adsabs/AstroCLIMB huggingface dataset:
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: Comparison of the reconstructed fields by UNet with the true fields for velocity (upper) and momentum (lower) for slices from the test set, using the “without Mhalo weighting” weighting scheme. Each slice volume is ﹩68\times 68\times 23\,{({h}^{-1}\,\mathrm{Mpc})}^{3}﹩. The sparse DM halo field (δs), the true velocity, and the reconstructed fields are displayed from left to right, along with the corresponding histograms. For each slice, the rightmost panel displays the statistical histogram distribution of the magnitude and direction of the velocity samples. The colored arrows in the velocity field indicate the magnitude and direction of the velocity. Through both visual and statistical analysis of the histogram, it can be observed that even in the absence of specific mass information for each DM halo, UNet is capable of accurately reconstructing the velocity/momentum fields.
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: Comparison of the UNet-predicted density power spectra with the true one. Each plot displays the predicted (blue) and true (black) values, along with the redshift-space power spectrum of the DM halos (red). The left and right panels illustrate the weighting schemes of “with Mhalo weighting” and “without Mhalo weighting.” A total of 25 boxes (each with a side length of 600 Mpc h−1) were employed in the test data set to estimate the mean and standard deviation (shaded region) for the power spectra. The relative deviations, R, are presented in the bottom panels. In all cases, the UNet model yields a good reconstruction performance, insensitive to the weighting scheme. Thus, using DM halo mass as a weight does not significantly affect the reconstruction of the DM density field.
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: Similar to Figure 6, but for the velocity divergence (θv) and the momentum divergence (θm), with the two mass-weighting schemes. The correlation between the predicted and true distributions remains strong even when the specific mass values are not considered. This demonstrates that our model is capable of accurately predicting the distribution of DM halos even in the absence of specific mass values. These findings indicate that the mapping from the sparse DM halo number density field in redshift space to the real-space DM velocity/momentum fields can be successfully and accurately learned by our model.
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: Comparison of the predicted joint distribution with the simulation truth for the “with Mhalo weighting” weighting scheme. The top-left and bottom-left panels show the joint distributions of density–velocity, ρ(δ∣v), and density-momentum, ρ(δ∣m), respectively. The top-right and bottom-right panels show the joint distributions of density–divergence, ρ(δ∣θv) and ρ(δ∣θm), respectively. These distributions were obtained using a large box with a side length of 600 Mpc h−1. The results demonstrate that for all DM halo number densities with δ + 1 ∈ [0, 8], the predicted velocity distributions exhibit good consistency with the true values.
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: Loss of the training (black) and validation (red) sets. The UNet model achieves convergence after approximately 1000 epochs of training for the DM density, DM velocity, and DM momentum (from left to right), respectively. The loss function utilized for all models is the MSE loss function, as defined in Equations (5) and (6).
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: Same as in Figure 8, but for the weighting scheme of “without Mhalo weighting.” It is evident that the predicted joint distributions remain consistent with the simulation truth, even in the absence of precise mass values.
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: Same as in Figure 4, but for the divergence fields for velocity (upper) and momentum (lower).
Paper: The Rotational Spectrum of 1-cyanocyclopentene and Its Search towards TMC-1
Authors: Sergio Mato, José Cernicharo, Iker León, Brett A. McGuire, Elena R. Alonso
Figure caption: (a) Broadband CP-FTMW spectrum of 1-CNCPE from 6 to 16.5 GHz, pointing out the a-type R-branches with their respective ﹩{J}^{{\prime} }\leftarrow J﹩. (b) Zoom section of the spectra where the pair 0+ (blue) and 0−(red) states for 21,1 ← 11,1 a-type transition is observable. (c) Comparative between CP-FTMW and MB-FTMW for the transition 11,1 ← 00,0. ﹩{F}^{{\prime} }\leftarrow F﹩ in transitions are shown in blue for 0+ and red for 0−. (d) Comparative between CP-FTMW and MB-FTMW for the transition 42,2 ← 31,2.
Paper: Dissecting the Mass Quenching in TNG50: Galaxy Size Determines the Quenching Mode
Authors: Haochen Jiang, Enci Wang, Kai Wang, Chengyu Ma, Xu Kong
Figure caption: The evolution history of three example quiescent galaxies selected at z = 0 from the TNG50 simulation. The left panels show the SFR evolution within two radii (black: twice the effective radius; blue: within the bound subhalo), and the magenta dashed line shows the threshold below which the galaxy is classified as quiescent. The look-back time and redshift are labeled on the bottom and top x-axis, respectively. The right panel shows the mass evolution for the stellar component (black), gaseous component (red), and the SMBH (green), defined with twice the effective radius. The green vertical dotted lines mark the moment the SMBH growth flattens and the kinetic AGN feedback is triggered. The magenta vertical dotted lines mark the last quenching event. These three example galaxies are selected from three types of quenching patterns: fast quenching (Fast-QG), rejuvenated quenching (Reju-QG), and slow quenching (Slow-QG).
Paper: The Rotational Spectrum of 1-cyanocyclopentene and Its Search towards TMC-1
Authors: Sergio Mato, José Cernicharo, Iker León, Brett A. McGuire, Elena R. Alonso
Figure caption: Selected lines of c–C5H7CN as observed with the QUIJOTE line survey toward TMC-1 (J. Cernicharo et al. 2021, 2024). The abscissa corresponds to the rest frequency of the lines adopting a velocity for the source of 5.83 km s−1 (J. Cernicharo et al. 2020). The ordinate is antenna temperature corrected for telescope and atmospheric losses. The rotational quantum numbers are indicated in each panel. Blanked channels correspond to negative features produced in the folding of the frequency switching data. The red line shows the synthetic spectrum obtained for a Trot of 8 K and a column density of 9 × 1010 cm−2. Other features arising from known and unknown species are indicated in blue. A 3σ value to the column density of 3 × 1010 cm−2 can be obtained by stacking the data for the 12 selected transitions.
Paper: The Rotational Spectrum of 1-cyanocyclopentene and Its Search towards TMC-1
Authors: Sergio Mato, José Cernicharo, Iker León, Brett A. McGuire, Elena R. Alonso
Figure caption: Molecular scheme depicting pure hydrocarbon five-membered cycles and their cyano derivatives. The species detected in the ISM are highlighted by blue stars.
Paper: The Rotational Spectrum of 1-cyanocyclopentene and Its Search towards TMC-1
Authors: Sergio Mato, José Cernicharo, Iker León, Brett A. McGuire, Elena R. Alonso
Figure caption: 3D structure of 1-CNCPE with principal inertial axes.
Paper: The Rotational Spectrum of 1-cyanocyclopentene and Its Search towards TMC-1
Authors: Sergio Mato, José Cernicharo, Iker León, Brett A. McGuire, Elena R. Alonso
Figure caption: (a) Low-resolution spectrum recorded in the 27–38.7 GHz range using the Stark-modulation spectrometer. (b) Zoomed-in section of the Stark-modulation low-resolution spectrum.
Paper: The Rotational Spectrum of 1-cyanocyclopentene and Its Search towards TMC-1
Authors: Sergio Mato, José Cernicharo, Iker León, Brett A. McGuire, Elena R. Alonso
Figure caption: Section of the millimeter-wave spectra.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: The surface brightnesses of the PPOs from the 1.3 mm and 3 mm observations in W51-E (left) and W51-IRS2 (middle). For 1.3 mm, the surface brightnesses are measured from the 1.3 mm images convolved to the 3 mm image beam. Models of MBB surface brightness with surface density Σ = 1021–1027 cm−2 are presented as dashed curves with colors denoting MBB temperature, T = 20, 40, 60, and 80 K, following Equation (4). The surface brightness parameter space that MBBs with T = 5–400 K can occupy is shaded with green colors. We can derive the MBB temperatures of the PPOs lying within the green area, and they are color coded based on the derived MBB temperatures. The PPOs outside the green area have empty symbols. Depending on which band the PPOs are resolved, they are represented as different shapes: circles (resolved in both 1.3 mm and 3 mm), triangles pointing up (resolved only in 3 mm) and pointing right (resolved only in 1.3 mm), and diamonds (unresolved in both bands). Since the upper limits of the size are imposed uniformly for unresolved sources, the derived temperatures are lower limits. The dashed diagonal lines are spectral index α = −1, 0, 1, 2, 3, and 4 measured from the integrated fluxes. The brightness temperature corresponding to a surface brightness of ﹩1\,{\rm{Jy}}\,{{\rm{arcsec}}}^{-2}﹩ is 27 K at 1.3 mm and 153 K at 3 mm.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Number of core fragments as a function of their core fluxes (upper row), core fluxes subtracted by their fragment fluxes (lower row), and masses (right). Each cyan (W51-E) and orange (W51-IRS2) data point with error bars represents the flux or the mass of the core vs. the number of fragments. For the core fluxes, we use the integrated flux measured from the ALMA-IMF 1.3 and 3 mm continuum data. The fluxes measured from another high-mass star-forming region, Sgr B2 (N. Budaiev et al. 2024), are rescaled to the distance of W51, 5.4 kpc, and the rescaled fluxes and the number of fragments are displayed for comparison. For the number of PPOs, a small random deviation on the y-axis is given to differentiate each other visually. The medians of the fluxes and masses for each PPO number bin on the y-axis are plotted with square marks and connected with dashed lines. The horizontal dashed lines and some absence of squares in the lower left panel are due to the negative medians of core residual flux at 3 mm within the range of uncertainties. Each solid line represents 100 Markov Chain Monte Carlo (MCMC) runs of the linear fits to ﹩\mathrm{log}{M}_{{\rm{core}}}﹩–Nfrag. The legend displays the median of the slope and the y-intercept of these MCMC runs.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Examples of core fragmentation in W51-E. The cyan ellipses are dust cores and the green ellipses are cores contaminated with free–free emission. The size of the ellipse represents the boundary of the core, defined as the sum of the FWHM of the core and the FWHM of the synthesized beam. The background image of the bottom is an ALMA-IMF 1.3 mm continuum map. The field of view of the high-res image is displayed with yellow (1.3 mm) and red (3 mm) circles at the top of the ALMA-IMF map. The region enclosed by the white square at the bottom of each image is magnified with a background image of a high-res Band 6 continuum at the top. The locations of PPOs are indicated by the arrows. The PPOs detected in both bands have arrows with blue (dust dominated), orange (possibly free–free contaminated), and green (free–free contaminated) colors. The yellow and magenta arrows indicate an object identified only in 3 mm and 1.3 mm, respectively.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: The same as Figure 9 for the W51-IRS2 region.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Left: histogram of the integrated fluxes of the PPOs excluding sources contaminated by free–free emission at 1.3 mm and 3 mm. Right: lower limits of PPO masses using the 3 mm integrated fluxes by assuming a constant dust temperature of 40 K (﹩{M}_{{\rm{PPO}},{\rm{lowlim}}}﹩).
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Cumulative distribution of the radii of the high-res sources. The cumulative function is generated by a survival analysis with the Kaplan–Meier estimator provided by the lifelines package. The function is censored on the left side by excluding unresolved or undetected sources in the analysis.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Histogram of the number of core fragments in W51-E (blue) and W51-IRS2 (orange). Cores without free–free emission in the same field of view of the high-res 3 mm images are used in the analysis.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: The dust temperatures estimated by the MBB model in Figure 6. The MBB temperatures for unresolved sources are the lower limits.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: The axis ratio between the major and the minor axes of the high-res sources.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Top left, top right, and bottom left panels show the density distribution as a function of heliocentric distance and position angle, measured from the solar north. The dates and times of the LASCO C2 images used to determine the densities are also shown in the respective titles. The bottom right panel shows a few 1D cuts at chosen heliocentric distances as a function of position angles at the three date/times shown in the other panels.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Left panel: shows the expected free–free emission for a 1 MK plasma of density 106 cm−3 in presence of different magnetic field strengths. Right panel: predicted brightness temperature for varying fraction of magnetized plasma due to combination of gyroresonance and thermal free–free emission. The magnetic field is assumed to be 10G.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Panels from top left in clockwise manner: 2024 April 12, April 14, April 11, and April 22. The colorbar shows the time difference in minutes from the event time shown in Figures 2, 5, and 7 for April 12, April 14, and April 22. April 22 shows a 1 hr window where we identified strong ionospheric activity. The black-dashed line marks the 0.1 MK brightness temperature. The left and right subpanels of each day show the flux density variation along a 1D cut aligned along the heliocentric longitude and latitude, respectively. The 1D cuts passes through the solar center on the sky plane.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Left panel: density difference between April 22 17:59 and 17:47 UT as a function of heliocentric distance and position angle, measured from solar north. The color scale has been saturated between −4 × 104 and 4 × 104 cm−3. Right panel: shows the density difference at 3.75 R⊙ as a function of position angle.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Shows a model gyrosynchrotron spectrum, which can explain the observed data from April 12 (Figure 2). The relevant parameters used to compute the model spectrum are indicated in the figure.