adsabs/AstroCLIMB huggingface dataset:
Paper: Multiwavelength Polarization Observations of Mrk 501
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Xiang-Gao Wang, Kishore C. Patra, Thomas G. Brink, Wei-Kang Zheng, Qi Wang, De-Feng Kong, Liang-Jun Chen, Ji-Wang Zhou, Jia-Xin Cao, Ming-Xuan Lu, Zi-Min Zhou, Yi-Ning Wei, Xin-Bo Huang, Xing-Lin Li, Hao Lou, Ji-Rong Mao, En-Wei Liang, Alexei V. Filippenko
Figure caption: Long-term light curves of Mrk 501 derived from observations with Fermi-LAT, Swift-XRT, IXPE, Kast, and the VLBA. The γ-ray light curve obtained with Fermi-LAT observations was binned in intervals of 3 days, and the triangle represents the upper limit value when TS < 9 for that time bin. The data for the Swift-XRT count rate were taken from the long-term Swift monitoring program of Fermi γ-ray sources (Stroh & Falcone 2013), where the open circles were derived through our data analysis. In the two bottom panels depicting the Π and ψ curves, blue circles represent the IXPE observation results in the 2–8 keV band (for the third IXPE observation, the ΠX and ψ X values are those in the 2–5 keV band); magenta circles and an orange circle (derived intrinsic value) indicate the Kast optical spectropolarimetry; open black circles represent the VLBA observations at 43 GHz taken from the VLBA-BU Blazar Monitoring Program. The horizontal gray dashed line and shaded area in the bottom panel represent the jet direction and the associated uncertainty of Mrk 501, taken from Weaver et al. (2022).
Paper: Multiwavelength Polarization Observations of Mrk 501
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Xiang-Gao Wang, Kishore C. Patra, Thomas G. Brink, Wei-Kang Zheng, Qi Wang, De-Feng Kong, Liang-Jun Chen, Ji-Wang Zhou, Jia-Xin Cao, Ming-Xuan Lu, Zi-Min Zhou, Yi-Ning Wei, Xin-Bo Huang, Xing-Lin Li, Hao Lou, Ji-Rong Mao, En-Wei Liang, Alexei V. Filippenko
Figure caption: Null hypothesis probability as a function of the number of time bins for the six IXPE observations of Mrk 501, following the method in Kim et al. (2024). The X-axis represents the number of time bins. The Y-axis represents the null hypothesis probability in logarithmic scale of the χ 2 test for time-dependent variation of the normalized Stokes parameters ﹩{ \mathcal Q }﹩ (red) and ﹩{ \mathcal U }﹩ (blue) with the constant model. The gray shaded area indicates that the null hypothesis probability is above the 1% significance level. The dashed and dotted black lines represent the 1% and 3σ (99.73%) probability, respectively.
Paper: Multiwavelength Polarization Observations of Mrk 501
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Xiang-Gao Wang, Kishore C. Patra, Thomas G. Brink, Wei-Kang Zheng, Qi Wang, De-Feng Kong, Liang-Jun Chen, Ji-Wang Zhou, Jia-Xin Cao, Ming-Xuan Lu, Zi-Min Zhou, Yi-Ning Wei, Xin-Bo Huang, Xing-Lin Li, Hao Lou, Ji-Rong Mao, En-Wei Liang, Alexei V. Filippenko
Figure caption: Normalized Stokes parameters ﹩{ \mathcal Q }﹩ and ﹩{ \mathcal U }﹩ in the 2–8 keV band, which were estimated using a model-independent method with the software ixpeobssim. The black, red, blue, and orange circles represent the results of the first, second, fourth, and sixth IXPE observations for Mrk 501, respectively. The black dashed line represents the jet direction of Mrk 501, and the cyan shaded area indicates its associated uncertainty (Weaver et al. 2022). The estimated polarization degree of the third and fifth IXPE observations is lower than its corresponding value of MDP99; thus, we excluded them in the presentation.
Paper: Multiwavelength Polarization Observations of Mrk 501
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Xiang-Gao Wang, Kishore C. Patra, Thomas G. Brink, Wei-Kang Zheng, Qi Wang, De-Feng Kong, Liang-Jun Chen, Ji-Wang Zhou, Jia-Xin Cao, Ming-Xuan Lu, Zi-Min Zhou, Yi-Ning Wei, Xin-Bo Huang, Xing-Lin Li, Hao Lou, Ji-Rong Mao, En-Wei Liang, Alexei V. Filippenko
Figure caption: Optical spectropolarimetry of Mrk 501 on 2022 April 1 using the Lick/Kast double spectrograph. From top to bottom: spectrum (line), normalized Stokes parameters ﹩{ \mathcal Q }﹩ (leftward-pointing triangles), ﹩{ \mathcal U }﹩ (rightward-pointing triangles), polarization degree ΠO (circles), and polarization angle ψ O (squares). The two cyan lines located at 6860 and 7600 Å represent telluric lines, Earth’s atmosphere absorption.
Paper: Multiwavelength Polarization Observations of Mrk 501
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Xiang-Gao Wang, Kishore C. Patra, Thomas G. Brink, Wei-Kang Zheng, Qi Wang, De-Feng Kong, Liang-Jun Chen, Ji-Wang Zhou, Jia-Xin Cao, Ming-Xuan Lu, Zi-Min Zhou, Yi-Ning Wei, Xin-Bo Huang, Xing-Lin Li, Hao Lou, Ji-Rong Mao, En-Wei Liang, Alexei V. Filippenko
Figure caption: Optical spectropolarimetry of Mrk 501 using the Kast double spectrograph. Symbols are the same as in Figure 2.
Paper: Evaluation of Scale-dependent Kurtosis with HelioSwarm
Authors: Francesco Pecora, Francesco Pucci, Francesco Malara, Kristopher G. Klein, Maria Federica Marcucci, Alessandro Retinò, William Matthaeus
Figure caption: (a) Probability density function of HS interspacecraft separations throughout the entire duration of the mission. A nominal d  i  scale of 100 km is indicated with a vertical dashed line. The configuration used in this work spans the range of scales indicated by the gray-shaded area. ((b), upper right) The black square represents the positions of HS at hour 570 of the planned trajectories (in Earth radii; geocentric solar ecliptic coordinate system). The orbit is color coded by nominal positions of the magnetosphere (blue), pristine solar wind (red), and magnetically connected regions (green). The other three panels illustrate the 36 separations between the nine spacecraft, projected onto an RTN reference frame. The three stripes in each panel indicate the MHD, transition, and kinetic ranges.
Paper: Evaluation of Scale-dependent Kurtosis with HelioSwarm
Authors: Francesco Pecora, Francesco Pucci, Francesco Malara, Kristopher G. Klein, Maria Federica Marcucci, Alessandro Retinò, William Matthaeus
Figure caption: Magnetic field power spectra computed over single spacecraft trajectories and then averaged for (a) isotropic and (b) anisotropic cases. k −5/3 and k −2 dashed and dotted–dashed lines are added as reference. The gray-shaded area indicates the range of scales covered by the HS separations. In (a) it is evident that higher intermittency (p = 0.9) generates slightly steeper spectra, though the extension of the inertial range remains intact. Correlation and “dissipation” scales are indicated with vertical dotted lines. In (b) the spectra are computed when the HS formation flies at angles θ = 1° and θ = 85° with respect to the mean field direction. The apparent flattening is only due to a downsampling of the measurements. The spectra would have a decay similar to that occurring near d  i  in (a) at k ∼ 67. The slopes have also been estimated using a fit in the region indicated by the reference lines obtaining −1.91 and −1.64 for θ = 1° and θ = 85° respectively.
Paper: Evaluation of Scale-dependent Kurtosis with HelioSwarm
Authors: Francesco Pecora, Francesco Pucci, Francesco Malara, Kristopher G. Klein, Maria Federica Marcucci, Alessandro Retinò, William Matthaeus
Figure caption: Kurtosis of the longitudinal magnetic field increments. Solid lines are obtained from millions of random paired points scattered throughout the whole volume—see case (i). Dashed lines result from a Taylor-like approach on single-spacecraft trajectories and are then averaged; see case (ii). Symbols are obtained from fixed interspacecraft separations; see case (iii).
Paper: Evaluation of Scale-dependent Kurtosis with HelioSwarm
Authors: Francesco Pecora, Francesco Pucci, Francesco Malara, Kristopher G. Klein, Maria Federica Marcucci, Alessandro Retinò, William Matthaeus
Figure caption: (a) Kurtosis obtained from the anisotropic fields in different directions θ with respect to the mean field using method (i). Indicated is the range of scales spanned by the spacecraft as a gray-shaded area. The dashed box indicates the region focus of (b) and (c). In (b) the HS κ values (symbols; method (iii)) are colored by the angle φ the vector separation  r   ij  makes with the ﹩\hat{z}﹩ direction. In (c), the stars are colored by the angle θ at which the observatory flies with respect to ﹩\hat{z}﹩. Notice the good agreement of method (iii) with the expected values when the angle φ is considered.
Paper: Evaluation of Scale-dependent Kurtosis with HelioSwarm
Authors: Francesco Pecora, Francesco Pucci, Francesco Malara, Kristopher G. Klein, Maria Federica Marcucci, Alessandro Retinò, William Matthaeus
Figure caption: (a) One magnetic field component, B  x , for intermittency levels p = 0.5 (red) and p = 0.9 (blue) sampled along a line s in any direction (the system is isotropic) with resolution δ s ≃ 30 km. (b) Increments δ B  x  = B  x (s) − B  x (s + δ s). The field with no intermittency, p = 0.5, does not show any “bursty” features. The field with higher intermittency (p = 0.9) shows large localized spikes, an indicator of intermittency.
Paper: Multiwavelength Polarization Observations of Mrk 501
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Xiang-Gao Wang, Kishore C. Patra, Thomas G. Brink, Wei-Kang Zheng, Qi Wang, De-Feng Kong, Liang-Jun Chen, Ji-Wang Zhou, Jia-Xin Cao, Ming-Xuan Lu, Zi-Min Zhou, Yi-Ning Wei, Xin-Bo Huang, Xing-Lin Li, Hao Lou, Ji-Rong Mao, En-Wei Liang, Alexei V. Filippenko
Figure caption: Photon spectral index (ΓX) vs. flux (F 0.3−10 keV) for Mrk 501, where ΓX and F 0.3−10 keV are derived with the Swift-XRT observations in the 0.3–10 keV band. The red circles represent the data obtained simultaneously with the IXPE observation epochs, while the black circles were derived from the Swift-XRT observations following the sixth IXPE observation, as listed in Table 4. The bootstrap method was employed to sample within the error range (Efron 1979) and estimate the correlation coefficient (r) between ΓX and F 0.3−10 keV, yielding a value of r = −(0.85 ± 0.03).
Paper: Multiwavelength Polarization Observations of Mrk 501
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Xiang-Gao Wang, Kishore C. Patra, Thomas G. Brink, Wei-Kang Zheng, Qi Wang, De-Feng Kong, Liang-Jun Chen, Ji-Wang Zhou, Jia-Xin Cao, Ming-Xuan Lu, Zi-Min Zhou, Yi-Ning Wei, Xin-Bo Huang, Xing-Lin Li, Hao Lou, Ji-Rong Mao, En-Wei Liang, Alexei V. Filippenko
Figure caption: Confidence contours of X-ray polarization for the first (left panel) and second (right panel) IXPE observations in the 2–8 keV (black), 2–5 keV (red), and 5–8 keV (green) bands, which are derived through spectropolarimetric fits of the IXPE data. Contours are shown at confidence levels of 68%, 90%, and 99%, respectively.
Paper: Multiwavelength Polarization Observations of Mrk 501
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Xiang-Gao Wang, Kishore C. Patra, Thomas G. Brink, Wei-Kang Zheng, Qi Wang, De-Feng Kong, Liang-Jun Chen, Ji-Wang Zhou, Jia-Xin Cao, Ming-Xuan Lu, Zi-Min Zhou, Yi-Ning Wei, Xin-Bo Huang, Xing-Lin Li, Hao Lou, Ji-Rong Mao, En-Wei Liang, Alexei V. Filippenko
Figure caption: Spectropolarimetric fit results of the first IXPE observation data for Mrk 501, in the 2–5 keV band (top panel) and the 5–8 keV band (bottom panel). Panels present the fits to IXPE Stokes parameters I, Q, and U with their associated residuals from left to right. In the I fit panels, the triangles indicate the background count spectra for three DUs.
Paper: New Insights into the Internal Structure of GJ 1214 b Informed by JWST
Authors: Matthew C. Nixon, Anjali A. A. Piette, Eliza M.-R. Kempton, Peter Gao, Jacob L. Bean, Maria E. Steinrueck, Alexandra S. Mahajan, Jason D. Eastman, Michael Zhang, Leslie A. Rogers
Figure caption: Left: best-fitting envelope mass fractions for GJ 1214 b as a function of envelope mean molecular weight. Solid lines (solid and dashed lines). Shaded regions around each line correspond to values that are consistent with the observed mass and radius to within 1σ. The total envelope fraction is shown in orange (uppermost lines), while the corresponding H2O and H/He fractions are shown in blue (middle lines) and green (bottom lines), respectively. The planet’s phase curve suggests that the atmospheric metallicity is at least 100× solar, equivalent to a total envelope mass fraction of at least 8.1%, while the transmission spectrum prefers metallicities ≥300× solar, yielding a minimum envelope fraction of 34.4%. The region of the figure showing models with metallicities <300× solar is shaded in gray. Right: same as left panel, but only showing H/He fraction on a linear scale for clarity. The maximum H/He mass fraction across all models considered is 5.8%.
Paper: New Insights into the Internal Structure of GJ 1214 b Informed by JWST
Authors: Matthew C. Nixon, Anjali A. A. Piette, Eliza M.-R. Kempton, Peter Gao, Jacob L. Bean, Maria E. Steinrueck, Alexandra S. Mahajan, Jason D. Eastman, Michael Zhang, Leslie A. Rogers
Figure caption: Mass and radius of GJ 1214 b from Mahajan et al. (2024). Mass–radius relations for best-fit models with a selection of atmospheric compositions are shown, assuming maximally reflective hazes. The 100×, 300×, and 500× solar composition atmospheres assume a haze production rate (HPR) of 10−11 g cm−2 s−1. For the pure water (steam) atmospheres, two values of the HPR are shown: 10−11 g cm−2 s−1 and 10−14 g cm−2 s−1. Percentages shown are the total envelope mass fractions; the relevant H/He and H2O mass fractions for each case can be calculated using the mass mixing ratios in Table 2. A steam atmosphere scenario with 50% H2O and 50% iron+rock is included for comparison, corresponding to the water world interior structure with no H/He from Luque & Pallé (2022). Gray points with error bars show planets with similar masses and radii that have been measured to better than 20% precision. Data taken from the NASA Exoplanet Archive.
Paper: New Insights into the Internal Structure of GJ 1214 b Informed by JWST
Authors: Matthew C. Nixon, Anjali A. A. Piette, Eliza M.-R. Kempton, Peter Gao, Jacob L. Bean, Maria E. Steinrueck, Alexandra S. Mahajan, Jason D. Eastman, Michael Zhang, Leslie A. Rogers
Figure caption: Model emission spectra from GENESIS with different compositions and haze production rates (HPR), compared to the MIRI dayside spectrum of GJ 1214 b. The top panels show models including Titan-like tholin hazes, while the bottom panels show models with maximally reflective, purely scattering hazes. Models with the smallest values of χ 2/n data have been chosen from a larger grid of compositions and haze production rates. Note that the water atmosphere models with HPRs of 10−13 and 10−14 g cm−2 s−1 overlap significantly.
Paper: New Insights into the Internal Structure of GJ 1214 b Informed by JWST
Authors: Matthew C. Nixon, Anjali A. A. Piette, Eliza M.-R. Kempton, Peter Gao, Jacob L. Bean, Maria E. Steinrueck, Alexandra S. Mahajan, Jason D. Eastman, Michael Zhang, Leslie A. Rogers
Figure caption:  P–T profiles of best-fitting GENESIS models to the emission spectrum of GJ 1214 b. The left-hand panel shows models with a fixed haze production rate (10−11 g cm−2 s−1) and varying compositions, while the right-hand panel shows profiles for a pure steam atmosphere with different haze production rates. These profiles are used to set the thermal structure of the outer envelope for the interior model grid.
Paper: Observations of the Formation and Disappearance of a Funnel Prominence
Authors: Bo Yang, Jiayan Yang, Yi Bi, Junchao Hong
Figure caption: (a–b) AIA 171 Å difference images displaying the prominence materials drag the U-shaped coronal loops down, leading to the compression of the U-shaped coronal loops at their base. (c–d) Distance–time plots from AIA 304 Å images for the two slits (AB and CD) as shown in Figures 2(b) and (c). The white dashed lines outline the motions of the rising cool column.
Paper: Particle Acceleration and Magnetic Field Amplification by Relativistic Shocks in Inhomogeneous Media
Authors: Kanji Morikawa, Yutaka Ohira, Takumi Ohmura
Figure caption: Mean time evolution of the particle energy for the four runs. t = 0 is defined by the time when each particle crosses the shock front for the first time. The solid curves are the simulation results averaged for the top 1000 particles. The dashed lines are the theoretical line of the Bohm rate in the upstream magnetic field strength, where the initial energy was ignored.
Paper: Particle Acceleration and Magnetic Field Amplification by Relativistic Shocks in Inhomogeneous Media
Authors: Kanji Morikawa, Yutaka Ohira, Takumi Ohmura
Figure caption: MHD simulation results at t = 3000 L cl/c. The top two panels show the two-dimensional distribution of the magnetic field strength in the z = 0 plane. The third and last panels show one-dimensional distributions of magnetic energy density and electric field strength associated with the downstream turbulence, respectively. The bottom two panels show quantities averaged over the y–z plane.
Paper: Particle Acceleration and Magnetic Field Amplification by Relativistic Shocks in Inhomogeneous Media
Authors: Kanji Morikawa, Yutaka Ohira, Takumi Ohmura
Figure caption: The representative particle trajectory for all the simulations. The top and bottom panels are for ρ cl,S/ρ 0,S = 2 and 10, respectively. The gray region represents the shock front.
Paper: Particle Acceleration and Magnetic Field Amplification by Relativistic Shocks in Inhomogeneous Media
Authors: Kanji Morikawa, Yutaka Ohira, Takumi Ohmura
Figure caption: Energy spectra of test-particle simulations. The top and bottom panels are for ρ cl,S/ρ 0,S = 2 and 10, respectively. The red and blue solid histograms are the energy spectra for R up,U/L cl = 0.26 and 26, respectively. The dotted histograms show the energy spectra without density fluctuations.
Paper: Particle Acceleration and Magnetic Field Amplification by Relativistic Shocks in Inhomogeneous Media
Authors: Kanji Morikawa, Yutaka Ohira, Takumi Ohmura
Figure caption: Mean downstream energy gain in the downstream rest frame for the top 103 energetic particles in the case of ρ cl,S/ρ 0,S = 10 and R up,U/L cl = 0.26. The horizontal axis is the incident energy from upstream to downstream, ﹩{{ \mathcal E }}_{\mathrm{ini},{\rm{D}}}﹩.
Paper: Scintillation Velocity and Arc Observations of FRB 20201124A
Authors: Ziwei Wu, Weiwei Zhu, Bing Zhang, Yi Feng, JinLin Han, Di Li, Dongzi Li, Rui Luo, Chenhui Niu, Jiarui Niu, Bojun Wang, Fayin Wang, Pei Wang, Weiyang Wang, Heng Xu, Yuanpei Yang, Yongkun Zhang, Dejiang Zhou, Yuhao Zhu, Can-Min Deng, Yonghua Xu
Figure caption: Upper panels: the 2D ACFs of FRB 20201124A with FAST on MJDs 59485 and 59612. In the two smaller side plots, the gray points are the 1D ACFs at zero frequency and time lag, the red dashed curves are the best fits from which the scintillation timescale τ d and scintillation bandwidth Δν d are derived, respectively. Bottom panels: the corresponding secondary spectra.
Paper: Scintillation Velocity and Arc Observations of FRB 20201124A
Authors: Ziwei Wu, Weiwei Zhu, Bing Zhang, Yi Feng, JinLin Han, Di Li, Dongzi Li, Rui Luo, Chenhui Niu, Jiarui Niu, Bojun Wang, Fayin Wang, Pei Wang, Weiyang Wang, Heng Xu, Yuanpei Yang, Yongkun Zhang, Dejiang Zhou, Yuhao Zhu, Can-Min Deng, Yonghua Xu
Figure caption: The dynamic spectrum of Stokes I of FRB 20201124A at MJD 59485. High-frequency noises are injected for calibration during the observation’s first and last minutes. The same printed contrast is applied to each frequency spectrum, and the lines have transparency.
Paper: Scintillation Velocity and Arc Observations of FRB 20201124A
Authors: Ziwei Wu, Weiwei Zhu, Bing Zhang, Yi Feng, JinLin Han, Di Li, Dongzi Li, Rui Luo, Chenhui Niu, Jiarui Niu, Bojun Wang, Fayin Wang, Pei Wang, Weiyang Wang, Heng Xu, Yuanpei Yang, Yongkun Zhang, Dejiang Zhou, Yuhao Zhu, Can-Min Deng, Yonghua Xu
Figure caption: Upper panel: measurements of parameter W of FRB 20201124A. The dashed curve represents the best-fitting anisotropic scattering model described in Section 3.2 using MCMC. The brightness of W depends on the number of blocks of data of each observation. Lower panel: the predicted scintillation arc using the best-fitting anisotropic scattering model. The black filled areas represent the scintillation arc curvature range.
Paper: Scintillation Velocity and Arc Observations of FRB 20201124A
Authors: Ziwei Wu, Weiwei Zhu, Bing Zhang, Yi Feng, JinLin Han, Di Li, Dongzi Li, Rui Luo, Chenhui Niu, Jiarui Niu, Bojun Wang, Fayin Wang, Pei Wang, Weiyang Wang, Heng Xu, Yuanpei Yang, Yongkun Zhang, Dejiang Zhou, Yuhao Zhu, Can-Min Deng, Yonghua Xu
Figure caption: The posterior probability distribution of all fitted parameters. In the 1D histograms, the red curves represent the kernel-density estimate smoothed versions of the distributions. From left to right, three black dashed lines denote the 10% fractional percentiles, the most likely values, and the 90% fractional percentiles, respectively. The most likely values and the upper/lower errors are indicated at the top of the 1D histograms.
Paper: The Delayed Radio Emission in the Black Hole X-Ray Binary MAXI J1348-630
Authors: Bei You, Shuai-kang Yang, Zhen Yan, Xinwu Cao, Andrzej A. Zdziarski
Figure caption: The evolution of the fluxes with time during the rising phase (panels (A)–(B)), the decaying phase (panels (C)–(D)) and the mini-outburst (panels (E)–(F)). Panel (A): the estimated Comptonization flux in the 0.1–100 keV band during the rising phase. Panel (B): the radio flux at 5.5 GHz by ATCA (red points) and MeerKAT (black points) during the rising phase. Panel (C): the estimated Comptonization flux in the 0.1–100 keV band during the decaying phase. Panel (D): the radio flux at 5.5 GHz by ATCA (red points) and MeerKAT (black points) during the decaying phase. Panel (E): the estimated Comptonization flux in the 0.1–100 keV band during the mini-outburst. Panel (F): the radio flux at 5.5 GHz by ATCA (red points) and MeerKAT (black points) during the mini-outburst. The radio emission was detected from the MAXI J1348-630 core location. The MeerKAT radio flux density at 1.28 GHz is converted to the 5.5 GHz monochromatic flux with the interpolated spectral index from the ATCA observations. The white, gray, and pink region represent the hard, intermediate, and soft states, respectively.
Paper: The Delayed Radio Emission in the Black Hole X-Ray Binary MAXI J1348-630
Authors: Bei You, Shuai-kang Yang, Zhen Yan, Xinwu Cao, Andrzej A. Zdziarski
Figure caption: Insight-HXMT lightcurves of MAXI J1348-630 in the HE (28–150 keV, red curve), ME (10–21 keV, blue curve), and LE (3–10 keV, black curve) bands. The two white regions indicate the hard states. The two light gray shaded regions indicate the intermediate states, and the light pink region represents the soft state. The light green shaded region indicates the hard-state-only mini-outburst. Vertical solid lines separate these epochs. Beyond MJD 58600, the count rate of LE is close to the count rate of ME, so it is hard to distinguish the two lightcurves in the figure visually.
Paper: The Delayed Radio Emission in the Black Hole X-Ray Binary MAXI J1348-630
Authors: Bei You, Shuai-kang Yang, Zhen Yan, Xinwu Cao, Andrzej A. Zdziarski
Figure caption: Panel (A): cross-correlation analysis between the radio and the X-ray fluxes during rising phase. Panel (B): cross-correlation analysis between the radio and the X-ray fluxes during decaying phase. Panel (C): cross-correlation analysis between the radio and the X-ray fluxes during mini-outburst. In all panels, the dashed and dotted histograms in blue are the cross-correlation centroid lag distribution and peak lag distribution obtained by the flux randomization/random subset sampling (FR/RSS) methods, respectively, the axis of which is provided on the right side.