adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Contour map of a source image made from ALMA continuum Cycle 4 image (left) and fitted model image (right). The quasar core component is subtracted off in both the maps. The color images and contours show the intensity of MG J0414+0534. Potential perturbation is not taken into account. Red points show the positions of caustics. The green X shows the position of the fitted quasar core.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Super-resolution achieved by de-lensing. Each colored circle shows a lensed image of a point source convolved with a PSF in the lens plane (left). The corresponding de-lensed (zoomed up) images in the source plane are shown with ellipses with the same color (right). The horizontal bars in both the figures indicate scale bars with the same angular size. Due to errors in the potential, de-lensed PSFs are not aligned for models with the background smooth potential (top right) but aligned for those with a perturbed true potential (bottom right).
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Mock ALMA continuum image (simulated Cycle 2 + Cycle 4 observations) of MG J0414+0434. The imaging was carried out with a Briggs weighting of robust = 0.5. The synthesized beam size is 0.″041 × 0.″037, and the P.A. is 54.°2. The background rms noise is 20 μJy beam−1.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: The master flowchart of overall procedure. Items marked in thin, thick, and dotted lines represent the pre-process, main process, and post-process, respectively. “Source plane+α χ 2” is described in Equation (1). “Visibility fit” is described in Section 6.3, and “lens-plane χ 2” is described in Section 6.4. The MIR data are obtained with Subaru (Minezaki et al. 2009) and Keck (MacLeod et al. 2013).
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Meshes in the lens plane (left) and source plane (right) for the fiducial smooth model.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Schematic picture of halos (yellow disks) and troughs (blue bars) in sight lines. The cylinder represents bundles of light rays that pass the vicinity of an Einstein ring in the lens plane.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Contour map of a de-lensed image made from simulated ALMA observations of a core-subtracted mock source. The color images and contours show the intensity. The black points show the centers of meshes. The red points show the positions of caustics. The green X shows the position of the fitted quasar core.
Paper: Internal and External Alignment of Carbonaceous Grains within the Radiative Torque Paradigm
Authors: Thiem Hoang, Vo Hong Minh Phan, Le Ngoc Tram
Figure caption: Top panels: grain size for efficient IA from inelastic relaxation (﹩{a}_{\min ,\mathrm{aJ}}^{\mathrm{high}-J}(\mathrm{iER})﹩, solid lines) and from NR (﹩{a}_{\min ,\mathrm{aJ}}^{\mathrm{high}-J}(\mathrm{NR})﹩ and ﹩{a}_{\max ,\mathrm{aJ}}^{\mathrm{high}-J}(\mathrm{NR})﹩, dotted and dashed lines respectively) vs. the gas density assuming grains aligned at high-J attractors by RATs with U = 103 (top left-hand panel) and 104 (top right-hand panel) with γ = 1 and ﹩\bar{\lambda }=2.5﹩                      μm. Regions of the parameter space where grains are expected to have right IA with inelastic and NR are marked with hatched and shaded areas, respectively. Bottom left-hand panel: same as the top panels bit for U = 105. Bottom right panel: same as the left-hand panel but for grains aligned at low-J attractors with Ω = Ω T .
Paper: Internal and External Alignment of Carbonaceous Grains within the Radiative Torque Paradigm
Authors: Thiem Hoang, Vo Hong Minh Phan, Le Ngoc Tram
Figure caption: Timescales for external alignment of HAC grains via k-RAT (red lines), B-RAT (green lines), and E-RAT (blue lines) vs. grain size. Results are shown for grains at both high-J (left-hand panel) and low-J (right-hand panel), assuming B = 5 μ G, n H = 10 cm−3, U = 1, γ = 0.3, and ﹩\bar{\lambda }=1.2\,\,\mu {\rm{m}}﹩ in the diffuse ISM. The gas-damping timescale is also overlaid for comparison (black lines).
Paper: Internal and External Alignment of Carbonaceous Grains within the Radiative Torque Paradigm
Authors: Thiem Hoang, Vo Hong Minh Phan, Le Ngoc Tram
Figure caption: Illustration of the torque-free motion of a spheroidal grain of principal axes ﹩{\hat{{\boldsymbol{a}}}}_{1}{\hat{{\boldsymbol{a}}}}_{2}{\hat{{\boldsymbol{a}}}}_{3}﹩. In the body frame, the angular momentum ( J ) and angular velocity (Ω) are both precessing around the axis of maximum inertia ﹩\hat{{\boldsymbol{a}}}﹩                      1 with the angular rate ω. Efficient internal relaxation would induce the alignment of both  J  and Ω with ﹩\hat{{\boldsymbol{a}}}﹩                      1 (IA). From Hoang et al. (2022).
Paper: Internal and External Alignment of Carbonaceous Grains within the Radiative Torque Paradigm
Authors: Thiem Hoang, Vo Hong Minh Phan, Le Ngoc Tram
Figure caption: Grain size for efficient IA from inelastic relaxation (﹩{a}_{\min ,\mathrm{aJ}}^{\mathrm{high}-J}(\mathrm{iER})﹩ and ﹩{a}_{\max ,\mathrm{aJ}}^{\mathrm{high}-J}(\mathrm{iER})﹩, solid-red lines) and from NR (﹩{a}_{\max ,\mathrm{aJ}}^{\mathrm{high}-J}(\mathrm{NR})﹩, solid-blue line) vs. the gas density, assuming grains rotating suprathermally at high-J attractors by RATs with U = 1, γ = 0.3, and ﹩\bar{\lambda }=1.2\,\mu {\rm{m}}﹩. We marked also the regions of the parameter space where grains are expected to have right IA with inelastic relaxation (red-hatched area) and NR (blue-shaded area), respectively. Grain sizes for efficient IA due to inelastic relaxation (﹩{a}_{\max ,\mathrm{aJ}}^{\mathrm{low}-{\text{}}J}(\mathrm{iER})﹩, dashed-red line) and NR (﹩{a}_{\max ,\mathrm{aJ}}^{\mathrm{low}-{\text{}}J}(\mathrm{NR})﹩, dashed-blue line) for grains aligned at low-J attractors are also shown.
Paper: Internal and External Alignment of Carbonaceous Grains within the Radiative Torque Paradigm
Authors: Thiem Hoang, Vo Hong Minh Phan, Le Ngoc Tram
Figure caption: Schematic illustration of the precession of the grain angular momentum ( J ) around the radiation direction ( k ) and the magnetic field ( B ), assuming the perfect IA of the grain shortest axis with  J . The grain’s magnetic moment is directed along  J  due to the Barnett effect. The fastest precession establishes the axis of grain alignment by RATs from Hoang et al. (2022).
Paper: Internal and External Alignment of Carbonaceous Grains within the Radiative Torque Paradigm
Authors: Thiem Hoang, Vo Hong Minh Phan, Le Ngoc Tram
Figure caption: Upper panel: grain size for efficient external alignment at high-J attractors. In this case, grains are externally aligned mostly via B-RAT and E-RAT. The parameter space of B-RAT and E-RAT is marked with the shaded red and blue regions, respectively. Grains at high-J attractor are assumed to rotate suprathermally via RAT in the ISRF with U = 1, γ = 0.3, and ﹩\bar{\lambda }=1.2\,\,\mu {\rm{m}}﹩. Lower panel: same as the upper panel but for external alignment at low-J attractors. Given the radiation field assumed, grains at low-J are more likely to be aligned via k-RAT (green-shaded region) and E-RAT (blue-shaded region).
Paper: Internal and External Alignment of Carbonaceous Grains within the Radiative Torque Paradigm
Authors: Thiem Hoang, Vo Hong Minh Phan, Le Ngoc Tram
Figure caption: Frequency-dependence susceptibility for different values of the nucleon number density n  n  = 1021 cm−3 (red), n  n  = 5 × 1021 cm−3 (green), and n  n  = 1022 cm−3 (blue). A rapid decrease of the susceptibility with increasing frequency is seen.
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a)–(c) Time evolution of electron temperature T  e . Ion-scale islands 1–3 are the same as those in Figure 1. T  e  becomes large in ion-scale islands (panel (b)). After those ion-scale islands are dissipated (panel (c)), T  e  still shows large values. (d) Energy spectra at these three times, in log–log scale, obtained in the x-interval marked by the red horizontal bar under the x-axis in each time. The horizontal red bar in panels (a), (b), and (c) covers the region 43 < x/d  i  < 45 (panel (a)), 45 < x/d  i  < 47 (panel (b)), and 47 < x/d  i  < 49 (panel (c)). (e) The same energy distributions as in panel (d), but in log-linear scale. In panels (d) and (e), black curves are spectra in the upstream region, at x = 500d  i . Nonthermal electrons are generated, and the spectra show a power law, with an index around 6.
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a)–(c) (Red) The trajectory of an electron accelerated in an ion-scale island in the x–y plane. (Black) Magnetic field lines. (d) The trajectory in the x–z plane. The position z is based on the time integral of v  z . (e) Time evolution of Lorentz factor γ. (f) The time evolution of the work done by the perpendicular electric field (W ⊥ in red), the work done by the parallel electric field (W ∥ in blue), and the sum of these two (W total in green). (g) Time evolution of the perpendicular momentum (p ⊥ in red) and the parallel momentum (p ∥ in blue). (h) Time evolution of the work done by the electric field E  x  (W  x  in red), by E  y  (W  y  in blue), and by E  z  (W  z  in green). In panels (e)–(h), the time interval between the two blue vertical lines represents when the electron is interacting with the ion-scale magnetic island.
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Profiles of y-averaged quantities. (a) 〈E  x 〉, (b) 〈E  y 〉, (c) 〈E  z 〉, and (d) 〈B  z 〉. 〈E  x 〉 is positive in the shock transition region, forming a large cross-shock potential. 〈E  z 〉 is fluctuating around the upstream value 0.067B 0. 〈B  z 〉 becomes negative in the shock transition region.
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a)–(c) The trajectory of another electron. (d)–(f) Time evolution of γ, W ⊥, W ∥, W total, p ⊥, and p ∥. Panels (a)–(f) are in the same format as in Figure 9. This electron shows clear signatures of Fermi acceleration. (g) Evolution of γ in the y–γ plane. The positions of X3 and X5 are shown by the vertical dashed lines. Each color shows a segment in each bounce motion, either from right to left or from left to right (denoted by R → L or L → R). At each bounce motion, γ increases. (h) γ as a function of time. Each color corresponds to the time interval in each segment shown in panel (g).
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a)–(l) Reduced 2D electron distribution functions at position A (X line), shown in Figure 6. Panels (a)–(c) are distribution functions at Ω i  t = 18.75, and the white lines in panels (b) and (c) show the direction of the magnetic field. Panel (a) shows the velocity plane perpendicular to the magnetic field. As time evolves, the temperature (thermal spread) increases, and multiple beams are generated. (m)–(o) Electron distributions at position A′ in Figure 6. Compared with panels (j)–(l) for position A, the thermal spread around each of multiple beams is larger, suggesting that heating occurs.
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a)–(d) Time evolution of electron temperature T  e . The magenta point (A) is the position of an X line, while the cyan point (B) is inside an ion-scale island. (e)–(f) Electron energy spectra at position A (panel(e)) and position B (panel (f)). At Ω i  t = 19.69 (panel (d)), there is no X line around position A, and the magnetic island above position A seen in panel (c) has already been dissipated in panel (d). Two positions, A and A′, are chosen in the region where T  e  is large (red color region).
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a)–(c) (Red) The trajectory of an electron in the x–y plane. (Black) Magnetic field lines. X1 and X2 denote the locations of X lines. (d) Time evolution of the Lorentz factor γ. (e) Time evolution of the work done by the perpendicular electric field (W ⊥ in red), the work done by the parallel electric field (W ∥ in blue), and the sum of these two (W total in green). (f) Time evolution of the perpendicular momentum (p ⊥ in red) and the parallel momentum (p ∥ in blue).
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Contours of electric fields: (a)–(c) E  x , (d)–(f) E  y , and (g)–(i) E  z . Black curves are magnetic field lines. In ion-scale islands, there are strong in-plane electric fields (E  x  and E  y ) pointing to the center of each island.
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Reduced 2D electron distribution functions at position B (magnetic island), shown in Figure 6. White lines show the direction of the magnetic field. As time evolves, the temperature (thermal spread) increases, and at the same time, a strong z-directional beam is generated.
Paper: The Imprint of Convection on Type I X-Ray Bursts: Pauses in Photospheric Radius Expansion Lightcurves
Authors: Simon Guichandut, Andrew Cumming
Figure caption: Results of the Schwarzschild run. Top: hydrogen profile after convective mixing. To avoid numerical difficulties during the hydrodynamic wind (see Section 3.3), the profile was smoothed using a monotonic cubic spline. The dashed lines show the minimum column reached by convection ﹩{y}_{{\rm{c}},\min }﹩, and the total column ejected by winds y w. Bottom: lightcurve of the burst. The pause occurs after surpassing L Edd of the accreted material (X = 0.7, bottom dotted line). The following rise takes place over a much longer timescale because ﹩{y}_{{\rm{w}}}\gg \,{y}_{{\rm{c}},\min }﹩. In general, the outgoing luminosity follows the Eddington luminosity of the material that is currently being ejected (blue dotted line), which we can track using y ej(t) (see Section 3.4).
Paper: The Imprint of Convection on Type I X-Ray Bursts: Pauses in Photospheric Radius Expansion Lightcurves
Authors: Simon Guichandut, Andrew Cumming
Figure caption: Composition profiles before (left) and after (right) the thermonuclear flash, which ignites at t = t 0. The lines for different elements have the same colors in the left and right panels. In the ∼1.4 s it takes to reach the Eddington luminosity, convection has significantly mixed the He and H layers. Dotted lines show the depletion column y d (left) and the minimum extent of convection ﹩{y}_{{\rm{c}},\min }﹩ (right). All runs shown in this paper begin at the ignited model t = t 0, which the left panel leads up to. The panel on the right shows the result of mixing using the Schwarzschild criterion prescription for convective boundaries (see Section 3.2).
Paper: The Imprint of Convection on Type I X-Ray Bursts: Pauses in Photospheric Radius Expansion Lightcurves
Authors: Simon Guichandut, Andrew Cumming
Figure caption: Results for all convective prescriptions and spatial resolutions tested in this work. Left: mass fraction of 1H in the atmosphere after the convective rise and before the ejection by winds. The circles label the locations of y w resulting from each simulations. The black line shows the hydrogen gradient at ignition, from which all runs start. Right: lightcurve of the bursts. The dotted lines mark the locations of L Edd for X = 0.7 and X = 0, as in Figure 6. Some simulations could not integrate through the decay phase and were stopped short at the “x” symbols. The inset zooms in on the pauses.
Paper: The Imprint of Convection on Type I X-Ray Bursts: Pauses in Photospheric Radius Expansion Lightcurves
Authors: Simon Guichandut, Andrew Cumming
Figure caption: Diagram illustrating the three main stages of the mixed H/He burst. (A) As hydrogen burns stably throughout accretion, distinct hydrogen and helium-rich layers build up in the envelope, their boundary being at a known column depth of y d (Equation (2)). We are interested in bursts that ignite at y > y d (red color indicates nuclear burning). (B) Heat from nuclear burning creates a growing convection zone (blue semicircles), which penetrates into the H-rich layer, resulting in additional nuclear burning. (C) As the convection zone retreats, it leaves behind a layer of constant hydrogen fraction at a column ﹩{y}_{{\rm{c}},\min }\lt {y}_{{\rm{d}}}﹩, a mixed H-He layer, and nuclear ashes at depth. Winds progressively eject the layers, up to a column ﹩{y}_{{\rm{w}}}\gt {y}_{{\rm{c}},\min }﹩, during which the observed luminosity at infinity is the Eddington luminosity, which depends on the hydrogen fraction X of the material. Because X is initially constant, we first observe a pause after the initial burst rise. After the H layer is ejected, the luminosity once again rises in a manner that depends on the hydrogen gradient dX/dy. See text for further details.
Paper: The Imprint of Convection on Type I X-Ray Bursts: Pauses in Photospheric Radius Expansion Lightcurves
Authors: Simon Guichandut, Andrew Cumming
Figure caption: Kippenhahn diagrams for the Schwarzschild run, centered on the moment of collision between the convection zone and the H layer. The bottom panel is zoomed in on a 1.5 ms window following the collision. The color scale traces the energy generation or loss (nuclear burning minus all neutrino losses), while the green hatches mark the convection zones. The solid black lines show the location of the depletion depth y d. In the top panel, the dashed line shows the luminosity coming out of the atmosphere, normalized by the Eddington luminosity of the accreted gas (scale on the right-hand side). In the bottom panel, it shows the integrated nuclear power (∫dm ϵ nuc). Moments where certain reactions dominate are labeled (see Section 3.2).
Paper: The Imprint of Convection on Type I X-Ray Bursts: Pauses in Photospheric Radius Expansion Lightcurves
Authors: Simon Guichandut, Andrew Cumming
Figure caption: The mass-loss rate of the wind as a function of time for the Schwarzschild run, in solid lines. The different colors show ﹩\dot{M}﹩ evaluated with Equation (4) at different locations (see text). The dashed lines show the ejected column y ej (scale on the right-hand side). The red shaded region marks the pause in the lightcurve (bottom panel of Figure 6).
Paper: The Imprint of Convection on Type I X-Ray Bursts: Pauses in Photospheric Radius Expansion Lightcurves
Authors: Simon Guichandut, Andrew Cumming
Figure caption: Kippenhahn diagram for the Schwarzschild run as in Figure 3, now with the color scale representing the hydrogen abundance. The solid black and gray lines show y d and ﹩{y}_{{\rm{c}},\min }﹩ (same values as in Figure 2). The dashed line shows the relative change in the total mass of hydrogen at a given time compared to the initial amount at ignition (scale on the right-hand side).
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: The top panel shows the 10 intensity-sliced spectra obtained by XMM-Newton pn in the 0.3–10.0 keV range. The ν F  ν  plot unfolded by the PL with an index of 2.0 is shown. The bottom panel shows the nine spectral ratios to the brightest spectrum A (black in the top panel). Note that both panels show adequately binned spectra to enhance visibility.
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: Locations of the FRB sample relative to their host-galaxy centroids along the major (δ  a ) and minor (δ  b ) axes in units of r  e , defined by the half-light radius determined by galfit. The gray dotted ellipses around each of the points show the FRB localization error relative to the size of the host (several are smaller than the symbols). In the case of FRB 20190711A, the FRB localization is almost 2 times the effective radius of the host, resulting in a fairly large ellipse around the central point. FRB 20191001A is highly offset along the minor axis (δ b ≈ 3), but less so along the major axis (δ a ≈ 1); see images in Mannings et al. (2021). The points cluster at δ  a , δ  b  < 1.5r  e . Therefore, the bursts are predominantly within the inner disks of the galaxies but rarely (if ever) from the nucleus itself (i.e., << r  e ).
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: Top: diamond points (colored by ﹩{\mathrm{log}}_{10}| {\mathrm{RM}}_{\mathrm{EG}}| ;﹩ the RM component excluding Milky Way contribution; see Section 3.1.1) present the global measures of stellar mass (M *) and star formation rate (SFR) for the host galaxies of our RM sample. The dashed line divides quiescent and star-forming hosts, and the 2D histogram describes the distribution for field galaxies from the PRIMUS survey (Moustakas et al. 2013). The majority of hosts lie in the star-forming region of the diagram, with two in the quiescent region. Bottom: color–magnitude diagram with points and histogram as above. The labels “Blue,” “Green,” and “Red” specify, in turn, blue galaxies thought to be currently star-forming with younger stellar populations, green hosts transitioning out of star formation, and “red and dead” galaxies where star formation has ceased and older stellar populations dominate the host. The majority of our sample populate the blue cloud or green valley, indicative of moderate star formation.