adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery of A Large-scale Bent Radio Jet in the Merging Cluster A514
Authors: Wonki Lee, John ZuHone, M. James Jee, Kim HyeongHan, Ruta Kale, Eunmo Ahn
Figure caption: Radio maps of PKS 0446-20 at 740 MHz (Band 4, 550–850 MHz, left) and smoothed radio maps with the beam size of 35″ at 410 MHz (Band 3, 250–500 MHz, middle left) and 190 MHz (Band 2, 120–250 MHz, middle right). The right panel depicts the spectral index map derived from the three frequency channels. The radio maps are smoothed to match the beam size of 35″. The annotated ellipse in the bottom right corner describes the synthesized beam size of each radio map. The overlaid contours mark the 5σ detection in the 740 and 410 MHz radio maps and the 3σ detection in the 190 MHz radio map. The contours are spaced by a factor of 2. The radio emission gets fainter and presents a steeper spectrum with increasing distance from the AGN.
Paper: Discovery of A Large-scale Bent Radio Jet in the Merging Cluster A514
Authors: Wonki Lee, John ZuHone, M. James Jee, Kim HyeongHan, Ruta Kale, Eunmo Ahn
Figure caption: Mock X-ray surface brightness map of the simulations overlaid with scalar field density map (green), which is normalized with the injected density. The scalar field contours (white) start at 10−5 and are spaced equally by a factor of 2. The cyan arcs mark the temperature discontinuity, which shows the shock fronts. At ∼0.5 Gyr after the first closest passage (top panel), the bubble extends by ∼0.4 Mpc in a direction similar to A514. At ∼1.0 Gyr after the second closest passage (∼4.5 Gyr after the first closest passage, bottom panel), the bubble stretches along the merger shock in the cluster outskirts.
Paper: Discovery of A Large-scale Bent Radio Jet in the Merging Cluster A514
Authors: Wonki Lee, John ZuHone, M. James Jee, Kim HyeongHan, Ruta Kale, Eunmo Ahn
Figure caption: Multiwavelength view of A514. uGMRT radio maps (green), adaptively smoothed XMM-Newton X-ray (red), and the red sequence number density contours are overlaid on the Magellan/Megacam optical color composite image. The radio map at a lower frequency is described with a darker green color scale. The number density contours mark the level of 1.7, 2.3, and ﹩3.0\,\mathrm{galaxy}\,{\mathrm{arcmin}}^{-2}﹩. The elongated X-ray and the two red sequence number density peaks suggest the collision between the northwest and the southeast clusters, while the southern AGN shows a large-scale bent radio jet with the largest linear size ∼0.7 Mpc. The inset figure shows the point-source subtracted X-ray map around the radio features of the southern AGN. The green 410 MHz radio contours start from 5σ and are spaced by a factor of 2. The cyan arc marks the X-ray surface brightness discontinuity, which we interpret as a cold front (Section 3.2).
Paper: A Formation Mechanism for “Wrong Way” Radio Relics
Authors: Ludwig M. Böss, Ulrich P. Steinwandel, Klaus Dolag
Figure caption: From left to right: X-ray surface brightness, CR electron energy of electrons with E > 1 GeV, synchrotron surface brightness at 1.4 GHz, and the slope of the synchrotron spectrum between 144 MHz and 1.4 GHz. The top three rows show the time evolution of the infalling group in the xz-plane of the simulation; the bottom row shows the same relic at z = 0.27 in the yz-plane. To obtain the images the SPH data are mapped to a grid with a resolution of Δpix ≈ 1 kpc, which corresponds to a resolution of θ pix ≈ 0.″24 at z = 0.27.
Paper: Betatron Acceleration of Suprathermal Electrons within a Small-scale Flux Rope in the Solar Wind
Authors: Weiduo Meng, Jianpeng Guo, Haibo Lin, Huishan Fu, Meng Zhou, Dan Zhao, Yan Chen, Linxia He, Xianghan Wang, Zelin Wang
Figure caption: Wind observations of a flux rope (FR) embedded within the leading portion of an HPS (yellow shaded region) on 2012 February 28. The format is the same as Figure 1, except that magnetic field components in GSE coordinates are also given and overplotted in the magnetic field strength panel. Two purple vertical solid lines mark the boundaries of the FR.
Paper: Betatron Acceleration of Suprathermal Electrons within a Small-scale Flux Rope in the Solar Wind
Authors: Weiduo Meng, Jianpeng Guo, Haibo Lin, Huishan Fu, Meng Zhou, Dan Zhao, Yan Chen, Linxia He, Xianghan Wang, Zelin Wang
Figure caption: Electron phase space density (PSD) as a function of pitch angle (PA) and electron energy. (a) PSD outside the FR but inside the HPS (at 15:00:09 UT); it is treated as the “source.” (b) PSD inside the FR (at 14:30:42 UT); it is treated as the “consequence” after acceleration from the assumptive source electrons. Solid curves represent the Wind observations, and dashed curves represent the modeling results. The betatron factor F  b  and Fermi factor F  f  are shown. (c) PSDs of quasi-perpendicular electrons (103–1113 eV) at 14:30:42 UT (blue solid curve) and 15:00:09 UT (green solid curve). The red solid curve shows the predicted values assuming betatron acceleration. These PSDs follow approximately a power law with an index of ∼−3.4.
Paper: Betatron Acceleration of Suprathermal Electrons within a Small-scale Flux Rope in the Solar Wind
Authors: Weiduo Meng, Jianpeng Guo, Haibo Lin, Huishan Fu, Meng Zhou, Dan Zhao, Yan Chen, Linxia He, Xianghan Wang, Zelin Wang
Figure caption: Electron omnidirectional differential fluxes and electron pitch angle (PA) distribution during the interval surrounding the FR. From top to bottom: (a)–(b) omnidirectional differential fluxes of the 0.92–8.87 keV and 103–1113 eV electrons, respectively, (c)–(h) PA distributions of electrons with central energies of 1113, 689, 427, 265, 165, and 103 eV, respectively, (i) magnetic field strength and three components in GSE coordinates. The yellow shaded region indicates the HPS interval. Two purple vertical solid lines mark the boundaries of the FR. The blue vertical dashed line marks the crossing of the HCS.
Paper: A Formation Mechanism for “Wrong Way” Radio Relics
Authors: Ludwig M. Böss, Ulrich P. Steinwandel, Klaus Dolag
Figure caption: Histograms of the sonic Mach number ﹩{{ \mathcal M }}_{s}﹩ for the three output times shown in Figure 2. The colors correspond to the different times and the dotted line indicates the critical Mach number beyond which CR (re)acceleration can occur in our model.
Paper: A Formation Mechanism for “Wrong Way” Radio Relics
Authors: Ludwig M. Böss, Ulrich P. Steinwandel, Klaus Dolag
Figure caption: Histograms of the synchrotron surface brightness (left) and spectral slope (right) obtained from the images in Figure 2. As before, colors correspond to the times in Figures 2 and 3. The dotted line indicates the same relic at z = 0.27 in the yz-plane of the simulation, as in the bottom row of Figure 2.
Paper: A Formation Mechanism for “Wrong Way” Radio Relics
Authors: Ludwig M. Böss, Ulrich P. Steinwandel, Klaus Dolag
Figure caption: A simplified schematic of the merger geometry that produces the “wrong way” relic. The initial merger between M 1 and M 2 drives two shocks, the weaker of which is subsequently impacted by a third substructure M 3. This impact deforms parts of the outward traveling shock S 1 and produces the WWR S 3.
Paper: A Formation Mechanism for “Wrong Way” Radio Relics
Authors: Ludwig M. Böss, Ulrich P. Steinwandel, Klaus Dolag
Figure caption: Time evolution of the synchrotron spectrum. Colors correspond to the times in Figures 2 and 3. Dashed lines and labels show the spectral slope in the indicated frequency ranges.
Paper: A Formation Mechanism for “Wrong Way” Radio Relics
Authors: Ludwig M. Böss, Ulrich P. Steinwandel, Klaus Dolag
Figure caption: Similar to Figure 2 we show our WWR at z = 0.29 and z = 0.27. The first and third rows show the default projection in the xz-plane; the second and fourth rows show the relic rotated into the merger plane. Please note that the lower limit in the leftmost column is 1 order of magnitude lower compared to Figure 2 to improve the visibility of the contact between the outward moving shock and the atmosphere of the infalling halo.
Paper: A Formation Mechanism for “Wrong Way” Radio Relics
Authors: Ludwig M. Böss, Ulrich P. Steinwandel, Klaus Dolag
Figure caption: From left to right we show an electron spectrum freely cooling due to IC scattering off CMB photons at z = 0 and its synchrotron emission scaling with observational frequency (middle) and magnetic field strength (right).
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: A total of 3 out of the 14 little red dots followed up with deep NIRSpec multiobject prism spectroscopy turn out to be brown dwarfs. This figure shows the 2D spectrum and the extracted 1D spectrum of the brown dwarf A2744-BD1.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Distribution of brown dwarfs and highly reddened AGNs on near- and mid-infrared color–color diagrams. Colored circles show the Sonora brown dwarf models, color-coded with their effective temperatures. Grey hexagons show the subsample of highly reddened AGNs from Labbe et al. (2023), which we could confirm as extragalactic sources at z spec ≳ 5. Black stars show the three brown dwarfs presented in this work, masquerading as highly reddened AGN in the color selection of Labbe et al. (2023). The brown dwarf initially discovered in NIRCam photometry by Nonino et al. (2023) is marked with a small white star at its center (see Section 2 for more details). The black plus sign shows the brown dwarf discovered in CEERS NIRCam photometry (Wang et al. 2023). The thin dashed black lines show the color selection criteria of Labbe et al. (2023). The top panel shows that as brown dwarfs become warmer, they resemble the mid-infrared colors of highly reddened AGNs more closely. The bottom panel shows that the brown dwarfs are generally much bluer than highly reddened AGNs in the near-infrared filters. This is evident by the horizontal separation between the brown dwarfs and highly reddened AGNs in this panel. We propose a cut at F150W−F200W = 0.25 mag to distinguish brown dwarfs from highly reddened AGNs; this is shown as the thick dashed orange line.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: The distant brown dwarfs discovered here have effective temperatures (T eff) and bolometric luminosities (L bol) consistent with those of benchmark brown dwarfs with similar spectral types. The small data points show the T eff vs. spectral type (left) and L bol vs. spectral type (right) for a compilation of 274 brown dwarfs, including all the 75 known benchmark brown dwarfs of spectral types L6-Y1. The large data points show the locations of A2744-BD1 (red), -BD2 (yellow), and -BD3 (green) on these diagrams; the error bars on T eff, L bol, and spectral type are smaller than the symbol size. We constrain the spectral type of A2744-BD3, indicated by the large green data point, to be later than T5.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Distances of the brown dwarfs discovered in this work, compared with the UltracoolSheet compilation of the literature ultracool brown dwarfs (types late-M and later). The gray histogram presents the distance distribution of a subsample of UltracoolSheet brown dwarfs with reliable parallax distances (see the main text). The colored vertical lines (shaded regions) indicate the distances (1σ uncertainties) of the brown dwarfs discovered in this work. A2744-BD1 at ∼4.8 kpc is the most distant brown dwarf discovered to date.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Reduced χ 2 vs. spectral type for A2744-BD1. The gray data points show the reduced χ 2 for each spectral template. The blue data points show the best-matching templates with the lowest reduced χ 2.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Best-matching templates (yellow lines) to the brown dwarf A2744-BD3 (black data points). The χ 2 of these templates are shown as the blue data points in Figure 18.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: The 2D spectrum and the extracted 1D spectrum of the brown dwarf A2744-BD3.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Best-matching templates (yellow lines) to the brown dwarf A2744-BD2 (black data points). The χ 2 of these templates are shown as the blue data points in Figure 16.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Best-matching templates (yellow lines) to the brown dwarf A2744-BD1 (black data points). The χ 2 of these templates are shown as the blue data points in Figure 14.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Same as Figure 14, showing the reduced χ 2 vs. spectral type for A2744-BD2.
Paper: Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Same as Figure 14, showing the reduced χ 2 vs. spectral type for A2744-BD3.
Paper: A Unified Theory of Jetted Tidal Disruption Events: From Promptly Escaping Relativistic to Delayed Transrelativistic Jets
Authors: Odelia Teboul, Brian D. Metzger
Figure caption: Schematic illustration of a misaligned jetted TDE. Stellar debris following the disruption return to the orbital pericenter and form an accretion disk in the orbital plane of the star whose normal is in general significantly misaligned by an angle ψ with respect to the SMBH spin axis. Matter falls back to the disk at a highly super-Eddington accretion rate ﹩{\dot{M}}_{\mathrm{fb}}﹩, driving a disk wind of velocity β w = v w/c and mass-loss rate ﹩{\dot{M}}_{{\rm{w}}}\approx {f}_{{\rm{w}}}{\dot{M}}_{\mathrm{fb}}﹩. The remainder of the fallback feeds the SMBH at a rate ﹩\dot{M}=(1-{f}_{{\rm{w}}}){\dot{M}}_{\mathrm{fb}}﹩, powering a jet of luminosity ﹩{L}_{{\rm{j}}}=\eta \dot{M}{c}^{2}﹩ and half-opening angle θ j. Due to rapid precession of the disk orientation, on sufficiently large scales ﹩(R\gtrsim {R}_{\min };﹩ Equation (29)) the wind will collide and mix with itself and generate an approximately spherical outflow. The jet precesses with the disk and its head propagates into the disk outflow with velocity β h; precession effectively spreads the jet energy across a wider cone of half-opening angle ψ, the disk/spin misalignment angle. The insert shows a zoomed-in image of quantities relevant to the propagation of the helical jet (see Section 4 for details). Here, H is the pitch of the helix and n is the number of precession cycles, such that nH is the total vertical distance traveled by the jet and ﹩\tan \psi =\rho /({nH})﹩, where ρ is the cylindrical radius of the jet.
Paper: A Unified Theory of Jetted Tidal Disruption Events: From Promptly Escaping Relativistic to Delayed Transrelativistic Jets
Authors: Odelia Teboul, Brian D. Metzger
Figure caption: Top left panel: inner radius of the accretion disk at either the ISCO or ISSO in units of gravitational radii, as a function of the SMBH spin a, for different values of the spin–disk misalignment angle ψ as marked. Other panels: precession period of the disk created by the tidal disruption of a Sun-like star as a function of the SMBH spin a, with different panels showing the separate effect of changing: (a) the SMBH mass M • (for fixed ψ = 30°, R out = R c); (b) the misalignment angle ψ (for fixed M • = 106 M ⊙ and R out = R c); (c) the outer radius R out (for fixed M • = 106 M ⊙, ψ = 30°), particularly whether R out = R c is fixed or whether the disk is allowed to expand viscously. In the latter case, the solid lines correspond to the fiducial spreading evolution, taking into account wind angular momentum losses R d ∝ t 2/5 (Equation (16)), while the dashed lines correspond to the fiducial expansion rate without wind angular momentum losses R out ∝ t 2/3.
Paper: A Unified Theory of Jetted Tidal Disruption Events: From Promptly Escaping Relativistic to Delayed Transrelativistic Jets
Authors: Odelia Teboul, Brian D. Metzger
Figure caption: Regimes of distinct jet alignment mechanisms (“magneto-spin” vs. “hydrodynamical”) in the parameter space of dimensionless SMBH spin a and jet efficiency η for M • = 106 M ⊙, the disruption of a solar-type star and a typical disk–spin misalignment angle ψ = 30°. For sufficiently powerful jets powered by the BZ process (η ≳ η BZ,align; Equation (24)), the magnetic field is sufficiently strong that magneto-spin alignment is the fastest process, occurring on a timescale as short as the fallback time over which most of the mass and magnetic flux is assumed to be accreted; we show this boundary separately for β = 1 and ﹩\beta ={\beta }_{\max }﹩ (Equation (2)). Our estimate of the minimum SMBH spin required for magneto-spin alignment (Equation (25) for β = 1) is also shown with a vertical line.
Paper: A Unified Theory of Jetted Tidal Disruption Events: From Promptly Escaping Relativistic to Delayed Transrelativistic Jets
Authors: Odelia Teboul, Brian D. Metzger
Figure caption: Diversity of outcomes of jetted TDEs depending on the initial misalignment angle ψ, jet efficiency η, orbital penetration factor β, and the physical mechanism responsible for alignment (Section 3.3). The jet alignment mechanism depends on both the jet efficiency η and orbital penetration factor β (Figure 3). The jet–spin misalignment angle ψ and wind properties f w and β w in part determine the critical efficiency η crit,2 (Equation (42)) needed to escape before alignment and after alignment η crit,1 (Equation (38)) and hence on the energy.
Paper: A Unified Theory of Jetted Tidal Disruption Events: From Promptly Escaping Relativistic to Delayed Transrelativistic Jets
Authors: Odelia Teboul, Brian D. Metzger
Figure caption: Two-component synchrotron emission model fit to the 15.4 GHz radio light curve of Swift J1644+57 as a relativistic jet that escapes from the TDE wind prior to alignment with the SMBH spin into an external medium with a wind-like density profile ρ ext = Ar −2, where A = 3 × 1011 g cm−1. Prior to alignment, the precession of the jet creates a large angular structure with E iso = 1053 erg and half-opening angle ψ = 20° corresponding to the misalignment angle. After alignment completes, the remainder of the jet energy is injected into a narrow jet with E iso = 6 × 1052 erg and half-opening angle θ j = 5° aligned with the SMBH spin axis and viewer line of site. The two vertical lines depict the dynamical times of interest: t RS, the shell crossing time, and t NR, the time when the blast wave transitions to the nonrelativistic Newtonian regime. The observation data are taken from Zauderer et al. (2011), Berger et al. (2012), and Eftekhari et al. (2018). We assume p=2.4 and ϵ  e  = ϵ  B  = 0.1 for the electron power law and shock equipartition parameters, respectively.
Paper: A Unified Theory of Jetted Tidal Disruption Events: From Promptly Escaping Relativistic to Delayed Transrelativistic Jets
Authors: Odelia Teboul, Brian D. Metzger
Figure caption: Synchrotron emission model of AT2018hyz as a delayed mildly relativistic jet that escapes at the time of alignment t align ∼ 920 days with the SMBH spin computed with the model described in Teboul & Shaviv (2021). The jet has an isotropic energy E iso = 8 × 1049 erg and half-opening angle θ j = 20°. As in the other jetted TDE, we assume the external medium possesses a wind-like density profile ρ ext = Ar −2, where A = 9 × 1012 g cm−1. The observation data are taken from Cendes et al. (2022) and upper limits are taken from Horesh et al. (2018) and Lacy et al. (2020). We assume p=2.25, ϵ  e  = 0.2, and ϵ  B  = 0.007 for the electron power law and shock equipartition parameters, respectively.
Paper: A Unified Theory of Jetted Tidal Disruption Events: From Promptly Escaping Relativistic to Delayed Transrelativistic Jets
Authors: Odelia Teboul, Brian D. Metzger
Figure caption: Parameter space of jet efficiency η vs. disk/jet–spin misalignment angle ψ or jet half-opening angle θ j required for successful escape of the TDE jet from the disk wind envelope for f w = 0.15, β w = 0.2. We show separately cases for a rapidly precessing misaligned jet (top panel) and an aligned jet (bottom panel). The critical minimum efficiency for a successful jet before (η crit,1; Equation (42)) and after alignment (η crit,1; Equation (38)) are shown with solid purple lines.
Paper: A Unified Theory of Jetted Tidal Disruption Events: From Promptly Escaping Relativistic to Delayed Transrelativistic Jets
Authors: Odelia Teboul, Brian D. Metzger
Figure caption: Synchrotron emission model of AT2022cmc as a relativistic jet that escapes from the TDE wind at the time of alignment with the SMBH spin computed with the model described in Teboul & Shaviv (2021). The relativistic jet has an isotropic energy E iso = 1 × 1053 erg and half-opening angle θ j = 10°. The external medium harbors a wind-like density profile ρ ext = Ar −2, where A = 3 × 1012 g cm−1. The observation data are taken from Andreoni et al. (2022) and Rhodes et al. (2023). We assume p=2.9, ϵ  e  = 0.2, and ϵ  B  = 0.002 for the electron power law and shock equipartition parameters, respectively.
Paper: Tilted Dark Halos Are Common and Long-lived, and Can Warp Galactic Disks
Authors: Jiwon Jesse Han, Vadim Semenov, Charlie Conroy, Lars Hernquist
Figure caption: Evolution of the tilt angle of the dark and stellar halo from 6 Gyr ago to present day in TNG50 Milky Way analogs (Pillepich et al. 2023). Each line represents a single halo. The first and second row panels show the evolution of the tilt angle of the dark matter and stellar halo, and the third row panels show the evolution of the dark halo triaxiality parameter T ≡ 1 − p 2/1 − q 2, where p and q are the major-to-intermediate and major-to-minor axis ratios. We increase the line thickness with time, and color each line according to its final dark halo tilt angle. On the right panel, we plot the cumulative distribution function (CDF) of the tilt angles at the present day, which reveals that around half of TNG50 Milky Way analogs have dark halo tilt angles greater than 10°. We find a diversity of triaxiality parameters for the tilted halos, ranging from prolate (T > 0.6) to oblate (T < 0.3).