adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Constraints on the UV Luminosity Density at Cosmic Dawn: Implications for 21 cm Cosmology
Authors: Sultan Hassan, Christopher C. Lovell, Piero Madau, Marc Huertas-Company, Rachel S. Somerville, Blakesley Burkhart, Keri L. Dixon, Robert Feldmann, Tjitske K. Starkenburg, John F. Wu, Christian Kragh Jespersen, Joseph D. Gelfand, Ankita Bera
Figure caption: The galaxy UV luminosity density, ρ UV, from HST (faint cyan triangles, Oesch et al. 2018; faint orange hexagons, Ishigaki et al. 2018; faint blue pentagons, Bouwens et al. 2015) and JWST (open lime circles, Donnan et al. 2023; open green diamonds, Harikane et al. 2022; magenta stars, Bouwens et al. 2022b), using the measured LF from z = 4 to z = 14 for different magnitude cutoffs M UV = − 18 (left panel) and M UV = − 13 (right panel). Error bars are added only to JWST data assuming 5% and 10% uncertainties in the faint-end slope at z < 10 and z > 10, respectively. The recently confirmed spectroscopic measurements reported by Harikane et al. (2023a) are shown as filled green diamonds. The red box depicts the UV luminosity density needed to produce a 21 cm global signal at 16 < z < 19 in the minimal coupling regime (Madau 2018). The brown and black boxes show the enhanced ρ UV required by the presence of a radio background excess produced by early black holes (Ewall-Wice et al. 2018) and following the claimed detection by ARCADE 2 (Feng & Holder 2018), respectively. If JWST LF measurements could be extrapolated down to M UV = − 13, the ensuing luminosity density would match the gradual redshift evolution predicted by Madau (2018) and the updated fit (red line), providing enough Lyα background radiation to mix the hyperfine levels of neutral hydrogen 200 Myr after the Big Bang. Due to the large uncertainty associated with cosmic variance/faint-end slope of the LF at these early epochs, the enhanced UV luminosity density required by the presence of a radio background excess (brown and black boxes) is also broadly consistent with current JWST and HST data, following shallow (brown line) or flat (black line) evolution in ρ UV.
Paper: VVV-WIT-12 and Its Fashionable Nebula: A 4 yr Long-period Young Stellar Object with a Light Echo?
Authors: Roberto K. Saito, Bringfried Stecklum, Dante Minniti, Philip W. Lucas, Zhen Guo, Leigh C. Smith, Luciano Fraga, Felipe Navarete, Juan Carlos Beamín, Calum Morris
Figure caption: Top: spectral energy distribution (SED) of VVV-WIT-12 covering 1–1000 μm, obtained with the Vizier photometry viewer (http://vizier.cds.unistra.fr/vizier/sed/). Solid circles mark the data points from VVV and WISE within the range 2 to 22 μm (see Section 2). Bottom: near-IR spectrum of the VVV-WIT-12 stellar source, acquired with the TripleSpec spectrograph at the SOAR telescope in Chile, on 2023 June 11 (JD 2460106, corresponding to ϕ = 0.17 cycles, see the right panel of Figure 2). This shows that the source is very red, with a featureless steadily rising continuum, lacking strong near-IR emission lines. Data appearing in the SED are described in Appendix C.
Paper: VVV-WIT-12 and Its Fashionable Nebula: A 4 yr Long-period Young Stellar Object with a Light Echo?
Authors: Roberto K. Saito, Bringfried Stecklum, Dante Minniti, Philip W. Lucas, Zhen Guo, Leigh C. Smith, Luciano Fraga, Felipe Navarete, Juan Carlos Beamín, Calum Morris
Figure caption: Composite VVV-WIT-12 K s-band image made using three different epochs: years 2010 (red), 2011 (green), and 2012 (blue). This is the discovery image for VVV-WIT-12, that shows the variation of the central source as well as the nebula. The image is 67″ on a side, centered in VVV-WIT-12 at R.A./decl. (J2000) = 17:17:20.29, −36:08:43.9 (l, b = 350.7080, +1.0259 deg), and oriented along Galactic coordinates. Sources that are nonvariable in the near-IR should look white, while variable sources are colored differently. The point source was brighter in 2010 and the nebula changed brightness in different parts along the epochs.
Paper: JWST Constraints on the UV Luminosity Density at Cosmic Dawn: Implications for 21 cm Cosmology
Authors: Sultan Hassan, Christopher C. Lovell, Piero Madau, Marc Huertas-Company, Rachel S. Somerville, Blakesley Burkhart, Keri L. Dixon, Robert Feldmann, Tjitske K. Starkenburg, John F. Wu, Christian Kragh Jespersen, Joseph D. Gelfand, Ankita Bera
Figure caption: Predicted galaxy UV luminosity function at z = 16. The Schechter function parameter ϕ ⋆ has been normalized to yield the luminosity density required in the minimal 21 cm coupling (solid red line; Madau 2018), the early black hole radio (brown solid line; Ewall-Wice et al. 2018), and the ARCADE 2 radio excess (black solid line; Feng & Holder 2018) scenarios, at fixed ﹩{M}_{\mathrm{UV}}^{\star }=-21.15﹩ and α = − 2.35. The cyan dashed and blue solid curves show the Harikane et al. (2023a) best-fit Schechter function obtained from the spectroscopically confirmed candidates at z = 9–12 and extrapolated to z ∼ 16, respectively. The upper limit (blue arrow) is obtained from photometric estimates at z ∼ 16, while the lower limits (cyan arrows) represent the spectroscopic constraints by Harikane et al. (2023a). The 21 cm signal constraints predict a much higher number of galaxies than the extrapolation of Harikane et al.'s (2023a) results from z = 9 to 12 by approximately 1–3 orders of magnitude at the faint end, depending on the presence and intensity of the radio background.
Paper: VVV-WIT-12 and Its Fashionable Nebula: A 4 yr Long-period Young Stellar Object with a Light Echo?
Authors: Roberto K. Saito, Bringfried Stecklum, Dante Minniti, Philip W. Lucas, Zhen Guo, Leigh C. Smith, Luciano Fraga, Felipe Navarete, Juan Carlos Beamín, Calum Morris
Figure caption: Left panel: light curve of VVV-WIT-12 covering years 2010–2022. Gray points represent the K  s -band observations from VVV/VVVX, and cyan points represent the W1-band observations from WISE (arbitrarily shifted by 3 mag). Right panel: VVV-WIT-12 light curves phased using P = 1525 days. The different cycles are color coded as labeled to show the amplitude changes. While the minimum light seems to be the same in the two cycles observed with the K  s -band, the maximum is about 0.3 mag brighter in the second cycle, indicating a possible eruption.
Paper: JWST Constraints on the UV Luminosity Density at Cosmic Dawn: Implications for 21 cm Cosmology
Authors: Sultan Hassan, Christopher C. Lovell, Piero Madau, Marc Huertas-Company, Rachel S. Somerville, Blakesley Burkhart, Keri L. Dixon, Robert Feldmann, Tjitske K. Starkenburg, John F. Wu, Christian Kragh Jespersen, Joseph D. Gelfand, Ankita Bera
Figure caption: Observed, sky-averaged brightness temperature at 21 cm. The red dashed and solid curves show the prediction from a minimal coupling scenario with a cutoff in the UV luminosity density at z = 20.5 and without a cutoff, respectively. The yellow curve shows the spectral feature claimed by the EDGES experiment. The models ignore X-ray heating as well as the possible presence of an excess (over the CMB) radio background.
Paper: VVV-WIT-12 and Its Fashionable Nebula: A 4 yr Long-period Young Stellar Object with a Light Echo?
Authors: Roberto K. Saito, Bringfried Stecklum, Dante Minniti, Philip W. Lucas, Zhen Guo, Leigh C. Smith, Luciano Fraga, Felipe Navarete, Juan Carlos Beamín, Calum Morris
Figure caption: Top: composite K s-band image made using a year 2010 image (with VVV-WIT-12 near phase ϕ ∼ 0.75 cycles) divided by a year 2015 (ϕ ∼ 0.05 cycles). The nebula varies in the K s band, appearing brighter in the first epoch. Bottom: composite J/K s image showing the spatial variation of the near-IR nebular color. Also, the color variations cover different places than the brightness variations. In both panels the field of view is 67″ on a side, oriented along Galactic coordinates, with longitude increasing to the left and latitude toward the top, and covers the same field as Figure 1. The color scale has been stretched to emphasize the changes. A horizontal bar shows the relative intensity in each case.
Paper: VVV-WIT-12 and Its Fashionable Nebula: A 4 yr Long-period Young Stellar Object with a Light Echo?
Authors: Roberto K. Saito, Bringfried Stecklum, Dante Minniti, Philip W. Lucas, Zhen Guo, Leigh C. Smith, Luciano Fraga, Felipe Navarete, Juan Carlos Beamín, Calum Morris
Figure caption: Variability of the scattered light from two regions of the VVV/VVVX K s images. Left: the emission was integrated inside the circular blue and red masks. A smaller mask was also placed on the object. The image orientation is the the same as in Figures 1 and 4. Right: the resulting light curves for the three regions covering the same epochs as Figure 2. All curves show the same periodicity behavior, but the red curve presents a substantial lag with respect to the point source, while the blue curve is in phase with VVV-WIT-12. Time in the x-axis is shown in years (top) and MJD (bottom).
Paper: Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
Authors: H. T. Li, X. Cheng, Y. W. Ni, C. Li, S. H. Rao, J. H. Guo, M. D. Ding, P. F. Chen
Figure caption: (a) CHASE Hα line center image of the full disk showing the location of the target filament pointed out by the white box. The two black boxes show the nearby quiescent regions. (b) The average Hα profiles of the entire active region (red) and filament (gray) as indicated by the cyan curve in in panel (c). (d) The Hα profile of the quiescent regions that is used for calibration. The shadow region indicates the wave band where the Hα line center is calculated.
Paper: Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
Authors: H. T. Li, X. Cheng, Y. W. Ni, C. Li, S. H. Rao, J. H. Guo, M. D. Ding, P. F. Chen
Figure caption: (a) AIA 304 Å image overlaid by the contours (±50 G) of the HMI line-of-sight magnetogram. The inserted panels are the zoom-in of the magnetograms for the region of interest with the contours in blue (green) representing the positive (negative) polarities of 50 G (–50 G). (b) Distance–time diagram of the AIA 304 Å images along the slit AB in panel (a). The dashed lines in white show the trajectories of the ejected jets. (c)–(d) The zoom-in of the distance–time diagram for the white boxes 1 and 2 in panel (b). The dashed red/blue lines indicate the trajectories of the upward/downward plasma. (e) Temporal evolutions of the integrated fluxes for the positive (purple) and negative (green) polarities, as well as the integrated AIA 304 Å intensity (red) as shown in the black box in panel (a).
Paper: Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
Authors: H. T. Li, X. Cheng, Y. W. Ni, C. Li, S. H. Rao, J. H. Guo, M. D. Ding, P. F. Chen
Figure caption: Schematic drawing of the formation of the long filament F3. The lines with different colors indicate magnetic field lines, which indicate magnetic flux rope structures of F1, F2, and F3. The blue arrow indicates the upward EUV jets caused by the reconnection between two threads of F1 and F2. The black threads represent the cold filament materials. The arrows in red represent downward-moving filament materials shown as Hα redshifts.
Paper: Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
Authors: H. T. Li, X. Cheng, Y. W. Ni, C. Li, S. H. Rao, J. H. Guo, M. D. Ding, P. F. Chen
Figure caption: (a) Dopplergram of the filament F3. The gray and black contours represent the positive and negative polarities of ±50 G. (b)–(d) Hα profiles (black) at points C, D, and E in panel (a). The gray lines display the Hα spectrum of the quiescent region. The dashed lines in red show the fitted results.
Paper: PSR J2150+3427: A Possible Double Neutron Star System
Authors: Q. D. Wu, N. Wang, J. P. Yuan, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, S. Q. Wang, S. N. Sun, F. F. Kou, D. Zhao, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang
Figure caption: Panel (a): the mass–mass diagram of PSR J2150+3427 obtained from pulsar timing assuming fully general relativity. The gray region is excluded based on the mass function (black dotted line) and orbital geometry. The red line corresponds to ﹩\dot{\omega }=0.0115(4)﹩ deg yr−1, and the dotted line shows the regions that are consistent within the error in ﹩\dot{\omega }﹩. Panel (b): mass–mass diagram for known pulsars and PSR J2150+3427. Panel (c): the Q–q diagram of PSR J2150+3427 and the systems with the NS mass measured. Here, q = M  p /M  c  is the system mass ratio, and Q = P  b /e (day) is the orbital factor. The blue diamonds are the DNS systems with individual NS mass measurements. The green dots are the NS–WD systems with individual NS mass measurements. The black and red stars of the PSR J2150+3427 system are calculated assuming the orbital inclination of i = 90° and 60°, respectively.
Paper: PSR J2150+3427: A Possible Double Neutron Star System
Authors: Q. D. Wu, N. Wang, J. P. Yuan, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, S. Q. Wang, S. N. Sun, F. F. Kou, D. Zhao, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang
Figure caption: The P–﹩\dot{P}﹩ diagram of the known pulsars, including PSR J2150+3427. The binary pulsars are indicated in black, DNS systems are represented by the blue circles, and PSR J2150+3427 is indicated by the red star. The blue and green dashed–dotted lines are the death lines predicted by the CR-induced space-charged-limited flow (SCLF) models and the inverse Compton scattering-induced SCLF model, respectively (Zhang et al. 2000). The blue dashed line is the death line predicted by the CR-induced vacuum gap model proposed by Zhang et al. (2000). The black line is a typical death line predicted by CR from the vacuum gap model (Ruderman & Sutherland 1975). The black dashed line is modeled by Equation (9) of Chen & Ruderman (1993). The green solid line is the death line model from Zhou et al. (2017).
Paper: PSR J2150+3427: A Possible Double Neutron Star System
Authors: Q. D. Wu, N. Wang, J. P. Yuan, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, S. Q. Wang, S. N. Sun, F. F. Kou, D. Zhao, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang
Figure caption: Panel (a): the observed Doppler-modulated spin period (P) vs. MJD. It clearly shows that the pulsar orbit has a significant eccentricity. The black line is a best-fit orbital model obtained using P  b  ∼ 10.592 (day), x  p  ∼ 25.488 (lt-s), e ∼ 0.601, T 0 ∼ 59626.993 (MJD), and ω ∼ 262.791 (deg). Panels (b) and (c) show plots for postfit residuals vs., respectively, the MJD and orbital phase for 92 TOAs over 91 epochs.
Paper: PSR J2150+3427: A Possible Double Neutron Star System
Authors: Q. D. Wu, N. Wang, J. P. Yuan, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, S. Q. Wang, S. N. Sun, F. F. Kou, D. Zhao, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang
Figure caption: Integrated polarization profiles of PSR  J2150+3427. In the upper panel, the black dots with error bars are the PA points. The total intensity, linearly polarized flux and the circular-polarized flux are shown in black, red, and blue, respectively, in the lower panel.
Paper: Solar Energetic Particle Track-production Rates at 1 au: Comparing In Situ Particle Fluxes with Lunar Sample-derived Track Densities
Authors: A. R. Poppe, P. S. Szabo, E. R. Imata, L. P. Keller, R. Christoffersen
Figure caption: The differential energy spectrum of Fe SEPs measured by ACE/ULEIS between 0.03 MeV nuc−1 and 3.0 MeV nuc−1. The best-fit power-law spectrum is denoted by the dashed red line. The approximate energy range in which Fe-group SEPs leave damage tracks in meteoritic materials is denoted by the vertical dotted lines.
Paper: Solar Energetic Particle Track-production Rates at 1 au: Comparing In Situ Particle Fluxes with Lunar Sample-derived Track Densities
Authors: A. R. Poppe, P. S. Szabo, E. R. Imata, L. P. Keller, R. Christoffersen
Figure caption: The electronic stopping power, S  e , for three incident ion species (Ar, red; Fe, green; Ni, blue) in a forsterite mineral. The green closed circle and red open circle represent experimental measurements by Szenes et al. (2010) that did and did not register tracks, respectively. Correspondingly, the minimum required S  e  for track formation estimated by Szenes et al. (2010) is shown as the horizontal line.
Paper: Solar Energetic Particle Track-production Rates at 1 au: Comparing In Situ Particle Fluxes with Lunar Sample-derived Track Densities
Authors: A. R. Poppe, P. S. Szabo, E. R. Imata, L. P. Keller, R. Christoffersen
Figure caption: The predicted track density as a function of depth for an object exposed for 2 Myr at 1 au as determined by the ACE in situ measurements (solid line). Solid dots reproduce the measurements of Keller et al. (2021) along with the ACE-predicted flux lowered by a factor of 25 (dashed line). The orange line is the result of a Monte Carlo model for track formation taking into account a charged-particle erosion rate of 7 μm Myr−1.
Paper: Solar Energetic Particle Track-production Rates at 1 au: Comparing In Situ Particle Fluxes with Lunar Sample-derived Track Densities
Authors: A. R. Poppe, P. S. Szabo, E. R. Imata, L. P. Keller, R. Christoffersen
Figure caption: The monthly averaged Fe SEP flux measured by ACE/ULEIS for two energy ranges: (blue) 0.03–3.0 MeV nuc−1 and (red) 0.50–3.0 MeV nuc−1. Average values for each separate energy range are shown as dashed lines. The SEP track formation flux at 1 au inferred from Keller et al. (2021) is shown as the black dashed line.
Paper: Radio Emission and Electric Gaps in Pulsar Magnetospheres
Authors: Ashley Bransgrove, Andrei M. Beloborodov, Yuri Levin
Figure caption: Global currents and e ± production in the aligned rotator. The white region above the polar cap is the zone of outflowing current, the shaded gray region indicates the bulk return current, and the thick black curve shows the separatrix return-current layer. The hatched area indicates the closed zone. The null charge line (dashed) is defined by ρ GJ = −Ω ·  B /(2π c) = 0; above the line ρ GJ < 0 and below ρ GJ > 0. Episodic e ± discharge occurs in the outflowing current above the polar cap (α > 1), in the bulk return current above the polar cap (α < 0), and in the bulk return current outside the null line (α > 1). Beam instabilities occur outside the light cylinder where e ± is created by the intersecting gamma-ray beams with different directions.
Paper: JWST Detects Neon Line Variability in a Protoplanetary Disk
Authors: C. C. Espaillat, T. Thanathibodee, C. V. Pittman, J. A. Sturm, M. K. McClure, N. Calvet, F. M. Walter, R. Franco-Hernández, J. Muzerolle Page
Figure caption: Hα profiles of SZ Cha (blue) and the accretion flow modeling fits (black/gray). We show the average accretion flow model fit (black line) from the top 100 best-fitting models (gray lines). The horizontal dotted line denotes the continuum, and the vertical dotted line marks the line center. Horizontal green lines mark regions included in the fit.
Paper: JWST Detects Neon Line Variability in a Protoplanetary Disk
Authors: C. C. Espaillat, T. Thanathibodee, C. V. Pittman, J. A. Sturm, M. K. McClure, N. Calvet, F. M. Walter, R. Franco-Hernández, J. Muzerolle Page
Figure caption: Left: JWST MIRI MRS spectrum from 2023 (black) and Spitzer IRS SH spectrum from 2008 (purple) of SZ Cha. We label the [Ar II], H2, [Ne II], and [Ne III] emission lines and a polycyclic aromatic hydrocarbon feature around 11 μm. Directly to the left of the [Ar II] line is an H2 line. To the right of the [Ar II] line is a feature where [He II], [H I], and [Ni II] emission lines may overlap. Right: comparisons between the [Ne II] and [Ne III] lines within the same observation.
Paper: JWST Detects Neon Line Variability in a Protoplanetary Disk
Authors: C. C. Espaillat, T. Thanathibodee, C. V. Pittman, J. A. Sturm, M. K. McClure, N. Calvet, F. M. Walter, R. Franco-Hernández, J. Muzerolle Page
Figure caption: Line fits (orange) to MIR spectra of [Ne II] 12.81 μm, [Ne III] 15.55 μm, and [Ar II] 6.99 μm (blue lines). The top row corresponds to JWST and the bottom row to Spitzer.
Paper: Radio Emission and Electric Gaps in Pulsar Magnetospheres
Authors: Ashley Bransgrove, Andrei M. Beloborodov, Yuri Levin
Figure caption: Excitation of waves in the pulsar magnetosphere. Color bar shows the components of the electromagnetic field multiplied by ﹩{(r/{r}_{\star })}^{2}﹩. Top : E ∣∣ in the quasi-steady state. The dashed white curve shows the null surface ρ GJ = 0 (the null surface breathes outside r LC due to plasmoid motion). Insets (i)-(iii): electromagnetic modes excited during e ± discharges at the polar cap, inner return current, and outer return-current gaps. Inset (iv): waves excited by a beam plasma instability. For insets (i) and (ii), δ E ⊥ is calculated by projecting δ  E  ⊥ onto a unit vector in the ﹩\hat{{\boldsymbol{\phi }}}\times {\boldsymbol{B}}﹩direction.
Paper: Radio Emission and Electric Gaps in Pulsar Magnetospheres
Authors: Ashley Bransgrove, Andrei M. Beloborodov, Yuri Levin
Figure caption: Beam instabilities in the outer magnetosphere. Left: parallel momentum (p ∣∣) distributions of e ± (gray) and gamma rays (black) in regions (a) and (b) in the right panel. For gamma rays, we show distributions of p ∣∣/2 (their momentum is split between the created e + and e −). (a) Gamma rays from the current sheet (black peak) inject e ± (gray peak). (b) Gamma rays from the separatrix (thin black peak) and current sheet (wider black peak) inject different e ± beams. Right: charge density ρ (color bar) and charge bunches.
Paper: Radio Emission and Electric Gaps in Pulsar Magnetospheres
Authors: Ashley Bransgrove, Andrei M. Beloborodov, Yuri Levin
Figure caption: Poloidal cross section of the magnetosphere in the quasi-steady state. Green curves show poloidal magnetic field lines, and background color shows plasma density. The clouds of plasma above the polar cap form in e ± discharges. The absence of plasma (dark zone) above the separatrix shows the return-current gaps in the unscreened state; it fills with plasma every ∼2R LC/c during discharge episodes. Magnetic reconnection forms a dynamic plasmoid chain in the equatorial current sheet.
Paper: High-energy Neutrino Emission Associated with GWs from Binary Black Hole Mergers in AGN Accretion Disks
Authors: Zi-Hang Zhou, Kai Wang
Figure caption: Cumulative detected neutrino number of a single source by IceCube with different accretion rates at two different locations, i.e., 100 and 200 Mpc. The green line indicates three detected neutrinos so that the neutrino detection by IceCube can be identified at a ∼3σ significance level.
Paper: High-energy Neutrino Emission Associated with GWs from Binary Black Hole Mergers in AGN Accretion Disks
Authors: Zi-Hang Zhou, Kai Wang
Figure caption: The three pictures on the left are schematic pictures of jet propagation in the AGN disk. There are four types of shocks in the jet, including forward shock (FS), reverse shock (RS), collimation shock (CS), and internal shock (IS). The picture on the far right is the schematic picture of an idealized jet used in our calculations. Each color corresponds to the same Lorentz factor in that region. The shocks are located at the junction of each shock area.