adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamical Masses of the Primary Be Star and Secondary sdB Star in the Single-lined Binary κ Dra (B6 IIIe)
Authors: Robert Klement, Dietrich Baade, Thomas Rivinius, Douglas R. Gies, Luqian Wang, Jonathan Labadie-Bartz, Pedro Ticiani dos Santos, John D. Monnier, Alex C. Carciofi, Antoine Mérand, Narsireddy Anugu, Gail H. Schaefer, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Stefan Kraus, Benjamin R. Setterholm, Aaron Labdon
Figure caption: Relative astrometric orbit for the secondary component of κ Dra. The measured positions are shown as error ellipses indicating ±5σ uncertainties (red for MIRC(-X) and green for MYSTIC) annotated with (HJD−2,400,000.5) dates. The corresponding points on the calculated orbit appear as crosses. The UD of the central star (including any contribution from the disk) measured in 2021 in the K band (0.405 mas) is shown as a cyan filled circle.
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Overview of B-field structures (red segments) in the W51 e2/e8 region with resolutions from about θ ∼3″ to 0.″1, covering scales from about 0.5 pc to 540 au. Contours are dust continuum. Panels from left to right display the distinct regimes as discussed in Section 5.1: envelope-to-core scale, global-collapsing-core scale, local-collapsing-core scale, and accreting-dust-lane scale. In panel (a) contours are 3, 6, 10, 20, 30, 40, … × σ, where 1σ is 27 mJy beam−1 with θ ∼ 2.″7 × 2.″0 at a wavelength λ around 1.3 mm. Contours are 3, 6, 10, 20, 35, 50, 65, 80, 95, … × σ, where 1σ is 75 mJy beam−1 with θ ∼ 2.″13 × 1.″88 and λ ∼ 0.87 mm in panel (b), 60 mJy beam−1 with θ ∼ 0.″7 × 0.″6 and λ ∼ 0.87 mm in panels (c) and (d), 6 mJy beam−1 with θ ∼ 0.″28 × 0.″26 and λ ∼ 1.3 mm in panels (e) and (f), and 1.2 mJy beam−1 with θ ∼ 0.″11 × 0.″10 and λ ∼ 1.3 mm in panels (g) and (h). Panels (b) to (f) are adapted from Koch et al. (2018).
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Local gravitational vector fields  g  loc for W51 e2 (left panel) and e8 (right panel) overlaid on dust continuum contours (blue). Vectors are displayed with a uniform length, giving the direction but not the absolute magnitude of local gravity. Vectors are selectively shown for the locations where polarized emission is detected and displayed at half of the synthesized beam resolution.
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Illustration of the difference between an isolated collapse (right side) and a collapse embedded in a dust lane (left side). The black circles symbolize spherical test volumes to initiate a collapse in the presence of a magnetic field (red lines). The local gravitational field,  g  loc, is shown with black arrows. In the case of the isolated collapse, this vector field points toward the center of the sphere, and the orientation of the magnetic field with respect to this vector field is irrelevant because  g  loc is azimuthally symmetric. For the embedded collapse,  g  loc is the result of the surrounding mass distribution. Illustrated is a typical situation as observed in Figure 3, where the local gravitational field along a filamentary dust lane is directed toward the dominating center of mass (in this case toward the right side). Generally, the individual vectors of  g  loc vary in length (i.e., strength of gravitational pull) and direction. The gravitational pull necessary for an embedded collapse, F loc,c, is shown with the blue dashed vectors along four symbolic directions (front, upper index “f;” back, upper index “b;” side, upper index “s”). Unlike for the isolated case, the relative orientation between field lines and  g  loc is pivotal because  g  loc is not azimuthally symmetric. As a consequence, the fraction and magnitude of  g  loc that is directed toward overcoming the field tension depends on this relative orientation. In particular, for the illustrated configuration, the net available gravitational pull from the sides, ﹩{F}_{\mathrm{loc},{\rm{c}}}^{{\rm{s}}}﹩, is very small if  g  loc and the magnetic field are prevailingly collinear.
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Identical to Figure 1 but for W51 e8.
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Overview of diagnostic tools in the W51 e2/e8 region. From left to right: on the envelope-to-core scale the local magnetic field dispersion can pick out the location and direction where a global collapse will start to happen (zones with larger dispersion values); on the global-collapsing-core scale, the small values of the magnetic field tension-to-gravity force ratio Σ B  across the core indicate that e2 as an entity can globally collapse (upper panel), and the measured magnetic field strength map reveals a clearly growing strength toward the center (lower panel); on the local-collapsing-core scale, the ﹩\sin \omega ﹩ measure locates regions where gravity is unobstructed (small values) and where the B-field can maximally slow down gravity (values close to one) toward locally collapsing smaller cores; on the accreting-dust-lane scale (rightmost panels), ridges formed by the locally converging gravitational field (gray arrows) appear in areas labeled as dust lanes in Figures 1 and 2, which typically also coincide with small angles ω (color scale). Low ﹩\sin \omega ﹩ values on the local-collapsing-core scale are signposts of the appearance of dust lanes at higher resolutions. Panels in the first three columns are adapted from Koch et al. (2012a, 2018).
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Identical to Figure 3 but with the gravitational vector field  g  loc oversampled to emphasize the gravitational local convergence toward ridges, before merging into local mass centers. These ridges form a gravitational skeleton (visible as thicker black zones) and are suggestive of gravitationally driven accretion regions and channels. This skeleton largely falls onto the dust lanes labeled in Figures 1 and 2.
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Local magnetic field strength maps (bottom row) derived from the stability and collapse criterion given in Equation (2). Separately displayed are the measurable input parameters ﹩\sin \omega ﹩ (top row) and ∣ g  loc∣ (middle row; arbitrary units) for W51 e2 (left column) and e8 (right column).
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Illustration of relevant angles. Angle ω measures the deviation between the magnetic field orientation (in the case of submillimeter dust polarization emission rotated by 90° from the originally detected polarization orientation) and the direction of local gravity  g  loc. Vector  n   B  is the unity vector perpendicular to a measured B-field orientation along the direction of the field tension force. Angle δ is the angle between a magnetic field orientation and the intensity gradient orientation.
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Visualization of the evolving roles of the magnetic field over the scales presented in Figures 8 and 9. Visualized are streamlines based on the detected magnetic field morphologies in Figure 8 using a line convolution algorithm for vector fields (e.g., Cabral & Leedom 1993). From left to right are envelope-to-core scale (first and second), global-collapsing-core scale (third), local-collapsing-core scale (forth), and accreting-dust-lane scale (fifth). No visualization is shown in black patches with too sparse sampling in the original data, which does not allow us to construct a connected convolution.
Paper: Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Mason Ng, Ronald A. Remillard, James F. Steiner, Deepto Chakrabarty, Dheeraj R. Pasham
Figure caption: Spectral evolution of NGC 300 ULX-1 with an absorbed power-law model as a function of time (MJD), using 1 yr of NICER observations with the contribution from X-1 accounted for (details in text). (a) Power-law index Γ. (b) Power-law normalization, in units of 10−4 photons/keV/cm2 at 1 keV. (c) Ratio of the C-statistic to the number of degrees of freedom (d.o.f.). (d) 0.4–4.0 keV absorbed flux in erg/s/cm2.
Paper: Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Mason Ng, Ronald A. Remillard, James F. Steiner, Deepto Chakrabarty, Dheeraj R. Pasham
Figure caption: Integrated image of the NGC 300 field from Swift/XRT observations. The image was generated on SAOImageDS9 and smoothed with a Gaussian kernel with radius 3. Events of X-1 (green; left) and ULX-1 (yellow; right) were taken from extraction regions 30″ and 35″ in radii, respectively. We used a nearby 120″ region for the background of both sources (magenta). The NICER field of view (30 arcmin2; white) is also shown for reference, centered on NGC 300 ULX-1. The best known source position for NGC 300 X-1 is α J2000 = 00h55m10.ˢ00 and ﹩{\delta }_{{\rm{J}}2000}=-37^\circ 42^{\prime} 12\buildrel{\prime\prime}\over{.} 2﹩ (Binder et al. 2011a), and for NGC 300 ULX-1 it is α J2000 = 00h55m04.ˢ85 and ﹩{\delta }_{{\rm{J}}2000}=-37^\circ 41^{\prime} 43\buildrel{\prime\prime}\over{.} 5﹩ (Binder et al. 2011b).
Paper: Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Mason Ng, Ronald A. Remillard, James F. Steiner, Deepto Chakrabarty, Dheeraj R. Pasham
Figure caption: Hardness–intensity diagram of ULX-1 with NICER data, where the intensity (0.4–12.0 keV) is plotted as a function of the soft color ((1.0–2.0 keV)/(0.4–1.0 keV)). The intensity is derived using the 5 day averaged spectra. The count rates in each energy band have been corrected for the contributions of the particle and X-1 background (see text for details). There is a clear correlation between the broadband intensity and soft color, where the dimming of the source is accompanied by a steeper spectrum in soft X-rays (i.e., 0.4–2.0 keV).
Paper: Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Mason Ng, Ronald A. Remillard, James F. Steiner, Deepto Chakrabarty, Dheeraj R. Pasham
Figure caption: Folded exposure-corrected 0.3–10.0 keV orbital profile with P orb = 32.788 ± 0.007 h and T 0 = MJD 57493.476 ± 0.017 (TDB). The orbital profile has been shifted so that phase 0 corresponds to the eclipse minimum. The orbital profile for the black hole + Wolf–Rayet binary NGC 300 X-1 was constructed using events from the Swift/XRT observations that spanned a time interval that included XMM-Newton and NICER data. Two orbital cycles are plotted for clarity.
Paper: Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Mason Ng, Ronald A. Remillard, James F. Steiner, Deepto Chakrabarty, Dheeraj R. Pasham
Figure caption: The 0.4–4.0 keV spectra corresponding to the brighter state of ULX-1 (MJD 58249) and the fainter state (MJD 58489). The absorption column density was fixed at n  H  = 0.11 × 1022 cm−2, and the best-fit power-law indices were ﹩{\rm{\Gamma }}={1.69}_{-0.09}^{+0.09}﹩ and ﹩{\rm{\Gamma }}={4.0}_{-0.5}^{+0.7}﹩ for the brighter and fainter states, respectively.
Paper: Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Mason Ng, Ronald A. Remillard, James F. Steiner, Deepto Chakrabarty, Dheeraj R. Pasham
Figure caption: 5 day averaged 0.4–12.0 keV light curve of ULX-1 over the span of 12 months of NICER monitoring (2018 May 1 to 2019 May 2), where the particle and X-1 background contributions have been subtracted. The flux from ULX-1 broadly varied by a factor of 25 throughout the span of the NICER observations.
Paper: Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Mason Ng, Ronald A. Remillard, James F. Steiner, Deepto Chakrabarty, Dheeraj R. Pasham
Figure caption: 0.2–10.0 keV Swift/XRT background-subtracted and exposure-corrected light curve of NGC 300 X-1 (red) and NGC 300 ULX-1 (blue), binned with 1 hr time bins. The gray shaded regions indicate the time span of the XMM-Newton data (left) and NICER data (right) used in this work.
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: Step-up light-curve case: the light curve is shown in the top panel. The ionizing flux increases by a factor of 10 in 0.01 s. In the panels below we show the time-dependent evolution of the concentrations relative to the hydrogen of O VIII, O IX, Fe XIX, and Fe XX for different gas densities and compared it with the ionic concentrations for a plasma in photoionization equilibrium (black stars).
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: Flaring light-curve case. The light curve is shown in the top panel. The ionizing flux symmetrically increases and decreases by a factor of 10 in 3 ks. The high state phase between the dashed gray vertical lines is 2 ks long. The onset and the end of the flare are marked by two dashed red vertical lines. In the middle and bottom panels, we show the time-dependent evolution of the concentrations relative to the hydrogen of O VIII, O IX, Fe XIX, and Fe XX for different gas densities and compared it with the ionic concentrations for a plasma in photoionization equilibrium (black stars).
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: Comparison between the X-ray transmission (line and continuum absorption) of a plasma in photoionization equilibrium (black solid line) and in non-photoionization equilibrium (magenta solid line). We assume a plasma with a density of n H = 106 cm−3 and an initial ionization parameter of ﹩\mathrm{log}\xi =1.8﹩. We show a comparison at three different epochs: from top to bottom 9, 18, 50, and 75 ks, which correspond to the black dashed lines in the light-curve panel on the right. In the top panel, we also plot the initially transmitted spectrum (black dotted line), right before the onset of the flare.
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: Step-down light-curve case: the light curve is shown in the top panel. The ionizing flux drops by a factor of 10 in 0.01 s. In the panels below, we show the time-dependent evolution of the concentration relative to the hydrogen of O VIII, O IX, Fe XIX, and Fe XX for different gas densities and compared with the ionic concentrations for a plasma in photoionization equilibrium (black stars).
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: X-ray transmission of an absorber assuming different densities (105 cm−3 in red, 107 cm−3 in turquoise, and 109 cm−3 in orange) and initial ionization parameters (﹩\mathrm{log}\xi =0.5﹩ top panel and ﹩\mathrm{log}\xi =1.8﹩ bottom panel). We extracted all the spectra at the peak of the flaring light curve (t = 9 ks, see Figure 9). In both panels, we overplot the initially transmitted spectrum (t  =  0, black dotted line) and the spectrum of a plasma in photoionization equilibrium with the ionizing source at t = 9 ks (black solid line).
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: Step-up light-curve case: the first two panels show, respectively, the time-dependent evolution of the electron temperature and the heating and cooling (solid and dashed lines) rates for a grid of density values. In the third panel, we compare the shape of the heating curves dividing them by their dependency on the gas density. The bottom panel illustrates the contribution of the main heating and cooling processes for a plasma with n H = 107 cm−3.
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: Step-down light-curve case: the first two panels show, respectively, the time-dependent evolution of the electron temperature and the heating and cooling (solid and dashed lines) rates for a grid of density values. In the third panel, we compare the shape of the cooling curves dividing them by their dependency on the gas density. The bottom panel illustrates the contribution of the main heating and cooling processes for a plasma with n H = 107 cm−3.
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: Flaring test case: the first two panels show, respectively, the time-dependent evolution of the electron temperature and the heating and cooling (solid and dashed lines) rates for a grid of density values. In the bottom panel, we display the contribution of the main heating and cooling processes for a plasma with density n H = 107 cm−3.
Paper: TPHO: A Time-dependent Photoionization Model for AGN Outflows 
Authors: Daniele Rogantini, Missagh Mehdipour, Jelle Kaastra, Elisa Costantini, Anna Juráňová, Erin Kara
Figure caption: Comparison between the step-up and step-down scenarios. In the top panel, we show the evolution of the O VIII concentration as a function of n H × t. In the same rest frame, the evolution of the plasma temperature is illustrated in the bottom panel.
Paper: Complexity of the Upper Solar Atmosphere Revealed from Spectropolarimetry during a Solar Eclipse
Authors: Z. Q. Qu, L. Chang, G. T. Dun, Z. Xu, X. M. Cheng, L. H. Deng, X. Y. Zhang, Y. H. Jin
Figure caption: Raw data images of polarimetric samples. From top to bottom: SE90-1 acquired in the quiet Sun region at the solar disk center before the eclipse, used for spectral line identification and polarimetric zero-level calibration; SE204-4, acquired about 1 minute before the totality; SE204-6, acquired about 11 s later than SE204-4; SE205-2, obtained closest to the totality; SE206-6, acquired during the totality. The light beams at the IFU slit end with numbers attached with letters on the right column correspond to the fiber code specified on the bottom right panel of Figure 1, and the two spectra with the same number but different letters are yielded from the same spatial volume in the Sun and form a couple with opposite polarimetric states produced by the polarizing beam splitter. The wavelengths of typical lines are indicated on the bottom in units of nanometers while the corresponding element symbols and ionization states of the producers are labeled on the top.
Paper: Complexity of the Upper Solar Atmosphere Revealed from Spectropolarimetry during a Solar Eclipse
Authors: Z. Q. Qu, L. Chang, G. T. Dun, Z. Xu, X. M. Cheng, L. H. Deng, X. Y. Zhang, Y. H. Jin
Figure caption: Approximate locations of the FOVs of the polarimetric samples analyzed in the present paper, directional indicator and the alignment configuration of the lenslet-coupled fiber array as the head of the IFU. Top panels: the bright sickles are the solar crescents formed by lunar occultation. The artificial white squares, not to scale, superposed in the monitoring images indicate the approximately estimated positions of FOVs of the sample acquisitions. The serial SE204 frames are labeled on the top-left panel where the FOV of SE204-4 was higher than that of SE204-6, and SE205-2 was acquired below SE206-6 in the top right panel. Note that the crescent disappeared when SE206 set was acquired during the totality. Bottom left panel: the directional indicator. Bottom right panel: the coded 5 × 5 array indicating the alignment configuration of the lenslets thus their following optically coupled fibers (correspondingly the spatial volumes) forming the pair of the heads of the IFU. They are related to the numbers plotted in the rightmost columns in Figure 2.
Paper: Complexity of the Upper Solar Atmosphere Revealed from Spectropolarimetry during a Solar Eclipse
Authors: Z. Q. Qu, L. Chang, G. T. Dun, Z. Xu, X. M. Cheng, L. H. Deng, X. Y. Zhang, Y. H. Jin
Figure caption: Comparison of Q/I spectra of SE90-1, acquired in the quiet Sun region at the disk center, demodulated respectively from the direct DBP, the five RPOS methods mentioned in the text. The top panel shows the Stokes I spectral image and the other panels the Q/I spectral images. It is easy to see the false signals showing spectral traces in the Q/I image from the DBP demodulation. This specifies that it cannot be used in the measurement of a weak polarization signal. Evidently, the polarimetric backgrounds from RPOS2, RPOS4, and RPOS5 are cleaner than the others.
Paper: Complexity of the Upper Solar Atmosphere Revealed from Spectropolarimetry during a Solar Eclipse
Authors: Z. Q. Qu, L. Chang, G. T. Dun, Z. Xu, X. M. Cheng, L. H. Deng, X. Y. Zhang, Y. H. Jin
Figure caption:  Q/I profiles drawn from the demodulated Q/I images of the previous figure at the 11th point, P11, obtained from, respectively, the DBP, RPOS1, RPOS2, RPOS3, RPOS4, and RPOS5 methods shown from top to bottom. It is outstanding that the difference among these RPOS-deduced profiles mainly locates at the amplitudes and polarimetric zero levels, and their dispersion distributions differ considerably from the DBP.