adsabs/AstroCLIMB huggingface dataset:
Paper: SLICE: SPT-CL J0546-5345—A Prominent Strong-lensing Cluster at z = 1.07
Authors: Joseph F. V. Allingham, Adi Zitrin, Miriam Golubchik, Lukas J. Furtak, Matthew Bayliss, Catherine Cerny, Jose M. Diego, Alastair C. Edge, Raven Gassis, Michael D. Gladders, Mathilde Jauzac, David J. Lagattuta, Gavin Leroy, Marceau Limousin, Guillaume Mahler, Ashish K. Meena, Priyamvada Natarajan, Keren Sharon
Figure caption: Color-composite image of SPT-CL J0546-5345 constructed from SLICE JWST and archival HST imaging of the cluster (red: F322W2; green: F150W2; blue: F814W). Strong-lensing multiple images are numbered and labeled in green. The yellow, blue, and red lines represent, respectively, the critical curves for source redshifts zs = 3.5 (System 3), zs = 4.5, and zs = 6, as computed from our strong-lensing model of the cluster. Galaxies left freely weighted in the modeling are marked with crosses. Highlighted in cyan squares are the images of System 5, the multiply imaged point-like nucleus—and potential AGN—reported in this work. Note that an artifact from the F150W2 band appears in green north of the cluster core. This is cosmetic only, and we verified that it has no substantial effect on our results (see Section 2.3).
Paper: SLICE: SPT-CL J0546-5345—A Prominent Strong-lensing Cluster at z = 1.07
Authors: Joseph F. V. Allingham, Adi Zitrin, Miriam Golubchik, Lukas J. Furtak, Matthew Bayliss, Catherine Cerny, Jose M. Diego, Alastair C. Edge, Raven Gassis, Michael D. Gladders, Mathilde Jauzac, David J. Lagattuta, Gavin Leroy, Marceau Limousin, Guillaume Mahler, Ashish K. Meena, Priyamvada Natarajan, Keren Sharon
Figure caption: The expected distribution of Einstein radii around zl ∼ 1.07 for a source at zs = 3, across the sky (shaded red), and for the SPT survey region (2500 deg2; shaded green), vs. the Einstein radius of SPT-CL J0546-5345  θE = 18﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 ± 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩8 (vertical blue shaded region), for the same source redshift. The (nominally, 1σ) scatter in the Einstein radius distribution was computed by probing clusters in the range z = 1–1.2 and from the scatter in the adopted c − M relation (for more details, see Section 4.3). As can be seen, clusters with such Einstein radii are expected to be rare at this redshift (see discussion in Section 4.3).
Paper: SLICE: SPT-CL J0546-5345—A Prominent Strong-lensing Cluster at z = 1.07
Authors: Joseph F. V. Allingham, Adi Zitrin, Miriam Golubchik, Lukas J. Furtak, Matthew Bayliss, Catherine Cerny, Jose M. Diego, Alastair C. Edge, Raven Gassis, Michael D. Gladders, Mathilde Jauzac, David J. Lagattuta, Gavin Leroy, Marceau Limousin, Guillaume Mahler, Ashish K. Meena, Priyamvada Natarajan, Keren Sharon
Figure caption: Reproduction of several systems by our model. For each system, we delens one image—typically the first one—to the source plane and back to the image plane, displaying the reproduction of the other images in that system. The upper row, for each system, shows the images as they appear in the red, green, and blue color image of the cluster (Figure 1), and the bottom row shows their reproduction by our model. As can be seen, the model does a very good job in reproducing the appearance of multiple images, strengthening their identification and showcasing its robustness.
Paper: SLICE: SPT-CL J0546-5345—A Prominent Strong-lensing Cluster at z = 1.07
Authors: Joseph F. V. Allingham, Adi Zitrin, Miriam Golubchik, Lukas J. Furtak, Matthew Bayliss, Catherine Cerny, Jose M. Diego, Alastair C. Edge, Raven Gassis, Michael D. Gladders, Mathilde Jauzac, David J. Lagattuta, Gavin Leroy, Marceau Limousin, Guillaume Mahler, Ashish K. Meena, Priyamvada Natarajan, Keren Sharon
Figure caption: Surface mass density map (left), in units of the critical density for lensing, and magnification map (right), both for an assumed source redshift of zs = 3.5, from the best-fit LTM model.
Paper: Two Types of 1/f Range in Solar Wind Turbulence
Authors: Zesen Huang, 泽森 黄, Marco Velli, B. D. G. Chandran, Chen Shi, 辰 时, Yuliang Ding, 宇量 丁, Lorenzo Matteini, Kyung-Eun Choi, 경은 최
Figure caption: Overview of 1/f range in the rectified trace magnetic PSD of solar wind turbulence. (a) Pristine Alfvénic (fast) wind from the perihelion of PSP E19, (b) Alfvénic wind from ±5 days of the E19 perihelion, (c) fast wind from outbound of E19, (d) Helios fast wind, (e) Solar Orbiter fast wind, (f) WIND fast wind, (g) Ulysses polar fast wind, (h) Helios mixed solar wind, (i) OMNI (LRO) mixed solar wind, (j) WIND slow wind. The vertical bars indicate the 1/f ranges, and the error bars show the averaged values (±1σ) of P(f) · f within the 1/f ranges.
Paper: Two Types of 1/f Range in Solar Wind Turbulence
Authors: Zesen Huang, 泽森 黄, Marco Velli, B. D. G. Chandran, Chen Shi, 辰 时, Yuliang Ding, 宇量 丁, Lorenzo Matteini, Kyung-Eun Choi, 경은 최
Figure caption: The 1/f range and magnetic field vector correlation. (a) and (b) are identical to (f) and (g) in Figure 2, respectively. The first six harmonics from Carrington rotation are highlighted with the dashed lines. (c) and (d) show the magnetic field vector autocorrelation as a function of f = 1/dt. Up to six inverses of Carrington rotation periods are highlighted with black dashed lines. The second and sixth harmonics are highlighted with red dashed lines. (e) and (f) show the absolute value of the autocorrelation function.
Paper: Two Types of 1/f Range in Solar Wind Turbulence
Authors: Zesen Huang, 泽森 黄, Marco Velli, B. D. G. Chandran, Chen Shi, 辰 时, Yuliang Ding, 宇量 丁, Lorenzo Matteini, Kyung-Eun Choi, 경은 최
Figure caption: Example interval from PSP E19 perihelion. (a) Trajectory of PSP in the Carrington corotating frame. Black dots are plotted every 8 hr. The green dot indicates the entering direction of the spacecraft. The interval is highlighted with the cyan bar. The radial dotted lines are plotted every 5° longitude. The dashed circles are plotted every 10 R⊙. (b) Trace magnetic PSD of the interval. (c) R-T-N components and magnitude of the magnetic field. (d) Trace magnetic wavelet spectrogram. (e) Radial solar wind speed from SPAN-ion Vr,SPAN and local Alfvén speed VA estimated from quasi-thermal-noise (QTN). (f) 1 minute rolling averaged cross-helicity σc (left) and proton plasma β (right). (g) Electron number density from QTN. (h) Solar wind advection time tadv = (R − R⊙)/Vr (left) and heliocentric distance (right).
Paper: Two Types of 1/f Range in Solar Wind Turbulence
Authors: Zesen Huang, 泽森 黄, Marco Velli, B. D. G. Chandran, Chen Shi, 辰 时, Yuliang Ding, 宇量 丁, Lorenzo Matteini, Kyung-Eun Choi, 경은 최
Figure caption: Left: radial dependence of P(f) · f for (a)–(g). The circles are averaged values of P(f) · f within the 1/f range, highlighted with vertical bars in Figure 3. The squares are values of P(f) · f at f = 10−1.5 Hz. For all intervals, 10−1.5 Hz is located deep within the inertial range. Right: the radial evolution of the frequencies of the 1/f range. The horizontal error bars indicate the heliocentric distance range of the intervals.
Paper: Two Types of 1/f Range in Solar Wind Turbulence
Authors: Zesen Huang, 泽森 黄, Marco Velli, B. D. G. Chandran, Chen Shi, 辰 时, Yuliang Ding, 宇量 丁, Lorenzo Matteini, Kyung-Eun Choi, 경은 최
Figure caption: Time dependence of the OMNI (LRO) trace magnetic PSD over solar cycles 22, 23, 24, and 25. Each line represents 2 yr worth of data. (a) Sunspot number from 1985 January to 2025 March, where each of the selected time ranges are highlighted with the corresponding colors. (b) Solar maximum. (c) Solar minimum. Dashed–dotted line: Carrington rotation. Dotted line: half-cycle Carrington rotation.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: The 2D histograms and radial profiles of O6+ (top left) differential flow normalized to the local Alfvén speed × ﹩\cos {\rm{\Theta }}﹩, (top right) differential streaming, (bottom left) scalar temperature ratio with protons, and (bottom right) temperature, all plotted against heliocentric distance from the Sun in au. The bottom right plot has a log-log scale, while the others are in linear scale. The background histograms are a distributions of counts in this parameter space that are column-normalized. The radial profiles have been binned by proton speed, where the mean is reported in the legend; see Section 3 for bin ranges. In the top and bottom left plots, we include observations of O6+ from L. Berger et al. (2011) and P. J. Tracy et al. (2016) as well as a prediction from J. Holmes et al. (2024).
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: The 2D histograms of differential streaming of O6+ normalized to the local Alfvén speed vs. angle between the radial direction and the local magnetic field, which we refer to as a “moth plot.” The left panel shows the distribution of all measurements taken, while the right panel shows the average temperature ratios (TO6+/Tp) within the parameter space for bins that contain at least five points. We overplot (solid lines) Equation (2) for different ΔU/VA for reference with amplitudes of ±1.3, 0.87, 0.43, and 0.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: Negative differential streaming periods due to an Alfvénic fluctuation. The top row shows three panels of 2D histograms with the radial component of the magnetic field, VO6+, and δB/B values across an individual Alfvénic fluctuation period highlighted in the shaded region shown in the time series below. In the time series plots, the top panel shows differential streaming in gray in association with the left vertical axis and the radial magnetic field, BR (where red is for positive and blue is for negative polarity), and magnitude, B, in black. The middle panel shows the proton (black) and O6+ (green) speed magnitude along with the proton + Alfvén speed (red). The bottom panel shows the proton and O6+ individual temperatures (right vertical axis; black and green, respectively) along with their ratio divided by 16 (gray), associated with the left axis, to show mass proportionality. The cartoon figure on the bottom right is adapted from M. D. McManus et al. (2022) for the case in this example; see details in the text.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: Same as Figure 4 but for a different case.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: High charge states of oxygen in the inner heliosphere: O6+ temperature and speed vs. heliocentric distance to the Sun between 0 and 1 au. The plots include observations from UVCS of O5+ in a polar coronal hole from S. R. Cranmer et al. (2008) and a streamer from L. Abbo et al. (2010, 2016), whose ranges are indicated by the red and green regions, respectively, extending between approximately the solar surface and 0.0186 au (1−4 R⊙). We also include the coverage of Parker between ∼9.86 and 155 R⊙.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: Moth plots of counts for differential streaming of O6+ normalized to the local Alfvén speed vs. angle between the flow direction and the local magnetic field, same as Figure B2.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: The orbital path of Solar Orbiter over the time frame covered in the analysis in this paper is plotted in dark green. The light green periods along the trajectory are locations where the HIS Level 3 data were available. The magenta markers and corresponding dates indicate perihelia.
Paper: Detection of Low-redshift Excess in Supernova-linked Gamma-Ray Bursts
Authors: Qin-Mei Li, Qi-Bin Sun, Sheng-Bang Qian, Fu-Xing Li
Figure caption: Distributions and correlations for the SN/GRBs sample: (a) duration (T90) distribution of SN/GRBs events; (b) bolometric luminosity distribution where individual points represent different SN/GRBs, with the line indicating the sensitivity limit of 1.0 × 10−8 erg cm−2 s−1; (c) in the Kendall τ correlation test, the red dotted line represents the null hypothesis (τ = 0), and the measured correlation strength of k = 4.64 suggests that the evolutionary dependence between luminosity and redshift has been effectively removed; (d) de-evolved luminosity function following L = L0(1 + z)4.64 for our sample of 56 SN/GRBs, removing the redshift evolution component.
Paper: An Upper Limit of 106 M⊙ in Dust from ALMA Observations in 60 Little Red Dots
Authors: Caitlin M. Casey, Hollis B. Akins, Steven L. Finkelstein, Maximilien Franco, Seiji Fujimoto, Daizhong Liu, Arianna S. Long, Georgios Magdis, Sinclaire M. Manning, Jed McKinney, Marko Shuntov, Takumi S. Tanaka
Figure caption: Our measured constraints on the stack of 60 LRDs (gold star) compared to other literature limits of dust emission around LRDs. The top panel plots the SED constraints in νLν and the bottom panel in observed flux density. Other limits from the literature are shown in dark teal (I. Labbe et al. 2023), light green (H. B. Akins et al. 2024), blue (M. Xiao et al. 2025), and purple (D. J. Setton et al. 2025). The M. Xiao et al. (2025) and D. J. Setton et al. (2025) limits are set for two different LRDs each: light blue represents ID9094 at z = 7.0388, dark blue is ID2756 at z = 7.1883, light purple is RUBIES-BLAGN-1 at z = 3.1034, and dark purple is A2744-45924 at z = 4.4655. Because these limits are all for unusually bright LRDs, we have scaled their limits down by a factor of 3, 10, 10, and 10 (respectively) to draw a more direct comparison to the LRDs targeted in our program. Two optical through radio SEDs are shown: the maximal SED from H. B. Akins et al. (2024), showing the maximum allowable dust SED around LRDs given the limits available (black), and the predicted LRD dust SED from C. M. Casey et al. (2024) in red. In the bottom panel we overplot simple modified blackbody SEDs with temperatures of 30 and 1500 K for comparison. Our new limit for this aggregate sample is fully in line with the predicted low-luminosity dust emission.
Paper: An Upper Limit of 106 M⊙ in Dust from ALMA Observations in 60 Little Red Dots
Authors: Caitlin M. Casey, Hollis B. Akins, Steven L. Finkelstein, Maximilien Franco, Seiji Fujimoto, Daizhong Liu, Arianna S. Long, Georgios Magdis, Sinclaire M. Manning, Jed McKinney, Marko Shuntov, Takumi S. Tanaka
Figure caption: Limits we place on dust mass and IR luminosity based on our measurements as a function of dust temperature. The rms per source ranges from 21 to 23 μJy at 1.3 mm, translating to a 3σ upper limit of 66 μJy; this sets an upper limit to the dust mass and IR luminosity of LRDs traced out by the red curves. We show the redshift dependence of this limit in different shades of red, from lightest (z ∼ 5) to darkest (z ∼ 8). The limited flux density for the stack, of 10.8 μJy at 3σ, is traced out by the blue line at the median redshift of the sample. We also show the measured limits to IR luminosity as a function of dust temperature from D. J. Setton et al. (2025), derived from detailed ALMA and JWST/MIRI constraints on two very luminous LRDs (in green). Despite uncertainty in the underlying dust temperature of the dust around LRDs, we place representative upper limits from these data of <107 M⊙ and <1012 L⊙ on individual sources and <106 M⊙ and <1011 L⊙ on the nondetection from the stack.
Paper: An Upper Limit of 106 M⊙ in Dust from ALMA Observations in 60 Little Red Dots
Authors: Caitlin M. Casey, Hollis B. Akins, Steven L. Finkelstein, Maximilien Franco, Seiji Fujimoto, Daizhong Liu, Arianna S. Long, Georgios Magdis, Sinclaire M. Manning, Jed McKinney, Marko Shuntov, Takumi S. Tanaka
Figure caption: JWST 5″ × 5″ tricolor cutouts (F150W, F277W, F444W) of our LRD sample overlaid with ALMA dust continuum contours. Blue contours denote positive SNR (integer multiples of σ beginning at 2σ) and red contours denote negative SNR (integer multiples of σ descending from −2σ). None of the 60 LRDs in this program were detected with 1σ rms in the range 21–23 μJy.
Paper: EP241021a: A Months-duration X-Ray Transient with Luminous Optical and Radio Emission
Authors: Xinwen Shu, Lei Yang, Haonan Yang, Fan Xu, Jin-Hong Chen, Rob A. J. Eyles-Ferris, Lixin Dai, Yunwei Yu, Rong-Feng Shen, Luming Sun, Hucheng Ding, WeiKang Zheng, Ning Jiang, Wenxiong Li, Ning-Chen Sun, Dong Xu, Zhumao Zhang, Chichuan Jin, Arne Rau, Tinggui Wang, Xue-feng Wu, Weimin Yuan, Bing Zhang, Kirpal Nandra, Alexei V. Filippenko, Frédérick Poidevin, Roberto Soria, Amit Kumar, David S. Aguado, Fangxia An, Tao An, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pietro Baldini, Thomas G. Brink, Pathompong Butpan, Zhiming Cai, Alberto J. Castro-Tirado, Huaqing Cheng, Weiwei Cui, Joseph Farah, Shaoyu Fu, Johan P.U. Fynbo, Xing Gao, Dawei Han, Xuhui Han, D. Andrew Howell, Jingwei Hu, Shuaiqing Jiang, Brajesh Kumar, Weihua Lei, Dongyue Li, Chengkui Li, Huaqiu Liu, Xing Liu, Yuan Liu, Xiaowei Liu, Alicia López-Oramas, David López Fernández-Nespral, Justyn R. Maund, Curtis McCully, Zexi Niu, Megan Newsome, Paul O'Brien, Haiwu Pan, Yu Pan, Estefania Padilla Gonzalez, Ismael Pérez-Fournon, Walter Silima, Hui Sun, Shengli Sun, Xiaojin Sun, Giacomo Terreran, Samaporn Tinyanont, Junxian Wang, Yanan Wang, Yun Wang, Klaas Wiersema, Yunfei Xu, Yongquan Xue, Yi Yang, Fabao Zhang, Juan Zhang, Pinpin Zhang, Wenda Zhang, Yonghe Zhang, Haisheng Zhao, Zipei Zhu, Liping Xin, Zhuheng Yao, Bertrand Cordier, Jianyan Wei, Yulei Qiu, Frédéric Daigne
Figure caption: Isotropic luminosity of repeating TDEs resulting from a relativistic jet and the X-ray luminosity in the 0.3–10 keV band. Circular markers denote EP observations, while diamond markers represent XMM-Newton data. Open markers indicate 3σ upper limits. The blue, green, and red dashed lines show the isotropic light curves of the first, second, and third TDEs, respectively. The total light curve (sum of three events; Equation (5)) is illustrated by the solid black line. The solid gray line represents the mass-fallback rate ﹩{\dot{M}}_{{\rm{fb}}}﹩. The horizontal gray line indicates the critical value of ﹩{\dot{M}}_{{\rm{cr}}}﹩, marking the transition from a super-Eddington to a sub-Eddington accretion state. The two vertical dashed lines denote the rebrightening time, and the dotted gray line indicates the time at which the jet shuts off.
Paper: EP241021a: A Months-duration X-Ray Transient with Luminous Optical and Radio Emission
Authors: Xinwen Shu, Lei Yang, Haonan Yang, Fan Xu, Jin-Hong Chen, Rob A. J. Eyles-Ferris, Lixin Dai, Yunwei Yu, Rong-Feng Shen, Luming Sun, Hucheng Ding, WeiKang Zheng, Ning Jiang, Wenxiong Li, Ning-Chen Sun, Dong Xu, Zhumao Zhang, Chichuan Jin, Arne Rau, Tinggui Wang, Xue-feng Wu, Weimin Yuan, Bing Zhang, Kirpal Nandra, Alexei V. Filippenko, Frédérick Poidevin, Roberto Soria, Amit Kumar, David S. Aguado, Fangxia An, Tao An, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pietro Baldini, Thomas G. Brink, Pathompong Butpan, Zhiming Cai, Alberto J. Castro-Tirado, Huaqing Cheng, Weiwei Cui, Joseph Farah, Shaoyu Fu, Johan P.U. Fynbo, Xing Gao, Dawei Han, Xuhui Han, D. Andrew Howell, Jingwei Hu, Shuaiqing Jiang, Brajesh Kumar, Weihua Lei, Dongyue Li, Chengkui Li, Huaqiu Liu, Xing Liu, Yuan Liu, Xiaowei Liu, Alicia López-Oramas, David López Fernández-Nespral, Justyn R. Maund, Curtis McCully, Zexi Niu, Megan Newsome, Paul O'Brien, Haiwu Pan, Yu Pan, Estefania Padilla Gonzalez, Ismael Pérez-Fournon, Walter Silima, Hui Sun, Shengli Sun, Xiaojin Sun, Giacomo Terreran, Samaporn Tinyanont, Junxian Wang, Yanan Wang, Yun Wang, Klaas Wiersema, Yunfei Xu, Yongquan Xue, Yi Yang, Fabao Zhang, Juan Zhang, Pinpin Zhang, Wenda Zhang, Yonghe Zhang, Haisheng Zhao, Zipei Zhu, Liping Xin, Zhuheng Yao, Bertrand Cordier, Jianyan Wei, Yulei Qiu, Frédéric Daigne
Figure caption: Left: observed multiwavelength afterglow of EP241021a and best-fit results from the three-jet model (solid curves). Shaded regions exhibit the 1σ confidence intervals of the model light curves derived from posterior distributions of model parameters. Both optical and radio light curves are well explained by this model, while the X-ray emission is underpredicted. A possible solution to this inconsistency is the inclusion of a jetted TDE (see Section 4.4). Right: the evolution of the kinetic energy, radius, and Lorentz factor for the three jets. The first, second, and third jets are represented by the blue, orange, and green curves, respectively.