adsabs/AstroCLIMB huggingface dataset:
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: A close-up view of the Swift UVW flux and X-ray hardness ratio from 2020 August to 2021 May, as well as in 2002. The uncertainties of the observed UVW2 flux are too small to be seen in the plotting scale. The 2002 UVW2 flux is obtained with the XMM-Newton Optical Monitor, while the Swift X-ray hardness ratio is simulated based on the best-fit model to this XMM-Newton observation.
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption: Left: Γ vs. ﹩\dot{M}﹩. The solid black line is our best fit. The purple line is the result by Huang et al. (2022). Right: dependence of Γ on ﹩\dot{M}﹩ and F X. The solid line is 1:1. The symbols are the same as in Figure 8.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: Best fit to the observed X-ray data of MR 2251-178 in 2002 and 2020. Transmission of the Galactic absorption (MW), warm absorber (WA), and X-ray obscurer (XO, 2020 only) are shown in the top panels. In the bottom panels, data (colored curved with 1σ uncertainties in gray) and model (black curves) of each instrument are rebinned for clarity. The flux differences in the hard X-ray band are due to the cross-calibration issue between XMM-Newton and NuSTAR.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: The soft X-ray spectra of MR 2251-178 in 2002 (top) and 2020 (bottom). The RGS spectra are rebinned for clarity. The black curves are the total flux, which consists of two warm emitter components (green and pink) and the continuum (blue).
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: XMM-Newton spectra of MR 2251-178 from 2002 May 18 (black) and 2020 December 16 (pink). The 2002 observation used the UVW2, UVM2, UVW1, and V filters, while the 2020 observation used all six optical and UV filters. The apparent lowering of the soft X-ray flux in 2020 is due to the presence of the obscurer.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). III. A Red Quasar with Extremely High Equivalent Widths Showing Powerful Outflows
Authors: Chenxu Liu, Karl Gebhardt, Wolfram Kollatschny, Robin Ciardullo, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Steven L. Finkelstein, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Lindsay House, Donald P. Schneider, Tanya Urrutia, Gregory R. Zeimann
Figure caption: Distributions of the rest-frame EW of the Lyα + N V λ1241 emission. HETDEX AGNs with continuum detection (>1σ) are shown in the red histogram. HETDEX AGNs without continuum detection (<1σ) are shown in the green histogram. SDSS quasars are indicated by purple histogram. The number of SDSS quasars in each bin is divided by 100 for presentation purposes. EW(Lyα+N V),rest of J1150+5048 is marked by the downward triangle.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: The Lyα line profiles. The single-orbit 2020 spectrum is rebinned for clarity. Vertical dotted lines in pink mark the UV warm absorbers. Vertical dashed line in purple marks the new blueshifted (∼−2530 km s−1) narrow absorption line. A weak blueshifted broad absorption trough is observed between ∼−3000 and ∼−10,000  km s−1 accompanied by a forest of narrow absorption lines (the shaded area in light blue).
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: Observed Balmer lines in the Keck (red) and Palomar (green) optical spectra compared to the observed He I* λ10830 line profile (black) after removing the nearby Paγ λ10938 broad emission line. For Hα, we show the line profile from the IRTF spectrum instead since this strong line was saturated in the Keck spectrum. The dashed blue vertical lines mark the Lyα absorption components observed with HST/COS (upper left panel of Figure 9).
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). III. A Red Quasar with Extremely High Equivalent Widths Showing Powerful Outflows
Authors: Chenxu Liu, Karl Gebhardt, Wolfram Kollatschny, Robin Ciardullo, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Steven L. Finkelstein, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Lindsay House, Donald P. Schneider, Tanya Urrutia, Gregory R. Zeimann
Figure caption: The HETDEX spectrum of J1150+5048 at the HETDEX coordinate in Table 1. Black data points with error bars are the observed spectrum shown in the rest frame. The red line is our best fit to the spectrum. The green shaded areas indicate the continuum windows used in the continuum fit. The cyan dashed line is our best-fit continuum model. The four panels in the bottom row are the continuum subtracted local areas of the four emission lines.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: Normalized flux of Lyα as a function of outflow velocity in 2011 (green) and 2020 (red) HST/COS spectra. In the 2020 spectrum, a forest of weak absorption features appears in the blue wing ranging from ∼−2530 to ∼−10,400  km s−1.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: Photoionization modeling of the new narrow absorption feature of Lyα using Cloudy (Ferland et al. 2017). With ﹩\mathrm{log}\xi =1.8﹩ and ﹩{f}_{\mathrm{cov}}^{\mathrm{UV}}={f}_{\mathrm{cov}}^{{\rm{X}}}=0.35﹩, a good fit can be achieved with a hydrogen column density of 3.2 × 1020 cm−2 and a turbulence velocity of 70 km s−1. The lower panel shows the transmission.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: Ionic column densities of the obscurer. This calculation is performed with the hydrogen column density and covering factor of the obscurer given in Table 5 and the incident ionizing SED shown in Figure 4. The pink shaded area marks the X-ray constraints (1σ uncertainty) of the ionization parameter.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: Observed and reconstructed He I* λ10830 line profile after removing the nearby Paγ λ10938 broad emission line. The dashed blue vertical lines mark the Lyα absorption components observed with HST/COS (upper left panel of Figure 9).
Paper: Common Envelope Mass Ejection in Evolved Stars: Modeling the Dust Emission from Post-RGB Stars in the LMC
Authors: Geetanjali Sarkar, Raghvendra Sahai
Figure caption: The circumstellar dust mass (M  d ) of our post-RGB objects is shown (colored horizontal lines) on a plot of theoretically estimated dust masses in the ejecta of common envelope systems vs. initial stellar mass, taken from Figure 2 of Lü et al. (2013). FGB refers to the first red giant branch. FG2006 refers to results by Ferrarotti & Gail (2006), showing the dust masses produced in the dust-driven outflows of AGB stars. M  d  scales in proportion to the thickness of the circumstellar component. Determination of the latter is constrained by the long wavelength limit of our data (24 μm). Our estimated M  d  values may be treated as lower limits to the actual dust mass in the shells.
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption:  P–﹩\dot{P}﹩ diagram for different neutron star classes. The names are shown for radio magnetars (also displayed with a gray circle), low-field magnetars, and long-period pulsars (including GLEAM-X J1627). Light gray lines correspond to constant magnetic fields, while the colored curves assumed magnetic field decay in the crust (see Section 4 for details). Colors refer to the surface dipolar magnetic field strength at the pole.
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption: Radio luminosity vs. rotational power of bright single-peak emission for all pulsar classes and the GLEAM-X J1627’s upper limits. Radio magnetars’ bright single pulses are labeled in green. The gray solid line marks the relation ﹩{L}_{\mathrm{radio}}={\dot{E}}_{\mathrm{rot}}﹩.
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption: From top to bottom: the combined average SALT spectra of G1, G3, and G4 in the range 4500–7000 Å showing absorption features typical of mid/late-type stars. The vertical lines report expected hydrogen Balmer (Hα and H β ) and helium lines (He I and He II). Telluric features are also marked using an encircled cross. The gap around 5000 Å is due to the mosaicked chips of the RSS detector. A residual artifact is present in the spectrum of G3 around the He II line.
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption: From left to right, top to bottom: SEDs of G1, G2, G3 , G4, G5, D1, and D2 adopting different extinction corrections, shown with their best-fitting blackbody models. The open circles report the SEDs without reddening corrections, while the filled triangles and circles report the SEDs corrected for the low and high values of extinctions, A  V , respectively, as reported in the text (see also Section 3.2). The shaded magenta areas comprise the range of blackbody temperatures and extinctions.
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption: The z-band DECAPS image of the field of GLEAM-X J1627. The position of the radio source and its 1σ error circle (with a radius of 2″) are reported. The positions of the five Gaia (G1, G2, G3, G4, G5) and two DECAPS (D1, D2) objects within 4″ are also reported. North is up and east is left.
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption: Upper limits at 3σ confidence level on the X-ray luminosity of GLEAM-X J1627 derived assuming either an absorbed power-law spectrum with Γ = 1–4 (left panel) or an absorbed blackbody spectrum with kT = 0.1–0.9 keV (right panel). The solid curves mark the limits derived assuming a distance of 1.3 kpc, while the shaded areas indicate the range of luminosities that account for the uncertainty in the source distance.
Paper: Polarization Observations of a Split-band Type II Radio Burst from the Solar Corona
Authors: R. Ramesh, C. Kathiravan
Figure caption: GRIP observations of Stokes I and V emission at 80 MHz corresponding to the H  L  and H  U  bands in Figure 1. Note that the Stokes I and V amplitude values are marked on the left and right-hand side ordinate axes, respectively.
Paper: Polarization Observations of a Split-band Type II Radio Burst from the Solar Corona
Authors: R. Ramesh, C. Kathiravan
Figure caption: F–H split-band type II burst observed with the GLOSS on 2021 May 22. The high and low frequency cutoff near ≈80 and 35 MHz in the spectrum are due to the use of low and high pass filters to suppress radio frequency interference above and below the respective frequencies.
Paper: Polarization Observations of a Split-band Type II Radio Burst from the Solar Corona
Authors: R. Ramesh, C. Kathiravan
Figure caption: GRAPH observations of the total intensity emission at 80 MHz during the interval ≈ 03:01–03:03 UT, the same period as the H  L  and H  U  band observations in Figure 2. The circle represents the limb of the Sun’s photosphere. Solar north is straight up and east is to the left in the image. The GRAPH “beam” at 80 MHz is shown near the lower right corner. The peak brightness temperature (T  b ) is ≈ 8.2 × 107 K, and it corresponds to the southern source. A comparison with the Stokes I observations in Figure 2 indicates that the intense (faint) source to the south (north) corresponds to the H  L  (H  U ) emission shown there.
Paper: Polarization Observations of a Split-band Type II Radio Burst from the Solar Corona
Authors: R. Ramesh, C. Kathiravan
Figure caption: Estimates of B at r ≈ 1.6 R ⊙ in the upstream corona ahead of a propagating MHD shock in the solar corona using observations of split-band type II bursts and the density jump across the shock. Red color square symbols represent the B values in both the upstream (r ≈ 1.6 R ⊙) and downstream (r ≈ 1.4 R ⊙) corona (with respect to the associated shock) from the circular polarization measurements in the present work. The blue color line like shows the Dulk & McLean (1978) model for the variation of B with r obtained from observations of different types of solar radio bursts.
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: Annual-mean zonally averaged insolation distribution and surface temperature are shown in (a) and (b). Climatological seasonal march of zonal mean surface temperature in color (K) and the insolation in contours (W/m2) for (c) ϕ = 0°, (d) ϕ  = 23.5°, (e) ϕ = 45°, and (f) ϕ = 60°. The global mean surface temperatures are shown in the upper right on each panel. All cases were run with a low resolution and parameterization for clouds.
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: The luminosity and temperature of 13 known Be+sdO binaries are plotted as open (Be) and filled (sdO) circles, with a line connecting the two components of each binary system. These parameters were estimated from this work and Chojnowski et al. (2018), Schootemeijer et al. (2018), and Wang et al. (2021). Each system is color-coded according to the mass of the Be component, with lighter colors indicating higher mass (maximum of 11.15 M ⊙ and minimum of 6.2 M ⊙). The Regulus system is plotted in a similar fashion with black squares, and κ Dra is plotted with stars, with errors as in Table 7.
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: Climatological seasonal march of zonal mean precipitation in color (mm/day) and the column water vapor in contours (kg/m2) for (a) ϕ = 0°, (b) ϕ  = 23.5°, (c) ϕ = 45°, and (d) ϕ = 60°. All cases were run with a low resolution and parameterization for clouds.
Paper: Critical Mach Numbers for Magnetohydrodynamic Shocks with Accelerated Particles and Waves
Authors: J. Martin Laming
Figure caption: Left: schematic diagram of wave propagation at the oblique shock, in the shock rest frame. Upstream (left), plasma moves toward the shock front with velocity  v  1, carrying with it magnetic field  B  1 at angle θ 1 to  v  1 (or the shock normal). Post-shock, the magnetic field is  B  2 at angle θ 2 to the shock normal, and the flow velocity is  v  2. In the preshock medium, waves are assumed to be parallel propagating along  B  1. Post-shock, the magnetosonic waves refract and travel at an angle θ 2W  to the shock normal. Alfvén waves refract at a slightly different angle, but this plays no role in their reflection and transmission coefficients. Right: contour plot of the first critical fast Mach number in the plasma β–θ 1 plane for ﹩{E}_{\mathrm{CR}}/{\rho }_{1}{v}_{1| | }^{2}=0﹩ (see Figure 4(c) in Edmiston & Kennel 1984).
Paper: Critical Mach Numbers for Magnetohydrodynamic Shocks with Accelerated Particles and Waves
Authors: J. Martin Laming
Figure caption: Contour plots of the first critical fast Mach number in the plasma β - θ 1 plane for ﹩{E}_{\mathrm{CR}}/{\rho }_{1}{v}_{1| | }^{2}=0.025﹩, 0.05, 0.1, and 0.2 are shown in the top left, top right, bottom left, and bottom right panels, respectively.
Paper: Critical Mach Numbers for Magnetohydrodynamic Shocks with Accelerated Particles and Waves
Authors: J. Martin Laming
Figure caption: Contour plots of the first critical fast Mach number in the plasma β - θ 1 plane for ﹩{E}_{\mathrm{CR}}/{\rho }_{1}{v}_{1| | }^{2}=0.025﹩ (left panels) and 0.1 (right panels), showing initially forward-propagating waves only (top panels), initially balanced waves (middle panels), and initially backward-propagating waves only (bottom panels).
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: Time-dependent effects in a synthetic RGS and Arcus spectra of an AGN (SED from Mrk 509) with a warm absorber in absorption. To simulate the data we computed the time-dependent photoionization model 25 ks after a sharp increase in the ionizing luminosity. In red, we show the best fit using a pion component and neglecting the time-dependent effects. The residuals are displayed in the bottom panels. The best fit using two pion components is shown in green.
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: Impact of the ionizing SED on the transmitted spectrum. In the top panel, we compare the X-ray transmission of two plasmas with a different ionizing SED and with the same initial ionizing parameter and density: the black line represents the transmittance for a plasma that does not vary the SED shape; instead, the yellow line shows the transmittance of a gas that sees an increase of the power-law index by 20%. The deviation between the two models is shown in the bottom panel.
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: Time-dependent effects in a synthetic XRISM spectra of an AGN (SED from Mrk 509) with a warm absorber in absorption. To simulate the data, we computed the time-dependent photoionization model 25 ks after a sharp increase in the ionizing luminosity. In red, we show the best fit using a pion component and neglecting the time-dependent effects. The residuals are displayed in the bottom panels. The best fit using two pion components is shown in green.
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: Stokes I and Q/I spectra of SE204-4, SE204-6, SE205-2, and SE206-6, demodulated with a threshold of 1/2I  c  + 1.2 × e × rms for each of the dual beams of SE204-4 and SE204-6, 1/2I  c  + 1/2 × e × rms for each beam of SE205-2 and 1/2I  c  + 1/4 × e × rms for SE206-6.
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: Five sets of Stokes I and their corresponding Q/I profiles drawn from the demodulated Q/I image of SE204-4 shown in Figure 7. The intensity is shown in detector CCD cts. From top to bottom: the 1st point P1; the 6th point P6; the 11th point P11; the 16th point P16’; and the 21st point P21. Note that the horizontal line segments in every I profile outline the demodulation thresholds and hereafter in the following figures, below that the exact demodulation is abandoned and the polarization is set to be zero before the polarization calibration. In some cases, the lines are merged in the continuum and thus become invisible.