adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Measurements of 13C, 18O, and 17O in the Atmosphere of Super-Jupiter VHS 1256 b
Authors: Siddharth Gandhi, Sam de Regt, Ignas Snellen, Yapeng Zhang, Benson Rugers, Niels van Leur, Quincy Bosschaart
Figure caption: Posterior distributions of the volume mixing ratios of the isotopologues of CO in the retrieval of VHS 1256 b. These show the dependence of one species on the other. Note that C and O refer to the main isotopologues, 12C and 16O, respectively.
Paper: JWST Measurements of 13C, 18O, and 17O in the Atmosphere of Super-Jupiter VHS 1256 b
Authors: Siddharth Gandhi, Sam de Regt, Ignas Snellen, Yapeng Zhang, Benson Rugers, Niels van Leur, Quincy Bosschaart
Figure caption: Marginalized posterior distributions for the volume mixing ratios of H2O, 12CO, CO2, and the overall atmospheric C/O ratio (right panel) from the retrieval of the ∼4.1–5.3 μm JWST observations of VHS 1256 b. The red dashed line shows the solar C/O ratio (Asplund et al. 2021).
Paper: JWST Measurements of 13C, 18O, and 17O in the Atmosphere of Super-Jupiter VHS 1256 b
Authors: Siddharth Gandhi, Sam de Regt, Ignas Snellen, Yapeng Zhang, Benson Rugers, Niels van Leur, Quincy Bosschaart
Figure caption: Signal-to-noise ratio (S/N) derived from the cross-correlation functions of the CO isotopologues.
Paper: JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M •–M ⋆ Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models
Authors: Fabio Pacucci, Bao Nguyen, Stefano Carniani, Roberto Maiolino, Xiaohui Fan
Figure caption: Overview of the data set used and the local M •–M ⋆ relation from Reines & Volonteri (2015). The dark-shaded region denotes the 1σ uncertainty from the linear fit, and the light-shaded region denotes the 0.55 dex rms deviation of the local observations from the local relation. The black hole masses are estimated from the Hα virial relation from Reines et al. (2013), with the parameters chosen by Reines & Volonteri (2015). At four different redshifts (z = 4, 5, 6, 7), the horizontal lines show the limiting sensitivities for a 3σ detection of the Hα line with NIRSpec (see Section 3.2 for a detailed description). Error bars indicate the 1σ uncertainty in the stellar and black hole masses. As a comparison, the dotted brown line displays the M •–M ⋆ relation by Greene et al. (2020).
Paper: JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M •–M ⋆ Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models
Authors: Fabio Pacucci, Bao Nguyen, Stefano Carniani, Roberto Maiolino, Xiaohui Fan
Figure caption: Left panel: expected surface density of sources with a mass M • ≲ 106.5 M ⊙, i.e., lighter than the smallest SMBH in our data set: JADES 62309 (Maiolino et al. 2023a), assuming the local M •–M ⋆ relation. The shaded regions account for uncertainties in the black hole mass measurement using the Hα line (Equation (2)) and the SMF (Equation (3)). The expected surface density is provided for different redshifts z ∼ 4, 5, 6, with a redshift binning of Δz = 1. Right panel: same as the left panel, but using our inferred high-z relation. The peaks of the distributions are shifted to hosts with lower stellar masses, and the surface density of observable light-mass black holes is higher.
Paper: JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M •–M ⋆ Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models
Authors: Fabio Pacucci, Bao Nguyen, Stefano Carniani, Roberto Maiolino, Xiaohui Fan
Figure caption: Left panel: expected surface density of sources with a mass <M •, for z = 4, 5, 6, assuming the local M •–M ⋆ relation. The two vertical lines indicate the lightest (JADES 62309; Maiolino et al. 2023a) and heaviest (GS 3073; Übler et al. 2023) black holes included in the data set. The horizontal line indicates the surface density of sources identified by Harikane et al. (2023a) in CEERS (eight sources in ﹩\approx 72\,{\mathrm{arcmin}}^{-2}﹩). The 1σ error bars account for uncertainties in the black hole mass measurement using the Hα line (Equation (2)) and the SMF (Equation (3)). Right panel: same as the left panel, but using the inferred high-z relation. Again, the surface density of observable black holes is higher for all redshifts.
Paper: JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M •–M ⋆ Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models
Authors: Fabio Pacucci, Bao Nguyen, Stefano Carniani, Roberto Maiolino, Xiaohui Fan
Figure caption: Qualitative representation of the current horizon within which black holes are detectable with JWST/NIRSpec. The galaxy + black hole systems used in this work are shown in blue. The farthest galaxy hosting an SMBH detected, GN-z11, is shown in red. The contours indicate typical heavy and light seeding distributions at z > 10. Some growth lines are also shown from the center of the seed distributions and assume several Eddington ratios (as indicated). The general distribution of lower-redshift quasars is displayed as a reference (Lyke et al. 2020; Fan et al. 2023).
Paper: JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M •–M ⋆ Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models
Authors: Fabio Pacucci, Bao Nguyen, Stefano Carniani, Roberto Maiolino, Xiaohui Fan
Figure caption: Left panel: in red, the high-z M •–M ⋆ relation derived from JWST data at z = 4–7. The dark-shaded 1σ uncertainty region is derived from sampling n = 1000 M •–M ⋆ relations randomly chosen within the 1σ three-dimensional contour of the fit parameters. The red dotted lines and light-shaded region represent the best-fit intrinsic scatter of 0.69 dex (defined as ﹩\sqrt{\nu }\sec \theta ﹩; see Section 3.4). Right panel: the posterior distribution of the parameters defining the M •–M ⋆. The solid blue line and black dashed lines of the one-dimensional distributions denote the median and 1σ uncertainties of the fit parameters, respectively. The solid contour lines in the two-dimensional distributions denote the 1σ, 2σ, and 3σ joint uncertainties.
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: Solar wind parameters observed by the Wind spacecraft from 2012 February 26 to March 1. From top to bottom: (a) omnidirectional differential flux of the 103–1113 eV electrons, (b) pitch angle (PA) distribution of the 427 eV electrons, (c) interplanetary magnetic field strength (∣B∣), (d) elevation angle (θ) and (e) azimuthal angle (ϕ) of field direction in GSE coordinates, (f) proton density (N  p ), (g) proton velocity (V  p ), (h) proton temperature (T  p ) overlaid with the expected temperature from the observed proton speed, and (i) proton β. The shaded regions indicate the magnetic cloud (MC) and heliospheric plasma sheet (HPS) intervals. The pink vertical dashed line marks the shock driven by the MC, and the blue dashed lines mark the multiple crossings of the heliospheric current sheet (HCS).
Paper: UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50
Authors: Vasily Kokorev, Seiji Fujimoto, Ivo Labbe, Jenny E. Greene, Rachel Bezanson, Pratika Dayal, Erica J. Nelson, Hakim Atek, Gabriel Brammer, Karina I. Caputi, Iryna Chemerynska, Sam E. Cutler, Robert Feldmann, Yoshinobu Fudamoto, Lukas J. Furtak, Andy D. Goulding, Anna de Graaff, Joel Leja, Danilo Marchesini, Tim B. Miller, Themiya Nanayakkara, Pascal A. Oesch, Richard Pan, Sedona H. Price, David J. Setton, Renske Smit, Mauro Stefanon, Bingjie Wang, 冰洁 王, John R. Weaver, Katherine E. Whitaker, Christina C. Williams, Adi Zitrin
Figure caption: BH mass vs. cosmic age. The red star shows the result presented in this work. The dark blue squares and violet diamonds show the results for z = 6–7 and >7 QSOs, respectively, as presented in Inayoshi et al. (2020), Maiolino et al. (2023a), and Fan et al. (2023). A triply lensed z = 7 QSO from Furtak et al. (2023a) is shown as a cyan square. A tentative M BH range for UHZ-1 at z = 10.1 from Goulding et al. (2023) is shown as a blue circle. Two high-z AGN candidates, namely, z = 8.7 AGN from CEERS (Larson et al. 2023) and GNz11 at z = 10.6 (Maiolino et al. 2023b), are shown as an open diamond and circle, respectively. Dashed lines show analytical models of BH mass accretion at an Eddington rate starting from a stellar seed (maroon) and a DCBH model (black).
Paper: UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50
Authors: Vasily Kokorev, Seiji Fujimoto, Ivo Labbe, Jenny E. Greene, Rachel Bezanson, Pratika Dayal, Erica J. Nelson, Hakim Atek, Gabriel Brammer, Karina I. Caputi, Iryna Chemerynska, Sam E. Cutler, Robert Feldmann, Yoshinobu Fudamoto, Lukas J. Furtak, Andy D. Goulding, Anna de Graaff, Joel Leja, Danilo Marchesini, Tim B. Miller, Themiya Nanayakkara, Pascal A. Oesch, Richard Pan, Sedona H. Price, David J. Setton, Renske Smit, Mauro Stefanon, Bingjie Wang, 冰洁 王, John R. Weaver, Katherine E. Whitaker, Christina C. Williams, Adi Zitrin
Figure caption: Derived M BH and L bol compared to the other high-z quasars. Our source is shown as a red star. Two high-z AGN candidates, CEERS_1019 at z = 8.7 (Larson et al. 2023) and GNz11 at z = 10.6 (Maiolino et al. 2023b), are shown as an open diamond and circle, respectively. JWST-detected AGN at z > 4 are shown as blue squares (Harikane et al. 2023; Kocevski et al. 2023; Maiolino et al. 2023a; Matthee et al. 2023). The cyan square shows the triply lensed quasar from Furtak et al. (2023a). A massive, bright z = 7.07 QSO from Matsuoka et al. (2019) is shown as an orange square. The dashed lines show the bolometric luminosities with Eddington ratios of L bol/L edd = 0.01, 0.1, and 1.0.
Paper: UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50
Authors: Vasily Kokorev, Seiji Fujimoto, Ivo Labbe, Jenny E. Greene, Rachel Bezanson, Pratika Dayal, Erica J. Nelson, Hakim Atek, Gabriel Brammer, Karina I. Caputi, Iryna Chemerynska, Sam E. Cutler, Robert Feldmann, Yoshinobu Fudamoto, Lukas J. Furtak, Andy D. Goulding, Anna de Graaff, Joel Leja, Danilo Marchesini, Tim B. Miller, Themiya Nanayakkara, Pascal A. Oesch, Richard Pan, Sedona H. Price, David J. Setton, Renske Smit, Mauro Stefanon, Bingjie Wang, 冰洁 王, John R. Weaver, Katherine E. Whitaker, Christina C. Williams, Adi Zitrin
Figure caption: Electron temperature (T e) as a function of the [O III]4364/[O III]5007 (RO3) ratio. In black, we present models from Nicholls et al. (2020) for different electron densities ranging from 1 to 104; the dynamic range does not allow us to distinguish between different lines, however. We show our observed line ratio in maroon, as well as in blue after the dust correction. The z = 8.5 source displaying extreme RO3 from Katz et al. (2023) is shown with a dashed green line. The shaded regions show the 1σ uncertainty. The extremely high line ratio we find is indicative of AGN-dominated ionization.
Paper: UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50
Authors: Vasily Kokorev, Seiji Fujimoto, Ivo Labbe, Jenny E. Greene, Rachel Bezanson, Pratika Dayal, Erica J. Nelson, Hakim Atek, Gabriel Brammer, Karina I. Caputi, Iryna Chemerynska, Sam E. Cutler, Robert Feldmann, Yoshinobu Fudamoto, Lukas J. Furtak, Andy D. Goulding, Anna de Graaff, Joel Leja, Danilo Marchesini, Tim B. Miller, Themiya Nanayakkara, Pascal A. Oesch, Richard Pan, Sedona H. Price, David J. Setton, Renske Smit, Mauro Stefanon, Bingjie Wang, 冰洁 王, John R. Weaver, Katherine E. Whitaker, Christina C. Williams, Adi Zitrin
Figure caption: BH-to-stellar mass relation. The color coding is the same as in Figure 3. The solid and dashed black lines show the best fits to the z = 0 AGN samples from Reines & Volonteri (2015) and Greene et al. (2016), respectively. The high-z trend from Pacucci et al. (2023) is shown as a dashed maroon line. Only an upper limit on M * is available for our source and the triply lensed quasar from Furtak et al. (2023a).
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: Apart from the three brown dwarfs presented in Figures 1–6, we confirm the remaining 11 targeted little red dots as extragalactic sources. For each spectrum, the MSA ID, spectroscopic redshift, and the ID in Labbe et al. (2023) are noted on top of its  corresponding panel. High S/N emission lines are marked with red stripes. MSA IDs 13123, 15383, and 16594 present the triply imaged AGN A2744-QSO1 at z spec = 7.05 (Furtak et al. 2023a, 2023b). MSA ID 20466 was recently confirmed as a broad-line AGN at z spec = 8.50 (Kokorev et al. 2023). The entire sample of these extragalactic sources was more recently analyzed in detail in Greene et al. (2023), further confirming MSA IDs 4286, 13821, 38108, and 41225 as broad-line AGNs.
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 Figures 2 and 4, but showing the photometry of 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: Photometry of A2744-BD1. Each inset presents a 2.″4 × 2.″4 cutout centered on the MSA slit that targeted the source. The bottom right inset shows the variance-weighted stack of F277W, F356W, and F444W images. The MSA slitlets are overlaid as the red rectangles.
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-fit model to A2744-BD1. The green line shows the observed NIRSpec prism spectrum of A2744-BD1, and the orange line shows the best-fit template from the grid of Sonora atmosphere models. The best-fit model parameters as well as the corresponding spectral classification are noted at the top of the figure.
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 2, but showing the photometry of 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 Figures 8 and 9; showing the best-fit model to 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: Same as Figure 8; showing the best-fit model to 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: The 2D spectrum and the extracted 1D spectrum of the brown dwarf A2744-BD2.
Paper: UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50
Authors: Vasily Kokorev, Seiji Fujimoto, Ivo Labbe, Jenny E. Greene, Rachel Bezanson, Pratika Dayal, Erica J. Nelson, Hakim Atek, Gabriel Brammer, Karina I. Caputi, Iryna Chemerynska, Sam E. Cutler, Robert Feldmann, Yoshinobu Fudamoto, Lukas J. Furtak, Andy D. Goulding, Anna de Graaff, Joel Leja, Danilo Marchesini, Tim B. Miller, Themiya Nanayakkara, Pascal A. Oesch, Richard Pan, Sedona H. Price, David J. Setton, Renske Smit, Mauro Stefanon, Bingjie Wang, 冰洁 王, John R. Weaver, Katherine E. Whitaker, Christina C. Williams, Adi Zitrin
Figure caption: Top: JWST/NIRCam 1.″5 stamps and the RGB color image comprised of the F277W, F356W, and F444W bands. The MSA slitlet layout is highlighted in white. An unambiguous pointlike morphology of ID 20466 can be observed in all filters. In each panel, we show the total magnitudes with 1σ  uncertainty, as presented in the UNCOVER photometric catalog of Weaver et al. (2023). Middle: 2D MSA PRISM spectrum produced by MSAEXP. We optimally scaled the trace to highlight all of the significant line detections. Bottom: collapsed 1D spectrum of our source. We show the data in black, while the uncertainty on the spectrum is in red. Assuming the best-fit MSAEXP z spec = 8.502 ± 0.003, we show the positions of all of the prominent emission with significant (>3σ) detections as solid vertical lines. Emission for which we only obtain an upper limit is shown with dashed lines.
Paper: UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50
Authors: Vasily Kokorev, Seiji Fujimoto, Ivo Labbe, Jenny E. Greene, Rachel Bezanson, Pratika Dayal, Erica J. Nelson, Hakim Atek, Gabriel Brammer, Karina I. Caputi, Iryna Chemerynska, Sam E. Cutler, Robert Feldmann, Yoshinobu Fudamoto, Lukas J. Furtak, Andy D. Goulding, Anna de Graaff, Joel Leja, Danilo Marchesini, Tim B. Miller, Themiya Nanayakkara, Pascal A. Oesch, Richard Pan, Sedona H. Price, David J. Setton, Renske Smit, Mauro Stefanon, Bingjie Wang, 冰洁 王, John R. Weaver, Katherine E. Whitaker, Christina C. Williams, Adi Zitrin
Figure caption: Top: best-fit narrow (blue) and broad (green) Gaussian line components fit to the Hβ, [O III] λ λ4959, 5007 line complex. A dual fit to the Hβ is necessary to account for both the broad (FWHM ∼ 3400 km s−1) and narrow (FWHM ∼ 200 km s−1) components. The combined fit is shown as a dashed maroon line. The error spectrum is shown as a dashed red line. Bottom left: zoom-in on the Hβ line. Bottom right: fit to the blended Hγ (red) and auroral [O III]4364 (blue) lines. As before, the combined fit is shown as a dashed maroon line.
Paper: Density Enhancement Streams in The Solar Wind
Authors: F. S. Mozer, O. Agapitov, S. D. Bale, R. Livi, O. Romeo, K. Sauer, I. Y. Vasko, J. Verniero
Figure caption: (a), (b) Dispersion of kinetic Alfvén waves in a proton plasma with an abundance of 5% alpha particles. From top to bottom: the normalized frequency ω/Ωp, the phase velocity V ph normalized to the proton Alfvén velocity V Ap, and the growth rate γ/Ωp vs. the normalized wavenumber kc/ω p are shown; ω p is the proton plasma frequency. (a) Vlasov approach with β e = 0.15, β p = 0.15. β e and β p are the electron and proton plasma beta, respectively. The temperature anisotropy that drives the kinetic Alfvén instability is T perp/T par = 6.5. The propagation angle is θ = 85°. (b) Frequency and phase velocity from Hall-MHD theory. (c) Dispersion of (linear) stationary waves k = k(U) related to the waves in (b). From top to bottom: real part k r, imaginary part k i, and frequency ω = k r U, U: velocity of the moving structure. (d)–(i) Results of the oscilliton theory: (d) Magnetic field hodogram B z-B z0 vs. B y, (e) electric field hodogram E x vs. E y, (f) electron density profile Ne(x), (g) electric field profile E x(x), (h) electric power spectrum ∣E x(k)∣2, and (i) magnetic power spectrum ∣B y(k)∣2.
Paper: Density Enhancement Streams in The Solar Wind
Authors: F. S. Mozer, O. Agapitov, S. D. Bale, R. Livi, O. Romeo, K. Sauer, I. Y. Vasko, J. Verniero
Figure caption: Power spectra of the electric field (black), plasma density (red), and magnetic field (green) in panel (a) at the time of the data in the remaining panels. The magnetic field spectrum appears normal with both a peak at ∼1 Hz (normally attributed to Alfvénic turbulence), a large decrease of power between 1 and 20 Hz, and a break in the spectrum near 10 Hz, at a frequency near the proton gyrofrequency (the dashed vertical line). The electric field and density spectra in the panel (a) display peaks at ∼1 Hz, 5 Hz, and harmonics, and have a much smaller decrease with frequency than the magnetic field. Because there is wave power in all three components near 1 Hz, this frequency signature must come from a mixture of electromagnetic and electrostatic waves, so it is not pure Alfvénic turbulence. The harmonic signatures at higher frequencies are purely electrostatic and the wave power is much greater than that expected for Alfvénic turbulence. The electric field, magnetic field, and density waveforms that produced these spectra are illustrated in panels (b), (c), and (d).
Paper: Density Enhancement Streams in The Solar Wind
Authors: F. S. Mozer, O. Agapitov, S. D. Bale, R. Livi, O. Romeo, K. Sauer, I. Y. Vasko, J. Verniero
Figure caption: Density streams during a 6 s interval (panel (a)), measured X- and Y-components of the electric field (panels (b) and (c)), and an estimate of the unmeasured EZ (panel (d)), obtained from the two measured electric field components and the assumption that the parallel electric field was zero. The EX electric field of panel (e) was computed from the Ohm’s law requirement that the pressure gradient due to the density fluctuations of panel (a) was balanced by the electric field. It is noted the EX was larger than the other two electric field components which shows that the electrostatic k-vector was in the X-direction, which was perpendicular to the background magnetic field. Also shown (panels (f) and (g)) are the four individual antenna voltages whose average is the spacecraft potential. All data in this figure, other than that in panels (f) and (g), are high pass filtered at 1 Hz.
Paper: Density Enhancement Streams in The Solar Wind
Authors: F. S. Mozer, O. Agapitov, S. D. Bale, R. Livi, O. Romeo, K. Sauer, I. Y. Vasko, J. Verniero
Figure caption: Panel (a) gives the electric field spectrum as a function of time, (b) gives the spectrum of density fluctuations, (c) gives the instantaneous perpendicular to parallel proton temperature ratio as the black dots and their 30 s averages as the red dots, (d) gives the electron and proton betas as computed from the quasi-thermal-noise, and (e) gives the alpha to proton density ratio. Note that the spike at 11:38 is an artifact. Three pairs of vertical dashed lines denote three of the about eight regions in which the proton and density fluctuations in panels (a) and (b) were large. These regions occurred near but not necessarily in regions where the temperature anisotropy in panel (c) was larger than 6 and in regions where the alpha to proton density ratio was maximum.
Paper: Density Enhancement Streams in The Solar Wind
Authors: F. S. Mozer, O. Agapitov, S. D. Bale, R. Livi, O. Romeo, K. Sauer, I. Y. Vasko, J. Verniero
Figure caption: 10 s of data in panel (a) that illustrate the power spectra of the electric field (black), the density fluctuations (red), and the magnetic field (green). The 1 and 7 Hz peaks contain electric field, magnetic field, and density maxima, indicating that both an electrostatic and electromagnetic wave existed at these frequencies. It is noted that the amplitude of the electrostatic wave at all frequencies was large compared to that of the Alfvénic turbulence expected from the magnetic field spectrum. Thus, this new wave mode may be an important contributor to the heating, scattering, and acceleration of the plasma.
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: X-ray surface brightness profile (black) over the bridge. The X-ray surface brightness profile is well described with a broken power law (red) with a compression ratio C ∼ 1.75 ± 0.25. The radio surface brightness profile (green) presents a peak at the X-ray surface brightness jump.