adsabs/AstroCLIMB huggingface dataset:
Paper: A Possible Formation Scenario of the Gaia BH1: Inner Binary Merger in Triple Systems
Authors: Zhuowen Li, Chunhua Zhu, Xizhen Lu, Guoliang Lü, Lin Li, Helei Liu, Sufen Guo, Jinlong Yu
Figure caption: The upper part shows the entire formation process from the triple to PMB to Gaia BH1. The lower part shows the orbit period, eccentricity, and mass as a function of time. The gray and red areas represent the RLOF phase and the Gaia BH1 phase, respectively.
Paper: A Possible Formation Scenario of the Gaia BH1: Inner Binary Merger in Triple Systems
Authors: Zhuowen Li, Chunhua Zhu, Xizhen Lu, Guoliang Lü, Lin Li, Helei Liu, Sufen Guo, Jinlong Yu
Figure caption: We use the MESA code to calculate the evolutionary tracks of the 12 M ⊙ merged products at Z = 0.014, with different rotations (ω/ω crit = 0.4 and 0.8) and different magnetic fields (B 0 = 0 and 5000 G). The left panel shows the evolutionary tracks in the H–R diagram. The black dotted line and the red dashed line represent the stellar equivalent radius lines and the Roche lobe radius of the observed Gaia BH1 at perihelion. The middle and right panels show the total angular momentum and total mass of the merged products as a function of time, respectively.
Paper: A Possible Formation Scenario of the Gaia BH1: Inner Binary Merger in Triple Systems
Authors: Zhuowen Li, Chunhua Zhu, Xizhen Lu, Guoliang Lü, Lin Li, Helei Liu, Sufen Guo, Jinlong Yu
Figure caption: The distribution of orbital periods and eccentricity for the core carbon-depleted PMB simulations in Figure 2 after undergoing an SN (left panel) or FSN (right panel). The red and green stars represent the positions of the PMB before the SN or FSN and Gaia BH1, respectively. The color mapping represents the density of a certain area; the darker the color, the more samples there are in that region, indicating higher density.
Paper: First Detection of Molecular Gas in the Giant Low Surface Brightness Galaxy Malin 1
Authors: Gaspar Galaz, Jorge González-López, Viviana Guzmán, Hugo Messias, Junais, Samuel Boissier, Benoît Epinat, Peter M. Weilbacher, Thomas Puzia, Evelyn J. Johnston, Philippe Amram, David Frayer, Matìas Blaña, J. Christopher Howk, Michelle Berg, Roy Bustos-Espinoza, Juan Carlos Muñoz-Mateos, Paulo Cortés, Diego García-Appadoo, Katerine Joachimi
Figure caption: Continuum and 12CO (1–0) line emission detections with ALMA Band 3. The left panel shows a color optical image (u, g, i, and z in blue, green, yellow, and red, respectively) from S. Boissier et al. (2016). The inset shows the central region where continuum and line emission are significant. The red ellipse in the lower left corner of each panel represents the ALMA synthesized beam size. In the main (left) panel, we show the contours of the 12CO (1–0) velocity-integrated map superimposed onto the optical image. The two panels on the right-hand side show the 3 mm continuum and 12CO (1–0) velocity-integrated flux map contours superimposed onto the Hα emission from Junais et al. (2024). Magenta contours for the line emission over the optical and Hα images start at 3σ and increase in steps of 1σ. For the continuum emission (bottom right panel) contours start at 3σ and increase in steps of 3σ.
Paper: First Detection of Molecular Gas in the Giant Low Surface Brightness Galaxy Malin 1
Authors: Gaspar Galaz, Jorge González-López, Viviana Guzmán, Hugo Messias, Junais, Samuel Boissier, Benoît Epinat, Peter M. Weilbacher, Thomas Puzia, Evelyn J. Johnston, Philippe Amram, David Frayer, Matìas Blaña, J. Christopher Howk, Michelle Berg, Roy Bustos-Espinoza, Juan Carlos Muñoz-Mateos, Paulo Cortés, Diego García-Appadoo, Katerine Joachimi
Figure caption: Disk location of the three tentative detections. We show here detections with 3 ≤ S/N ≤ 4 of the peak of the collapsed lines, as indicated in the bottom right panel, where they are superimposed over a composite optical image (S. Boissier et al. 2016). Line detections denoted as TD1, TD2, and TD3 are amplified in the other panels. The corresponding line emission profiles are shown in Figure 4. Other fainter emissions in the disk have S/N smaller than 2 and are not considered, but they are also shown in this figure.
Paper: First Detection of Molecular Gas in the Giant Low Surface Brightness Galaxy Malin 1
Authors: Gaspar Galaz, Jorge González-López, Viviana Guzmán, Hugo Messias, Junais, Samuel Boissier, Benoît Epinat, Peter M. Weilbacher, Thomas Puzia, Evelyn J. Johnston, Philippe Amram, David Frayer, Matìas Blaña, J. Christopher Howk, Michelle Berg, Roy Bustos-Espinoza, Juan Carlos Muñoz-Mateos, Paulo Cortés, Diego García-Appadoo, Katerine Joachimi
Figure caption: Line profile for the 12CO (1–0) central detection in Malin 1. The dotted line represents the 1σ noise level, estimated as the rms measured in the cube without primary beam correction rescaled by the square root of the ratio between the area of the aperture and the area of the synthesized beam. The line is at the 6σ significance level, which is measured in the image obtained by collapsing the orange channels and comparing the peak of the signal with the rms of the background. The line is detected at a systemic velocity of approximately −140 km s−1 relative to the heliocentric redshift of the galaxy (z = 0.082702). The parameters of the best-fit Gaussian are shown in the upper right corner.
Paper: Spectral Characteristics of Fundamental–Harmonic Pairs of Interplanetary Type III Radio Bursts Observed by PSP
Authors: Ling Chen, 玲 陈, Bing Ma, 兵 马, Dejin Wu, 德金 吴, Zongjun Ning, 宗军 宁, Xiaowei Zhou, 晓伟 周, Stuart D. Bale
Figure caption: The spectral characteristics of all the six F-H pairs radio bursts. Panels (a)–(b) and (c) show the F-H frequency ratio f H/f F and the frequency-drift rate D abs. The maximal flux densities corresponding to each given frequency Fluxtmax for events 1–6 are shown in panels (d)–(i), respectively. Panels (j)–(o) present the relative bandwidth as a function of the central frequency for events 1–6, respectively. The black, blue, orange, purple, green, and red colors denote events 1–6 shown in Figures 1(a)–(f), respectively. The results representing H are shifted to the frequency of f H/2.
Paper: Dynamics of Binary Planets within Star Clusters
Authors: Yukun Huang, 宇坤 黄, Wei Zhu, 伟 祝, Eiichiro Kokubo, 保英一郎 小久
Figure caption: Left: ionization fraction f ion (+) and wide binary fraction f wide (×) from stellar flyby simulations as a function of the binary period P. Each symbol represents the result of 5000 JuMBOs with the same mass (from right to left, m = 1, 2, 5, and 10 M J, respectively) and a 0 (grouped by the same color) interacting with random solar-mass stars multiple times. The impact parameter b is generated from a realistic distribution, assuming a density-weighted residence time of χ = 2 × 104 Myr pc−3, and v ∞ follows a Maxwellian distribution. The range of f wide potentially consistent with the JWST discovery (1%–10%) is highlighted in yellow. Right: Histograms of semimajor axes and eccentricities of wide JuMBOs (a > 25 au) generated from multiple stellar flybys. The red dashed line indicated a power-law scaling of d N/d a ∝ a −2.5.
Paper: On the Acceleration of the Young Solar Wind from Different Source Regions
Authors: Yiming Jiao, Ying D. Liu, Wenshuai Cheng, Hao Ran, Rui Wang
Figure caption: Radial evolution of the solar wind parameters. (a) Radial velocity. (b) Electron density. (c) Proton temperature. (d) Electron temperature. The PSP data are binned every 5 R  S , and the data points and error bars are the mean values and standard deviations within the bins. The fitted power-law functions are shown as equations. The solid lines indicate profiles given by our isopoly model.
Paper: On the Acceleration of the Young Solar Wind from Different Source Regions
Authors: Yiming Jiao, Ying D. Liu, Wenshuai Cheng, Hao Ran, Rui Wang
Figure caption: PSP measurements at encounter 10 as an example of data classification. The shaded areas indicate CH wind (red), streamer wind (blue), and LMBL wind (green). (a) PSP heliocentric distance. (b) Proton radial velocity. (c) Magnetic field strength and radial component (red) normalized to 1 au values. (d) QTN electron density normalized to 1 au values. (e) Proton temperature and electron core temperature (red). (f) Alpha-to-proton density ratio. The horizontal dashed line marks the value of 0.02. (g) radial Alfvén Mach number.
Paper: Spectral Characteristics of Fundamental–Harmonic Pairs of Interplanetary Type III Radio Bursts Observed by PSP
Authors: Ling Chen, 玲 陈, Bing Ma, 兵 马, Dejin Wu, 德金 吴, Zongjun Ning, 宗军 宁, Xiaowei Zhou, 晓伟 周, Stuart D. Bale
Figure caption: Two F-H pairs of IP type III radio bursts observed by PSP. (a) F-H pairs radio burst with pairs transitioning into a single band. (b) F-H pairs radio burst with a single band splitting into pairs. The fitting curve (black curve) of the frequencies of maximal flux density corresponding to each fixed time (c)–(d), Stokes polarization V/I (e)–(f), F-H frequency ratio f H/f F (g)–(h), and the absolute frequency-drift rate D abs (i)–(j) for the two bursts are shown. The results of the absolute frequency-drift rate D abs representing H are shifted to the frequency of f H/2.
Paper: On the Acceleration of the Young Solar Wind from Different Source Regions
Authors: Yiming Jiao, Ying D. Liu, Wenshuai Cheng, Hao Ran, Rui Wang
Figure caption: Relationships of proton and electron temperatures with the radial velocity. The V  R , T  p , and T  e  data are scaled to the same distance (14 R  S ) and binned every 50 km s−1. The dashed lines indicate the fitted functions for protons and electrons, respectively. The box marks the LMBL wind with extremely low velocity and an extremely low proton temperature.
Paper: Spectral Characteristics of Fundamental–Harmonic Pairs of Interplanetary Type III Radio Bursts Observed by PSP
Authors: Ling Chen, 玲 陈, Bing Ma, 兵 马, Dejin Wu, 德金 吴, Zongjun Ning, 宗军 宁, Xiaowei Zhou, 晓伟 周, Stuart D. Bale
Figure caption: Six typical F-H pairs of IP type III radio bursts observed by PSP. (a) F-H pairs with similar spectral characteristics between F and H (event 1). (b) F-H pairs with F being structured and H being smooth (event 2). (c) F-H pairs with F being shorter duration than H (event 3). (d) F-H pairs with the emission intensity of H being higher than F (event 4). (e) F-H pairs with H being wider bandwidth than F (event 5). (f) F-H pairs with the emission intensity of F being higher than H (event 6). (g) The fitting curves (black curves) of the frequencies of maximal flux density corresponding to each fixed time for event 1. The magenta dashed line represents the time (09:45:44 UT) slice from the spectrogram, which is presented in panel (k). (h)–(l) F-H frequency ratio f H/f F, the absolute frequency-drift rate D abs, the maximal flux density corresponding to each given frequency Fluxtmax, a time (09:45:44 UT) slice, and relative bandwidth for event 1, respectively. The results representing H are shifted to the frequency of f H/2.
Paper: Astroparticles from X-Ray Binary Coronae
Authors: K. Fang, Francis Halzen, Sebastian Heinz, John S. Gallagher
Figure caption: Broadband spectral energy distribution of Cygnus X-1 measured by BeppoSAX, INTEGRAL, COMPTEL, and Fermi-LAT (F. Frontera et al. 2001; T. Di Salvo et al. 2001; J. Poutanen & I. Vurm 2009; A. A. Zdziarski et al. 2017) during its hard (blue) and soft (red) states. Black and gray colors indicate state-averaged or state-insensitive observations in radio (triangle markers; A. M. Stirling et al. 2001; R. P. Fender et al. 2006), infrared (square markers; P. Persi et al. 1980; I. F. Mirabel et al. 1996), gamma ray by MAGIC (light gray limits; A. Fernández-Barral et al. 2018) and HAWC (gray limits; A. Albert et al. 2021), and high-energy neutrinos by IceCube (black dashed limits corresponding to the 90% C.L. median sensitivities for time-integrated searches using track-like events in 10 year IceCube data with both ﹩{dN}/{dE}\propto {E}^{-2}﹩ and E −3 assumptions and scaled to all-flavor flux; M. G. Aartsen et al. 2020; R. Abbasi et al. 2022b). The dotted, dashed–dotted, and dashed curves correspond to the inverse Compton radiation by secondary electrons and cascaded electrons, synchrotron radiation by electrons and protons, and neutrino emission by protons in the coronal emission models, respectively. The solid curves denote the total electromagnetic radiation in the two states by summing the background radiation (see Appendix A) and emission originated from nonthermal protons in the corona.
Paper: Astroparticles from X-Ray Binary Coronae
Authors: K. Fang, Francis Halzen, Sebastian Heinz, John S. Gallagher
Figure caption: Inelastic optical depth to protons (dashed curves) due to proton–proton interaction (orange), photopion production (green), Bethe–Heitler process (sky blue), and synchrotron radiation (magenta) as a function of the proton energy and optical depth to gamma rays due to pair production (solid red curve) as a function of the gamma-ray energy during the hard (left) and soft (right) state of Cygnus X-1. For reference, the black thin dotted line indicates an optical depth of 1. Parameters in use include ξ  B  = u  B /u  X  = 1, ﹩{{ \mathcal R }}_{\mathrm{rel}}\equiv R/{R}_{g}=100﹩ for hard state and 30 for soft state. For protons, the confinement time is assumed to be the diffusion time in the hard state and advection time in the soft state. The photon confinement time is the light-crossing time t cross. The proton number density is set to n  p  m  p  = n  e  m  e . The radiation background is the same as in Figure A1, which is computed using parameters in Table A1.
Paper: Astroparticles from X-Ray Binary Coronae
Authors: K. Fang, Francis Halzen, Sebastian Heinz, John S. Gallagher
Figure caption: Timescales of proton acceleration (solid curves) and escape (dashed–dotted curves) in the units of light-crossing time t cross ≡ R/c as a function of the proton energy. In the hard state (blue), stochastic acceleration (Equation (3) with η = 10) and particle diffusion (Equation (4)) in a turbulent magnetic field are assumed to occur in a region of size R = 100 R  g . The magnetic field strength is computed using the X-ray luminosity in Supplementary Table A1 for the assumed coronal size. In the soft state (red), magnetic reconnection (Equations (5) and (6)) with β rec = 0.1 is assumed. The ratios of the timescales to the light-crossing time in this scenario do not depend on the coronal size.
Paper: Astroparticles from X-Ray Binary Coronae
Authors: K. Fang, Francis Halzen, Sebastian Heinz, John S. Gallagher
Figure caption: Spectral energy distribution of Cygnus X-1 from soft X-ray to MeV gamma ray in the hard (blue) and soft (red) states (F. Frontera et al. 2001; T. Di Salvo et al. 2001; J. Poutanen & I. Vurm 2009; A. A. Zdziarski et al. 2017). The spectra at soft X-rays correspond to the unabsorbed, intrinsic emission. The dotted, dotted–dashed, and dashed curves denote the emission from the thermal and nonthermal electrons in the accretion flow and the accretion disk, respectively. The solid curves are the sum of all emission components.
Paper: Astroparticles from X-Ray Binary Coronae
Authors: K. Fang, Francis Halzen, Sebastian Heinz, John S. Gallagher
Figure caption: Same as Figure 2 but focusing on the gamma-ray spectrum of Cygnus X-1. The black curve corresponds to a state-averaged emission by assuming that source spends 80% and 20% of time in hard and soft states, respectively. The black square markers indicate a time-integrated observation by LHAASO (LHAASO Collaboration 2024).
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: (Left) Schematic illustration of a black hole accretion disk illustrating how photons can follow different paths between a single point in the flow and the observer. The colored disk shows emission on an equatorial slice in a snapshot from a GRMHD simulation, with a linear color map showing the number of photons that were produced from that part of the midplane and then captured by the observer. The black hole has a * = 0.9375 with the spin axis pointing up, and its event horizon is depicted as a filled black sphere. The observer is located at an inclination of i = 17° to the right of the spin axis. We highlight a single emission point left of the black hole with a red circle. The path followed by the direct emission (n = 0) is shown in blue, that by the first-order indirect emission (n = 1) is shown in red, and that by the second-order emission (n = 2) is shown in green. Emission originating from any point in the solid colored geodesic path would appear in the corresponding subimage (i.e., emission along the solid red segment would also appear in the n = 1 subimage). (Right) Ray-traced image of the GRMHD snapshot on the left; the total observed flux (top) can be decomposed into the n = 0, 1, 2, … subimages (bottom). The n = 0 subimage does not contain the sharp bright ring feature seen in the total image, while the higher-order subimages are dominated by that feature, which becomes thinner and sharper as n increases.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: (Left) Light curves from the same a * = 0.9375 MAD GRMHD simulation shown in Figure 1. The total light curve (black) has been decomposed into light curves for the n = 0 direct emission (blue), n = 1 indirect emission (red), and n = 2 doubly indirect (green) subimages. The flux decreases by about an order of magnitude between different values of n. The three light curves are similar, but they are offset by about 16 GM/c 3, which is the approximate amount of time it takes for light emitted near the black hole to travel around its far side. As an example, the peak in the direct emission at the vertical black dashed line is delayed in the first-order indirect emission (n = 1; the dark gray shaded region denotes a delay of 16 GM/c 3) and further delayed in the second-order light curve (n = 2; the light gray shaded region denotes a delay of 32 GM/c 3). (Right) Correlations between different light curves as a function of time delay. The dashed black curve shows the autocorrelation of the total light curve, and the colored curves correspond to the correlation between the n = 0 and n = 1 emission (magenta), n = 1 and n = 2 (yellow), and n = 0 and n = 2 (cyan). Although the autocorrelation of the total light curve does not show an echo peak, echo peaks can be clearly seen in the correlations between the subimage light curves. The peak time delay between emission separated by one order is between 15 and 20 GM/c 3 (the dark gray shaded interval), while the peak time delay between the n = 0 and n = 2 light curves is about twice as long, as expected.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Location of observed emission relative to the time delay between n = 0 and n = 1 geodesics connecting that location to the observer. The data used for this figure come from the same a * = 0.9375 simulation used in Figures 1 and 2, which observe the accretion flow at an inclination of i = 17° (indicated by the white arrow). The color map corresponds to the azimuthally averaged emissivity plotted in the y = 0 plane and is shown in a linear scale. The contours depict isodeltachrones, surfaces where the n = 1 emission would arrive at the observer with a fixed time delay relative to the n = 0 emission. Most emission comes from regions where the time delay is in the range 10–20 GM/c 3.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Similar to the right panel of Figure 7 but exploring different model parameters. (Left) The normalized correlation between the total light curve and the visibility amplitude time series at different baseline lengths (red and blue) for observational frequency 230 GHz (solid curves) and 345 GHz (dashed curves). The echo signature is mildly suppressed in the 345 GHz observations because the long baseline signal is less correlated with the zero-baseline time series (see text for more details). (Center) Similar to the left panel but for different GRMHD simulations and radiative transfer parameters over the same 1000 GM/c 3 time window. The KHARMA85 simulation has a * = 0.85 and r low = 10 (the remaining parameters match the other simulations). An echo signature is detectable in each simulation. (Right) Similar to the other panels, but here we explore whether the echo signal can be detected in different windows of the full simulation. We consider nonoverlapping windows with different durations (color) from the full time series. Although the echo signature differs across the windows, it is present in each of the correlation functions.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Demonstration of echo detection using the correlation method described in this Letter applied along the v = 0 axis of the data seen in previous figures. (Left) The color map shows the correlation between the zero-baseline time series and the time series at a longer baseline (y-axis) as a function of time delay offset between the two time series (x-axis). As baseline length is increased beyond about 40 Gλ, a second peak in the correlation signal appears near Δt = 10–20 GM/c 3. (Right) We highlight several horizontal cross sections from the left panel (with matching line styles). The echo peak at 10–20 GM/c 3 is visible starting around ∼40 Gλ for this particular model (see the dark gray shaded region). The correlations shown in this figure were performed over time series of total length 2000 GM/c 3.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Isodeltachrones and spatial distribution of observed emission similar to Figure 3 but for different observer inclination angles i = 0°, 17°, and 60°. The emissivity typically peaks in regions where the time delay is between 10 and 20 GM/c 3; however, for the higher-inclination i = 60° simulation, the emission also peaks in a region with a time delay of ∼5–10 GM/c 3. Unlike in Figure 3, we do not azimuthally average the emission maps so that the left–right asymmetry due to Doppler boosting is visible.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Comparison of echo detectability for three different models of the astrophysical correlations in the direct image. We adopt the echo model of Section 2.4 and take the time delay between the n = 0 and n = 1 emission to be Δt = τ and the Lyapunov exponent to be γ = π. (Top) Definition of the (hypothetical) direct emission astrophysical autocorrelation C 0(Δt). For comparison, we also show the same quantity for a GRMHD simulation as a dashed black curve. (Center) The autocorrelation of the total light curves for each of the models. When the astrophysical autocorrelation falls off more slowly, the echo signature is suppressed. (Bottom) The correlation we would measure if we could directly access the L 0 and L 1 light curves, which is a translated copy of the astrophysical correlation. For all three models, a clear echo peak is present when we correlate L 0 and L 1.