adsabs/AstroCLIMB huggingface dataset:
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Same as Figure 11 but for Mrk 335 in the 2019, 2021, and 2022 seasons.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Same as Figure 5, but for Mrk 1239. There is not a reliable time lag in the 2021 season due to small variability in the Hβ light curve. In the 2019 season, the Hβ data points at JD 2458792 and 2458866 marked by open circles are treated as outliers (due to poor weather conditions) and excluded in the time lag analysis.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Same as Figure 5, but for PDS 456.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: A comparison of Hβ time lags between seasons from the ICCF (top) and MICA (bottom) methods. The horizontal black lines inside the violin plots represent 68.3% confidence intervals. Vertical dashed lines represent the means of all ICCF and MICA lags and are plotted to guide the eye.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Same as Figure 5, but for Mrk 509. In the 2020 season, the Hβ light curve has no large variation structure and the obtained time lags are unreliable. Note that the SAAO data (green points) are not included in the time lag analysis due to their large scatter.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Same as Figure 11 but for Mrk 509 in the 2019, 2021, and 2022 seasons.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Same as Figure 5, but for Mrk 335.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Same as Figure 11 but for Mrk 1239 in the 2019 and 2020 seasons.
Paper: NuSTAR Observation of the TeV-detected Radio Galaxy 3C 264: Core Emission and the Hot Accretion Flow Contribution
Authors: Ka-Wah Wong, Colin M. Steiner, Allison M. Blum, Dacheng Lin, Rodrigo Nemmen, Jimmy A. Irwin, Daniel R. Wik
Figure caption: Smoothed 3–7 keV (left-hand panel) and 15–20 keV (middle panel) NuSTAR images of 3C 264. The circle at the center of the image indicates the 30″ radius spectral extraction region. The circle on top is the background spectral extraction region with the same radius of 30″. Using a larger background region gives essentially the same results. A 0.3–6 keV Chandra subpixel resolution image is shown in the right-hand panel, with one image pixel size = 0.″123. The two circles indicate the 3σ position errors of the emission peaks measured with NuSTAR in different energy bands. Relative astrometric correction has been made so that the peak of the NuSTAR 3–7 keV aligns with that of the Chandra emission (see the text). The arc feature at about 0.″8 southeast from the center is an artifact of the Chandra PSF (Section 3.2).
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: The time lag analysis of the full-span light curves using MICA for IC 4329A, Mrk 335, Mrk 509, and Mrk 1239, from top to bottom. For each object, the left panels show the photometric (top) and Hβ (bottom) light curves. The photometric light curves are converted from magnitudes and normalized with their means. The Hβ fluxes are in a unit of 10−13 erg s−1 cm−2. The gray shaded bands represent reconstruction. The right panels show the obtained transfer function (top) and posterior distribution of the time lag (bottom). The gray shaded areas represent the uncertainties of the transfer function. For Mrk 509, two Gaussian components in the transfer function are needed to appropriately fit the light curves and the time lag distributions shows two separate modes accordingly.
Paper: NuSTAR Observation of the TeV-detected Radio Galaxy 3C 264: Core Emission and the Hot Accretion Flow Contribution
Authors: Ka-Wah Wong, Colin M. Steiner, Allison M. Blum, Dacheng Lin, Rodrigo Nemmen, Jimmy A. Irwin, Daniel R. Wik
Figure caption: Radial surface brightness profiles in the soft (3–7 keV, left-hand panel) and hard (15–20 keV, right-hand panel) bands. NuSTAR data of 3C 264 are shown in blue circles. The Cyg X-1 data, represented by purple circles with much smaller error bars, are normalized to match the surface brightness model of 3C 264. The green and red lines represent the point source model and the background used to fit the 3C 264 data, respectively. The total emission profiles are shown in orange. The very good fitting indicates that both the soft and hard X-ray emissions are unresolved by NuSTAR.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: The virial products (M vir) for different types of Hβ line widths. Solid and open points are for mean and rms spectra, and circles and squares are for FWHM and line velocity dispersion, respectively. Note that the black hole mass can be obtained by multiplying M vir with the virial factor f BLR (see Equation (11)), which depends on the adopted measure of line width (e.g., Ho & Kim 2014).
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: The relationship between BLR size and AGN 5100 Å luminosity. Gray points are from the compilation by Du & Wang (2019) plus the RM campaign by Li et al. (2021). Dotted and dashed lines with shaded bands represent the best fits and scatter for sub- and super-Eddington AGNs from Du et al. (2018; see the text in Section 6.2).
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Same as Figure 11 but for PDS 456 over the whole monitoring period.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: The ratios of virial factors for different measures of the Hβ line width with respect to the Hβ FWHM of the mean spectrum. From left to right are the line dispersion of the mean spectrum, FWHM, and line dispersion of the rms spectrum, respectively.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: HST image decomposition using GALFIT for IC 4329A, Mrk 335, Mrk 509, and Mrk 1239, from top to bottom. The red rectangle in the second panel from left shows the slit positioning and apertures used for spectral extraction. The central region (≤0.″8) of Mrk 1239 is masked due to flux saturation.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Cloud (top) and dust (bottom) mass evolution for a disrupted cloud simulation with a = 0.1 μm dust grains. See Figure 4 for a full description of this figure. The initial cloud and dust masses are 6.2 × 103 M ⊙ and 63 M ⊙, respectively. This cloud exhibits signs of growth, with its total mass increasing slightly before significant cloud material begins to exit the simulation volume. After 53 Myr (5.3 t sp,w), 28% of the initial dust mass is destroyed, mostly in the hot phase.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Resolution study for the destroyed, disrupted, and survived cloud simulations (described in Table 1). All runs use the same initial conditions (except the r cl/64 survived cloud, which was run in a box twice the length as the lower-resolution runs). Note that some box sizes are slightly different than noted in Table 1 (namely, the destroyed and disrupted clouds use ﹩100\times 15\times 15\,{r}_{\mathrm{cl}}^{3}﹩ and ﹩64\times 16\times 16\,{r}_{\mathrm{cl}}^{3}﹩ boxes, respectively), but these box sizes are kept consistent between each resolution. The solid line shows the total amount of dust in the volume, the dotted line shows an estimate of how much dust has left the volume, and the dashed line is the total fraction of dust sputtered. Overall, the total amount of dust sputtered does not change with resolution.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Dust-to-gas ratio of cool-phase gas as a function of distance for a snapshot at ∼20 Myr of a disrupted (blue line) and survived (pink line) cloud. The initial dust-to-gas ratio of each simulation is 0.01. The decrease in dust-to-gas ratio with distance is a reflection of the constant dust mass as the clouds accrete gas from the wind.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Evolution of the dust mass with distance due to sputtering for dust moving at 103 km s−1 in a hot wind. The partially shielded curve represents a continuation of the simulation discussed in Section 4.1, beginning at a distance of r = 0.5 kpc from the base of the outflow. The unshielded curve shows what happens to dust that is never inside of a cloud, and travels from the base of the wind fully exposed to the hot phase. As dust moves outward, the sputtering timescale evolves according to analytic fits to the CGOLS hot-phase profiles. A total of 50% of the initial dust density is sputtered in the partially shielded case. 48% of the initial dust density is sputtered in the unshielded case.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Slice of a survived cloud simulation showing the variation in dust-to-gas ratio throughout the cloud (over a distance of 7.0 kpc). The head of the cloud is at roughly the initial dust-to-gas ratio (0.01), but the cloud becomes less dusty with distance from the head, declining by roughly an order of magnitude. This results from the condensation of the mixed phase, which is composed of dust-rich gas from the cloud and dust-free gas from the hot phase.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Dust mass evolution for the same simulation setup as described in Figure 9, but with a = 0.01 μm dust grains. After 49 Myr (49 t sp,w), 73% of the initial dust mass is destroyed, with a higher fraction of destruction occurring in T < 106 K gas. This is due to the relatively short mixed-phase sputtering time at this grain size—t sp,minmix ∼ 250 kyr. This is comparable to t cool,minmix, so mixed-phase sputtering becomes efficient.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Comparison between drag (solid line) and nonthermal sputtering (dashed line) times for the hot (pink), mixed (orange), and cool (green) phases of outflows for a = 0.1 μm silicate grains.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: The fraction of dust destruction seen for varying grain sizes in survived cloud simulations (where t cool,minmix ≪ t shear, described in Section 4.2). Essentially all sputtering occurs in T < 106 K gas.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: The average cloud x-velocity as a function of time for our survived and disrupted cloud simulations (described in Table 1).
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: An on-disk apparent current sheet on 2012 January 1 (case 1; L. Li et al. 2016a). Panels (a1)–(a3): the SDO/AIA EUV images in 335 Å wavelength. Panels (c1)–(d4): the EM ((c1)–(c4)) and temperature ((d1)–(d4)) maps derived from the DEM analysis method. The red rectangle in panel (a1) outlines the FOV in Figure 2. The red and white dotted lines in panels (a1)–(a2), (c1), (c3), (d1), and (d3) represent two independent atmospheric structures prior to the occurrence of magnetic reconnection, while the purple and cyan ones in panels (a2)–(a3), (c3)–(c4), and (d3)–(d4) denote the newly formed structures after the reconnection. The green arrows in panels (a1)–(a3), (c1)–(c4), and (d1)–(d4) represent the current sheet. The red dotted–dashed line in panel (a2) denotes a slit along the length direction of the current sheet, and the red solid lines represent the slits along the width direction. Panel (b): the length (red solid histogram), width (blue), and aspect ratio (black) of the current sheet. The red and blue dotted histograms represent the error bars of the length and width measurements, respectively. The black solid histogram is fitted with a power-law function of the time-aspect ratio (see the black curve), and the temporal evolution of the aspect ratio follows a power law with exponent 1.05.
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: A limb apparent current sheet on 2017 September 10 (case 3; R. Patel et al. 2020). Panels (a1)–(a3): the SDO/AIA EUV images in 131 Å wavelength. The red dotted–dashed line in panel (a1) denotes a slit along the length direction of the current sheet, and the red solid lines represent the slits along the width direction. The red rectangle in panel (a2) outlines the FOV in Figure 8, and the green arrows represent the current sheet. Panels (b)–(c): the width (b) and the length (c) of the current sheet. The blue arrows in panel (b) denote the thinning processes of the current sheet. The blue and red dotted histograms in panels (b)–(c) represent the error bars of the obtained width and length values, respectively. Panel (d): the aspect ratio of the current sheet (the black solid histogram). The temporal evolution of the aspect ratio is fitted with a power-law function (see the black curve), following a power law with exponent 2.82.
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: Density maps displaying the evolution of the on-disk apparent current sheet in Figure 1. The cyan arrows in panels (a1)–(a5) represent the initial characteristics of the current sheet, and the white ones in panels (a8)–(a12) mark a plasmoid. The white solid curves in panels (a6)–(a10) denote the normalized density variations along the current sheet outlined by the dotted curves in each panel. The eight white balls in panel (a6) are based on the peak positions of the white solid curve and represent the plasmoids.
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: Similar to Figure 1 but for case 2 (on 2019 November 1; T. Ding et al. 2022).
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Ratio of the norm of the radiation stress-energy tensor ﹩{}_{\ \nu }^{\mu }﹩ to the norm of the plasma stress-energy tensor ﹩({T}_{p}{)}_{\ \nu }^{\mu }﹩. The tensors are extracted from a flow field averaged over azimuthal angle ϕ and times greater than 25 ms.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: The Lagrangian derivative in pressure due to change in electron fraction from the emission and absorption of neutrinos. Averaged over time and azimuthal angle ϕ. Left: averaged for times less than 25 ms. Right: averaged for times greater than 25 ms. Note the difference in scales.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Angular distributions of neutrinos for 500 ms snapshot. Crossings no longer exist for these late-time snapshots and the disk becomes fully leptonizing.
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: Similar to Figure 2 but for case 2.
Paper: Magnetic Field of the Quasar 1604+159 from Parsec to Kiloparsec Scale
Authors: Xu-Zhi Hu, Xiaoyu Hong, Wei Zhao, Liang Chen, Wei-Yang Wang, Linhui Wu
Figure caption: Distributions of linear polarization (sticks) and fractional polarization (color) at 8.5 and 22.5 GHz for the observation on 2000 December 1 superimposed on the corresponding total intensity contours. Contours are 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128). The blue arrow indicates the jet direction at the parsec scale. There is a hotspot located on the eastern side (EH), which has been detected in two other VLA observations (Figures 3 and 5). There exists a western counterpart, which is not detected at this epoch due to the limited sensitivity. Distributions of fractional polarization and polarized intensity along a slice across the curved jet indicate the enhancement in the magnetic field at the jet edges.
Paper: Magnetic Field of the Quasar 1604+159 from Parsec to Kiloparsec Scale
Authors: Xu-Zhi Hu, Xiaoyu Hong, Wei Zhao, Liang Chen, Wei-Yang Wang, Linhui Wu
Figure caption: Distributions of RM, RM-corrected EVPA, and spectral index for the observation on 1998 September 21 superimposed on the 1.7 GHz total intensity contours. Contours are 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128). The blue arrow indicates the jet direction at the parsec scale. The bottom-left panel plots a transverse RM gradient, in which the start point “S” is labeled in the RM map.
Paper: Magnetic Field of the Quasar 1604+159 from Parsec to Kiloparsec Scale
Authors: Xu-Zhi Hu, Xiaoyu Hong, Wei Zhao, Liang Chen, Wei-Yang Wang, Linhui Wu
Figure caption: Distributions of linear polarization (sticks) and fractional polarization (color) at 8.5 and 22.5 GHz for the observation on 1999 January 29 superimposed on the corresponding total intensity contours. Contours are 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128). The blue arrow indicates the jet direction at the parsec scale. Two hotspots are located on the eastern and western sides, labeled as “EH” and “WH.” The diffuse emissions around EH at 8.5 GHz come from the eastern lobe, as plotted in Figure 4.
Paper: Magnetic Field of the Quasar 1604+159 from Parsec to Kiloparsec Scale
Authors: Xu-Zhi Hu, Xiaoyu Hong, Wei Zhao, Liang Chen, Wei-Yang Wang, Linhui Wu
Figure caption: Distributions of linear polarization (sticks), fractional polarization (color in upper panel), and total intensity (color in bottom panel with Jy beam−1 unit) at the L band for the observation on 1998 September 21 superimposed on the corresponding total intensity contours. To show the extended emissions, the pixels with values >0.15× peak intensity were replaced with 0.15× peak intensity in the bottom plot. Contours are 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128).