adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining the Baryon Content of Cosmic Filaments Using Localized Fast Radio Bursts and DESI Imaging Data
Authors: Jian-Feng Mo, Weishan Zhu, Qi-Rui Yang, Yi Zheng, Long-Long Feng
Figure caption: Top: Distributions of DMobs (left) and DMobs–DMMW,ISM (right) and redshifts for 37 well-localized FRBs in the DESI area, divided into “Pass” (circles) and “NoPass” (yellow triangles) groups. Circle color and size indicate the number of intersected filaments. Bottom Left: DMIGM versus redshift for the same FRBs. Dashed lines show best-fit linear trends for each group; error bars represent uncertainties of ∼60 pc cm−3. Bottom right: same as the left, but with filament contributions subtracted: DMIGM,Pass-corr = DMIGM,Pass–DMfila (open circles), using central gas overdensity in filaments δ0 = 20.78. The black dashed line shows the corresponding linear fit.
Paper: Constraining the Baryon Content of Cosmic Filaments Using Localized Fast Radio Bursts and DESI Imaging Data
Authors: Jian-Feng Mo, Weishan Zhu, Qi-Rui Yang, Yi Zheng, Long-Long Feng
Figure caption: Top: the sky area (blue region) in the DESI Legacy Imaging Surveys and positions of localized FRBs (red pentagrams). Middle: filaments and galaxies at z = 0–0.05 across the northern sky. Red lines show filament skeletons identified by DisPerSE with nsig=3 and nsig=5 thresholds; green shading indicates galaxy density. Bottom: red lines show filament counts for nsig=3 (dashed) and nsig=5 (solid); blue line shows galaxy counts per redshift bin.
Paper: Constraining the Baryon Content of Cosmic Filaments Using Localized Fast Radio Bursts and DESI Imaging Data
Authors: Jian-Feng Mo, Weishan Zhu, Qi-Rui Yang, Yi Zheng, Long-Long Feng
Figure caption: Upper: example of an FRB intersecting a filament in 2D. The solid green line marks the filament spine, and “d” indicates its angular width. Bottom: 3D illustration of an FRB-filament intersection. The black dashed line shows the filament’s skeleton, the cyan cylinder marks its region with radius Rfila, the blue line is the sightlines to FRB, and the red segment indicates the intersecting path.
Paper: Different Origins of Nucleated and Nonnucleated Dwarf Elliptical Galaxies: Identified by Deep Learning
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Daya Nidhi Chhatkuli, Woong-Bae G. Zee, Jaewon Yoo, Binod Adhikari
Figure caption: Comparison of our dE identification with that of the NGVS in the core region of the Virgo cluster. NGVS dEs are represented by filled circles, color-coded by magnitude as indicated in the legend, while our identified dEs are marked with black crosses. Cross marks that do not overlap with filled circles represent additional dEs that were not identified by the NGVS. The inset shows the recovery fraction of dEs as a function of brightness, illustrating detection efficiency across different luminosities.
Paper: Different Origins of Nucleated and Nonnucleated Dwarf Elliptical Galaxies: Identified by Deep Learning
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Daya Nidhi Chhatkuli, Woong-Bae G. Zee, Jaewon Yoo, Binod Adhikari
Figure caption: The luminosity−size relation of early-type galaxies, including both dEs and massive early-type galaxies. Our identified Virgo cluster dEs are shown in red, while a reference sample from I. Misgeld & M. Hilker (2011) is displayed in light gray. The black error bar represents the 1σ scatter of the reference sample in 1 magnitude bins.
Paper: Different Origins of Nucleated and Nonnucleated Dwarf Elliptical Galaxies: Identified by Deep Learning
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Daya Nidhi Chhatkuli, Woong-Bae G. Zee, Jaewon Yoo, Binod Adhikari
Figure caption: The commutative recovery fraction (100 −False −ve) of our dE detection model compared to the NGVS catalog in the core region of the Virgo cluster. For dEs brighter than mg < 20 mag, our model achieves a recovery fraction of 81%, with an overall false positive rate of 15%. The upper panel displays the cumulative distribution of dEs as a function of magnitude used in this comparison.
Paper: Different Origins of Nucleated and Nonnucleated Dwarf Elliptical Galaxies: Identified by Deep Learning
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Daya Nidhi Chhatkuli, Woong-Bae G. Zee, Jaewon Yoo, Binod Adhikari
Figure caption: The galaxy distribution maps are generated using 2D Gaussian kernel density estimation (KDE), following the same method as in Figure 4. We give the K-L divergence score for both nucleated and non-nucleated dEs at the bottom of each panel, comparing with that of massive galaxies.
Paper: Different Origins of Nucleated and Nonnucleated Dwarf Elliptical Galaxies: Identified by Deep Learning
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Daya Nidhi Chhatkuli, Woong-Bae G. Zee, Jaewon Yoo, Binod Adhikari
Figure caption: The two-point angular cross-correlation functions are shown for nucleated dEs with massive galaxies (red) and nonnucleated dEs with massive galaxies (blue). Error bars are derived from jackknifed subsamples.
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: The dynamic spectra of the variability of the 6.7 GHz methanol maser lines toward the targets as monitored using the 32 m Torun dish. The epochs corresponding to each observation are marked by the small ticks on the lower x-axes of all figures.
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: The SED plots with the spectral index α fitted and marked by the dashed lines. The vertical gray lines correspond to C- and K-band ranges. The lower limits of the flux densities are marked by the downward-pointing filled triangles.
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: The images of radio-continuum emission at 6 and 22 GHz created homogenously for the SED analysis. The contours in panels (a), (b), (d)-(f) are the same as in panels (a) in Figures 1–6, in a case of panel (c), K-band data 1σ is marked. A synthesized beam size of 0﹩\mathop{.}\limits{^{\prime\prime} }﹩30 × 0﹩\mathop{.}\limits{^{\prime\prime} }﹩30 (marked by a gray circle) and a pixel size of 0﹩\mathop{.}\limits{^{\prime\prime} }﹩06 were used for all images at the C and K bands. The integrated fluxes at both transitions are listed.
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: Dependences of radio luminosity of the methanol ringlike sources on the bolometric (top), methanol (middle), and water maser luminosities (bottom). The gray dot corresponds to the most circular target G23.657−00.127. The dotted lines refer to fits by A. Sanna et al. (2018, their Figure 5), and their parameters are also listed in the top left corners.
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: Similar to Figure 1 but for G31.047+00.356: (a) The contours of the K-band emission correspond to 3σ.
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: Similar to Figure 1 but for G30.400−00.296: (a) The contours of the K-band emission correspond to 3σ, 7σ, 11σ, and 13σ.
Paper: The ALMA-QUARKS Survey: Evidence of a Candidate High-mass Prestellar Core Aside a Bright-rimmed Cloud IRAS 18290-0924
Authors: Dongting Yang, Hong-Li Liu, Sheng-li Qin, Tie Liu, Anandmayee Tej, Siju Zhang, Xunchuan Liu, Fengwei Xu, Guido Garay, Lei Zhu, Patricio Sanhueza, Xiaofeng Mai, Wenyu Jiao, Paul F. Goldsmith, Sami Dib, Pablo García, Di Li, Jinhua He, A. Y. Yang, Prasanta Gorai, Suinan Zhang, Yankun Zhang, Jianjun Zhou, Mika Juvela, James O. Chibueze, Chang Won Lee, Jihye Hwang, Leonardo Bronfman, Xindi Tang, Archana Soam, Tapas Baug, Yichen Zhang, Swagat Ranjan Das, L. K. Dewangan, L. Viktor Tóth
Figure caption: QUARKS 1.3 mm dust continuum image (color scale) overlaid with ATOMS 3 mm dust continuum emission (in gray dashed contours, identical to those in Figure 1). The black contours are at levels of [3, 6, 12, 24, 48] × σ1.3 mm, with σ1.3 mm ∼  0.14 mJy beam−1. The blue ellipses correspond to the FWHM sizes of the C2 core estimated from the ATOMS 3 mm image using the task CASA imfit. The synthesized beam sizes of the QUARKS and ATOMS survey are shown in the left and right bottom (panel (a)), respectively. The 0.01 pc scale bar is shown in the upper right corner. Panel (a): CO (2–1) outflow is overlaid on the QUARKS 1.3 mm dust continuum map. The blue and red contour levels are [3, 6, 12, 24, 48] × σco, with σco ∼ 0.08 Jy beam−1 km s−1 for the blue lobes and ∼0.06 Jy beam−1 km s−1 for the red lobes. The corresponding velocity ranges are plus/minus 5−30 km s−1 relative to VLSR (∼84.5 km s−1) of the C2 core. Panel (b): zoom-in view of the C2 core. The black ellipses correspond to the FWHM sizes of the condensation estimated from the QUARKS 1.3 mm image using the task CASA imfit.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: M16 in the far-IR, mid-IR, and optical. (A) Herschel 500, 160, 70 μm in red, green, and blue, and 870 μm in black contours. Features are marked with colored lines. The NGC 6611 cluster center is marked with a group of magenta stars, and W584 is marked separately. IRAS 18156–1343 (left) and IRAS 18152–1346 (right) are marked with gray stars. (B) WISE 22, 12, and 4.6 μm in red, green, and blue, and (C) optical DSS2 R band. Dashed black or white lines in all images outline the infrared lobes, and the Bright Northern Ridge is marked in red in the optical, where it is not visible.
Paper: The ALMA-QUARKS Survey: Evidence of a Candidate High-mass Prestellar Core Aside a Bright-rimmed Cloud IRAS 18290-0924
Authors: Dongting Yang, Hong-Li Liu, Sheng-li Qin, Tie Liu, Anandmayee Tej, Siju Zhang, Xunchuan Liu, Fengwei Xu, Guido Garay, Lei Zhu, Patricio Sanhueza, Xiaofeng Mai, Wenyu Jiao, Paul F. Goldsmith, Sami Dib, Pablo García, Di Li, Jinhua He, A. Y. Yang, Prasanta Gorai, Suinan Zhang, Yankun Zhang, Jianjun Zhou, Mika Juvela, James O. Chibueze, Chang Won Lee, Jihye Hwang, Leonardo Bronfman, Xindi Tang, Archana Soam, Tapas Baug, Yichen Zhang, Swagat Ranjan Das, L. K. Dewangan, L. Viktor Tóth
Figure caption: Average spectra of the C2 core/condensation. (a): average spectra extracted from two ATOMS wideband SPWs over the C2 core. (b): same as panel (a) but for four QUARKS SPWs over the C2 condensation. (c): zoom-in view of the molecular lines detected in the six SPWs (corresponding to panels (a) and (b)). The dashed line indicates the systemic velocity of the C2 core (∼84.5 km s−1). Note that the absorption dips present in both 13CO and CO spectra are artifacts arising from the missing flux by ALMA, which will be addressed in future, more in-depth studies by combining our QUARKS data with new single-dish observations.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: The Northern Cloud (12CO J = 1–0; cyan) obscures the eastern part of the M16 H II region in the optical (DSS2 red optical filter; red). The PMO CO observations are integrated within VLSR = 10–21 km s−1 to show the Northern Cloud. The dashed white lines on the top panel outline the eastern and western cavities (Section 3.5). Note the anticorrelation between the Northern Cloud CO emission and the optical emission from the H II region behind it.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: 12CO(J = 1–0) integrated intensities in four different velocity intervals. The leftmost panel shows the PMO and FUGIN observations overlaid. The FUGIN observations cover ∣b∣ < 1°, but M16 extends slightly above b = 1°. The PMO observations cover a smaller area but reach up to ﹩b\approx 1\mathop{.}\limits^{^\circ }3﹩. Green crosses show early-type members of NGC 6611 (Section 7). The two rows to the right show PMO observations on top and FUGIN observations on the bottom. The velocity intervals used for each column are marked on the bottom row. PMO observations are made with a 55″ beam, and FUGIN survey observations using Nobeyama have a 20″ beam.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: M16 in Spitzer IRAC 5.8 and 8.0 μm (blue, green) and MIPS 24 μm (red). The Pillars of Creation, Spire, and N19 ring are marked. The IRAC images are shown with a linear stretch, and the MIPS band with a square root stretch. Black diamonds show early-type members of NGC 6611 (Section 7).
Paper: The ALMA-QUARKS Survey: Evidence of a Candidate High-mass Prestellar Core Aside a Bright-rimmed Cloud IRAS 18290-0924
Authors: Dongting Yang, Hong-Li Liu, Sheng-li Qin, Tie Liu, Anandmayee Tej, Siju Zhang, Xunchuan Liu, Fengwei Xu, Guido Garay, Lei Zhu, Patricio Sanhueza, Xiaofeng Mai, Wenyu Jiao, Paul F. Goldsmith, Sami Dib, Pablo García, Di Li, Jinhua He, A. Y. Yang, Prasanta Gorai, Suinan Zhang, Yankun Zhang, Jianjun Zhou, Mika Juvela, James O. Chibueze, Chang Won Lee, Jihye Hwang, Leonardo Bronfman, Xindi Tang, Archana Soam, Tapas Baug, Yichen Zhang, Swagat Ranjan Das, L. K. Dewangan, L. Viktor Tóth
Figure caption: Average spectra of H13CO+ from the ATOMS survey and average spectra of N2D+ from the QUARKS survey.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: The edge of the western cavity described in Section 3.5. From left to right: DSS2 red optical, 70, and 22 μm. All three images show the same area of the sky. The optical map uses a square root color stretch; the others use a linear stretch. The edge of the western cavity, marked with green-dashed lines, appears in emission at the center of each image.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Color composite showing the diffuse emission extracted from Chandra ACIS X-ray observations over the 8 μm image. 8 μm is shown in red, the 0.5–2 keV band in green, and the 2–7 keV band in blue. The extraction region for the analyzed spectrum is outlined in white. The harder band is less susceptible to extinction. The brightest X-ray emission surrounds NGC 6611, whose immediate area is masked out since it is dominated by point sources. The X-ray-dark region to the left of NGC 6611 is spatially correlated with Northern Cloud CO emission. The X-ray emission at the top left lies toward the inside of the eastern lobe, and emission to the right of the Pillars lies inside the western lobe.
Paper: Probing the Physical Origin of the Balmer Decrement in the Broad-line Region of Nearby Active Galactic Nuclei via Spectral Variability
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Ruancun Li
Figure caption: Comparison of the temporal variation between the Balmer decrement and the flux ratio of the continua at 3800 and 5100 Å. The various lines represent the temporal variation predicted solely by the intrinsic extinction of AGNs, under the assumption that the accretion disk and BLR share the same extinction. The blue dotted, solid, and dashed lines correspond to the predictions based on the extinction curve of E. L. Fitzpatrick (1999) with RV = 1.5, 3.1,  and 5.5, respectively. The red and green lines are derived from the extinction curves of star-forming galaxies (D. Calzetti et al. 2000) and AGNs (C. M. Gaskell et al. 2004), respectively. The black dashed line denotes the orthogonal distance regression of the observed data.
Paper: Probing the Physical Origin of the Balmer Decrement in the Broad-line Region of Nearby Active Galactic Nuclei via Spectral Variability
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Ruancun Li
Figure caption: (a) Comparison of the broad Hα luminosity with its EW. The red diamonds denote the LRDs at z ≈ 5 drawn from J. Matthee et al. (2024). (b) Comparison of the temporal variation between the BLR Balmer decrement and the EW of the broad Hα. The dashed line shows the best-fit linear regression. The density contour is shown on a logarithmic scale.
Paper: Probing the Physical Origin of the Balmer Decrement in the Broad-line Region of Nearby Active Galactic Nuclei via Spectral Variability
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Ruancun Li
Figure caption: Example of the spectral fitting. (a) The black solid line represents the original data in the rest frame, corrected for the Milky Way reddening. The cyan line denotes the continuum from the accretion disk, modeled with a power law plus polynomial terms, along with Fe II multiplets, while the magenta line shows the host galaxy component. The red line represents the best-fit model. Spectral decomposition of the (b) Hβ and [O III] and (c) Hα and [N II] region. The black histogram shows the residual spectrum after subtracting the continuum fit. The blue lines represent the broad components of Hβ and Hα, while the green lines represent the narrow components of Hβ and Hα, with the [O III] doublet and [N II], respectively. The red line indicates the total best-fit model.
Paper: Probing the Physical Origin of the Balmer Decrement in the Broad-line Region of Nearby Active Galactic Nuclei via Spectral Variability
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Ruancun Li
Figure caption: Comparison of temporal variation of the Balmer decrement with AGN brightness indicated by the continuum flux at 5100 Å. The density contour is shown on a logarithmic scale.
Paper: Probing the Physical Origin of the Balmer Decrement in the Broad-line Region of Nearby Active Galactic Nuclei via Spectral Variability
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Ruancun Li
Figure caption: Comparison of temporal variation between the Balmer decrement and AGN brightness indicated by the flux of broad Hα emission. The dashed line shows the best-fit linear regression. The density contour is shown on a logarithmic scale.
Paper: Probing the Physical Origin of the Balmer Decrement in the Broad-line Region of Nearby Active Galactic Nuclei via Spectral Variability
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Ruancun Li
Figure caption: Balmer decrement versus (a) continuum luminosity at 5100 Å and (b) Eddington ratio. The dashed line shows the best-fit linear regression. The density contour is shown on a logarithmic scale.
Paper: Ionization Rate of Interstellar Neutral Helium from New Horizons/SWAP Observations
Authors: Małgorzata Antonik, Paweł Swaczyna, David J. McComas, Heather A. Elliott, Maciej Bzowski
Figure caption: Upper panel: example of a SWAP daily averaged spectrum with Poisson uncertainties (black dots with error bars) with fit models (solid lines). The graph shows both the core solar wind (H+, He2+, He+) and PUIs (H+ PUIs, He+ PUIs). The core solar wind protons are shown in orange, alpha particles in green, He+ ions in red, H+ PUIs in purple, and He+ PUIs in brown. The data points used for the fit are marked in pink (see text). The gray dashed line is the background. The fit values of the most important parameters are listed in the figure. Lower panel: residual signal between the total model and SWAP data normalized by the statistical uncertainty, with a thin black line marking zero. In the selected case, the low solar wind speed shifts the energy cutoff of the He+ PUI distribution close to the upper limit of the SWAP energy range.
Paper: Ionization Rate of Interstellar Neutral Helium from New Horizons/SWAP Observations
Authors: Małgorzata Antonik, Paweł Swaczyna, David J. McComas, Heather A. Elliott, Maciej Bzowski
Figure caption: Left panel: the time variations of the helium SWAP ionization rates (orange) and the photoionization rates derived from the model (green), and their ratio. The helium ionization rate ratio indicates that the SWAP ionization rates are higher than the photoionization rates from solar UV spectra and 10.7 radio flux. Right panel: the relation between helium SWAP ionization rates and photoionization rates with uncertainties. The gray dashed line represents a one-to-one relationship. The red solid line shows the model assuming proportionality of values, and the orange dashed line is the linear model. The model with only the scaling parameter fit shows that the helium ionization rates estimated from SWAP observations are 43% higher than the photoionization rates based on solar UV spectra and 10.7 radio flux.
Paper: Investigation on the Predictive Potentiality of Photospheric Magnetic Parameters for Distinguishing Confined from Eruptive Solar Flares
Authors: Jinhui Pan, Rui Liu
Figure caption: Distribution of the physical parameters for all the events. The red bars represent eruptive flares, and the blue bars represent confined flares. The overlapping portion is shown in deep brownish red. The dotted lines indicate the mean values of the parameters for eruptive flares (red) and confined flares (blue).
Paper: Investigation on the Predictive Potentiality of Photospheric Magnetic Parameters for Distinguishing Confined from Eruptive Solar Flares
Authors: Jinhui Pan, Rui Liu
Figure caption: Correlation matrix showing the Spearman correlation coefficient between different physical parameters for all the flares investigated. The correlation coefficients between Φ, Ef, d, and Θ are highlighted by red bounding boxes.