adsabs/AstroCLIMB huggingface dataset:
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Model fits to the median ECO+RESOLVE-B M H I,grp–M halo relation derived using the G3 compared to the FoF algorithms, illustrating inconsistency between these group finders. The best-fitting parameters of each model are listed in Table 2 along with the model parameters for other RESOLVE and ECO samples. Error bars come from bootstrapping.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Sky map of the ECO survey illustrating new H I data in ECO DR3 (orange) compared with ECO DR2 (black; Eckert et al. 2017). Orange points within the RESOLVE-A footprint (<5° decl.) represent new H I data for ECO galaxies located at lower redshifts than RESOLVE-A (which is limited to 4500–7000 km s−1, while ECO reaches down to 3000 km s−1).
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Plots illustrating R proj (left) and Δv proj (right) for giant-only FoF group galaxies as a function of N giants. The triangles represent the median relative projected radii and velocities of giant galaxies in N giants > 1 FoF groups (red points), as a function of N giants. The blue lines show our best fit to the medians using Equations (4) and (5), and the green dashed–dotted lines show the boundaries we use for merging giant-only FoF groups and associating dwarfs to these groups (Section 3.3). For visual clarity, N giants ≥ 20 groups are omitted from the plot, but the median values for these groups are consistent with the trend shown.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Scatter plot comparing group-finding performance for different parameter choices for the giant-only merging and dwarf association techniques presented in Sections 3.2–3.3. Each column corresponds to a different set of parameters for ﹩{R}_{\mathrm{proj}}^{\mathrm{fit}}﹩ and ﹩{\rm{\Delta }}{v}_{\mathrm{proj}}^{\mathrm{fit}};﹩ e.g., (1,2,300) corresponds to ﹩1{R}_{\mathrm{proj}}^{\mathrm{fit}}﹩ and ﹩2{\rm{\Delta }}{v}_{\mathrm{proj}}^{\mathrm{fit}}+300﹩ km s−1 . The plotted markers in each column show the mean purity and completeness (left y-axis) as well as halo mass error (right y-axis) statistics corresponding to each set of candidate parameters. Solid red and blue lines show the product of purity and completeness for the g → h and h → g mappings, respectively. The black bracket marks the range of parameters that best balances purity and completeness and yields low halo mass error.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Multiplicity functions for groups in RESOLVE-B and ECO. The left panel shows groups constructed with the G3 algorithm described in Sections 3.1–3.4. The right panel shows groups as published in Eckert et al. (2017), constructed with friends-of-friends and false-pair splitting. In both panels, the shaded (ECO) and hatched (RESOLVE-B) regions highlight dwarf-only groups. The purple line is a model fit to the ECO G3 multiplicity function and is shown for reference in both panels.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Violin plot illustrating distributions of R proj,gal conditioned on group halo mass for true giant-hosting groups and true dwarf-only groups from the mock catalogs. Diamonds represent median quantities, and solid bars represent 90th percentiles. Violin widths represent the frequency distribution of y-axis data points in each horizontal bin.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Scatter plot comparing group-finding performance for different parameter choices for the dwarf-only group-finding technique from Section 3.4. Each column corresponds to a different set of parameters for ﹩{R}_{\mathrm{proj},\mathrm{fit}}^{\mathrm{gi},\mathrm{dw}}﹩ and ﹩{\rm{\Delta }}{v}_{\mathrm{proj},\mathrm{fit}}^{\mathrm{gi},\mathrm{dw}};﹩ e.g., (1, 2, 300) corresponds to ﹩1{R}_{\mathrm{proj},\mathrm{fit}}^{\mathrm{gi},\mathrm{dw}}﹩ and 2Δproj, fitgi,dw + 300 km s−1 . Symbols and markers are as in Figure 10.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Flow chart conceptualizing the new RESOLVE Gas in Galaxy Groups (G3) group-finding algorithm, consisting of four distinct group-finding processes: (1) giant-only FoF to construct initial giant-only groups, (2) giant-only merging to refine giant-only groups, (3) dwarf association to construct groups containing both giants and dwarfs, and (4) identification of dwarf-only groups.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Scatter plots of stellar mass (left) and cold baryonic mass (right, M * + 1.4M H I) as functions of absolute r-band magnitude for RESOLVE galaxies. The red lines illustrate our definition of the dwarf–giant divide in luminosity, stellar mass, and cold baryonic mass. We use this scale to divide our group finder into four discrete steps, as discussed in Section 3.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Calibration of boundaries used to perform iterative combination in dwarf-only group finding. Data points represent the on-sky distances (left) and relative velocities (right) of giant or dwarf galaxies in giant-hosting groups (i.e., not dwarf-only groups) and are colored by N giants. Black triangles represent the medians of these radii and velocities in different group luminosity bins. The red lines show fits to the black triangles as a function of group-integrated luminosity. The blue dashed lines are the scaled fits, which define the group boundaries for dwarf-only group finding, as described in Section 3.4.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Halo masses in the RESOLVE and ECO G3 group catalogs as a function of group-integrated r-band luminosity. The masses are determined using halo abundance matching as described in Section 3.6.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Linewidths and rms noise levels for ALFALFA-100 detections (Haynes et al. 2018) in the ﹩2530\lt {v}_{{\rm{H}}\,{\rm\small{I}}}\left[\mathrm{km}\,{{\rm{s}}}^{-1}\right]\lt 7470﹩ range, to be used in optical–H I cross-matching and in calculating value-added H I upper limits. (a) Distribution of 21 cm 50% peak linewidths (W 50) of galaxies detected in ALFALFA-100, with black lines marking the 50th, 70th, and 90th percentiles. (b) decl.-dependent rms noise from 21 cm spectra of galaxies detected in ALFALFA-100. Black stars are binned medians and the dashed line is a quartic least-squares fit to those medians.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Summed pulse profiles for the five pulsars in this analysis that were observed at additional telescopes/frequencies. Each profile has been normalized to the same peak height, shows the emission from one full rotation of the pulsar, and is divided into 128 bins. They were generated from all data that were within the degradation tolerances described in Section 3. The telescopes used were LWA1 (57 MHz), LOFAR (149 MHz), GBT (350, 820, 1500, and 2000 MHz), and AO (430 and 1380 MHz). We also show the 149 MHz LOFAR profile of PSR J1816+4510, which is the same profile shown in Stovall et al. (2014). The center frequency of the observations used to generate each profile and the estimated flux density S  ν  at that frequency are listed to the left of each profile. We did not estimate S  ν  from LOFAR profiles, and we estimated S  ν  separately for each LWA1 subband, so we do not list S  ν  estimates beside those profiles. Below each pulsar’s name, we give its DM and spin period.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Summed pulse profiles for 16 of the pulsars in this analysis. Each profile has been normalized to the same peak height, shows the emission from one full rotation of the pulsar, and is divided into 128 bins. They were generated using all GBT data that were within the degradation tolerances described in Section 3. We show 350 MHz profiles in red and 820 MHz profiles above them in blue. Below each pulsar’s name, we give its DM and spin period.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: A skymap showing the GBNCC survey’s sky coverage and its discoveries, which are differentiated between normal (“slow”) pulsars, RRATs, and MSPs. Each pointing is colored based on the date on which it was observed.
Paper: The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps
Authors: Yaqiong Li, Emily Biermann, Sigurd Naess, Simone Aiola, Rui An, Nicholas Battaglia, Tanay Bhandarkar, Erminia Calabrese, Steve K. Choi, Kevin T. Crowley, Mark Devlin, Cody J. Duell, Shannon M. Duff, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Carlos Hervías-Caimapo, Adam D. Hincks, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Arthur Kosowsky, Thibaut Louis, Maya Mallaby-Kay, Jeff McMahon, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas, Eve M. Vavagiakis, Yuhan Wang, Edward J. Wollack
Figure caption: Left: histogram of the distance to each detection’s nearest neighbor with a bin size of 5′. The peak close to zero indicates there are clusters of spurious detections in many of the maps so we cut any candidate with a nearest neighbor of 20′or less. Center: histogram of each candidate’s distance from the nearest zero inverse variance contour, defined to be an inverse variance of less than 1.5 × 10−5 K, with a bin size of 3 pixels. There is a large peak of candidates near zero inverse variance contours, which drops after 3 pixels. We mask out to 5 pixels, cutting 74% of all sources. Right: histogram of each candidate’s distance from the map edge in pixel units with a bin size of 3 pixels. As expected, there is an excess number of candidates near the edge of the map as the map edges are noisy and so appear variable when sampled every 3 days. At a mask size of 5 pixels, we cut off the peak of candidates near the edge.
Paper: The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps
Authors: Yaqiong Li, Emily Biermann, Sigurd Naess, Simone Aiola, Rui An, Nicholas Battaglia, Tanay Bhandarkar, Erminia Calabrese, Steve K. Choi, Kevin T. Crowley, Mark Devlin, Cody J. Duell, Shannon M. Duff, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Carlos Hervías-Caimapo, Adam D. Hincks, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Arthur Kosowsky, Thibaut Louis, Maya Mallaby-Kay, Jeff McMahon, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas, Eve M. Vavagiakis, Yuhan Wang, Edward J. Wollack
Figure caption: 10′ × 10′ 3 day thumbnail maps for each transient. The upper row represents the intensity map with a ±5000 μK color range. The bottom row represents the S/N map after applying a matched filter, with a ±5 color range. Due to the conjugate gradient iteration used to solve the maximum-likelihood mapmaking equation only being run for 10 steps, these maps are effectively mildly high pass filtered. The affected scales have negligible weight in the matched filter. Events 2, 9, 10, and 13 at the bottom of the table represent the four events that are difficult to determine if they are real transients.
Paper: The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps
Authors: Yaqiong Li, Emily Biermann, Sigurd Naess, Simone Aiola, Rui An, Nicholas Battaglia, Tanay Bhandarkar, Erminia Calabrese, Steve K. Choi, Kevin T. Crowley, Mark Devlin, Cody J. Duell, Shannon M. Duff, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Carlos Hervías-Caimapo, Adam D. Hincks, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Arthur Kosowsky, Thibaut Louis, Maya Mallaby-Kay, Jeff McMahon, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas, Eve M. Vavagiakis, Yuhan Wang, Edward J. Wollack
Figure caption: Process of the initial detection, with each plot showing a 0.°3 × 0.°3 map. The first step is to make a mask (middle) on the S/N map (left) selecting pixels that have S/N > 5. The mask is then applied to the flux map (right), and the candidate position, shown as the red cross mark, is evaluated as the center of mass weighted by the flux values within the selected pixels.
Paper: The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps
Authors: Yaqiong Li, Emily Biermann, Sigurd Naess, Simone Aiola, Rui An, Nicholas Battaglia, Tanay Bhandarkar, Erminia Calabrese, Steve K. Choi, Kevin T. Crowley, Mark Devlin, Cody J. Duell, Shannon M. Duff, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Carlos Hervías-Caimapo, Adam D. Hincks, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Arthur Kosowsky, Thibaut Louis, Maya Mallaby-Kay, Jeff McMahon, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas, Eve M. Vavagiakis, Yuhan Wang, Edward J. Wollack
Figure caption: Left: the three transient events consistent with Hygiea observations. Right: the five transient events consistent with Davida observations. All of the plotted positions and observation times are consistent with the asteroids’ paths. The position errors are on the order of 0.′1.
Paper: The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps
Authors: Yaqiong Li, Emily Biermann, Sigurd Naess, Simone Aiola, Rui An, Nicholas Battaglia, Tanay Bhandarkar, Erminia Calabrese, Steve K. Choi, Kevin T. Crowley, Mark Devlin, Cody J. Duell, Shannon M. Duff, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Carlos Hervías-Caimapo, Adam D. Hincks, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Arthur Kosowsky, Thibaut Louis, Maya Mallaby-Kay, Jeff McMahon, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas, Eve M. Vavagiakis, Yuhan Wang, Edward J. Wollack
Figure caption: Light curves for 18 detected transient events on day timescales from the peak. Each frequency is denoted by a different color. We see that in most cases the peak is correlated with all frequencies.
Paper: The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps
Authors: Yaqiong Li, Emily Biermann, Sigurd Naess, Simone Aiola, Rui An, Nicholas Battaglia, Tanay Bhandarkar, Erminia Calabrese, Steve K. Choi, Kevin T. Crowley, Mark Devlin, Cody J. Duell, Shannon M. Duff, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Carlos Hervías-Caimapo, Adam D. Hincks, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Arthur Kosowsky, Thibaut Louis, Maya Mallaby-Kay, Jeff McMahon, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas, Eve M. Vavagiakis, Yuhan Wang, Edward J. Wollack
Figure caption: Surface density of transients for each frequency split between day and night data. The surface density is found by counting the number of transients we are able to detect given the sensitivity level divided by the map area at that sensitivity or lower.
Paper: The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps
Authors: Yaqiong Li, Emily Biermann, Sigurd Naess, Simone Aiola, Rui An, Nicholas Battaglia, Tanay Bhandarkar, Erminia Calabrese, Steve K. Choi, Kevin T. Crowley, Mark Devlin, Cody J. Duell, Shannon M. Duff, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Carlos Hervías-Caimapo, Adam D. Hincks, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Arthur Kosowsky, Thibaut Louis, Maya Mallaby-Kay, Jeff McMahon, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas, Eve M. Vavagiakis, Yuhan Wang, Edward J. Wollack
Figure caption: High-resolution light curves for transient events on minute timescales. Events 1, 2, 5, 6, 7, 8, 9, 10, 13, 14, and 15 show strong signal variation within a space of 4 minutes.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: Top: height–time plot at PA161. This is the direction where the shock was first observed in EUVI 195 Å. On the available points, we applied (a) a linear regression fit and (b) a second-order polynomial fit. The linear fit is represented by the red curve, while the polynomial fit is the blue curve. Bottom: distribution of the calculated speeds for the shock (diamonds) and CME (circles) on top of a COR2A frame at 17:16 UT. It is evident that the CME is expanding asymmetrically, moving faster to the south instead of the north. The highest speeds (above 1800 km s−1) are observed for the shock in the southern part, with a maximum speed of 2260 km s−1, while the lowest speeds are observed in the northern part, with a minimum speed of 950 km s−1. The position of PSP at this time is represented by the green star.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: Eruptive events, i.e., CMEs associated with a solar flare, which either produced SEPs or did not (non-SEPs). Strong solar flares that did not produce an SEP event are depicted with black diamonds. The SEP events with E > 100 and 300 MeV are presented with yellow circles and blue crosses, respectively. The parametric space is the maximum magnitude of the SXR flux on the x-axis and the POS CME speed on the y-axis. Each contour level represents a probability level, with a step of 10%, of an event to produce (or not) an SEP. We apply an ML model (second-order polynomial logistic regression) to distinguish the SEP productive events from the non-SEP cases. The decision boundary level (red line) is 30%. We overplot the 2022 September 5 and 2012 July 23 events with their corresponding probabilities (98% and 96%, respectively) that could produce an SEP event. The metrics of accuracy, MSE, and R 2 are denoted in the top left corner.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: Top row: EUVI 195 Å frames from STEREO-A. At the top of each image, we see the height of the apex in solar radii, the date and time, and the PA where the apex is observed. The shock appeared around 16:00:30 (a) and was observed well up to 16:18:30 (d) at a PA of 160°. The outer part of the shock is denoted with the white dashed line. Bottom row: first appearance of the CME at COR2A (e) at PA ∼ 112° at 16:26. The shock appeared at COR2A at the same PA ∼ 160° as in EUVI-A at around 16:31 (f). Also shown is a clear view of the asymmetric CME and the surrounding shock almost 1 hr later, at 17:16 (g).