adsabs/AstroCLIMB huggingface dataset:
Paper: Decoding Long-duration Gravitational Waves from Binary Neutron Stars with Machine Learning: Parameter Estimation and Equations of State
Authors: Qian Hu, Jessica Irwin, Qi Sun, Christopher Messenger, Lami Suleiman, Ik Siong Heng, John Veitch
Figure caption: Structure of our flow-based BNS analysis pipeline. The normalizing flows learn transformations between a Gaussian distribution and the target posterior distribution. The first flow is conditioned on the preprocessed (via multibanding and heterodyning) and compressed (by a neural network) GW strain data and generates a source PE, which then conditions the second flow to generate a reduced representation of the NS EOS. The reduced representation and original EOS can be transformed into each other by an neural autoencoder.
Paper: Colors and Dynamics of a Near-Sun Orbital Asteroid Family: 2021 PH27 and 2025 GN1
Authors: Scott S. Sheppard, Henry H. Hsieh, Petr Pokorný, David J. Tholen, Audrey Thirouin, Carlos Contreras, Marcelo D. Mora, Mauricio Martinez, Ivonne Toro
Figure caption: Sloan optical colors of low-perihelion asteroids (q < 0.15 au). 2021 PH27 is shown by the red filled circle and 2025 GN1 by the green filled triangle. Other low-perihelion asteroids are from D. Jewitt (2013) and C. Holt et al. (2022) and shown by blue squares (uncertainties have been removed for clarity, but are generally 0.05–0.1 mag or better). The color of the Sun is denoted by a black star, and the very blue Phaethon is labeled. The general range for the colors of the C-type, S-type, X-type, and V-type asteroids is shown by their first letter and range bars, according to A. Parker et al. (2008) and A. Sergeyev & B. Carry (2021). The z’-band allows the silicate feature to be probed as a turn over in the color, which is signified by a significant negative i’ − z’ color and the V-type asteroids, according to A. Parker et al. (2008) and A. Sergeyev & B. Carry (2021). Several of the low-perihelion objects appear to have silicate features, though 2021 PH27 does not. 2021 PH27 and 2025 GN1 appear to have optical colors near the X-type asteroids, which are between the main C-type and S-type classes.
Paper: Colors and Dynamics of a Near-Sun Orbital Asteroid Family: 2021 PH27 and 2025 GN1
Authors: Scott S. Sheppard, Henry H. Hsieh, Petr Pokorný, David J. Tholen, Audrey Thirouin, Carlos Contreras, Marcelo D. Mora, Mauricio Martinez, Ivonne Toro
Figure caption: Numerical orbital simulations of 2021 PH27 (blue) and 2025 GN1 (yellow) and their clones over 30 kyr starting 20 kyr in the past. Bold middle color lines show the median orbital parameters and the thin color lines the 1σ median value of each orbital element. 2021 PH27 experiences a very close encounter with Venus that is within 10 s of Venus radii in about 1150 yr. 2025 GN1 experiences a very close encounter with Venus in about 2300 yr, with some clones even hitting Venus. The orbits of the two objects significantly diverge at these Venus encounters. Backward orbital numerical integrations show 2021 PH27 had another close encounter with Venus about −11,620 yr ago, while 2025 GN1 may have encountered Venus around −11,000 yr ago. These frequent encounters within the Hill sphere of Venus significantly alter the orbits of these objects and suggest that the 2021 PH27 and 2025 GN1 pair was created around the last Venus encounter some 11 kyr ago or within the last several kiloyears afterwards in order to still have such similar orbits that we see today.
Paper: On the Formation of S stars from a Recent Massive Black Hole Merger in the Galactic Center
Authors: Tatsuya Akiba, Smadar Naoz, Ann-Marie Madigan
Figure caption: (Top) Kick magnitude as a function of the mass ratio, q, according to the analytical prescription of C. O. Lousto et al. (2010, 2012). The light purple region shows 106 Monte Carlo evaluations assuming a random spin distribution for each black hole, where the spin direction is drawn from an isotropic distribution and the spin magnitude is drawn from a uniform distribution between 0 and 1 in magnitude for both of the premerger black holes. The thick purple line shows the average kick magnitude dependence obtained from the 106 trials. (Bottom) Alignment of the eccentricity vector, ﹩|\langle {\boldsymbol{e}}\rangle |﹩, in the range a = 0.04–0.5 pc as a function of the mass ratio, q, of the black holes assuming the average result from the top panel. e0 corresponds to the prekick eccentricities in the stellar disk. m1 and M2 are the masses of the less massive and more MBH, respectively. The dotted black line corresponds to our fiducial model run of e = 0.3 corresponding to a recoil kick of vkick ≈ 60 km s−1 in both panels.
Paper: On the Formation of S stars from a Recent Massive Black Hole Merger in the Galactic Center
Authors: Tatsuya Akiba, Smadar Naoz, Ann-Marie Madigan
Figure caption: (Top) Timescales of relevant physical processes: general relativistic precession, two-body relaxation, resonant relaxation, and the EKL mechanism (see S. Naoz 2016 for a review) for our simulations as a function of semimajor axis. The black crosses show the numerically estimated precession timescales. (Bottom) The corresponding relative changes to angular momentum for the same processes, an alternative comparison method suggested by S. Naoz et al. (2022; see also D. Melchor et al. 2024). The line styles are the same in both panels. The EKL quadrupole timescale matches the numerically estimated precession timescales quite well and is the most dominant driver of secular torques in our simulations. The general relativistic precession timescale is longer than the simulation time and is thus neglected in our current work. From the bottom panel, one can see that all relaxation processes are relevant within a simulation time.
Paper: On the Formation of S stars from a Recent Massive Black Hole Merger in the Galactic Center
Authors: Tatsuya Akiba, Smadar Naoz, Ann-Marie Madigan
Figure caption: A schematic diagram illustrating the proposed process for forming the Galactic center structure within the central 0.5 pc. (1) An MBH falls toward Sgr A* with accompanying (A) gas, (B) young stars, or a combination of both. (2) The black holes inspiral and merge. (3) The merger remnant receives a gravitational recoil kick. (4) The kick induces an eccentric, apse-aligned disk of stars or gas (from which stars can form). (5) Stars near the inner edge of the eccentric disk undergo EKL oscillations caused by the asymmetric gravitational potential of the eccentric disk. The inner stars are driven to high eccentricities and inclinations. (6) The S stars and the surrounding disk are produced within a few Myr of the merger.
Paper: On the Formation of S stars from a Recent Massive Black Hole Merger in the Galactic Center
Authors: Tatsuya Akiba, Smadar Naoz, Ann-Marie Madigan
Figure caption: Orbits zoomed in from ≈0.5 pc to ≈0.02 pc at (left) t = 0 and (right) t = 2 Myr for our fiducial model simulation: e = 0.3, σi = 3∘. We emphasize orbits with i > 30∘ in magenta, while low-inclination orbits are plotted in teal. After 2 Myr, the initially unoccupied region of a < 0.04 pc is populated with high-inclination, high-eccentricity orbits reminiscent of the S stars. At length scales > 0.1 pc, orbits remain in a coherent disk with low inclinations while apsidal alignment is damped.
Paper: New Clues on the Extended He II Ionization in IZw18 from GTC/MEGARA and JWST/MIRI
Authors: A. Arroyo-Polonio, C. Kehrig, J. M. Vílchez, J. Iglesias-Páramo, E. Pérez-Montero, S. Duarte Puertas, J. Gallego, D. Reverte
Figure caption: Maps of the flux (left), radial velocity (middle), and radial velocity dispersion (right) of the selected emission lines: Hβ (top) and He IIλ4686 (bottom). The isocontours overplotted in all panels (except for the top-left one) represent the Hβ flux for reference. The white bar shown in the top-left panel represents 1″ (i.e., ∼88 pc), which is the FWHM of the Gaussian kernel used to smooth the data. Black spaxels represent those that do not follow our criterion (S/N > 3 and σ > σins). In all figures in the Letter, north is up and east is to the left.
Paper: New Clues on the Extended He II Ionization in IZw18 from GTC/MEGARA and JWST/MIRI
Authors: A. Arroyo-Polonio, C. Kehrig, J. M. Vílchez, J. Iglesias-Páramo, E. Pérez-Montero, S. Duarte Puertas, J. Gallego, D. Reverte
Figure caption: (Left panel) The MEGARA Hβ emission map as a color-filled contour plot, smoothed using bilinear interpolation. For reference, the isocontours of the MEGARA He IIλ4686 and the MIRI [Ne V]14.32 μm emissions are overplotted in white and black, respectively. (Right panel) Color-composite image in three bandpasses: near-infrared JWST NIRCam/F115W continuum at ∼1.15 μm (red), optical HST Advanced Camera for Surveys F606W continuum at ∼6060 Å (green), and HST WFC3/UVIS/F225W at ∼2250 Å (blue); the same isocontours of He IIλ4686 and [Ne V]14.32 μm line emissions are displayed.
Paper: New Clues on the Extended He II Ionization in IZw18 from GTC/MEGARA and JWST/MIRI
Authors: A. Arroyo-Polonio, C. Kehrig, J. M. Vílchez, J. Iglesias-Páramo, E. Pérez-Montero, S. Duarte Puertas, J. Gallego, D. Reverte
Figure caption: (Left panel) The MIRI Huα emission map. For reference, the isocontours of the MEGARA Hβ emission are overplotted in white. (Right panel) The MIRI [Ne V]14.32 μm emission map. Again, for reference, the isocontours of the MEGARA Hβ emission are overplotted in white.
Paper: New Clues on the Extended He II Ionization in IZw18 from GTC/MEGARA and JWST/MIRI
Authors: A. Arroyo-Polonio, C. Kehrig, J. M. Vílchez, J. Iglesias-Páramo, E. Pérez-Montero, S. Duarte Puertas, J. Gallego, D. Reverte
Figure caption: Line profiles of Hβ (in red) and He IIλ4686 (in blue). In the upper part, solid lines represent the observed line profiles and dashed lines the best Gaussian fit of each line. Vertical dotted lines represent the centroid of each Gaussian. Vertical solid lines represent the centers of mass of each profile. In the bottom part, the residuals (observation—Gaussian fit) are represented. The flux of each line is normalized to its peak value.
Paper: Gas-poor Hosts and Gas-rich Companions of z ≈ 3.5 Radio Active Galactic Nuclei: ALMA Insights into Jet Triggering and Feedback
Authors: Wuji Wang, 无忌 王, Carlos De Breuck, Dominika Wylezalek, Matthew D. Lehnert, Andreas L. Faisst, Andrey Vayner, Nicole Nesvadba, Joël Vernet, Pranav Kukreti, Daniel Stern
Figure caption: On the left we show [C II] moment 0 maps, while on the right we present spectra of the companions around TN J0121+1320. (a) Contours of [C II] moment 0 maps integrated from velocity channels of each line emission as indicated at the bottom right. The contours are shown in [3, 4, 5, ...]σ levels (for [C II]-B, only odd levels are shown for better visualization). The grayscale image is [O III]λ5007 surface brightness integrated from three wavelength channels around Δv = 0 km s−1. The color dotted ellipses mark the apertures where the [C II] spectra in panel (b) are extracted. The purple star marks the position of the radio core. The ALMA Band 8 synthesized beam and representative NIRSpec IFU point-spread function are given at the bottom left corner. The Very Large Array X-band radio map with a synthesized beam size of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩24 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩24 is shown in dark green contours. (b) Spectra showing [C II] emission at the position of the companions. The dark magenta lines show the best single Gaussian fits to the [C II] emission. Black histograms are normalized [O III]λ5007 spectra extracted from the same apertures as the [C II] spectra. We note that J0121-[C II]-A is outside the NIRSpec IFU field of view. Red histograms with gray shades are [C I] spectra at the same positions as the [C II] emitters but from an aperture the size of the Band 3 beam size, θ100 GHz = 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩98 × 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩47 (green ellipse). We show the single Gaussian fits to the [C I] lines in the red dashed curve. In the zoom-in panel, [−600, 600] km s−1, we compare the [C I] spectrum extracted at radio core to [C I] at J0121-[C II]-B.
Paper: Gas-poor Hosts and Gas-rich Companions of z ≈ 3.5 Radio Active Galactic Nuclei: ALMA Insights into Jet Triggering and Feedback
Authors: Wuji Wang, 无忌 王, Carlos De Breuck, Dominika Wylezalek, Matthew D. Lehnert, Andreas L. Faisst, Andrey Vayner, Nicole Nesvadba, Joël Vernet, Pranav Kukreti, Daniel Stern
Figure caption: Similar to Figure 1, [C II] moment 0 map and spectra of companions of 4C+03.24. (a) The dotted green contours are the optical continuum emissions detected by NIRSpec IFU. The light blue triangle marks the position of the [O III] companion, 4C03-[O III] (W. Wang et al. 2025), where the spectrum in Figure 5 is extracted. The Very Large Array Ku-band radio map with a synthesized beam size of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩24 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩24 is shown in dark green. (b) The vertical red dotted line indicates the velocity shift of [C I] detection reported in S. Kolwa et al. (2023), Δ[C I],K23 =1123 km s−1, with respect to zsys = 3.5657. [C I] spectra are extracted at the same positions as the [C II] companions from an aperture with the size of one Band 3 beam, θ100 GHz = 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩23 × 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩62 (green ellipse).
Paper: Gas-poor Hosts and Gas-rich Companions of z ≈ 3.5 Radio Active Galactic Nuclei: ALMA Insights into Jet Triggering and Feedback
Authors: Wuji Wang, 无忌 王, Carlos De Breuck, Dominika Wylezalek, Matthew D. Lehnert, Andreas L. Faisst, Andrey Vayner, Nicole Nesvadba, Joël Vernet, Pranav Kukreti, Daniel Stern
Figure caption: Similar to Figure 1, [C II] moment 0 maps and spectra of the companions of TN J0205+2242 (a, b) and 4C+19.71 (c, d). Very Large Array X-band (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩20 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩20) and C-band (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩25 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩24) radio maps are shown for TN J0205+2242 and 4C+19.71, respectively. The vertical dashed black line in panel (d) marks Δv[O III] = 268 km s−1 (z[O III] = 3.5933, which might be the systemic redshift of the radio AGN, see Section 3). The horizontal black bar indicates the 250 km s−1 range where the L[C II] upper limit at the radio core is integrated. For TN J0205+2242, the [C I] spectrum is extracted from an aperture the size of one Band 3 beam, θ100 GHz = 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩28 × 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩81 (green ellipse), and is further binned by a factor of 4, i.e., 56 km s−1 per channel. For 4C+19.71, its [C I] spectrum is extracted from an aperture the size of one Band 3 beam, θ100 GHz = 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩98 × 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩81 (green ellipse). Only the radio core of 4C+19.71 is shown where the lobes are outside the field of view (W. Wang et al. 2024).
Paper: Gas-poor Hosts and Gas-rich Companions of z ≈ 3.5 Radio Active Galactic Nuclei: ALMA Insights into Jet Triggering and Feedback
Authors: Wuji Wang, 无忌 王, Carlos De Breuck, Dominika Wylezalek, Matthew D. Lehnert, Andreas L. Faisst, Andrey Vayner, Nicole Nesvadba, Joël Vernet, Pranav Kukreti, Daniel Stern
Figure caption: Sample properties and comparison: (a) L[C II] vs. ﹩{M}_{{{\rm{H}}}_{2},[{\rm{C}}\,{\rm\small{I}}]}﹩, (b) LIR vs. L[C II]/LIR, and (c) M⋆ vs. SFR. In panel (a), we show the ﹩{M}_{\,{{\rm{H}}}_{2}}-{L}_{[{\rm{C}}\,{\rm\small{II}}]}﹩ relation with uncertainties (A. Zanella et al. 2018). For comparison in panels (b) and (c), we include z > 5 radio-loud quasar host measurements (red filled squares; C. Mazzucchelli et al. 2025). We also include measurements of 4 < z < 6 star-forming main sequence galaxies from the ALPINE survey (green circles; M. Béthermin et al. 2020; A. L. Faisst et al. 2020; O. Le Fèvre et al. 2020; D. Schaerer et al. 2020). We include LIR measured from the CRISTAL survey (i.e., deeper observations covering part of the ALPINE targets, see, e.g., I. Mitsuhashi et al. 2024). We also add measurements of Spiderweb (open red markers, z = 2.16 radio galaxy; panel (b); N. Seymour et al. 2012; C. De Breuck et al. 2022). The SFRs of the ALPINE galaxies used here are from SED fitting. Our M⋆ are estimated assuming M⋆ = Mdyn/2 (see text). We also give the Mdyn of 4C19-[C II] and J0121-[C II]-B derived based on the rotational disk fit in open yellow thin diamond and diamond symbols, respectively (W. Wang et al. 2025). We give a rough direct M⋆ ∼ 109.9 M⊙ estimate of J0121-[C  II]-B from its optical continuum in small yellow diamond markers with grey edges.
Paper: Gas-poor Hosts and Gas-rich Companions of z ≈ 3.5 Radio Active Galactic Nuclei: ALMA Insights into Jet Triggering and Feedback
Authors: Wuji Wang, 无忌 王, Carlos De Breuck, Dominika Wylezalek, Matthew D. Lehnert, Andreas L. Faisst, Andrey Vayner, Nicole Nesvadba, Joël Vernet, Pranav Kukreti, Daniel Stern
Figure caption: [O III]λ5007 spectrum from r = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩11 aperture overlaid with a normalized [C I] spectrum at the position of 4C03-[O III]. The [C I] spectrum is extracted at the same position. The black (narrow) and dark green (broad) shaded Gaussians mark the kinematic components reported as a [O III] companion in W. Wang et al. (2025). The vertical dotted line marks the Δv of the [C I] detection in S. Kolwa et al. (2023), Δv[C I],K23 = 1123 km s−1, the same as in Figure 2(b).
Paper: On the Formation of S stars from a Recent Massive Black Hole Merger in the Galactic Center
Authors: Tatsuya Akiba, Smadar Naoz, Ann-Marie Madigan
Figure caption: The inclination and eccentricity distributions of the S stars and disk stars at (left) t = 0 and (right) t = 2 Myr for our fiducial model. The simulation S stars are shown in magenta cross markers, whereas the observed S star population taken from S. Gillessen et al. (2017) is shown with pink triangle markers. The simulation disk stars are marked by teal isoproportional density contours that divide the population into equal quintiles, and the dark teal circle marker indicates the observed mean eccentricity and inclination of the disk stars (H. Bartko et al. 2009; J. R. Lu et al. 2009; S. Yelda et al. 2014). The initial eccentric disk is thin and tightly clustered at e = 0.3, with no S stars present. After 2 Myr, many stars have migrated inward of 0.04 pc and exhibit much more extended distributions in both eccentricity and inclination. The right panel shows a qualitative match between observations and simulations for both the S stars and the disk stars.
Paper: On the Formation of S stars from a Recent Massive Black Hole Merger in the Galactic Center
Authors: Tatsuya Akiba, Smadar Naoz, Ann-Marie Madigan
Figure caption: Evolution of apsidal alignment (blue) and the mean scalar eccentricity (orange) for our simulation runs. The scalar eccentricity only takes into account the magnitude of each star’s orbit, whereas ﹩|\langle {\boldsymbol{e}}\rangle |﹩ takes into account both the eccentricity magnitude as well as alignment. For e = 0.3 simulations, the apsidal alignment is erased during the course of the simulation. The alignment is maintained, and the eccentric disk is stable for the e = 0.8 simulation runs.
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: The schematic of visibility of each satellite, which refers to the time period when data are available (instrument is turned on, and the satellite is not in the SAA area) and the source is in the field of view of the instrument. It should be noted that GECAM-C also excludes high-latitude regions. The shaded area represents the time interval that is visible to the instrument.
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Multiple instrument light curves for an X-ray transient. Time zero (vertical red dashed line) is the start time of the EP/WXT X-ray transient reported in GCN or ATel. The shaded regions correspond to the visible time periods of each satellite as depicted in Figure 1. The range of the x-axis of this plot is the search time window for the gamma-ray counterpart. In addition to the main detectors, the light curve of ACD detectors are also plotted for GECAM and HXMT.
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Distribution of spectral parameters of sources with counterparts (red line) in GRB samples. GRB sample data (blue line) are from the Fermi/GBM Gamma-Ray Burst Spectral Catalog (S. Poolakkil et al. 2021).
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: The left and right panels, respectively, show the flux diagrams of peak flux and derived average flux in the 0.4–4 keV range reported by EP/WXT. The duration is reported by EP/WXT. The red data points represent the X-ray transients for which gamma-ray counterparts have been found, while the blue points indicate the sources without counterparts.
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Multiple instrument light curves for 14 EP/WXT X-ray transients whose gamma-ray counterpart is found in this work. Caption is the same as Figure 2.
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Property comparison of gamma-ray counterparts with gamma-ray samples. GRB sample data (blue line) are from Fermi/GBM Gamma-Ray Burst Spectral Catalog (A. von Kienlin et al. 2020; S. Poolakkil et al. 2021).