adsabs/AstroCLIMB huggingface dataset:
Paper: Two Candidate KH 15D–like Systems from the Zwicky Transient Facility
Authors: Wei Zhu, 伟 祝, Klaus Bernhard, Fei Dai, 飞 戴, Min Fang, 敏 房, J. J. Zanazzi, Weicheng Zang, 伟呈 臧, Subo Dong, 苏勃 东, Franz-Josef Hambsch, Tianjun Gan, 天君 干, Zexuan Wu, 泽炫 吴, Michael Poon
Figure caption: Schematic of the one-sided, fully opaque screen model used in this work. The model is described by five parameters: the time and perpendicular velocity of the star at epochs of ingress (with subscript “in”) and egress (with subscript “out”), respectively, and the orbital period of the star. The bottom panel shows an example light curve from the model.
Paper: Two Candidate KH 15D–like Systems from the Zwicky Transient Facility
Authors: Wei Zhu, 伟 祝, Klaus Bernhard, Fei Dai, 飞 戴, Min Fang, 敏 房, J. J. Zanazzi, Weicheng Zang, 伟呈 臧, Subo Dong, 苏勃 东, Franz-Josef Hambsch, Tianjun Gan, 天君 干, Zexuan Wu, 泽炫 吴, Michael Poon
Figure caption: Similar to Figure 2 but for the Bernhard-2 system.
Paper: Divergence in Mass Ratio Distributions between Low-mass and High-mass Coalescing Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Yuan-Zhu Wang, 远瞩 王, Shao-Peng Tang, 少 鹏 唐, Qiang Yuan, 强 袁, Yi-Zhong Fan, 一中 范, Da-Ming Wei, 大明 韦
Figure caption: (a) Primary mass and mass ratio posteriors for the 63 BBH candidates (including GW190814) in the LVKC GWTC-3 catalog (The LIGO Scientific Collaboration et al. 2021a) with FARs below 0.25 yr−1, as obtained under a default prior. Each shaded region (black point) represents the central 90% credible posterior bounds (median m 1 and median q value) of a given BBH. The red and green regions represent the three asymmetric systems GW190814 and GW190412. (b) The same as (a), but the posterior samples are reweighted by the POWERLAW PEAK with the half-Gaussian mass ratio model (Equation (2)) described in Section 2.2. (c) The same as (a), but the posterior samples are reweighed by POWERLAW PEAK with the m 1-dependent mass ratio model of Equation (6) described in Section 2.2. (d) The same as (a), but the posterior samples are reweighted by the POWERLAW PEAK with the m 1-dependent mass ratio model of Equation (7) described in Section 2.2.
Paper: Divergence in Mass Ratio Distributions between Low-mass and High-mass Coalescing Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Yuan-Zhu Wang, 远瞩 王, Shao-Peng Tang, 少 鹏 唐, Qiang Yuan, 强 袁, Yi-Zhong Fan, 一中 范, Da-Ming Wei, 大明 韦
Figure caption: 1σ width of the mass ratio distribution as a function of the primary mass; the shaded regions stand for the 90% credible interval, and the solid curves are the mean values. (a) and (b) are the results obtained using Model II with σ knot = 1.0 and σ knot = 0.5.
Paper: Divergence in Mass Ratio Distributions between Low-mass and High-mass Coalescing Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Yuan-Zhu Wang, 远瞩 王, Shao-Peng Tang, 少 鹏 唐, Qiang Yuan, 强 袁, Yi-Zhong Fan, 一中 范, Da-Ming Wei, 大明 韦
Figure caption: The upper row shows the median (solid) and 90% credible intervals (shaded) of the inferred perturbation functions, f(m 1); the cases for σ knot = 0.2 are not shown here because the f(m 1) is nearly flat. The lower row shows the posterior distribution of f(m 1) as sliced at the three most apparent inferred perturbations in the posterior, which roughly lie at ∼9 M ⊙ (left column), ∼13 M ⊙ (middle column), and ∼25 M ⊙ (right column).
Paper: Divergence in Mass Ratio Distributions between Low-mass and High-mass Coalescing Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Yuan-Zhu Wang, 远瞩 王, Shao-Peng Tang, 少 鹏 唐, Qiang Yuan, 强 袁, Yi-Zhong Fan, 一中 范, Da-Ming Wei, 大明 韦
Figure caption: (a) Posterior distributions of ﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{low}}﹩ (﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{high}}﹩) that describe the mass ratio distribution of BBHs in the lower (higher) mass ranges, and the split point m cut obtained by Model I. (b) Posterior distributions of ﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{low}}-{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{high}}﹩; when we change the primary mass distribution model, the value is still confidently positive, but the credibility becomes lower in the absence of GW190412.
Paper: Divergence in Mass Ratio Distributions between Low-mass and High-mass Coalescing Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Yuan-Zhu Wang, 远瞩 王, Shao-Peng Tang, 少 鹏 唐, Qiang Yuan, 强 袁, Yi-Zhong Fan, 一中 范, Da-Ming Wei, 大明 韦
Figure caption: (a) Posterior distributions of ﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{PL}}﹩ (﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{{\rm{G}}}﹩) that describe the mass ratio distribution of BBHs in the power-law (Gaussian) component obtained by Model III. (b) Posterior distributions of ﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{PL}}-{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{{\rm{G}}}﹩. When we exclude the GW190412, ﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{PL}}﹩ shifts to a smaller value, but the value of ﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{PL}}-{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{{\rm{G}}}﹩ is still confidently positive.
Paper: Divergence in Mass Ratio Distributions between Low-mass and High-mass Coalescing Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Yuan-Zhu Wang, 远瞩 王, Shao-Peng Tang, 少 鹏 唐, Qiang Yuan, 强 袁, Yi-Zhong Fan, 一中 范, Da-Ming Wei, 大明 韦
Figure caption: (a) Posterior distributions of ﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{low}}﹩ (﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{high}}﹩) that describe the mass ratio distribution of BBHs in the lower (higher) mass ranges, and the split point m cut obtained by the Extended Model I. (b) Posterior distributions of ﹩{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{low}}-{\mathrm{log}}_{10}{\sigma }_{{\rm{q}}}^{\mathrm{high}}﹩.
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Magnetic Structure and Plasma Thermodynamics
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Physical quantities related to the flux rope. (a) Overview of the magnetic field lines at t = 794.03 s. The green and purple field lines show the same flux rope as that in Figure 3(d) but from another perspective, while the field lines within the current shell are plotted in red and indicated by the white arrow. We select a slice (the transparent one in the image) to show the main physical parameters in the following panels. (b) Distribution of current density on the selected slice at the same time as in (a). The black arrow indicates the current sheet below the flux rope, and the white arrow marks the current shell. (c) Distribution of resistive dissipation on the selected slice at 794.03 s. (d) Distribution of viscous dissipation on the selected slice at 794.03 s. (e) A highlight of field lines corresponding to the arcades concave upward (pink arrow) and postflare loops (yellow arrow) formed after reconnection. (f) Distribution of plasma velocity on the selected slice at the same time as in (e), showing the high-speed bidirectional outflows (orange arrows) at both ends of the current sheet and the chromospheric evaporation (green arrows) in the postflare loops. The 3D visualization is produced by VAPOR.
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Magnetic Structure and Plasma Thermodynamics
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Evolution of the magnetic flux rope before and during the eruption. (a) Coronal magnetic field configuration at t 0: a magnetic flux rope (purple arrow), two groups of low-lying arcades (yellow arrows) on both sides of the flux rope, and a group of large-scale overlying arcades (orange arrow) above. The colors of the field lines indicate the temperature of the local plasma, with the color bar shown at the bottom-right corner. The red, green, and blue arrows refer to the x-, y-, and z-axes in the simulation, respectively. (b)–(d) Magnetic field of the flux rope at different time instants. The white circle in (c) marks the position of flux transfer at the footpoint during the eruption. The 3D visualization is produced by VAPOR (Li et al. 2019).
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Magnetic Structure and Plasma Thermodynamics
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Distribution of plasma parameters at two time instants of t = 608.06 s (top row) and t = 780.81 s (bottom row). Overplotted are selected magnetic field lines characterizing the event (flux rope in purple, low-lying arcades in yellow, and reconnected lines in red). (a) 3D distribution of the EM in the temperature range of 0.03–1 MK (green-colored structure) at t = 608.06 s. (b) Similar to (a) but at t = 780.81 s. (c) 3D distribution of the EM in the temperature range of more than 10 MK (orange-colored structure) at t = 608.06 s. (d) Similar to (c) but at t = 780.81 s. (e) Distribution of plasma density on the selected slice shown in Figure 4(a) at t = 608.06 s. (f) Similar to (e) but at t = 780.81 s. The inset in (f) shows an enlarged view of the density within the postflare loops. (g) Distribution of plasma temperature on the selected slice shown in Figure 4(a) at t = 608.06 s. (h) Similar to (g) but at t = 780.81 s. The inset in (h) shows an enlarged view of the temperature within the postflare loops. The 3D visualization is produced by VAPOR.
Paper: Fermi-LAT Detection of a GeV Afterglow from a Compact Stellar Merger
Authors: Hai-Ming Zhang, Yi-Yun Huang, Jian-He Zheng, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Left panel: light curves of the GeV emission of GRB 211211A measured by Fermi-LAT and the modeling of the multiwavelength afterglow light curves. The red, blue, and green data points represent the GeV, X-ray, and early optical flux of GRB 211211A, respectively. X-ray data are downloaded from the UK Swift Science Data Centre (UKSSDC; Evans et al. 2007, 2009). The optical data are obtained from Rastinejad et al. (2022). The solid lines represent the synchrotron emission at GeV, X-ray, and optical bands, while the dashed line represents the SSC component at the GeV band in our modeling. Right panel: the measured spectrum and modeling of the GeV emission of GRB 211211A during 395–30,780 s. The parameters used in the modeling are E k,iso = 1 × 1053 erg, Γ0 = 100, n = 10−4 cm−3, p = 2.2, ε e = 0.1, ε B = 6 × 10−5, θ j = 1.°0, and η acc = 0.01 (see the text for more details).
Paper: Fermi-LAT Detection of a GeV Afterglow from a Compact Stellar Merger
Authors: Hai-Ming Zhang, Yi-Yun Huang, Jian-He Zheng, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: 3° × 3° TS map of the gamma-ray emission in 0.1–10 GeV measured by Fermi-LAT around GRB 211211A in 395–30,780 s after the BAT trigger. The cyan cross represents 4FGL J1410.4+2820, which is suggested to be associated with a BL Lacertae RX J1410.4+2821 by the Fermi-LAT Collaboration (Abdollahi et al. 2020). The magenta point indicates the best localization of GRB 211211A. The two green lines represent the localization contours of GRB 211211A at 68% and 90% confidence levels, respectively. The red star represents the localization of GRB 211211A by Swift/XRT (D’Ai et al. 2021).
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Magnetic Structure and Plasma Thermodynamics
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Photospheric magnetogram of the simulation at t 0. (a) The magnetogram of the full simulation domain at t 0. The region of interest is marked by the white dotted box. (b) A zoomed-in view of the region of interest shown in panel (a). There are two bipoles that are labeled N1, P1 and N2, P2. The white arrow V1 and the black arrow V2 indicate the two viewing directions for synthesizing the AIA images. Note that the coordinates are relative ones that only measure the size of the region.
Paper: Fermi-LAT Detection of a GeV Afterglow from a Compact Stellar Merger
Authors: Hai-Ming Zhang, Yi-Yun Huang, Jian-He Zheng, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Light curve of 4FGL J1410.4+2820 in 0.1–10 GeV (blue data) in comparison with the GeV flux (red data) from GRB 211211A.
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: Power spectrum of the z = 0.1 Lyα forest in TNG (black lines) and Illustris (red line). The fundamental mode for the simulations is ﹩{k}_{\max }=2\pi /{v}_{\max }=8.8\times {10}^{-4}﹩ s/km for z = 0.1. We overplot the COS data presented in Khaire et al. (2019) in blue. The dashed red line shows Illustris with a rescaled UVB.
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: The various Lyα statistics presented in this paper for the TNG50-1, TNG100-1, and TNG300-1 simulations. The highest-resolution realizations, TNG50-1, TNG100-1, and TNG300-1, include 2 × 21603, 2 × 18203, and 2 × 25003 resolution elements, respectively. The simulation box sizes go as 35, 75, and 205 Mpc h−1 for TNG50-1, TNG100-1, and TNG300-1 respectively.
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: The Lyα statistics for different resolution elements in TNG100. TNG100-1 (black solid line) has 2 × 18203 resolution elements. TNG100-2 (black dashed line) decreases the resolution elements to 2 × 9103. TNG100-3 (dotted black line) decreases the resolution elements to 2 × 4553.
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: The Lyα statistics for different resolution elements in TNG300. TNG300-1 (black solid line) has 2 × 25003 resolution elements. TNG300-2 (black dashed line) decreases the resolution elements to 2 × 12503. TNG300-3 (dotted black line) decreases the resolution elements to 2 × 6253. The box size of TNG300 is 205 Mpc h −1.
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: Flux PDF of the z = 0.1 Lyα forest in TNG (black line) and Illustris (red line). The dashed red line is the UVB correction for Illustris.
Paper: Black Hole to Photosphere: 3D GRMHD Simulations of Collapsars Reveal Wobbling and Hybrid Composition Jets
Authors: Ore Gottlieb, Matthew Liska, Alexander Tchekhovskoy, Omer Bromberg, Aretaios Lalakos, Dimitrios Giannios, Philipp Mösta
Figure caption: Time evolution in the simulation with σ 0 = 15. Panel (a): Accretion onto the BH initially decreases due to the inflation of the cocoon, before plateauing after a few seconds. Panel (b): The jet luminosity, which is calculated as the radial energy flux excluding the rest energy flux, scales proportionally to the mass accretion rate. Panel (c): The jet-launching efficiency, η, remains of order unity at all times, signaling that the system is accreting in the MAD regime. The jet–cocoon outflow unbinds most of the stellar envelope, ejecting ∼90% of the total stellar mass by t ≈ 16 s (panel (d)). As most of the stellar mass becomes unbound early on, the available gas for accretion is limited such that the BH mass M BH increases only by a few percent over the duration of the simulation (panel (e)). The red lines show moving averages of the highly variable quantities.
Paper: Black Hole to Photosphere: 3D GRMHD Simulations of Collapsars Reveal Wobbling and Hybrid Composition Jets
Authors: Ore Gottlieb, Matthew Liska, Alexander Tchekhovskoy, Omer Bromberg, Aretaios Lalakos, Dimitrios Giannios, Philipp Mösta
Figure caption: Top: 3D rendering of the σ 0 = 15 jet in the inner 2 × 109 cm shows a significant tilt of the disk (orange) and jet (red) axis (horizontal) with respect to the rotation axis of the star at 45°. Although the jet is launched at different orientations at different times, it is deflected by the heavy outer cocoon material (blue gray) that engulfs the jet region toward the rotation axis at 45°. Bottom: 3D rendering of the logarithm of jet magnetization shows the deflection of the jet propagation and a drop in the magnetization from σ ∼ 10 to σ ∼ 1. Here, the jet head is located at r = 0.1 R ⋆. Movies showing the full evolution of the disk–jet tilt are available at http://www.oregottlieb.com/collapsar.html.
Paper: Insight-HXMT Discovery of the Highest-energy CRSF from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124
Authors: Ling-Da Kong, Shu Zhang, Shuang-Nan Zhang, Long Ji, Victor Doroshenko, Andrea Santangelo, Yu-Peng Chen, Fang-Jun Lu, Ming-Yu Ge, Peng-Ju Wang, Lian Tao, Jin-Lu Qu, Ti-Pei Li, Cong-Zhan Liu, Jin-Yuan Liao, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui
Figure caption: We combine the observations from November 3 to November 8 in 2017 for the pulse-profile analysis and the phase-resolved spectral analysis. Left panel: pulse profile evolves with energy. The background-subtracted pulse profiles are normalized by the mean count rate. The green dashed line is at 1.0, and the gray dotted line is at 0. Right panel: fitting results of the phase-resolved spectral analysis. The red points show the parameters of the CRSF.
Paper: Insight-HXMT Discovery of the Highest-energy CRSF from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124
Authors: Ling-Da Kong, Shu Zhang, Shuang-Nan Zhang, Long Ji, Victor Doroshenko, Andrea Santangelo, Yu-Peng Chen, Fang-Jun Lu, Ming-Yu Ge, Peng-Ju Wang, Lian Tao, Jin-Lu Qu, Ti-Pei Li, Cong-Zhan Liu, Jin-Yuan Liao, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui
Figure caption: The net flux of LE, ME, and HE is shown in black, red, and green points, respectively. The flux and background are obtained from the phase-resolved spectrum in phase interval 0.8–0.9. The gray line shows the systematic errors of the background flux; for the exposure time of ∼20 ks, we choose the systematic errors of 2.5%, 1.5%, and 1.5% for LE, ME, and HE, respectively, based on the HXMT background models (Liao et al. 2020a; Guo et al. 2020; Liao et al. 2020b). For such a long exposure, the statistical errors of the background flux are completely negligible.
Paper: Insight-HXMT Discovery of the Highest-energy CRSF from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124
Authors: Ling-Da Kong, Shu Zhang, Shuang-Nan Zhang, Long Ji, Victor Doroshenko, Andrea Santangelo, Yu-Peng Chen, Fang-Jun Lu, Ming-Yu Ge, Peng-Ju Wang, Lian Tao, Jin-Lu Qu, Ti-Pei Li, Cong-Zhan Liu, Jin-Yuan Liao, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui
Figure caption: We combine the observations from November 3 to November 8 in 2017 for spectral fittings. Left panel: spectral fitting and residuals of the phase-averaged spectrum. Right panel: spectral fitting and residuals of the spectrum at phase 0.8–0.9.
Paper: Insight-HXMT Discovery of the Highest-energy CRSF from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124
Authors: Ling-Da Kong, Shu Zhang, Shuang-Nan Zhang, Long Ji, Victor Doroshenko, Andrea Santangelo, Yu-Peng Chen, Fang-Jun Lu, Ming-Yu Ge, Peng-Ju Wang, Lian Tao, Jin-Lu Qu, Ti-Pei Li, Cong-Zhan Liu, Jin-Yuan Liao, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui
Figure caption: The two-dimensional (2D) maps describe the evolution of the pulse profile with time; the colors plot the values of the pulse values normalized by (Pulse – PulseMin)/(Average count rate – PulseMin), where PulseMin is the minimum value of the pulse intensity. The pulse profiles are folded from the background-subtracted light curves. The main pulse at phase 0.6–1.0 is above the mean count rate, and the minor peak at phase 0.2–0.4 is close to or lower than the average corresponding to the negative value for 70.0–90.0 keV and 90.0–120.0 keV.
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: Possible correlation between variables. Values are extracted from pixels after smoothing the parameter maps to the same angular resolution and plotted with a bivariate Gaussian kernel density estimate as contours. B0, B1, and B2 are plotted, with the Spearman’s rank correlation coefficient ρ given in red, blue, and yellowish green, respectively, while the correlation coefficient of the entire target is given in black. The pixels where the NH3 (5,5) and (6,6) lines show <5σ emission are blank.
Paper: Are the Magnetic Field Directions of Surrounding Loops a Key Parameter for Confining a Solar Filament Eruption?
Authors: Tao Ding, Jun Zhang, Junchao Hong
Figure caption: Images of Hα and multiband EUV displaying four flattening structures of the filament and an X-type structure with a current sheet. Panels (a) and (b): Hα observations showing the four flattening structures “FS1”–“FS4,” which are underlined by red, yellow, green, and cyan dotted lines, respectively. “P1,” “P2,” and “P3” represent three intersections between FS1 and FS2, between FS2 and FS3, and between FS3 and FS4, separately. “BP” in panel (a) labels a bright point. Panel (c): composite of 171, 193, and 211 Å images exhibiting FS1, FS2, P1, and BP in AIA EUV channels. These specific features including “FS1,” “FS2,” “P1,” and “BP” in panels (a) and (c) are used for the coalignment of NVST and SDO images. Panel (d): a 131Å image displaying the X-type structure with a current sheet.
Paper: Are the Magnetic Field Directions of Surrounding Loops a Key Parameter for Confining a Solar Filament Eruption?
Authors: Tao Ding, Jun Zhang, Junchao Hong
Figure caption: Overview of the erupting filament “F” in the NVST Hα image (panel (a)) and EUV loops “L1”–“L3” in SDO/AIA 171 Å image (panel (b)). The red square in panel (a) outlines the FOV in Figures 2 and 4(a1) and (b1), and the yellow square the FOV in Figures 3 and 5. The red and blue curves in panels (a)–(b) are contours of the SDO/HMI LOS magnetogram (panel (c)) at +30 G and −30 G, respectively. “P,” “N1,” and “N2” in panel (c) represent three magnetic patches in which the footpoints of the filament and the loops are rooted. Magnetic field directions relevant to the filament and the loops are denoted by corresponding arrows on the curves, and the green quadrilateral outlines the projection area in which the filament eruption is involved (panel (c)).
Paper: Jansky Very Large Array Detections of CO(1–0) Emission in H I-absorption-selected Galaxies at z ≳ 2
Authors: B. Kaur, N. Kanekar, M. Rafelski, M. Neeleman, J. X. Prochaska, M. Revalski
Figure caption: The ratio of the CO(3–2) line luminosity to the CO(1–0) line luminosity (r 31), plotted as a function of (A) redshift and (B) SFR surface density, for the H I-selected galaxies of this work (red symbols), BzK galaxies at z ≈ 1.5 (green crosses; Daddi et al. 2015), and main-sequence galaxies at z > 2 (blue pentagons; Riechers et al. 2010; Brisbin et al. 2019; Boogaard et al. 2020; Henríquez-Brocal et al. 2021). The left panel also shows the median r 31 value for submillimeter galaxies at z > 2 (inverted black triangles; Sharon et al. 2016). The dashed horizontal line in both panels indicates r 31 = 1, for thermal excitation.