adsabs/AstroCLIMB huggingface dataset:
Paper: Abundance Pattern Fitting with Bayesian Inference: Constraining First Stars’ Properties and Their Explosion Mechanism with Extremely Metal-poor Stars
Authors: Ruizheng Jiang, Haining Li, Gang Zhao, Qianfan Xing, Wenyu Xin
Figure caption: Distribution of the abundance residuals between predictions and observations over their corresponding observational uncertainties. The left (gray) and right (white) boxes represent the NLTE-corrected and LTE abundances from the literature. Each box extends from the first to the third quartile of the corresponding abundance residuals, with a red solid line indicating the median value. Whiskers extend to the furthest abundance residuals lying within 1.5× the interquartile range (IQR)s from the boxes. The dashed horizontal lines signify the deviations of 1σ and 3σ of observational uncertainty.
Paper: Abundance Pattern Fitting with Bayesian Inference: Constraining First Stars’ Properties and Their Explosion Mechanism with Extremely Metal-poor Stars
Authors: Ruizheng Jiang, Haining Li, Gang Zhao, Qianfan Xing, Wenyu Xin
Figure caption: Progenitor distribution derived from abundances of EMP stars and explodability constraints inferred from neutron star mass maximum. The probability densities of progenitor models are color coded following the colorbar in the right panel, with models having posterior probabilities below 10−3 shown in black. Nonexploding models are indicated by region hatched with cross lines, and pre-excluded models are shaded in gray.
Paper: Abundance Pattern Fitting with Bayesian Inference: Constraining First Stars’ Properties and Their Explosion Mechanism with Extremely Metal-poor Stars
Authors: Ruizheng Jiang, Haining Li, Gang Zhao, Qianfan Xing, Wenyu Xin
Figure caption: IMF (upper panel) and energy distribution function (bottom panel) of the first stars in CDF. The blue dots represent the derived CDF of mass and energy distribution from the EMP star sample, while the red lines with shaded regions standards for their corresponding best-fit distribution as defined in Equation (15). In each panel, the shaded gray zones are the assumed successfully explosive models from concentrated intervals in the derived mass distribution. The Salpeter IMF (E. E. Salpeter 1955) is coded with black for comparison.
Paper: Abundance Pattern Fitting with Bayesian Inference: Constraining First Stars’ Properties and Their Explosion Mechanism with Extremely Metal-poor Stars
Authors: Ruizheng Jiang, Haining Li, Gang Zhao, Qianfan Xing, Wenyu Xin
Figure caption: Deviation of the measured abundances ﹩\delta {\mathrm{log}}\,\epsilon ﹩, which is defined as Equation (1), as a function of surface gravity ﹩{\mathrm{log}}\,g﹩ and their corresponding distributions. Target stars sourced from different samples are coded as in Figure 1. Abundance deviation ﹩\delta {\mathrm{log}}\,\epsilon ﹩ caused by different atmospheric models mostly falls within the typical observational uncertainty of 0.1 dex, represented as the horizontal dashed lines. However, the most significant deviations occur at the low surface gravity with ﹩{\mathrm{log}}\,g\lt 2﹩.
Paper: Abundance Pattern Fitting with Bayesian Inference: Constraining First Stars’ Properties and Their Explosion Mechanism with Extremely Metal-poor Stars
Authors: Ruizheng Jiang, Haining Li, Gang Zhao, Qianfan Xing, Wenyu Xin
Figure caption: The sensitivity of progenitor-mass derivation for different elements. In each panel, the scattered points correspond to individual EMP stars from different samples, while the horizontal solid line and shaded regions indicate the 50th, 16th, and 84th percentiles of the sensitivities. The sensitivity is expressed in the unit of dex−1.
Paper: Abundance Pattern Fitting with Bayesian Inference: Constraining First Stars’ Properties and Their Explosion Mechanism with Extremely Metal-poor Stars
Authors: Ruizheng Jiang, Haining Li, Gang Zhao, Qianfan Xing, Wenyu Xin
Figure caption: Deviation in progenitor mass caused by the nondetection (blue, left) and observational uncertainty (red, right) of each element, summarized in boxplots. The definition of boxes and whiskers follows that in Figure 4. NLTE abundances are adopted for Na, Mg, and Al in this analysis.
Paper: Abundance Pattern Fitting with Bayesian Inference: Constraining First Stars’ Properties and Their Explosion Mechanism with Extremely Metal-poor Stars
Authors: Ruizheng Jiang, Haining Li, Gang Zhao, Qianfan Xing, Wenyu Xin
Figure caption: Comparison between the resolution-normalized results. The first (orange), second (translucent orange), third (blue), and right (translucent blue) bars, respectively, represent the resulting IMFs of this work and R. Jiang et al. (2024), the normalized and raw results of M. N. Ishigaki et al. (2018).
Paper: Abundance Pattern Fitting with Bayesian Inference: Constraining First Stars’ Properties and Their Explosion Mechanism with Extremely Metal-poor Stars
Authors: Ruizheng Jiang, Haining Li, Gang Zhao, Qianfan Xing, Wenyu Xin
Figure caption: NLTE correction A(X) with its corresponding NLTE uncertainty as a function of ﹩{\mathrm{log}}\,\epsilon ﹩ abundance in the literature. The color coding is the same as Figure 1.
Paper: The First LWA Swarm Calibrator Survey
Authors: C. A. Taylor, G. B. Taylor, J. Dowell, S. Pezzaioli
Figure caption: Postage stamp continuum images from the first LWA Swarm Calibrator Survey (45–84 MHz). Peak flux, rms noise, and first contour levels are listed in Table 1. Target sources’ 3C identifier, postcalibration averaged center frequency, and observing epoch are listed at the top of each image. Beam size and size scale bars (if redshift is available) are shown in the bottom corners, assuming a Hubble constant of H0 ≈ 73.04 km s−1 Mpc−1 from the SH0ES collaboration (A. G. Riess et al. 2022).
Paper: The First LWA Swarm Calibrator Survey
Authors: C. A. Taylor, G. B. Taylor, J. Dowell, S. Pezzaioli
Figure caption: Image plane rms noise is plotted against the peak flux for the radio sources observed in this survey from Table 1. Dashed horizontal lines correspond to the theoretical estimates for the three-element LWA Swarm, including one Swarm station and two standard stations, using the equations in Section 3 at practical zenith angles observed in the survey. Averaging across the survey observing band of 45–84 MHz, Equation (3) estimates the noise to be approximately 7 mJy at θz = 0∘, 9 mJy at θz = 30∘, and 21 mJy at θz = 60∘.
Paper: The First LWA Swarm Calibrator Survey
Authors: C. A. Taylor, G. B. Taylor, J. Dowell, S. Pezzaioli
Figure caption:                         Example (u, v)-coverage for an 8 hr observing run of 3C 147. Note that the final form of the data is split into 40 IFs to help with image synthesis, as seen in the coverage map. An image corresponding to this (u, v)-coverage map can be found in the Figure 4 postage stamps.
Paper: The First LWA Swarm Calibrator Survey
Authors: C. A. Taylor, G. B. Taylor, J. Dowell, S. Pezzaioli
Figure caption: LWA Swarm 3C 286 field observed on 2024 September 3. Radio source (a) 3C 286 is imaged with identified VLSSr field sources (b) NVSS J133053+303758, (c) 4C 31.42, (d) WISEA J133148.78+302928.9, and (e) WISEA J133148.48+303147.3.
Paper: The First LWA Swarm Calibrator Survey
Authors: C. A. Taylor, G. B. Taylor, J. Dowell, S. Pezzaioli
Figure caption: Map of calibrator sources observed in the LWA Swarm Calibrator Survey. Marker size is scaled by the peak flux observed by the LWA and by the VLSSr peak flux at 74 MHz of each unobserved target (W. M. Lane et al. 2014).
Paper: The First LWA Swarm Calibrator Survey
Authors: C. A. Taylor, G. B. Taylor, J. Dowell, S. Pezzaioli
Figure caption: Same as Figure 1, but plotting the bandpass for the 74 MHz tuning from LWA1.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: The Peterson diagram of the double-mode HADS stars. Red squares represent five pure double-mode HADS stars, and blue triangles are 13 HADS in this group. The shaded bands represent the period ratios of the first three overtone modes to fundamental mode, as well as the period ratio of the second overtone to first overtone mode (R. F. Stellingwerf 1979).
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: The upper panel shows a portion of the light curve of TIC 16283570 for about 3 days. The middle panel shows the phase diagram folded by the fundamental frequency f = 11.02399 c day−1. The lower panel shows the Fourier amplitude spectra.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: Top panel: a portion of the light curve of TIC 710783 for about 3 days. Middle panel: phased diagram (folded by the dominant frequency f = 12.74450 c day−1). Bottom panel: amplitude spectra with a frequency range of 0 c day−1 < f < 80 c day−1.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: The upper panel shows a portion of the light curve of TIC 7082633 for about 3 days. The middle panel shows the phase diagram folded by the fundamental frequency f = 10.32293 c day−1. The lower panel shows the Fourier amplitude spectra.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: The upper panel shows a portion of the light curve of TIC 8765832 for about 3 days. The middle panel shows the phase diagram folded by the strongest frequency, f = 12.70964 c day−1. The lower panel shows the Fourier amplitude spectra.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: The upper panel shows a portion of the light curve of TIC 1973623 for about 3 days. The middle panel shows the phase diagram folded by the strongest frequency, f = 7.88921 c day−1. The lower panel shows the Fourier amplitude spectra.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: The upper panel shows a portion of the light curve of TIC 32302937 for about 3 days. The middle panel shows the phase diagram folded by the strongest frequency, f = 3.82072 c day−1. The lower panel shows the Fourier amplitude spectra.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: The upper panel shows a portion of the light curve of TIC 17153995 for about 3 days.; The middle panel shows the phase diagram folded by the fundamental frequency f = 8.54480 c day−1. The lower panel shows the Fourier amplitude spectra.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: Corner plot showing the χ2 distribution across the model parameter space for knot A1. Each panel represents the χ2 minimization map for a pair of free parameters (b, vs, nH, and G0), with χ2 values minimized over all remaining parameters. Lighter colors correspond to lower χ2 values, indicating better agreement between the observed and modeled H2 column densities. The best-fit solution is marked with a black cross.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: H2 radial velocity maps obtained from the pure rotational 0–0 S(1)–S(8) transitions. Black stars indicate the source positions. The MIRI FOV varies with wavelength, from 6″ × 15″ for the 0–0 S(8) map at 5.05 μm to 8″ × 17″ for the 0–0 S(1) map at 17.04 μm. The overall morphology remains similar across lines tracing different excitation conditions, although the mean velocity values vary inversely with wavelength. The same color scale is adopted for all maps to enable direct comparison.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: Rotational diagrams for pure rotational v = 0 lines. Squares represent the data. Colors correspond to the different instruments, with red and blue being MIRI and NIRSpec, respectively. The black open circles are the best model for each region.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: NIRSpec/G235H spectra extracted for the five representative regions located in the redshifted cavity, using a circular aperture with a radius of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩4. The main detected atomic (blue) and H2 molecular (magenta) emission lines are indicated. The discontinuity visible between 2.4 and 2.5 μm corresponds to the detector gap of NIRSpec.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: NIRSpec/G395H spectra extracted for the five representative regions located in the redshifted cavity, using a circular aperture with a radius of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩4. The main detected molecular H2 (magenta) and CO (green) lines are indicated. The discontinuity visible between 4.1 and 4.2 μm corresponds to the detector gap of NIRSpec.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: Rotational diagrams for pure rotational v = 0 lines obtained for regions where just MIRI data are available. Squares represent the data. The black open circles are the best model for each region.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: MIRI spectra extracted for the 13 representative regions located in both the red- and blueshifted cavities, using a circular aperture with a radius of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩4. The main detected atomic (blue) and H2 molecular (magenta) emission lines are indicated.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: Best shock models (black open circles) for the representative regions. Red and blue points represent MIRI and NIRSpec data, respectively, while the symbols—squares, triangles, circles, and stars—correspond to vibrational levels from v = 0 to v > 2.
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Visualization of partial correlation analysis. The plot displays the partial correlation coefficients (Spearman’s ρ, Y-axis) and their corresponding p-values, for all three SE models (X-axis). The purple points represent the partial correlation between SE and UV luminosities after controlling for PC luminosity, while the green points indicate the partial correlation between SE and PC luminosities after controlling for UV luminosity. Across all SE models, the partial correlation between SE and UV (purple) is consistently stronger than the correlation between SE and PC (green).
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Intrinsic SE–UV and SE–PC relations as revealed by luminosity–ratio correlations. The top three panels (in purple) illustrate the intrinsic correlation between SE and UV luminosities, with both scaled by PC luminosity, under different SE models (blackbody, power law, and cutoff power law). The bottom three panels (in green) similarly show the intrinsic correlation between SE and PC luminosities, scaled by UV luminosity. The results highlight a strong intrinsic link between SE and UV luminosities (pnull ∼ 2 × 10−7), even after removing PC contributions. The correlation between SE and PC is also statistically significant (pnull ∼ 6 × 10−3) but is generally weaker than the SE–UV correlation.
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Normalized UV-to-X-ray SEDs for our sample. The absorption corrected best-fit X-ray model spectrum (model 3) is shifted to the rest frame, scaled to the simultaneous rest frame 2500 Å flux, and color coded based on αoX (the power-law slope of the dashed color lines).
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Multiple linear regression slopes of SE on UV (purple) and PC (green) luminosities. Similar to Figure 6, but with the Y-axis showing regression slopes from the relation ﹩{L}_{{\rm{SE}},0.5-2}\sim {L}_{{\rm{UV}}}^{{\beta }_{1}}\cdot {L}_{{\rm{PC}},2-10}^{{\beta }_{2}}﹩. SE depends more strongly on UV (β1 ∼ 0.72) than on PC (β2 ∼ 0.27).
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Relation between q and PC photon index ΓPC for different SE models. No correlation is observed when SE is fitted with a blackbody (left panel). However, a mild anticorrelation emerges for the power-law model (middle) and the cutoff power-law model (right).
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Relation between SE strength q and Eddington ratio λEdd for different SE models reveals a significant correlation across all models.
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Relation between SE strength (q) and UV–PC luminosity ratio (LUV/LPC,0.5−10). Shown are Spearman’s ρ, null-hypothesis probability pnull, OLS slope β, and OLS bisector slope βbi. The shaded region marks the 1σ confidence interval of the bisector fit. Unless noted otherwise, the same legend format applies to all scatter plots in this paper.
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Relation between αoX and soft X-ray spectral slope (α0.5−2, purple) or hard X-ray spectral slope (α2−10, green). A 1:1 reference line is shown in gray for comparison.
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Luminosity–luminosity correlation for SE vs. UV (left), SE vs. PC (middle), and PC vs. UV (right). Model 3 is used to derive SE and PC luminosities.
Paper: Dual Origins of Rapid Flare Ribbon Downflows in an X9-class Solar Flare
Authors: Ryan J. French, William H. Ashfield, Cole A. Tamburri, Maria D. Kazachenko, Marie Dominique, Marcel Corchado Albelo, Amir Caspi
Figure caption: Overview of the X9.0 flare observed on 2024 October 3: Top row: SJI 1330 Å snapshots (full FOV) of the flare ribbon evolution. The first four snapshots are sequentially 90 s apart during the impulsive phase, and the final snapshot is later in the gradual phase. The vertical black line is the location of the IRIS slit. The horizontal dashed line marks the lower extent of the FOV of subsequent panels. Second row: sit-and-stare Si IV 1402.77 Å intensity map (along a subrange of the slit), computed by line integration. The dark green line outlines the southern flare ribbon mask. Green circles highlight high-redshift pixels examined in Figure 5. Third row: same as above, showing Si IV 1402.77 Å Doppler velocity determined from the line moment centroid. Fourth row: progression of IRIS Si IV 1402.77 Å exposure time throughout the raster, alongside the number of saturated pixels per time step. Fifth row: reconnection flux rate (magnitude) for the southern (AIA 1600 Å and SJI 1330 Å) and northern (AIA 1600 Å) flare ribbons). Bottom row: time-series of GOES 0.5–4 Å SXRs, and ASO-S HXI 10–20, 20–50, 50–100, and 100–300 keV HXRs. ASO-S HXI measurements are multiplied by 1 × 10–8 for comparison to GOES. Vertical dashed gray lines mark the location of SJI snapshots in the top row.
Paper: Dual Origins of Rapid Flare Ribbon Downflows in an X9-class Solar Flare
Authors: Ryan J. French, William H. Ashfield, Cole A. Tamburri, Maria D. Kazachenko, Marie Dominique, Marcel Corchado Albelo, Amir Caspi
Figure caption: Panel (A): max and mean (×5) Si IV 1402.77 Å Doppler velocity across the ribbon mask. The black line marks the smoothed time series. Panel (B): max and mean Si IV 1402.77 Å intensity across the ribbon mask. The black line marks the smoothed time series. Panel (C): ASO-S HXI HXR time series. Panel (D): LYRA Lyα time series. Vertical dashed lines mark the locations of local peaks in the smoothed maximum Si IV Doppler velocity (black line). We use yellow and blue background shading to highlight our two stages of rapid Si IV Doppler velocities, the impulsive (∼12:15–12:19 UT) and nonimpulsive (∼12:23–12:28 UT) phases.