adsabs/AstroCLIMB huggingface dataset:
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: All-sky map of our visually inspected area. We show the visually inspected areas of groups (shown in green) and fields (shown in blue) with circles of radius 2.°5 and 1.°0, respectively. We also mark the Virgo and Fornax regions by the red circles of radius 15° and 10°, respectively. The small black circles represent bright (M  K  < −21 mag) galaxies at z < 0.01.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: The g-band magnitude distributions of our dE sample (green) and a subset having radial velocity information (blue). The vertical dashed line represents the magnitude limit of the spectroscopic target selection of the SDSS.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: The g-band mean surface brightness distribution of our sample dEs. The vertical dashed line represents the surface brightness limit that is customarily used to define UDGs.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: Comparison between our g-band magnitude and the Legacy survey’s pipeline-based g-band magnitude. In the top panel, we show a median error in our g-band photometry.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: The CMR of our sample dEs. We show cluster, group, and field dEs with red, green, and blue circles, respectively. The dashed line represents an average CMR measured by Janz & Lisker (2009) for the Virgo Cluster dEs using the SDSS data. The SDSS magnitudes are converted to the Legacy DECaLS filter system according to the transformation formula provided by the Legacy web page. We show a typical error bar for each magnitude bin in black.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: Distribution of nucleated dEs (red circles) and nonnucleated dEs (blue circles) inside the Virgo and Fornax Clusters. Fornax is shown on the left, centering at NGC 1407, and Virgo is shown on the right, centering at M87. The positions of bright member galaxies of clusters are shown by black squares. The black concentric rings represent the annular aperture of 1° width, where we measure the nucleated fraction. The results are shown in the top panels.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: Top: the distribution of sky-projected separation of dEs from the host center. The x-axis is normalized by the assumed viral radius of each cluster, group, and field. Red, blue, and green histograms are for clusters, groups, and fields, respectively. Bottom: phase-space distribution of our spectroscopic dE sample. Red, blue, and green circles are for clusters, groups, and fields, respectively.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: Examples of nonnucleated (top row) and nucleated (bottom row) dEs. All stamp images have an FOV of 1′ × 1′.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: Frequency of bright galaxies around different types of dEs. The first to last rows are for all, field, group, and cluster dEs. The blue (red) histograms represent the number of Sfs (Es) around dEs within the 300 kpc sky-projected radius.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: The luminosity−size relation of early-type galaxies. Data for Es/dEs (gray circles) are from Janz & Lisker (2008). The symbol color represents cluster, group, and field dEs according to Figure 8.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: Redshift distribution of dEs, for which radial velocity information is available. We also highlight the position of two clusters, Virgo and Fornax, by the vertical lines.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: Exemplary dEs of the different classes of dEs according to their morphological feature and color (see text for detail).
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: The g − r color distribution of our sample dEs. The bin positions of the group and field samples are shifted by +0.01 and −0.01 mag, respectively.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: The scaling relations between the structural parameters (R  h  and 〈μ  g 〉) and M  g  of our sample dEs. Green and black circles represent dEs and UDGs, respectively. The thresholds on 〈μ  g 〉 and R  h  that are used to define UDGs are shown by the dashed lines. The red circles with a 1σ standard deviation represent the median values of the distribution.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: We compare dE detection in two groups, NGC 3379 and NGC 3627, with detection of C22, where the circle represents our search area. Giant galaxies are shown in green. C22-identified star-forming (dSf) and non-star-forming (dE C ) dwarf galaxies are shown in blue and red, respectively. Our identified dEs (dE o ) are shown in black. The solid and dashed circles represent our and C22 search areas, respectively.
Paper: An Extensive Catalog of Early-type Dwarf Galaxies in the Local Universe: Morphology and Environment
Authors: Sanjaya Paudel, Suk-Jin Yoon, Jaewon Yoo, Rory Smith, Daya Nidhi Chhatkuli, Rajesh Kumar Bachchan, Binil Aryal, Binod Adhikari, Namuna Adhikari, Amrit Sedain, Sharup Sheikh, Sarashwati Dhital, Ashutosh Giri, Rabin Baral
Figure caption: Top: the nucleated dwarf fraction with respect to magnitude. The black line represents the nucleated dE fraction measured by Sánchez-Janssen et al. (2019) for the Virgo Cluster, and the red line represents a nucleated fraction of our entire dE population. The nucleated fractions of dEs for clusters, groups, and fields are shown with magenta, green, and blue lines, respectively. Bottom: magnitude distribution of nucleated (red histogram) and nonnucleated (blue) dEs.
Paper: The [S II] Spectral Images of the Planetary Nebula NGC 7009. II. Major Axis
Authors: Siek Hyung, Seong-Jae Lee, Masaaki Otsuka
Figure caption: Keck HIRES [S II] 6731 Å 2D spectra, and PV density diagram along the major axis (PA = +77°; 1998 August 15 UT). All the used slit lengths are 14″, and all the exposures are 2 minutes. (a)–(c) The left panels show the nebular image with the 14″ × 0.″862 slit entrance placed along the major axis and the right panels show close-up [S II] 6731 Å 2D spectral flux images in logarithmic scale from the left panel, obtained from the slit entrance placed at the W–SW, CSPN, and E–NE positions along the major axis. West (W–SW) is upward and east (E–NE) is downward; north (N–NW) is left and south (S–SE) is right. (d)–(f): PV density diagrams derived from the [S II] 6716/6731 Å ratio. The white vertical line in (e) indicates V  r  = 0.0 km s−1. The tilted sky blue line is a redefined kinematic baseline of the prolate ellipse. See the text.
Paper: The [S II] Spectral Images of the Planetary Nebula NGC 7009. II. Major Axis
Authors: Siek Hyung, Seong-Jae Lee, Masaaki Otsuka
Figure caption: Schematic diagram for a circular shell (CM3) projected to the sky plane with ψ = 18.°3. The diagram shows that the radius r of point A is greater than the distance from the center to the projected point α 1 along Figure B1’s major axis (the tilted kinematic baseline in Figure 2): r A > ﹩\overline{{\rm{o}}-{\alpha }_{1}}﹩                       ﹩\gt \,\overline{{\rm{o}}-{\alpha }_{2}}﹩. A(x, y): the coordinates of A on an imaginary CM3 circle with radius r A, where y = y 1 − x · tan(ϕ A) and A(x, y) = A(r A, ϕ A).
Paper: The [S II] Spectral Images of the Planetary Nebula NGC 7009. II. Major Axis
Authors: Siek Hyung, Seong-Jae Lee, Masaaki Otsuka
Figure caption: Schematic diagram for a prolate ellipse (EM2) projected to the sky plane with ψ = 18.°3. Points p(﹩x^{\prime} ,y^{\prime} ﹩) and β(x, y) are on EM2. ﹩\overline{{\rm{o}}-{\beta }_{s}}﹩ = 5.″5 (Figure 2); ﹩\overline{{\rm{o}}-{\beta }_{1}}﹩ = 5.″8; and ﹩\overline{{\beta }_{1}-{\beta }_{2}}﹩ = ﹩x^{\prime} \cdot ﹩ tan(ψ), where a point (x, y) is on EM2 and y = ﹩\overline{{\rm{o}}-{\beta }_{1}}﹩. β(x, y): y = ﹩y^{\prime} ﹩ – ﹩\overline{{\beta }_{1}-{\beta }_{2}}﹩. See Table B1.
Paper: The [S II] Spectral Images of the Planetary Nebula NGC 7009. II. Major Axis
Authors: Siek Hyung, Seong-Jae Lee, Masaaki Otsuka
Figure caption: Expansion velocity and the line-of-sight component. (a) Expansion velocity vs. latitude (V                      ﹩{}_{\exp }﹩ and ϕ  β ). (b) Expansion velocity vs. radial velocity along the line of sight (V los and ﹩{\phi }_{\beta }^{\prime} ﹩). (c) Figure 2(d) is rotated and reproduced relative to the new kinematic center line or the major axis.
Paper: The [S II] Spectral Images of the Planetary Nebula NGC 7009. II. Major Axis
Authors: Siek Hyung, Seong-Jae Lee, Masaaki Otsuka
Figure caption: Expansion velocity in a spherical shell. (a) Expansion velocity vs. latitude (ϕ, or 90° − E). (b) Expansion velocity vs. radial velocity along the line of sight (﹩\phi {{\prime} }_{{\rm{A}}}﹩). A solid circle: an imaginary circle drawn by the median value of the knot A and D distances from the center (dashed arc). (c) The projections of two points α and α 1 on the sky plane and their line-of-sight components. Two imaginary circles show that A’s radius (r) depends on A’s position along the line of sight. Thus, the radius r of A determines the latitude of A and the value of the expansion velocity ﹩{V}_{\exp }﹩. CM3's predicted line-of-sight velocity for r should match the observed (negative) radial velocity. Improper selection of r can cause the computational model to yield positive line-of-sight values for A. Therefore, the observed radial velocity becomes a constraint. See the text.
Paper: The [S II] Spectral Images of the Planetary Nebula NGC 7009. II. Major Axis
Authors: Siek Hyung, Seong-Jae Lee, Masaaki Otsuka
Figure caption: HST image of NGC 7009 and Keck HIRES slit direction on the nebular image. The HST WFPC2 image with the F658N filter shows the main shell, outer shell, and caps/ansae (NASA/ESO). The 14″ × 0.″862 slit entrance was placed at the W–SW, the center, and the E–NE areas along the major axis (PA = +77°). See Table 1.
Paper: The [S II] Spectral Images of the Planetary Nebula NGC 7009. II. Major Axis
Authors: Siek Hyung, Seong-Jae Lee, Masaaki Otsuka
Figure caption: Schematic diagram of the main shell, four knots, and a hot bubble (FLIERs). The projection angle of the major axis onto the sky plane is ψ ≃ 18.°3. The four knots expand along nearly the same axis, ∣ϕ∣ ≃ 35° (± 3°), relative to the major axis. The approximate knot velocity is given in parentheses. See Tables 2–4 for the densities and expansion velocities.
Paper: The [S II] Spectral Images of the Planetary Nebula NGC 7009. II. Major Axis
Authors: Siek Hyung, Seong-Jae Lee, Masaaki Otsuka
Figure caption: Prolate ellipse (EM1).
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Isothermal temperatures in the east and west quiescent streamer regions covered by the AIR-Spec slits. The top two panels show temperatures obtained from simultaneous (a) EIS and (b) AIA observations. The bottom two panels show temperatures obtained from simultaneous (c) AIR-Spec and (d) AIA observations.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Predicted and measured radiance of the main four AIR-Spec lines above the east and west limbs. The hotter S XI lines are stronger above the east limb, while the cooler Fe IX line is stronger above the west limb. Predictions with (solid line) and without (dashed line) PE were made using the quiescent streamer density model of Del Zanna et al. (2018) and an isothermal temperature of 1.3 MK. This model fits the west region best but does not represent well the east region.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Electron densities on the east and west limbs during the 2019 total eclipse. The left panels compare densities obtained from EIS and AIR-Spec without correcting for LOS effects. The right panels compare radial density measurements obtained from AIR-Spec and PolarCam with the radial density model in Del Zanna et al. (2018).
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Overlay of temperatures from EIS, AIR-Spec, and AIA observations in the east (top) and west (bottom). For clarity, the data from Figure 7 have been smoothed before plotting.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: The DEMs for the off-limb west and east regions obtained from Hinode EIS. The points are plotted at the temperature ﹩{T}_{\max }﹩ of maximum emissivity and at the theoretical vs. observed intensity ratio multiplied by the DEM value. The wavelength (Å) and ions of a few key lines are shown.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Narrowband images of the solar corona during the 2019 total eclipse in Fe X 637.4 nm, Fe XI 789.2 nm, Fe XIII 1074.7 nm, and Fe XIV 530.3 nm (private communication S. Habbal to J. Samra, image credit S. Habbal and M. Druckmüller). The AIR-Spec slits are overlaid in green.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: False-color images of the solar corona during the 2019 total eclipse in three SDO AIA channels. The bottom right image is a composite obtained from AIA 171 Å (green) and 211 Å (red). The AIR-Spec slits and EIS FOVs are shown in white.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Electron densities obtained from the HAO PolarCam during the 2019 total eclipse. The AIR-Spec slits and EIS FOV are overlaid.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Measured and predicted AIA count rates in the west region. Symbols indicate the measured count rates. Solid lines show the predicted count rates using a spherical symmetry model, photospheric abundances, and assuming an isothermal and constant temperature of 1.3 MK. Dashed lines indicate the predicted signal increased by a factor of four. Dotted–dashed lines show the values with the 1.2 MK isothermal model.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Fraction of line intensity contributed by each 0.025 R ⊙ along the LOS. Each curve sums to 1 along the “LOS Distance” coordinate. The 1.92 μm line has a smaller contribution from the POS than the 1.39 μm line, resulting in a lower line ratio (and higher density) when only the POS intensity is taken into account instead of the entire LOS integration.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Hinode EIS spectra for the off-limb observation above the east and west limbs (120 s, 2″ slit), around 1.09 R ⊙. The dashed lines are the scaled ground-calibration effective area, to show why spectral lines in the middle of the two SW and LW detectors are stronger.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Contribution functions of the main AIR-Spec lines, calculated with PE at 1.1 R ⊙.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Density as a function of S XI 1.92 μm/1.39 μm line ratio and distance from Sun center.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Results of the analysis to obtain the EIS off-limb pointing in the east and west, by comparing the predicted AIA signal with the observed one.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Emissivity ratios of a selection of EIS lines for the off-limb QS observation of 2019 June 28.
Paper: Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization
Authors: Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera
Figure caption: Results of the analysis to obtain the EIS SW radiometric calibration relative to AIA 193 Å.