Figure 1). The top (bottom) panel shows the results from the XID2028 (J1652) field. We also include the ﹩{S}_{2}^{{\prime} }(r)﹩ of J1652’s tidal gas for comparison. Vertical dashed lines represent the FWHM of the PSF for the two fields. The gray dotted–dashed curve illustrates ﹩{S}_{2}^{{\prime} }(r)﹩ modeled with a Kolmogorov 2/3 slope, after convolution with the average PSF size of the two fields. The VSFs measured from the inner and outer regions of the XID2028 field display comparable amplitudes, while the inner VSF of the J1652 systemic gas exhibits a lower amplitude compared to its outer region, suggesting more energetic turbulent motions in the outer regions of J1652. Additionally, both the inner and outer regions of the J1652 systemic gas show a higher VSF amplitude compared to the tidal component.
Paper: Evaluating the Potential to Constrain Dark Matter Annihilation with Fermi-LAT Observations of Ultrafaint Compact Stellar Systems
Authors: Antonio Circiello, Alex McDaniel, Alex Drlica-Wagner, Christopher Karwin, Marco Ajello, Mattia Di Mauro, Miguel Á. Sánchez-Conde
Figure caption: Top: J-factor for the selected UFCSs derived using the scaling relations of A. B. Pace & L. E. Strigari (2019). We use the photometric J-factor relation (Equation (3)) for all the sources except UMa III, which is instead derived from the velocity dispersion scaling relation of A. B. Pace & L. E. Strigari (2019) as reported by M. Crnogorčević & T. Linden (2024). We included the average J-factors, with their uncertainties, for the dSphs (gray band) and the inclusive sample of UFCSs (purple band) Bottom: γ-ray flux upper limits in the [0.5 GeV–1 TeV] energy band at 95% confidence level for the selected UFCSs. The green and yellow containment bands are obtained by selecting blank fields that reside at the same Galactic latitude as each target (within ±5°).
Paper: Evaluating the Potential to Constrain Dark Matter Annihilation with Fermi-LAT Observations of Ultrafaint Compact Stellar Systems
Authors: Antonio Circiello, Alex McDaniel, Alex Drlica-Wagner, Christopher Karwin, Marco Ajello, Mattia Di Mauro, Miguel Á. Sánchez-Conde
Figure caption: V-band absolute magnitude vs. physical half-light radius for MW globular clusters, dSphs, and UFCSs. The dashed lines mark the minimum surface brightness used to select the inclusive (﹩\mu \gt 24\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩) and nominal (﹩\mu \gt 25\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩) samples, based on the model of V. Manwadkar & A. V. Kravtsov (2022). The light and dark gray-shaded areas represent the regions of inclusive and nominal selections, respectively. The purple points are the UFCSs in the inclusive sample. The UFCSs that are also included in the nominal sample are circled in red. A complete list of both samples is reported in Table 1. The gray points are the UFCSs that fall outside our selections and were excluded from the analysis for this reason. The cyan points are the confirmed dSphs from dmsky (https://github.com/fermiPy/dmsky). The dark blue triangles are the confirmed globular clusters from the Local Volume Database (A. B. Pace 2024).
Paper: Evaluating the Potential to Constrain Dark Matter Annihilation with Fermi-LAT Observations of Ultrafaint Compact Stellar Systems
Authors: Antonio Circiello, Alex McDaniel, Alex Drlica-Wagner, Christopher Karwin, Marco Ajello, Mattia Di Mauro, Miguel Á. Sánchez-Conde
Figure caption: Maximum TS over all cross-section values versus mass for the individual UFCSs in the ﹩b\mathop{b}\limits^{\unicode{x00304}}﹩ (left) and τ+τ− (right) channels. The colored lines highlight the targets that show a TS excess over the 97.5% and 84% containment regions for the individual blank fields (green and yellow bands).
Paper: Resolving Turbulence Drivers in Two Luminous Obscured Quasars with JWST/NIRSpec Integral Field Unit
Authors: Mandy C. Chen, Hsiao-Wen Chen, Michael Rauch, Andrey Vayner, Weizhe Liu, David S. N. Rupke, Jenny E. Greene, Nadia L. Zakamska, Dominika Wylezalek, Guilin Liu, Sylvain Veilleux, Nicole P. H. Nesvadba, Caroline Bertemes
Figure caption: From left to right: the columns display the continuum- and quasar-subtracted [O III] narrowband image, the LOS velocity map, the best-fit unidirectional velocity gradient, and the residual LOS velocity map with the unidirectional gradient removed. The contours in the first column correspond to surface brightness levels of [5, 10, 50, 100]﹩\times 1{0}^{-17}{\rm{erg}}\,{{\rm{s}}}^{-1}\,{{\rm{cm}}}^{-2}\,{{\rm{arcsec}}}^{-2}﹩. The top row presents the field of XID2028 at z = 1.5933, while the middle and bottom rows show the signal from the systemic and tidally stripped gas, respectively, in the field of J1652 at z = 2.9489. Note that the velocity panels only highlight spaxels included in the VSF measurements (see Section 2.3), and the narrowband image of J1652 shows the combined flux from outflows, systemic gas, and tidally stripped gas (see Section 2.2). The cross in each panel indicates the location of the quasar, and the black circle represents the size of the PSF in the data. The dashed circles in the second column represent the division of the inner versus outer regions for the VSF measurements (see Section 3.3). Both fields show extended emission reaching up to  ~ 20 kpc and the associated velocity fields appear to be turbulent.
Paper: MLody—Deep Learning–generated Polarized Synchrotron Coefficients
Authors: J. Davelaar
Figure caption: The ground truth values of MLody are plotted as a function of their corresponding fit function values. A perfect diagonal would mean identical values for both methods. The largest discrepancies are found for the rotation and conversion coefficients, ρQ and ρV.
Paper: MLody—Deep Learning–generated Polarized Synchrotron Coefficients
Authors: J. Davelaar
Figure caption: The same as Figure 1 but now as a function of the predictions of MLody. Compared to Figure 1 the performance is much higher, especially for the conversion and rotation coefficients.
Paper: MLody—Deep Learning–generated Polarized Synchrotron Coefficients
Authors: J. Davelaar
Figure caption: Loss as a function of epoch for the training and validation set. Both sets perform equally well, which is a clear indicator that we do not overfit the training data.
Paper: Metal Pollution in Sun-like Stars from Destruction of Ultra–short-period Planets
Authors: Christopher E. O'Connor, Dong Lai
Figure caption: Top: forced eccentricity of a USP on a 1-day orbit due to external companions of various masses m2 and eccentricities e2, as a function of the companion's semimajor axis a2. Dissipation in the planet dominates its tidal evolution when e1f exceeds the critical value e1cr, marked with a blue horizontal line. Bottom: same as the top panel, but for the estimated inspiral lifetime ﹩\tau =0.5| {a}_{1}/{\dot{a}}_{1}| ﹩ from a 1-day orbit. The orange shaded region marks the range of derived USP lifetimes τ in Table 1. We set M⋆ = M⊙, R⋆ = R⊙, m1 = M⊕, R1 = R⊕, k2,1ΔtL1 = 100 s, and ﹩{Q}_{\star }^{{\prime} }=3\times 1{0}^{6}﹩ in all calculations.
Paper: Metal Pollution in Sun-like Stars from Destruction of Ultra–short-period Planets
Authors: Christopher E. O'Connor, Dong Lai
Figure caption: Variation of 〈yu〉 (orange curves) and 〈yz〉 (blue) vs. Σ0 (top) and τ (bottom) under the constant-source-function population model (Equations (8)). In each panel, the other model parameter is held fixed at the value indicated in the lower right corner. Note in particular the simple behaviors that occur for Σ0τ ≪ 1.
Paper: Metal Pollution in Sun-like Stars from Destruction of Ultra–short-period Planets
Authors: Christopher E. O'Connor, Dong Lai
Figure caption: Time evolution of yu (orange curves) and yz under the constant-source-function model, using parameters derived from L. Spina et al. (2021; solid curves), A. Behmard et al. (2023a; dotted–dashed), and F. Liu et al. (2024; dashed).