adsabs/AstroCLIMB huggingface dataset:
Paper: Bridging Machine Learning and Spectroscopy: A New Analysis for Astrochemical Target Selection
Authors: Hannah Toru Shay, Gabi Wenzel, Ci Xue, Brett A. McGuire
Figure caption: The top 25 species assessed by metric 1. The formulas and assessed visibility percentages are provided. Formulas are given in skeleton format.
Paper: Bridging Machine Learning and Spectroscopy: A New Analysis for Astrochemical Target Selection
Authors: Hannah Toru Shay, Gabi Wenzel, Ci Xue, Brett A. McGuire
Figure caption: The top 26–50, as assessed by metric 1. The formulas and assessed visibility percentages are provided. Formulas are given in skeleton format.
Paper: Bridging Machine Learning and Spectroscopy: A New Analysis for Astrochemical Target Selection
Authors: Hannah Toru Shay, Gabi Wenzel, Ci Xue, Brett A. McGuire
Figure caption: Metric 1 applied to legacy data, resulting 26–50 molecules and visibility percentages.
Paper: Bridging Machine Learning and Spectroscopy: A New Analysis for Astrochemical Target Selection
Authors: Hannah Toru Shay, Gabi Wenzel, Ci Xue, Brett A. McGuire
Figure caption: Metric 1 applied to legacy data, resulting 1–25 molecules and visibility percentages.
Paper: Bridging Machine Learning and Spectroscopy: A New Analysis for Astrochemical Target Selection
Authors: Hannah Toru Shay, Gabi Wenzel, Ci Xue, Brett A. McGuire
Figure caption: The top 25 species assessed by metric 2. The formulas and assessed visibility percentages are provided. Formula are given in skeleton format.
Paper: Bridging Machine Learning and Spectroscopy: A New Analysis for Astrochemical Target Selection
Authors: Hannah Toru Shay, Gabi Wenzel, Ci Xue, Brett A. McGuire
Figure caption: The top 26–50, as assessed by metric 2. The formulas and assessed visibility percentages are provided. Formula are given in skeleton format.
Paper: The Aromatic Infrared Bands around the Wolf–Rayet Binary WR 140 Revealed by JWST
Authors: Kotomi Taniguchi, Ryan M. Lau, Takashi Onaka, Macarena Garcia Marin, Hideo Matsuhara, Anthony Moffat, Theodore R. Gull, Thomas I. Madura, Gerd Weigelt, Riko Senoo, Alan T. Tokunaga, Walter Duley, Peredur M. Williams, Noel D. Richardson, Joel Sanchez-Bermudez
Figure caption: Plots of projected distance from the central stars vs. peak wavelength (upper), FWHM (middle), and integrated intensity (lower) obtained from the Gaussian fitting for three features. The blue-filled circle and red open circle indicate on-shell and off-shell positions, respectively. The green dashed horizontal line in the top left panel indicates the peak wavelengths of He II = 6.95 μm. The orange dashed line in the top middle panel shows the wavelength of He II = 7.457 μm, and that in the top right panel indicates He II = 11.304 μm, respectively. The green dashed lines in the top right panel indicate He II and He I lines. Since the I2 position does not show a clear emission feature at 6 and 7.7 μm and the fitting results are poor, we indicate parentheses. All of the plots include error bars, but most of them are smaller than the data points. The E1 position is contaminated by atomic emission lines.
Paper: The Aromatic Infrared Bands around the Wolf–Rayet Binary WR 140 Revealed by JWST
Authors: Kotomi Taniguchi, Ryan M. Lau, Takashi Onaka, Macarena Garcia Marin, Hideo Matsuhara, Anthony Moffat, Theodore R. Gull, Thomas I. Madura, Gerd Weigelt, Riko Senoo, Alan T. Tokunaga, Walter Duley, Peredur M. Williams, Noel D. Richardson, Joel Sanchez-Bermudez
Figure caption: Plots using integrated-intensity ratios. The left and middle panels show the dependence of the 6/11.2 μm and 7.7/11.2 μm integrated-intensity ratios on the projected distance from the central stars, respectively. The blue-filled and red-open circles represent on-shell and off-shell positions, respectively. The points without their position names indicate the positions on Shell 2 (S2, EE2, and E2). The right panel indicates a positive correlation between these two integrated-intensity ratios. The orange dashed line indicates the best-fit function including S1 (y = 2.6004x − 2.1795), whereas the green line shows the best-fit function excluding S1 (y = 1.374x + 0.0836). The Pearson’s correlation coefficients r for these pairs are derived to be 0.972 and 0.985 for with S1 and without S1, respectively.
Paper: The Aromatic Infrared Bands around the Wolf–Rayet Binary WR 140 Revealed by JWST
Authors: Kotomi Taniguchi, Ryan M. Lau, Takashi Onaka, Macarena Garcia Marin, Hideo Matsuhara, Anthony Moffat, Theodore R. Gull, Thomas I. Madura, Gerd Weigelt, Riko Senoo, Alan T. Tokunaga, Walter Duley, Peredur M. Williams, Noel D. Richardson, Joel Sanchez-Bermudez
Figure caption: (Left) The 7.1 μm cube image. The yellow circle indicates the position of WR 140, and the cyan circles represent positions where we analyzed spectra. Table 1 summarizes their coordinates and distances from the central binary. The radius of the circular apertures used to extract the spectra are 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩35. (Middle and Right) The MIRI MRS spectra (5–27 μm) toward on-shell positions located on the dust shells of Shell 1 and Shell 2, and off-shell positions, respectively. The distance from the star position is indicated in each panel.
Paper: The Aromatic Infrared Bands around the Wolf–Rayet Binary WR 140 Revealed by JWST
Authors: Kotomi Taniguchi, Ryan M. Lau, Takashi Onaka, Macarena Garcia Marin, Hideo Matsuhara, Anthony Moffat, Theodore R. Gull, Thomas I. Madura, Gerd Weigelt, Riko Senoo, Alan T. Tokunaga, Walter Duley, Peredur M. Williams, Noel D. Richardson, Joel Sanchez-Bermudez
Figure caption: Comparisons of the observed spectra (black and blue) and typical AIB emission features named classes A–D (red). The left panels show observed spectra at two on-shell positions, S1 (black) and S2 (blue), and the right panels show those at two off-shell positions, I3 (black) and I4 (blue), respectively. The typical AIB emission features are as follows: class A is the compact H II region IRAS 23133+6050; class B is the post-AGB star HD 44179; class C is the post-AGB star IRAS 13416-6243 (E. Peeters et al. 2002); and class D is the post-AGB star IRAS 22272+5435 (M. Matsuura et al. 2014).
Paper: The Aromatic Infrared Bands around the Wolf–Rayet Binary WR 140 Revealed by JWST
Authors: Kotomi Taniguchi, Ryan M. Lau, Takashi Onaka, Macarena Garcia Marin, Hideo Matsuhara, Anthony Moffat, Theodore R. Gull, Thomas I. Madura, Gerd Weigelt, Riko Senoo, Alan T. Tokunaga, Walter Duley, Peredur M. Williams, Noel D. Richardson, Joel Sanchez-Bermudez
Figure caption: Comparison of the spectra at WR 140 S2 (top panel) and the diffuse ISM toward the Galactic plane obtained from J. Kahanpää et al. (2003) (bottom panel). The red dashed lines indicate the peak wavelengths attributed to AIBs. Note that there is a prominent [S IV] 10.51 μm emission line feature at S2 that is not associated to dust. Note that the unit of the vertical axis in the bottom panel is not the unit of Jy.
Paper: The Aromatic Infrared Bands around the Wolf–Rayet Binary WR 140 Revealed by JWST
Authors: Kotomi Taniguchi, Ryan M. Lau, Takashi Onaka, Macarena Garcia Marin, Hideo Matsuhara, Anthony Moffat, Theodore R. Gull, Thomas I. Madura, Gerd Weigelt, Riko Senoo, Alan T. Tokunaga, Walter Duley, Peredur M. Williams, Noel D. Richardson, Joel Sanchez-Bermudez
Figure caption: Comparison of AIBs at S1 (on Shell 1) and S2 (on Shell 2). Black lines and the red curves indicate the observed spectra and the Gaussian fitting results, respectively. The filled regions highlight the Gaussian fitting results. The gray lines indicate residuals.
Paper: Peculiar Disk Substructures Associated with the Young Eruptive Star EX Lupi
Authors: Masayuki Yamaguchi, Hauyu Baobab Liu, Michihiro Takami, Pin-Gao Gu
Figure caption: Gallery of ALMA (PRIISM) continuum images and their residual maps at 3.2 mm/93 GHz (Band 3, bottom row) and 2.0 mm/153 GHz (Band 4, top row) of the EX Lupi disk. The same linear color scale is adopted. A white bar of ﹩0\mathop{.}\limits{^{\prime\prime} }1﹩ (= 16 au) is provided to reference the angular scales. The central stellar symbol (⋆) indicates the stellar position measured in Gaia observations. Left: model image reconstructed using PRIISM imaging. The image initially has a unit of janskys per pixel (Jy pixel−1; Section 2.3), while it is converted to millijanskys per square arcsecond (﹩{\rm{mJy}}\,{{\rm{arcsec}}}^{-2}﹩) for comparison with the restored image (middle). The filled white ellipse denotes the effective spatial resolution θeff. The resolution is estimated from an artificial point-source injection method (Appendix B.2). Middle: restored image after convolution with an elliptical Gaussian representing the main lobe of the synthesized beam, along with adding the dirty map of residuals (right). Each white contour corresponds to [3, 4, 5] × σnoise, where σnoise is the rms noise value calculated from the emission-free area (36 μJy beam−1 for Band 3 and 48 μJy beam−1 for Band 4). The restored image is expressed in a unit of Jy beam−1, while being converted to ﹩{\rm{mJy}}\,{{\rm{arcsec}}}^{-2}﹩. Right: dirty map of the residuals, obtained by subtracting the model from the observations in the visibility domain. The unit is expressed in image rms noise. The black contours represent the same as the white ones on the restored image (middle).
Paper: Peculiar Disk Substructures Associated with the Young Eruptive Star EX Lupi
Authors: Masayuki Yamaguchi, Hauyu Baobab Liu, Michihiro Takami, Pin-Gao Gu
Figure caption: Left: the best-fit ellipse to the outer ring overlaid on the restored Band 4 image, with contour levels at ﹩[3,4,5]\times {\sigma }_{{\rm{noise}}}^{{\rm{B4}}}﹩, where ﹩{\sigma }_{{\rm{noise}}}^{{\rm{B4}}}﹩ is the rms noise of 48 μJy beam−1. The purple curves represent the distribution of solutions considering the estimated 1σ error. The white dots along the outer ring indicate the radially averaged peak positions, spaced at 20∘ intervals. The outer peak in the PA of 140∘ ∼ 160∘ could not be identified due to insufficient angular resolution or low SNR, and was therefore excluded from the fit. Right: the deprojected image with the inclination (=42﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6) and PA (=51﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7) derived from the best-fit ellipse. The center of the ellipse fit is used as the center position for deprojection. The purple circle indicates the best-fit model, while the white star symbol indicates the position of EX Lupi.
Paper: Peculiar Disk Substructures Associated with the Young Eruptive Star EX Lupi
Authors: Masayuki Yamaguchi, Hauyu Baobab Liu, Michihiro Takami, Pin-Gao Gu
Figure caption: Top panel: deprojected PA profile of the outer ring of EX Lupi, derived from the Band 4 restored image. The contour levels are [3, 4, 5] × σnoise. Note that the emission from the inner arc (r < 20 au) is removed. The center coordinates are set based on an ellipse fit to the outer ring. Bottom panel: radial intensity profile averaged over the full azimuthal angle, displayed on a linear color scale. The profile (solid purple curve) is linearly interpolated onto radial grid points spaced by 0.1 au using interpolate.interp1d from the SciPy module. The light purple ribbon represents the error of the mean at each radius. The dashed orange curve corresponds to the best-fit Gaussian profile to the observed data. The geometric mean of the spatial resolution is shown in the inset at the top-right corner.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Dependence of the Ca II K and H equivalent width on stellar masses as a function of impact parameters. Left: star-forming galaxies. Right: quiescent galaxies. The median stellar masses are listed in the lower left. The blue shaded bands in the right panel correspond to the two highest mass bins for star-forming galaxies in the left panel. The cyan and yellow square data points are the K line measurements from K. H. R. Rubin et al. (2022) multiplied by a factor of 1.69 to compare with our doublet measurements.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Dependence of Ca II on the azimuthal angles for galaxies with ﹩{\mathrm{log}}_{10}({M}_{* }/{M}_{\odot })\,\geqslant \,9.5﹩. Examples of the the galaxy–quasar pairs are shown at the top: from left to right are edge-on galaxies categorized into three azimuthal angles: disk, between disk and pole, pole; followed by face-on galaxies. The galaxies are located at the center, while the quasars are indicated by the cyan arrows. In the bottom panel, the gray band shows the measurements of the face-on samples.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Best-fit amplitudes as a function of median stellar masses for two redshift bins. The solid and open points represent low- and high-redshift samples, respectively. The solid and dashed lines in the left panel are the best-fit power laws for the low- and high-redshift samples.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Dependence of the Ca II K and H equivalent width on stellar masses as a function of normalized distances. Left: star-forming galaxies. Right: quiescent galaxies. The median stellar masses are listed in the lower left.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Best-fit amplitudes A100 as a function of SFR for star-forming galaxies. The solid and open points represent the low- and high-SFR groups, respectively, with matched median stellar masses. The lines correspond to the best-fit power law obtained from simultaneous fitting.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Dependence of the Ca II K and H equivalent width on stellar mass as a function of impact parameters, separating the samples into two redshift bins: z = 0.15 for star-forming galaxies (left), and z = 0.17 for quiescent galaxies (right). The median stellar masses are listed in the lower left. The solid lines follow the exponents fitted in Figure 3.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Best-fit amplitudes A100 as a function of stellar masses. The data points are plotted with their median stellar masses and respective ranges. The black line is the best-fit power law for the star-forming galaxies.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Examples of composite spectra as a function of impact parameters. The shades underneath are the associated uncertainties via bootstrapping. The solid blue lines are the best-fit absorption profiles of Ca II K and H. The vertical dashed lines are the central wavelengths of K and H lines. The median impact parameter is displayed in the lower right corner. Note that the scale of the y-axis changes as a function of impact parameters.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Equivalent width of AGN samples as a function of impact parameters. The shaded bands correspond to the two highest mass bins (109.9 and 1010.7 M⊙) from star-forming galaxies in Figure 3. The dotted line is calculated using Equation (3) with M* = 1010.2M⊙.
Paper: Improving Solar Flare Nowcasting with the Hot Onset Precursor Event Technique
Authors: Anant Telikicherla, Thomas N. Woods, Bennet D. Schwab
Figure caption: Correlation of onset parameters with the logarithm of the background-subtracted peak flux (in Wm−2). The first row depicts the logarithm of the background-subtracted peak flux, logarithm of the running difference EM (ΔEM), and running difference temperature (ΔT) at the first trigger in the first, second, and third panels, respectively. The second row shows the same parameters at the local maximum of the derivative of the running difference EM (Δ2EM). C-class flares are depicted using blue symbols, M-class flares using yellow symbols, and X-class flares using red symbols. The dashed gray lines in the first column indicate the y = x line to show how much lower the onset flux is compared to the peak flux. The dashed black lines show the least-squares fit lines to the parameters. In the bottom middle plot, the 95th percentile value of the running difference EM for C-class flares is depicted using a yellow vertical dashed line, and the 95th percentile of the M-class flares is depicted using a red vertical dashed line.
Paper: Improving Solar Flare Nowcasting with the Hot Onset Precursor Event Technique
Authors: Anant Telikicherla, Thomas N. Woods, Bennet D. Schwab
Figure caption: The figure shows the variation of the model output metrics for different model parameters. The first row shows the variation of the total recall value (black symbols) with integration time (ti), EM threshold (ΔEM), and running difference time (td) in the first, second, and third panels, respectively. The second row shows the variation of the correlation between the value of ΔEM and the same model parameters. This correlation is computed as shown for two points in the time series, the first trigger (blue) and at the local maximum of Δ2EM (green). The blue symbols are offset slightly in the x-axis so that they are visible, even though the blue and green symbols correspond to the same x-value. The third row shows the variation of the mean of the time difference (in minutes) between the flare peak and the first trigger. This is shown for C-class flares using blue symbols, M-class flares using yellow symbols, and X-class flares using red symbols. The yellow and blue symbols are slightly offset in the x-axis so that they are clearly visible, even though they are at the same x-value.
Paper: Improving Solar Flare Nowcasting with the Hot Onset Precursor Event Technique
Authors: Anant Telikicherla, Thomas N. Woods, Bennet D. Schwab
Figure caption: Application of the HOPE-based nowcasting methodology developed in this study to generate early radio blackout alerts. The left panel shows an example time series of the GOES-XRS-A (green) and XRS-B (purple) flux for an X2.8 flare on 2024 May 27. The vertical red line indicates the first HOPE alert, and the vertical gray lines represent the subsequent HOPE alerts. The vertical brown line shows the HOPE X-class flare alert, and the vertical yellow line shows the NOAA R3 radio blackout alert. The middle panel shows a histogram of the time difference between the NOAA R3 alert and the first HOPE alert for all category (c) X1.0 and above flares described in the previous section. The right panel shows a histogram of the time difference between the NOAA R3 radio blackout alert and the HOPE X-class flare alert.