adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: ALMA spectra of J1211–0118 (top), J0235–0532 (middle), and J0217–0208 (bottom) around the redshifted frequency of the CO(6–5) emission line (black histogram) extracted by placing a beam aperture (for details, see the text in Section 4.1). The dotted vertical line corresponds to the systemic redshift determined with the FIR emission lines of [O III] and [C II] (Harikane et al. 2020b). The red curve in the middle panel represents the best-fit Gaussian function to the CO(6–5) emission line.
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: CO(6–5) contours for J0235–0532. The red (blue) contours are multiples of 0.5σ (−0.5σ) starting at 2σ (−2σ). The synthesized beam is shown in the bottom left corner. The gray background is the Subaru HSC z-band image of J0235–0532 that captures the rest-frame UV continuum emission. The positions of the CO(6–5) and UV continuum emission are consistent within the large uncertainties (light red cross) estimated from the Monte Carlo simulations (for details, see the text in Section 4.1). The yellow and green crosses denote the positions of the [C II] and [O III] emission, respectively, and the sizes of the crosses are their uncertainties (Harikane et al. 2020b), which are also consistent with that of CO(6–5). The size of the image is 10″ × 10″.
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: Zeroth-moment images showing the integrated CO(6–5) flux densities of J1211–0118 (top), J0235–0532 (middle), and J0217–0208 (bottom). The synthesized beam is shown in the bottom left corner in each image. The size of each image is 30″ × 30″. The range of the color bar for the flux densities corresponds to ±3 times the standard deviation.
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: ALMA spectra of J1211–0118 (left), J0235–0532 (center), and J0217–0208 (right) around CO(6–5), [O III] 88 μm, and [C II] 158 μm from top to bottom. The CO spectra are the same as the ones shown in Figure 1, but the velocity range is limited to [−1000 km s−1, 1000 km s−1]. The spectra for [O III] 88 μm and [C II] 158 μm have been obtained in Harikane et al. (2020b).
Paper: Turbulent Reacceleration of Streaming Cosmic Rays
Authors: Chad Bustard, S. Peng Oh
Figure caption: Top: CR streaming energy-loss time (in units of the eddy turnover time) compared to the approximation L 0/v A (dashed line). Each simulation has M s ≈ 0.5 and streaming-dominated transport, with κ ∼ 0.15L 0 c  s , hence ﹩{L}_{0}/{v}_{{\rm{A}}}={\tau }_{\mathrm{stream}}\lt {L}_{0}^{2}/\kappa ={\tau }_{\mathrm{diff}}﹩ for β ⪅ 100. At high β, turbulence easily tangles field lines, and the energy-loss time approaches L 0/v A. At low β, when there is a strong guide field, field line tangling is more difficult, and misalignment between the magnetic field and the CR pressure gradient suppresses energy loss by a factor ∼0.1. The amount of energy loss is resolution dependent for low β.
Paper: Turbulent Reacceleration of Streaming Cosmic Rays
Authors: Chad Bustard, S. Peng Oh
Figure caption: Testing growth time convergence with respect to the reduced speed of light, v  m  (relative to the fastest propagation speed, c  s ), and numerical resolution. Simulations with v  m /c  s  = 50 appear well converged. Magenta and green points denote simulations with 1283 and 2563 resolution, respectively, for which the velocity divergence and hence compressional heating is slightly larger and decreases the reacceleration time in the well-trapped κ < v ph L 0 regime. For large κ, CRs diffuse quickly over small-scale structures, which then do not need to be well resolved to get converged reacceleration rates.
Paper: Turbulent Reacceleration of Streaming Cosmic Rays
Authors: Chad Bustard, S. Peng Oh
Figure caption: Slice plots for three 2563 simulations, each with initial P  g /P CR ∼ 100 but with β ∼ 1, M A ∼ 0.35 (left), β ∼ 10, M A ∼ 1.1 (middle), and β ∼ 100, M A ∼ 3.5 . The top row shows gas density with magnetic field streamlines overlaid. The middle row shows the misalignment between   B  and ∇P CR. The bottom row shows the field-aligned CR scale length relative to the outer eddy scale. Notably, the higher β simulations result in more field line tangling, generally greater alignment between   B  and ∇P CR (leading to more CR energy loss), and shorter CR scale lengths.
Paper: The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos
Authors: Yoshihide Yamato, Kenji Furuya, Yuri Aikawa, Magnus V. Persson, John J. Tobin, Jes K. Jørgensen, Mihkel Kama
Figure caption: Top: observed spectra of NH3 (3,3), NH3 (4,4), NH3 (5,5), NH2D 31,3–30,3, and NH2D 41,4–41,4 in brightness temperature (T B) (black) extracted toward the continuum peaks of 4A1. The model spectra generated by 20 randomly selected parameter samples from the Markov Chain Monte Carlo (MCMC) chains of the fits with fixed (blue) and free (orange) ortho-to-para ratios of NH3 are overlaid. Bottom: residual of observations and fitted model with fixed (blue) and free (orange) ortho-to-para ratio of NH3. Each data point corresponds to the randomly selected models from MCMC chains. The gray-shaded regions indicate the 2σ RMS range. For both the top and bottom panels, while the zero flux levels are indicated by gray dashed horizontal lines, the vertical dotted lines indicate the systemic velocity.
Paper: Turbulent Reacceleration of Streaming Cosmic Rays
Authors: Chad Bustard, S. Peng Oh
Figure caption: Top: streaming energy-loss time as a function of additional diffusivity; all simulations here were run on a 643 grid. The solid lines now show v A/L CR, where L CR ∼ κ/v when diffusion dominates and L CR = L 0 for the streaming-dominated simulation. At high β, these approximations are well reproduced. Bottom: streaming loss time as a function of β for a mixture of solenoidal and compressive driving, controlled by the parameter f shear. All simulations were run on a 2563 grid. For increasingly solenoidal driving (increasing f shear), loss times and reacceleration times both increase.
Paper: Turbulent Reacceleration of Streaming Cosmic Rays
Authors: Chad Bustard, S. Peng Oh
Figure caption: Top: two representative simulations starting from P CR/P  g =1/100 and 1, run out to hundreds of eddy turnover times. Growth is exponential, with increasing growth times and a transition to quasi-linear growth once P CR > P g. Bottom: simulated growth time vs. P CR/Pg for simulations with constant κ < v ph L 0 and varying P CR > P  g . We expect (and find) that ﹩{t}_{\mathrm{grow}}\,\propto {v}_{\mathrm{ph}}^{2}\propto {P}_{\mathrm{CR}}/{P}_{g}﹩, consistent with Equation (2).
Paper: The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos
Authors: Yoshihide Yamato, Kenji Furuya, Yuri Aikawa, Magnus V. Persson, John J. Tobin, Jes K. Jørgensen, Mihkel Kama
Figure caption: Gallery of velocity-integrated intensity maps of NH3 and NH2D transitions. Transitions are indicated at the upper left in each panel. The continuum emission peaks for 4A1 and 4A2 are indicated by black crosses in each panel. The gray dashed contours start from 3σ, followed by steps of 3σ. The beam size and scale bar of 300 au are shown in lower right and left in each panel, respectively. We note that the color scale is saturated at the lower end of 0.0.
Paper: The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos
Authors: Yoshihide Yamato, Kenji Furuya, Yuri Aikawa, Magnus V. Persson, John J. Tobin, Jes K. Jørgensen, Mihkel Kama
Figure caption: The 22.3 GHz continuum emission maps toward IRAS 4A1 and IRAS 4A2. The contours (white dashed lines) correspond to [10, 20, 30, 50, 100, 150, 200, 250, 300] ×  σ RMS, where σ RMS = 7.4 μJy beam−1. The beam sizes of 0.″99 × 0.″75 (P.A. = 82°) and scale bars of 300 au are shown at lower left and right. We note that the color scales employ arcsinh stretches, with the lower end saturating at 0.0.
Paper: Recurrent Narrow Quasiperiodic Fast-propagating Wave Trains Excited by the Intermittent Energy Release in the Accompanying Solar Flare
Authors: Xinping Zhou, Yuandeng Shen, Hongfei Liang, Zhining Qu, Yadan Duan, Zehao Tang, Chengrui Zhou, Song Tan
Figure caption: Panel (a) is an enlargement of the wave Train-2 shown in Figure 2. Panel (b) shows the wave front profile at times marked by the red arrow in panel (a). The red dotted curve results from fitting the wave profile using the harmonic function, which shows the wavelength of 44 Mm. Panel (c) is the same as panel (a) but for base-ratio images. Panel (d) displays the horizontal slices at the selected distance in panel (c), i.e., temporal profiles of intensity base ratio at locations marked by the green cross signs. Successive curves at greater distances are shifted upward, and the periods between two slanted lines used to trace the troughs of the wave fronts are listed in the figure. Panel (e) shows the κ–ω diagrams obtained from the Fourier analysis of a three-dimensional data cube of 171 Å running-difference images during 6:50:00 UT–07:03:48 UT, whose spatial dimension is indicated by the white box in Figure 1(d). The uncertainties in panels (a) and (e) are estimated by making the fit 10 times.
Paper: Recurrent Narrow Quasiperiodic Fast-propagating Wave Trains Excited by the Intermittent Energy Release in the Accompanying Solar Flare
Authors: Xinping Zhou, Yuandeng Shen, Hongfei Liang, Zhining Qu, Yadan Duan, Zehao Tang, Chengrui Zhou, Song Tan
Figure caption: Panel (a) displays the GOES 1–8 Å X-ray flux curve, its time derivative curve, and normalized AIA 131 Å light flux curve within the eruption source region outlined by the black box in Figure 1(a). Panel (b) is the TDSP obtained from the AIA 171 Å running-difference images along the slice OC shown in Figure 1, in which the three green boxes labeled with Train-1, Train-2, and Train-3 point to the locations of the wave trains, while the white horizontal dashed line marks the position for extracting the signals for wavelet analysis in Section 2.1.
Paper: Recurrent Narrow Quasiperiodic Fast-propagating Wave Trains Excited by the Intermittent Energy Release in the Accompanying Solar Flare
Authors: Xinping Zhou, Yuandeng Shen, Hongfei Liang, Zhining Qu, Yadan Duan, Zehao Tang, Chengrui Zhou, Song Tan
Figure caption: Periodicity analysis for the associated flare pulsation and the narrow QFP wave train. The yellow curve in panel (a) is the time derivative signal of GOES 1–8 Å X-ray flux after subtracting its 120 s smoothed intensity profile, while the yellow curve in panel (b) is the smoothed intensity profile along the horizontal white dashed line shown in Figure 2(b). Their corresponding wavelet spectrums are displayed in panels (a) and (b). In each spectrum, the dotted line in global power indicates the 95% significance level, and the green horizontal dashed line marks the period. The corresponding periods P are also listed in the figure. The uncertainty of each period is estimated by the FWHM of each peak on the global power curve. The crosshatched areas overlaid on the wavelet spectrum indicate the cone influence region due to the edge effect of the data.
Paper: Recurrent Narrow Quasiperiodic Fast-propagating Wave Trains Excited by the Intermittent Energy Release in the Accompanying Solar Flare
Authors: Xinping Zhou, Yuandeng Shen, Hongfei Liang, Zhining Qu, Yadan Duan, Zehao Tang, Chengrui Zhou, Song Tan
Figure caption: Panel (a) shows the average temperature in the 3.0–3.5 MK using the regularized inversion technique developed by Hannah & Kontar (2012). Panel (b) displays the variation in temperature and density in the region marked by the red rectangle in panel (a) using Equations (2) and (3). The percentage increase in density and temperature due to the waves passage are listed in the figure.
Paper: Using Gravitational Waves to Distinguish between Neutron Stars and Black Holes in Compact Binary Mergers
Authors: Stephanie M. Brown, Collin D. Capano, Badri Krishnan
Figure caption:                    ﹩\mathrm{ln}{ \mathcal B }﹩ for each detector with m BH = 5 M ⊙. The vertical line spans the range of Bayes factors for a given detector. The red line on the left indicates a variable equation of state run, and the blue line on the right indicates a constant equation of state. The horizontal black line corresponds to the ﹩\mathrm{ln}{ \mathcal B }=10﹩ cutoff. As the 3G detectors have significantly higher Bayes factors than current detectors, the plots are split with different y-axes for current and third-generation detectors.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: Evolution of the time-integrated Poynting flux (left) and internal energy in the 3D simulation volume (right). The colors correspond to the following simulations: black = tuned driver, low density, radiation included; green = tuned driver, high density, no radiation; red = detuned driver, higher density, no radiation; black dashed = detuned driver, low density, radiation included; blue = tuned driver, higher density, radiation included. Note that the internal energy plot shows the change in internal energy in the 3D domain, normalized against the initial internal energy.
Paper: Using Gravitational Waves to Distinguish between Neutron Stars and Black Holes in Compact Binary Mergers
Authors: Stephanie M. Brown, Collin D. Capano, Badri Krishnan
Figure caption:                    ﹩\mathrm{ln}{ \mathcal B }﹩ for each detector with m BH = 10 M ⊙. The vertical line spans the range of Bayes factors for a given detector. The red line on the left indicates a variable equation of state run, and the blue line on the right indicates a constant equation of state. The horizontal black line corresponds to the ﹩\mathrm{ln}{ \mathcal B }=10﹩ cutoff.
Paper: Using Gravitational Waves to Distinguish between Neutron Stars and Black Holes in Compact Binary Mergers
Authors: Stephanie M. Brown, Collin D. Capano, Badri Krishnan
Figure caption: Mass–radius and mass-tidal deformability curves for the two equations of state used in this analysis compared to commonly used equations of state. The dashed horizontal line is at 1.4 M ⊙. The two equations used in this paper are labeled as “stiff” and “maximum likelihood.” The stiff and maximum likelihood equations of state correspond to Λ = 369 and Λ = 162 for a 1.4 M ⊙ neutron star, respectively.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: AIA 171 Å (normalized) intensity along a line of sight perpendicular to the loop at time = 1931 s, for the low-density tuned simulation (left), the high-density, tuned simulation (middle), and the low-density, detuned simulation (right). In each case, the intensity has been normalized to the maximum intensity at the start of the simulation.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: The time-integrated Poynting flux on the lower boundary for the tuned (left) and detuned (right) simulations. Positive values correspond to energy entering the domain.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: Evolution of the total (i.e., volume integrated) vorticity (left) and current (right) for the low-density, tuned simulation (solid black line), the high-density, tuned simulation (blue line), and the low-density, detuned simulation (dashed black line). Optically thin radiation is included in all three cases.
Paper: (When) Can Wave Heating Balance Optically Thin Radiative Losses in the Corona?
Authors: I. De Moortel, T. A. Howson
Figure caption: Evolution of the ohmic heating (thick lines) and heating resulting from the shock viscosities in Lare3D (thin lines). The colors correspond to the following simulations: black = tuned driver, low density, radiation included; black dashed = detuned driver, low density, radiation included; blue = tuned driver, higher density, radiation included.
Paper: The Solar Disk at High Energies
Authors: Miguel Gutiérrez, Manuel Masip, Sergio Muñoz
Figure caption: Absorbed proton and He fluxes during a solar maximum (thick) and a solar minimum (thin). On the right, typical CR trajectories at different energies.
Paper: The Solar Disk at High Energies
Authors: Miguel Gutiérrez, Manuel Masip, Sergio Muñoz
Figure caption: Schematic CR trajectories in the vicinity of the Sun. The solar magnetism does not create anisotropies in the flux reaching the Earth, but the average depth of solar matter crossed by CRs grows with the energy, increasing their probability to be absorbed and thus the integrated CR shadow observed by HAWC.
Paper: New Constraint on the Tensor-to-scalar Ratio from the Planck and BICEP/Keck Array Data Using the Profile Likelihood
Authors: Paolo Campeti, Eiichiro  Komatsu
Figure caption: Summary of 95% C.L. upper limits on r for data sets considered in this work. The darker shaded bars indicate the upper limit from the profile likelihood, whereas the lighter shaded bars the MCMC one. The best-fitting r values from the profile likelihood analysis are shown as the black dots. Negative (unphysical) values of r are indicated by the hatched dark gray region. The baseline result of this work is highlighted in bold.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: The graphs of the time variations of the density of the envelope at different distances from the center of Jupiter based on the models described by Lozovsky et al. (2017). Shown are gas densities of 10−6 g cm−3 (dotted line), 10−5 g cm−3 (small dashed line), 10−4 g cm−3 (large dashed line), and 10−3 g cm−3 (solid line).
Paper: New Constraint on the Tensor-to-scalar Ratio from the Planck and BICEP/Keck Array Data Using the Profile Likelihood
Authors: Paolo Campeti, Eiichiro  Komatsu
Figure caption: Profile likelihoods for r from the data sets combinations considered in this work. The points are the ﹩{\chi }^{2}-{\chi }_{\min }^{2}﹩ values obtained from the likelihood maximization, whereas the parabolic fits are shown as the solid lines. The dashed lines indicate the upper limits at 95% C.L. according to the FC prescription. Unphysical (negative) values of r are shown as the dark gray hatched area. The baseline result is shown in the thick red line.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the vaporization of 1 km pure-ice planetesimals for two values of Saturn’s mass. The top panel corresponds to 1/3 of Saturn’s mass, showing only 1% vaporization, and the bottom panel corresponds to 1/10 of Saturn, showing 1.5% vaporization. See Section 3.1 and Table 3 for more details.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Black squares, red diamonds, and green dots illustrate the dark matter, star, and total density profiles, calculated in spherical shells centered on six Sag-like systems. Here, all particles at the corresponding radial ranges are used to calculate the true profiles. Solid curves with corresponding colors show the best-fitting profiles by JAM, based on the NFW model profile. Notably, the red solid curves are based on deprojections of the two-dimensional MGEs, which are created with stars bound to the dwarfs. The magenta solid curves denote the best-fitting total profiles based on the double power-law model profile, with the inner slopes allowed to be free, but the outer slopes are fixed to 3. For simplicity, the M/L of the luminous component is also fixed to unity when we use the double power-law model. Shaded regions show the 1σ uncertainties of the best fits, while the error bars of the true profiles are the 1σ uncertainties of 100 boot-strapped subsamples of all particles. Only bound star particles are used as tracers, without the inclusion of observational errors. The gas and black hole components are significantly subdominant and are thus not shown. The x-axis range is chosen to be larger than 0.2 kpc, to avoid the very central regions that are affected by the resolution. Black vertical lines mark the half-mass radii. The numbers in each panel give the corresponding host system number and the satellite ID.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Differences between the best-fitting total mass between 200 and 300 pc and the truth in log space (y-axis), reported as a function of the dynamical status of tracer star particles between 200 and 400 pc (x-axis). The dynamical status is quantified by the medians of the radial action angle. A median of 0.5 refers to the steady state. The larger the median deviating from 0.5, the more unrelaxed the system is. The adopted potential model to recover the underlying mass profiles, free parameters of the model, and the meanings of filled symbols with different colors and shapes are the same as those in Figure 3. The statistical uncertainties in the best fits are smaller than or comparable to the symbol size. The horizontal and vertical black dashed lines mark zero bias in best fits and perfect steady state (θ med = 0.5), respectively. Systems with underestimated M(200–300 pc) are more likely to have the medians of their radial action angle distribution biased to be larger than 0.5, and vice versa.