adsabs/AstroCLIMB huggingface dataset:
Paper: Analysis of the Stellar Occultations during the Unprecedented Long-duration Flare
Authors: K. Bicz, R. Falewicz, P. Heinzel, M. Pietras, P. Preś
Figure caption: Panels (a), (b), and (c) show the eclipsing part of the loop arcade during the phases of maximum occultation, as indicated by the arrows in Figure 1(a). The orange contours indicate the fully covered flaring region. Panel (d) presents the arcades during the selected phase when they do not obscure the flaring region, allowing for size comparisons between the arcades. The brown structure corresponds to the first eclipse, the purple to the second, and the red to the third eclipse. The black cross marks the position of the star’s pole. The opaque segments of the arcades denote the fragments responsible for the eclipses observed in the light curve, while the transparent segments represent the entire possible arcade. Gray contours denote the starspots on the star from Paper I, the orange region indicates the flaring region, and the black contours outline the star.
Paper: Analysis of the Stellar Occultations during the Unprecedented Long-duration Flare
Authors: K. Bicz, R. Falewicz, P. Heinzel, M. Pietras, P. Preś
Figure caption: Evolution of the temperature of the flaring region during the whole event.
Paper: Analysis of the Stellar Occultations during the Unprecedented Long-duration Flare
Authors: K. Bicz, R. Falewicz, P. Heinzel, M. Pietras, P. Preś
Figure caption: Flow diagram showing the operations made during the light-curve modeling.
Paper: Parabolic-like Trend in SiO Ratios throughout the Central Molecular Zone: Possible Signature of a Past Nuclear Activity in the Galactic Center
Authors: Shunya Takekawa, Tomoharu Oka, Shiho Tsujimoto, Hiroki Yokozuka, Nanase Harada, Miyuki Kaneko, Rei Enokiya, Yuhei Iwata
Figure caption: (a)–(d) SiO intensity ratios of SiO clouds as a function of the Galactic longitude. Each data point represents an individual SiO cloud. Clouds with diameters d larger than 5 pc are shown in dark blue. Panel (a) displays the ratio of SiO/H13CN, (b) SiO/CS, (c) SiO/H13CO+, and (d) SiO/SO. (e)–(f) Spatial and velocity distributions of SiO clouds with colors assigned according to the SiO/H13CN ratio. In the l–b plane (e), the diameter of each circle corresponds to the diameter d of the SiO cloud. In the l–V plane (f), the width and height of each rectangle represent the cloud’s diameter d and velocity width, respectively. The velocity width is defined as ﹩2\sqrt{2\mathrm{ln}2}{\sigma }_{V}﹩. The star symbol in panel (e) and vertical dashed lines in the other panels indicate the position of Sgr A*.
Paper: Parabolic-like Trend in SiO Ratios throughout the Central Molecular Zone: Possible Signature of a Past Nuclear Activity in the Galactic Center
Authors: Shunya Takekawa, Tomoharu Oka, Shiho Tsujimoto, Hiroki Yokozuka, Nanase Harada, Miyuki Kaneko, Rei Enokiya, Yuhei Iwata
Figure caption: (a) SiO intensity ratios of SiO clouds as a function of their average density. Red and blue dots indicate the SiO/H13CN and SiO/CS ratios, respectively. The best-fit lines are represented as dashed lines. (b)–(c) SiO/H13CN and SiO/CS intensity ratios of the SiO clouds within the restricted average density ranges as a function of the Galactic longitude, respectively. Green points are the clouds with average densities from 102.5 to 103.0 cm−3, and orange points have average densities from 103.0 to 103.5 cm−3. The vertical dashed lines indicate the position of Sgr A*.
Paper: Various Features of the X-class White-light Flares in Super Active Region NOAA 13664
Authors: Ying Li, Xiaofeng Liu, Zhichen Jing, Wei Chen, Qiao Li, Yang Su, De-Chao Song, M. D. Ding, Li Feng, Hui Li, Weiqun Gan
Figure caption: HMI (a) and WST (b) images at the WL brightening time for the 12 X-class flares. The red contours with fixed levels for on-disk (except FL3 and FL7 having a weak WL emission) and off-limb flares, respectively, in the images indicate the WL brightenings that correspond to those as seen in the running- or base-difference images in Figure 3. Note that FL1 is not a detectable WLF without showing the WL contours and that FL2 without the HMI contour is due to data missing during its WL brightening period.
Paper: Parabolic-like Trend in SiO Ratios throughout the Central Molecular Zone: Possible Signature of a Past Nuclear Activity in the Galactic Center
Authors: Shunya Takekawa, Tomoharu Oka, Shiho Tsujimoto, Hiroki Yokozuka, Nanase Harada, Miyuki Kaneko, Rei Enokiya, Yuhei Iwata
Figure caption: (a)–(c) Integrated intensity maps of the SiO J = 2–1 (a), H13CN J = 1–0 (b), and CS J = 2–1 (c) lines. The velocity range for the integration is V LSR = −220 to +220 km s−1. Note that, in the region west of l = −0.°4, H13CO+ emission was slightly detected in the velocity range −120 to −100 km s−1, which contaminated the SiO velocity range of +200 to +220 km s−1. Therefore, for the SiO map west of l = − 0.°4, the integration range is limited to +200 km s−1. The unit of intensity is K km s−1. (d)–(e) Contours of the SiO clouds projected onto the l–b plane (d) and the l–V plane (e). Contours with the same assigned color in both panels correspond to the same SiO cloud.
Paper: Various Features of the X-class White-light Flares in Super Active Region NOAA 13664
Authors: Ying Li, Xiaofeng Liu, Zhichen Jing, Wei Chen, Qiao Li, Yang Su, De-Chao Song, M. D. Ding, Li Feng, Hui Li, Weiqun Gan
Figure caption: Overview of the 12 X-class flare events in super AR NOAA 13664. (a) GOES SXR flux during 2024 May 7–16. The blue vertical dashed lines in the panel denote the peak times of the 12 X-class flares. (b) AIA 1600 Å (green) and 131 Å (red) images around the peak times of the 12 flares. The blue contours in the images mark the HMI 6173 Å brightenings, which are the same as the red contours in Figure 2(a).
Paper: Parabolic-like Trend in SiO Ratios throughout the Central Molecular Zone: Possible Signature of a Past Nuclear Activity in the Galactic Center
Authors: Shunya Takekawa, Tomoharu Oka, Shiho Tsujimoto, Hiroki Yokozuka, Nanase Harada, Miyuki Kaneko, Rei Enokiya, Yuhei Iwata
Figure caption: Schematic of the nuclear outburst scenario. Fast wind (or ejecta) driven by a past nuclear activity within the last ∼105 yr sequentially induced the SiO enhancement via strong shocks. SiO was depleted over time after the shock dissipated, thereby reducing the temporarily enhanced SiO. Thus, a parabolic-like SiO trend emerges.
Paper: Various Features of the X-class White-light Flares in Super Active Region NOAA 13664
Authors: Ying Li, Xiaofeng Liu, Zhichen Jing, Wei Chen, Qiao Li, Yang Su, De-Chao Song, M. D. Ding, Li Feng, Hui Li, Weiqun Gan
Figure caption: HMI (a) and WST (b) running- (for on-disk flares) or base-difference (for off-limb flares) images at the WL brightening time for the 12 X-class flares. The cyan contours (with 20% level at the maximum) in the images mark the HXI HXR sources for the WLFs that have available HXI data at the corresponding time. The red boxes denote the regions integrated over for the HMI and WST emission curves in Figure 4. The red arrow in the WST image of FL2 indicates the visible 3600 Å brightening though its enhancement is below our threshold.
Paper: Various Features of the X-class White-light Flares in Super Active Region NOAA 13664
Authors: Ying Li, Xiaofeng Liu, Zhichen Jing, Wei Chen, Qiao Li, Yang Su, De-Chao Song, M. D. Ding, Li Feng, Hui Li, Weiqun Gan
Figure caption: HXR and WL emission curves from HXI, HMI, and WST for the 12 X-class flares. The HMI and WST emissions are integrated over the same flaring region marked by the red box in Figure 3. For FL4, we also overplot the HMI emission curve (in gray) integrated over the compact WL sources only for reference. In each panel, the three vertical dotted lines indicate the flare onset, peak, and end times. The yellow shaded area denotes the duration of the WL emission at WST 3600 Å. Note that the time periods affected by the radiation belt are indicated in gray in the HXR 50–100 keV curve and that the poor HXR data during the times of the South Atlantic Anomaly (SAA) and HXI night are not displayed.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Histogram of sizes compared in this work. For the SCs, we report the size of the H II regions, R H II , the SC radius, R SC (defined as the radius that contains 50% of member stars), and R TS and R B (defined in the text). For the gamma-ray sources we report different sizes: with Fermi-LAT unassociated sources being mostly point like, we report their positional uncertainty, derived from the 68% confidence ellipse; LHAASO and H.E.S.S. sources are instead fitted with Gaussians, and the σ and the 39% containment radius are reported.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Left: infrared (22 μm) luminosity and extension of WISE H II regions for which we know the flux and distance. The color code indicates the number of Fermi-LAT-unidentified sources that overlap these objects. Right: the WISE 22 μm map toward the young massive cluster NGC 3603. The H II regions considered in this work are drawn in white, while the Gaia SCs are drawn in orange, dashed orange lines are for R B, and solid orange lines are for R TS. Light-blue circles indicate the Fermi 4FGL centroid uncertainty, ΔR 68; among these, sources overlaid with a cross are unassociated. For the latter, the name, as reported in the catalog, is also reported. The map has been obtained from https://alasky.cds.unistra.fr/hips-image-services/hips2fits, a service provided by the Strasbourg astronomical Data Center.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Significance of the correlation between SC catalogs (horizontal lines) and their subsamples divided by extension (red points) and luminosity (blue points) on the left and by age (red points) and the number of SN explosions (blue points) on the right. The indicated luminosity refers to the wind luminosity for Gaia SCs and to the IR luminosity for the WISE SCs. Results obtained with WISE SCs are marked as diamond, while Gaia SCs are indicated by circles, squares, and stars, depending on the matching radius considered among the bubble, the termination shock, or the stellar radius, respectively. The different rows from top to the bottom report results obtained with the Fermi-LAT, H.E.S.S.-HGPS, LHAASO-WCDA, and LHAASO-KM2A, respectively. Note that in the case of WISE SCs with L w > 1039 erg s−1 one match is found in the real catalog, but zero matches are found in the 1000 realizations; therefore, the matching significance is formally infinite, and thus it falls out of the plot axis.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Left: significance of the correlation between the considered SC catalogs and the different gamma-ray catalogs. The different colors refer to the different SC samples and the different matching radii used in the matching, as indicated in the legend. Right: significance of the correlation between gamma-ray source catalogs and Gaia-identified clusters of different ages. In this case, the radius used for correlation is the stellar core radius, R SC.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Distribution of matches, M sim, of the simulated catalogs, with the different SC catalogs, and within different matching radii, as indicated in each panel. The black dashed line indicates the average of M sim; the yellow area indicates the zone where 99% of occurrences are contained, the dotted–dashed light-blue line indicates the events at three standard deviations (﹩{\sigma }_{{\rm{sim}}}﹩) from the average, and the red line indicates the number of real matches.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Surface brightness (in arbitrary units) against compactness, expressed as the ratio between R TS and R SC, for the Gaia SCs. The different colors indicate if the clusters overlap a source of a given catalog, as indicated in the legend. Sources that contain also a pulsar are indicated with a black cross. The SC’s name is indicated for matching compact (R TS/R SC > 1) SCs.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Longitude and latitude distribution of the Fermi-LAT 2082 nonassociated sources (blue lines) compared to the same distributions of one realization of synthetic clusters (red bars).
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Longitude and latitude cumulative distribution of the Fermi-LAT 2082 nonassociated sources.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Physical properties of the analyzed sample of SCs that are considered in the discussion. Left: the age distribution of the Gaia sample. Right: the distribution of wind luminosity, as calculated by S. Celli et al. (2024), and of IR luminosity of WISE H II regions for the available objects.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Distribution of the Gaia SCs in terms of the number of SN explosions estimated to have occurred during the age of the SCs.
Paper: On the Correlation between Young Massive Star Clusters and Gamma-Ray Unassociated Sources
Authors: Giada Peron, Giovanni Morlino, Stefano Gabici, Elena Amato, Archana Purushothaman, Marcella Brusa
Figure caption: Longitude and latitude distribution of the real Fermi-LAT sources (blue) and of one simulated catalog (red).
Paper: Long-lived Equilibria in Kinetic Astrophysical Plasma Turbulence
Authors: Mario Imbrogno, Claudio Meringolo, Sergio Servidio, Alejandro Cruz-Osorio, Benoît Cerutti, Francesco Pegoraro
Figure caption: (a) Magnetic power spectrum at a time beyond the peak of nonlinear activity vs. kd  e . The vertical (orange) line represents the persistent structure wavenumber k 0 d  e , which identifies the typical scale of the vortices. (b) 2D contour of the magnetic vector potential component a  z  (right side) and the cosine angle between the current density and the total magnetic field (left side). The y-axis is normalized to both the electron (left side) and the proton skin depth d  p  (right side).
Paper: Long-lived Equilibria in Kinetic Astrophysical Plasma Turbulence
Authors: Mario Imbrogno, Claudio Meringolo, Sergio Servidio, Alejandro Cruz-Osorio, Benoît Cerutti, Francesco Pegoraro
Figure caption: (a) Radial behavior of the angle between the current density and the total magnetic field (azimuthal averages) for each structure depicted in Figure 1(b). (b) Force-free parameter λ(r). We define r 0 as the vortex eye radius, namely, the position of the first spiraling arm.
Paper: Long-lived Equilibria in Kinetic Astrophysical Plasma Turbulence
Authors: Mario Imbrogno, Claudio Meringolo, Sergio Servidio, Alejandro Cruz-Osorio, Benoît Cerutti, Francesco Pegoraro
Figure caption:  Merging history of two long-lived structures as a function of Alfvénic crossing time (from top to bottom). The plot shows the plasma density (left column), the (force-free) cosine angle (middle column), and the magnetic helicity density (right column). Circumferences (in black) represent the eye of each vortex.
Paper: Long-lived Equilibria in Kinetic Astrophysical Plasma Turbulence
Authors: Mario Imbrogno, Claudio Meringolo, Sergio Servidio, Alejandro Cruz-Osorio, Benoît Cerutti, Francesco Pegoraro
Figure caption: Radial behavior of the magnetic field components of all the long-lived vortices appearing during the simulation (points). Components have been rescaled to the field at the center B 0 and using their typical gradient ξ. The GH solution (shaded) describes qualitatively well the profiles near the eye.
Paper: Long-lived Equilibria in Kinetic Astrophysical Plasma Turbulence
Authors: Mario Imbrogno, Claudio Meringolo, Sergio Servidio, Alejandro Cruz-Osorio, Benoît Cerutti, Francesco Pegoraro
Figure caption: (a) Total magnetic field and current density components for the central vortex in Figure 1 (open symbols) and the KVR model (solid lines). Data have been averaged over time in the vortex frame.
Paper: Long-lived Equilibria in Kinetic Astrophysical Plasma Turbulence
Authors: Mario Imbrogno, Claudio Meringolo, Sergio Servidio, Alejandro Cruz-Osorio, Benoît Cerutti, Francesco Pegoraro
Figure caption: The rms of the vertical component of the current density (black solid line). Dotted red and dashed blue lines represent the time of most intense nonlinear activity and the analysis time, respectively.
Paper: Long-lived Equilibria in Kinetic Astrophysical Plasma Turbulence
Authors: Mario Imbrogno, Claudio Meringolo, Sergio Servidio, Alejandro Cruz-Osorio, Benoît Cerutti, Francesco Pegoraro
Figure caption: Components of the momentum equation for the fluid approximation in the vortex eye.
Paper: Long-lived Equilibria in Kinetic Astrophysical Plasma Turbulence
Authors: Mario Imbrogno, Claudio Meringolo, Sergio Servidio, Alejandro Cruz-Osorio, Benoît Cerutti, Francesco Pegoraro
Figure caption: Average error estimated by considering all the vortex profiles. The best choice for the free parameters is highlighted by a cyan circle.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: The property maps of MaNGA 9885-9102. Panel (a): the velocity map of emission lines. Panel (b): the velocity dispersion map of emission lines. All data are taken from the DAP. The value shown beside the blobs is the average and its uncertainty of pixels in the circle. Panel (c): the map of [O III]λ5007/[O II]λ3727 flux ratios. Panel (d): the map of Hα/Hβ flux ratios.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: The incident spectra of MF87, UVsoft, HE0238, Free α, and 5 × 104 K blackbody. The α OX and α UV of the “Free α” spectra adopt the values of the upper blob. The vertical solid black line represents the first ionization energy of hydrogen (i.e., 13.6 eV or 1 Ryd), the dashed dark blue curve represents the transmission of the UVW2 band of UVOT, and the dashed gray curve represents the transmission of neutral hydrogen with N H = 1021 cm−2.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: Left: the UVOT UVW2 image of 9885-9102. Middle: the mock image of the two blobs with the dust-corrected luminosity estimated by the star formation model. The size is determined by the PSF of UVW2. Right: the image superimposed by the first two. This shows that the obvious features of the blobs on the UV image should be clearly seen in case of star formation origin, but we cannot actually see.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: The relative values of the line ratios from photoionization models (R model) and the observed line ratios (R obs). The closer it is to 1 (the horizontal solid black line), the more the model conforms to the observation. The different bar colors represent the different incident spectra used in the photoionization model.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: The scaling relationships of 9885-9102. (a) The star formation main sequence. (b) The mass–metallicity relation. The red stars represent 9885-9102, and the green areas represent the distribution of other MaNGA galaxies.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: Surface brightness profiles in the DESI g-, r-, z-bands of MaNGA 9885-9102. The black dashed black line is the exponential fitting of the g-band image. The horizontal axis is the projection-corrected distance to the center.
Paper: Sudden Polarization Angle Jumps of the Repeating Fast Radio Burst FRB 20201124A
Authors: J. R. Niu, W. Y. Wang, J. C. Jiang, Y. Qu, D. J. Zhou, W. W. Zhu, K. J. Lee, J. L. Han, B. Zhang, D. Li, S. Cao, Z. Y. Fang, Y. Feng, Q. Y. Fu, P. Jiang, W. C. Jing, J. Li, Y. Li, R. Luo, L. Q. Meng, C. C. Miao, X. L. Miao, C. H. Niu, Y. C. Pan, B. J. Wang, F. Y. Wang, H. Z. Wang, P. Wang, Q. Wu, Z. W. Wu, H. Xu, J. W. Xu, L. Xu, M. Y. Xue, Y. P. Yang, M. Yuan, Y. L. Yue, D. Zhao, C. F. Zhang, D. D. Zhang, J. S. Zhang, S. B. Zhang, Y. K. Zhang, Y. H. Zhu
Figure caption: The PA orthogonal jump of the three FRB 20201124A bursts. Panel (a) shows the degrees of linear and circular polarization. Panel (b) shows the bin-to-bin difference of the PA curve. The red error bars in the panel (c) represent the measured PA swing of the three FRB bursts. Panel (d) shows the intensity of the three bursts in time and frequency. For Burst #1 we show only the burst in a frequency range of 1000–1200 MHz. For Burst #2 and Burst #3 we show the full 1000–1500 MHz band. Using the outliers in the bin-to-bin difference of PA (marked as red dots in panel (b)), we find the time range in which the PA jumps occur and mark them with the dotted vertical line in panel (a), (b), and (c).
Paper: Sudden Polarization Angle Jumps of the Repeating Fast Radio Burst FRB 20201124A
Authors: J. R. Niu, W. Y. Wang, J. C. Jiang, Y. Qu, D. J. Zhou, W. W. Zhu, K. J. Lee, J. L. Han, B. Zhang, D. Li, S. Cao, Z. Y. Fang, Y. Feng, Q. Y. Fu, P. Jiang, W. C. Jing, J. Li, Y. Li, R. Luo, L. Q. Meng, C. C. Miao, X. L. Miao, C. H. Niu, Y. C. Pan, B. J. Wang, F. Y. Wang, H. Z. Wang, P. Wang, Q. Wu, Z. W. Wu, H. Xu, J. W. Xu, L. Xu, M. Y. Xue, Y. P. Yang, M. Yuan, Y. L. Yue, D. Zhao, C. F. Zhang, D. D. Zhang, J. S. Zhang, S. B. Zhang, Y. K. Zhang, Y. H. Zhu
Figure caption: Comparing FRB 20201124A OPM jump bursts #2 and #3 with the single pulse and integrated profile of Pulsar J0358+5413 and J1136+1551. In panel (a), (b), and (c), we show bursts #2 and PSR J1136+1551's single pulse and integrated PA, polarization profile, and waterfall, respectively. In panel (d), (e), and (f), we show the same information for bursts #3 and PSR J0358+5413. The dotted horizontal lines show the 0° PA. The polarization profiles are shown in the panel (b) and (e), with linear polarization in red, circular polarization in blue, and total intensity in black. The intensity of the profiles is normalized such that the off-pulse rms equals unity. The positions of the dotted vertical lines indicate the time (phase) of the orthogonal jumps.