adsabs/AstroCLIMB huggingface dataset:
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Correlations of the line emission contribution with AGN and outflow properties. The line emission contribution from Campbell et al. (2025, submitted) is plotted as a function of the AGN luminosity (top left), Eddington ratio (top middle), dust mass (top right), dust temperature (bottom left), mass outflow rate (bottom middle), and outflow kinetic energy (bottom right). The outflow mass rates using optical [O III] emission (blue) and MIR [Ne V] emission (red) are displayed. These values are shown in Table 1.
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: Stellar and gas overlay image pairs (left and right of each pair, respectively) for the nine low-velocity galaxies with optical counterparts. For most stellar images, the blue, green, and red colors are from DECaLS g-, r-, and z-band images. In the cases of WALLABY J130213–171416 and WALLABY J130311–172230, where the r-band images are not available, the green color is generated by an average (g + z)/2 image. The raw images are processed with CARTA to have a logarithmic stretch and adjustments to the bias and contrast, then passed through GIMP for coloring and further balancing to make the final three-color stellar images. In the gas overlay panels, the green–red colors (approaching–receding) are set by the moment 1 map with the intensity set by the moment 0 map. The color map itself is a custom COSMOSCANVAS map. The white line shows the size of the WALLABY beam.
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: The structural parameters of the 11 low-velocity galaxies compared to the larger WALLABY sample (gray circles). The filled symbols indicate that the optical and kinematic inclinations agree. Detections with open symbols either are missing optical inclinations (see N. Deg et al. 2024 for details) or have optical and kinematic inclinations that disagree with each other. Squares show detections with kinematic inclinations below 40°, while stars show those with inclinations above 40°. WALLABY J125907–121329 is indicated by a triangle even though it has an inclination of 41° as it does not have robust uncertainties measured for its structural parameters (see N. Deg et al. 2024 for details on the uncertainty derivations). The red lines and shaded regions are the best-fit and 1σ widths derived from the full set of WALLABY PDR galaxies in N. Deg et al. (2024).
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: An example diagnostic plot comparing 3DBAROLO, FAT, and WKAPP models to the underlying MCGSUITE model for a test mock galaxy used in Section 3. The test galaxy is listed at the top, named by the size (ba = beams across) and logarithmic mass. The black, red, yellow, and blue (missing in this case) lines in the rotation curve and surface density panels (lower left and right panels, respectively) show the underlying MCGSUITE model and the FAT, 3DBAROLO, and WKAPP models, respectively. Similarly, the values for the geometric parameters (inclination, position angle, centroid, and systematic velocity) and the velocity dispersion for the underlying model and each fit are listed in the table below. In this particular case, the various fits do not agree with the underlying model.
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: An example diagnostic plot comparing 3DBAROLO, FAT, and WKAPP models to the underlying MCGSUITE model for a test mock galaxy used in Section 3. The test galaxy is listed at the top, named by the size (ba = beams across) and logarithmic mass. The black, red, yellow, and blue lines in the rotation curve and surface density panels (lower left and right panels, respectively) show the underlying MCGSUITE model and the FAT, 3DBAROLO, and WKAPP models, respectively. Similarly, the values for the geometric parameters (inclination, position angle, centroid, and systematic velocity) and the velocity dispersion for the underlying model and each fit are listed in the table below. In this particular case, all fits agree with the underlying model.
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: Biases in the rotation curves from fits to the sample of low-mass galaxies that do not agree with the initial MCGSUITE model. Solid and dashed lines are for the normal and VD populations, respectively. The line colors show the difference between the true and measured inclination.
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: The channel maps for an MCGSUITE mock cube made with ﹩{\mathrm{log}}_{10}({M}_{{\rm{H}}\,{\rm\small{I}}}/{M}_{\odot })=8.04﹩, DH I = 4 (beams), and ikin = 56°. The mass, diameter, and inclination are set based on the measurements of WALLABY J131206+052832. The magenta circle in the lower left shows the size of the beam.
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: The results of fitting the extended VD suite of models at 4 km s−1 spectral resolution for 3DBAROLO and FAT. Symbols and colors are the same as Figure 3.
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: The channel maps for WALLABY J131206+052832. The magenta circle in the lower left shows the size of the beam.
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: The DSS-II blue images for the two galaxies without DECaLS data. The yellow contour shows the 1 M⊙ pc−2 surface density limit.
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: Top and middle: the sum of fragment fluxes as a function of core fluxes (top) and core envelope fluxes (middle) at 1.3 mm and 3 mm. If the integrated flux of more than one PPO is missing in the plotted band, the PPO fluxes are represented as empty circles; otherwise, they are shown as filled circles. The diagonal dashed lines mark the fragmentation efficiency ϵfrag = 1, 0.1, and 0.01 in the top row and ϵfrag = 0.5, 0.1, and 0.01 in the middle row. Bottom: fragmentation efficiencies (ϵfrag) as a function of core masses. The fragmentation efficiency is defined as the ratio between the sum of all the PPO fluxes and core fluxes in each band. The horizontal dashed line marks ϵfrag = 1. Some cores with ϵ > 1 are not physically plausible and are instead attributed to measurement uncertainties.
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: Upper left: the thermal Jeans masses of the cores in W51-E and W51-IRS2. Upper right: the Jeans number and number of core fragments. The ratio of the actual number of fragments to the Jeans number is the Jeans efficiency, indicated as gray dashed lines. The average Jeans efficiency in each region is plotted as colored thin dashed lines. Lower left: histogram of Jeans efficiency. For comparison, the Jeans efficiencies of envelopes in Perseus (R. Pokhrel et al. 2018) are also displayed in green. The average of Jeans efficiency in W51-E and W51-IRS2 is 5% and 20%, respectively, which are lower than the average in Perseus (∼40% for core to envelope and ∼50% for envelope to protostellar object). Lower right: core masses and Jeans efficiencies in W51-E, W51-IRS2, and Perseus (R. Pokhrel et al. 2018).
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 fragmentation efficiency (ϵfrag; left), the number of fragments (Nfrag; middle), and the ratio between the brightest and the second brightest PPOs (second(FPPO)/max(FPPO); right) as a function of the brightest PPO flux (max(FPPO)) at 3 mm in W51-E and W51-IRS2. The color of each data point denotes core temperature. The filled and empty circles denote the complete and incomplete samples, respectively, the as same as Figure 14.
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: An example of 2D Gaussian modeling for the ALMA 1.3 mm flux measurement of PPOs (#2) in W51-E. Upper row: the 1D profile of the continuum image and the model along the major axis (left) and minor axis (center). The solid lines indicate the image profile before (black) and after background subtraction (blue). The orange dashed lines represent the model profile fitted to the background-subtracted image profile. The residual, the image profile subtracted by the model, is presented on the upper right panel. Bottom row: cutouts of the original image (lower left), the model (lower center), and the residual image (lower right). The cyan solid ellipse at the center indicates the FWHM of the 2D Gaussian model whereas the cyan dashed ellipses are the annulus where the local background value is evaluated. The size of the synthesized beam of the image is displayed in the left lower corner.
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: Comparison of 1.3 and 3 mm fluxes and spectral index groups (optically thick dust emission or possibly free–free contaminated and free–free contaminated), defined in Section 3.2, of ciPPOs, caPPOs, and ffcaPPOs in W51-E (top row) and W51-IRS2 (bottom). The core samples used in this plot have masses higher than the completeness limit of W51-E, 3.86 M⊙. The median of each quantity is denoted by a vertical dashed line. The p-values of the two-sample K-S test for ciPPOs and caPPOs, caPPOs and ffcaPPOs, and ciPPOs and ffcaPPOs are displayed at the top of each panel.
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: Comparison between the Jeans masses of the cores and the PPO masses associated with each core estimated from the constant temperature model (T = 40 K). The PPOs associated with the same core are connected with vertical dashed lines. A majority of the PPOs exhibit a lower mass limit exceeding the Jeans mass of the core.
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: Top and middle: the 1.3 and 3 mm fluxes of all PPOs as a function of their parent core fluxes (top) and core envelope fluxes (middle). Bottom: the PPO flux ratios normalized to the brightest PPO flux. For clarity, the flux of the brightest PPO in each core is omitted. Only cores in which there are at least two fragments are displayed in this plot. In all panels, the fluxes of the PPOs associated with the same parent core are connected with vertical dashed lines.
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 fluxes of the brightest PPO associated with each core as a function of 1.3 and 3 mm core fluxes (top), core fluxes subtracted by the sum of their fragment fluxes (middle), and core masses (bottom). The error bars denote the errors of the core fluxes and those of the integrated PPO fluxes. If the integrated flux of more than one PPO is missing in the plotted band, the PPO fluxes are represented as empty circles; otherwise, they are shown as filled circles. The dashed lines in the top row indicate the one-to-one line.
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: Histograms of temperatures, sizes, masses, and mass densities of the unfragmented and fragmented cores in W51-E (top) and W51-IRS2 (bottom). The median of each quantity is denoted by the vertical dashed line. The p-values from the two-sample Kolmogorov–Smirnov (K-S) test for the W51-IRS2 cores are displayed on the bottom row.
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: contours at 43 MHz and 17:16 on 2024 April 12 are overlaid on the nearest LASCO C2 difference image. Difference has been taken with respect to a 2 hr prior image. The lowest contour is at 0.04 MK and then increases in multiples of 2. Middle panel: multiple frequency radio contours are overlaid on the same LASCO C2 difference image. The outer contour level at each frequency is at 0.04 MK. Black-dashed circle in the left and middle panels shows the radio Sun at 43 MHz. The solid circles show the optical disk of the Sun. Right panel: shows the spectrum extracted from the region marked in the left panel. The spectrum has been extracted from the original image before any smoothing was done. Circles have been used to denote detections. The black line shows a spectrum following ν−2 dependence, where ν is the observation frequency. All radio contours, except the ones shown in the left panel using blue color, have been obtained by smoothing the images using a Gaussian function with standard deviation of ﹩7\mathop{.}\limits^{{\rm{^{\prime} }}}5﹩.
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 panel: radio contours at 34 MHz and 16:48 on 2024 April 14 are overlaid on the nearest LASCO C2 difference image. Difference has been taken with respect to an LASCO C2 image 1 hr prior to this time. The lowest contour is at 0.08 MK and then increases in multiples of 2. Negative contour at −0.08 MK (corresponding to lowest positive contour) is drawn using a cyan-dashed line. The fact that no dashed line is visible indicates the absence of any negative peak whose absolute value exceeds or is equal to 0.08 MK. Top middle panel: multiple frequency radio contours are overlaid on the same LASCO C2 difference image. The outer contour level at each frequency is at 0.08 MK. The black-dashed line in left and middle panel shows the radio Sun at 34 MHz. The solid circles show the optical disk of the Sun. Top right panel: brightness temperature spectrum of two regions shown. The marker color used to show the spectrum of each region is same as that used to indicate the location of the corresponding region in the top left panel. Properties of the markers and colors are the same as those in Figure 2. Triangles have been used to denote the nondetections and represent the 5σ upper limit. The red and magenta lines show the spectra following ν−2 dependence, where ν is the observation frequency. Bottom panels: difference 34 MHz images for 16:45, 16:48, and 16:51 UT are shown in the bottom left, bottom middle, and bottom right panels, respectively. Difference has been taken with respect to the image at 16:32. The color bar is highly saturated and nonlinear and is the same for the three images.