adsabs/AstroCLIMB huggingface dataset:
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Fast EUV wave, radio bursts, and associated CME for E3 on 2014 March 28. (a1)–(a3) AIA 211 Å running-difference images showing a large-scale EUV wave associated with the filament eruption and jet. (b1) AIA 304 Å image displaying remote ribbons R4 and R5 during the eruption. (b1)–(b4) LASCO C2 (2–6 R⊙) and STEREO-A COR2 (2–15 R⊙) images depicting the CME and shock. FR is the flux rope. (c1)–(c3) GOES soft X-ray flux profile in the 1–8 Å channel, AIA 304 Å peak counts extracted from regions R3 and R5 (within the box marked in (b1)), and the radio flux-density profile (1 s cadence) at 245 MHz from the RSTN Sagamore Hill Radio Observatory, respectively. The vertical dashed line indicates the onset of energy release at N2. (c4) Dynamic radio spectrum in 25–180 MHz from the RSTN Palehua Radio Observatory.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Schematic diagram of the energy release process in a nested-null-point topology. (a) Initial magnetic configuration of the nested fan-spine topology, along with inflows toward the inner null N1 during the preeruption phase. (b) Slow magnetic reconnection at the BCS near N1 (formation of arcades below N1). Simultaneous slow flare reconnection (brightenings) below the rising filament-channel core builds the flux rope (FR). (c) Explosive breakout reconnection near N1 produces ribbons R3 (quasi circular) and R4 (remote). Simultaneous explosive flare reconnection at the FCS generates a typical two-ribbon flare. Quasiperiodic intensity fluctuations at ribbons R3 and R4 and simultaneous metric–decimetric Type III radio bursts. A fast shock wave forms ahead of the erupting flux rope (onset of Type II radio burst). (d) Interaction of the shock and CME near null point N2 (second breakout reconnection), leading to the appearance of the remote ribbon R5. Slow-mode waves were observed after the passage of the shock through N2 (MHD wave mode conversion).
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: SDO/AIA observations of E3 on 2014 March 28. (a1)–(a3) AIA 211 Å intensity and running-difference images during preeruption opening (marked by arrows) above the right lobe of the pseudostreamer. The first image is overlaid with cotemporal HMI magnetogram contours of positive (white) and negative polarities, scaled at ±100 G. (b1)–(b4) and (c1)–(c4) AIA 211 Å images of the region outlined by the white box in (a1) illustrating a confined filament eruption followed by a successful eruption associated with a recurring jet and an M2.0 flare.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: SEPs (electrons and protons) during all events (E1–E4). (a) Electron flux (12 s cadence) measured by Wind/3DP at different energies ranging from 28 to 523 keV. (b) Electron flux (1 minute cadence) detected by SOHO/EPHIN at different energies ranging from 0.25 to 10 MeV. (c) Proton flux (1 minute cadence) detected by SOHO/ERNE at different energies ranging from 14.5 to 90 MeV. No SEPs were detected from E2 on March 30.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Magnetic connectivity. (a)–(b) magnetic connectivity maps (two different views) for Earth and STEREO-A on 2014 March 29, at 17:45 UT (E1). (c)–(d) the footpoint connectivity of the Earth-directed field lines (from 2.5 R⊙ back to the solar surface) using the PFSS extrapolation for March 29 (pink) and March 30 (green).
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Dynamic radio spectra for E1. (a)–(b) Dynamic radio spectra from e-Callisto (Roswell Observatory, New Mexico). The white line plots the 410 MHz radio flux-density profile (1 s cadence) from the RSTN Sagamore Hill Radio Observatory (scale is on the right y-axis). (c) Dynamic radio spectrum from the RSTN Sagamore Hill Radio Observatory in the 25–180 MHz range. The Type II bursts are indicated by “1” and “2.”
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: LASCO C2 and STEREO-B COR1 observations of the CME for E2 on 2014 March 30. (a1)–(a3) and (b1)–(b3) LASCO C2 (2–6 R⊙) and STEREO-B COR1 (1.4–4 R⊙) running-difference images of the CME and the associated shock (marked by arrows). The flux rope structure is evident in panel (b3). (c1)–(c2) Dynamic radio spectra from the RSTN San Vito station in the 25–180 MHz range and from Wind/WAVES (0.02–13.82 MHz).
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: LASCO C2 observations of the CME and slow blob for E1 on 2014 March 29. (a)–(f) LASCO C2 (2–6 R⊙) running-difference images of the CME and the associated shock (marked by arrows). FR represents the flux rope. Panel (e) illustrates the interaction between the CME shock and the blob.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Evolution of velocity in the midplane at four times during the simulated eruption. The color bar represents the velocity scale. The surface gray shading and the field line colors are consistent with those in the previous figure.
Paper: Dynamical Properties and Velocity Dispersion–Mass Relation of z ∼ 1 Galaxy Clusters from the GOGREEN and GCLASS Surveys
Authors: Shrouk Abdulshafy, Mohamed H. Abdullah, Gillian Wilson, Michael L. Balogh, Raouf H. Mabrouk
Figure caption: Projected phase-space diagrams where vpec and rp are the peculiar velocity and the projected distance, respectively. Application of the GalWeight technique results in the solid black line (cluster boundary) within which are enclosed spectroscopically confirmed galaxies that are identified as cluster members. Black points show all spectroscopically confirmed galaxies within the field of view (shown also in Figure 1), and red points indicate cluster members identified by the GalWeight technique (black contour) but which also fall within R200 (dashed vertical line). Blue circles denote cluster members identified by Biv21.
Paper: Resolving the Nuclear Environments of Tidal Disruption Event Host Galaxies within 45 pc
Authors: Megan Newsome, Iair Arcavi, K. Decker French, Curtis McCully, Ann Zabludoff, Nicholas Stone, Sjoert van Velzen, Tinggui Wang
Figure caption: Top: a close-up of the nuclear spectrum of ASASSN-14li (with an extraction radius within 44 pc of the host center, in black with error ranges in gray) and the averaged spectrum from the extractions at ±88 pc (purple, with error ranges in light purple), both smoothed to visually emphasize the similarities in absorption features. We label the key lines used to analyze the stellar ages: Ca K λ3933 and neutral metals Mg I λλ3832,3838, Fe I λ4046, and Ca I λ4226 (blue vertical lines); and the Balmer series. Bottom: the late-time plateau of ASASSN-14li likely arises from an accretion disk (that was either obscured or only recently formed) as modeled by M. Guolo & A. Mummery (2025) and reproduced here in blue. The black line shows our original nuclear spectrum as observed, while the red line shows how the spectrum of the host nucleus changes without the disk contribution. This does not significantly change the overall flux redward of 4000 Å, which defines the strength of the absorption lines used to determine SFHs with BAGPIPES; however, the strong disk contribution on the bluest end does give the nucleus a steeper upturn blueward of the 4000 Å break, which can still impact stellar population age and mass estimates. We use the resulting subtracted spectrum in red for our BAGPIPES fits.
Paper: Resolving the Nuclear Environments of Tidal Disruption Event Host Galaxies within 45 pc
Authors: Megan Newsome, Iair Arcavi, K. Decker French, Curtis McCully, Ann Zabludoff, Nicholas Stone, Sjoert van Velzen, Tinggui Wang
Figure caption: The nuclear spectrum of each TDE host as taken by HST (black, with errors ranges shown in gray) compared to the SDSS spectrum of each host (red). Each panel is a different host: ASASSN-14li (first/top), ASASSN-14ae (second), PTF09ge (third), and iPTF15af (fourth/bottom). For ASASSN-14li (top panel) we also show the averaged spectrum from the HST extractions at ±88 pc (purple, with error regions shown in light purple). Lines either expected based on ground-based spectra, or newly identified from these data, are marked with vertical lines and labeled in the third panel. Specific lines identified only for one source, as discussed in Section 3, are labeled with vertical lines in the corresponding panel (forbidden lines in ASASSN-14li, top panel; iron lines in PTF09ge, third panel). There are several differences between the archival SDSS spectra and the nuclear spectrum of each host from HST, most notably the identification of forbidden lines in both ASASSN-14li and PTF09ge, as well as the lack of nuclear oxygen emission lines in ASASSN-14ae in contrast with its SDSS spectrum.
Paper: Resolving the Nuclear Environments of Tidal Disruption Event Host Galaxies within 45 pc
Authors: Megan Newsome, Iair Arcavi, K. Decker French, Curtis McCully, Ann Zabludoff, Nicholas Stone, Sjoert van Velzen, Tinggui Wang
Figure caption: The nuclear spectrum of ASASSN-14li (with an extraction radius within 44 pc of the host center, in black) and the averaged spectrum from the extractions centered at ±88 pc (purple), both smoothed to show the emission lines of ionized gas either detected in galaxy-integrated ground-based spectra or detected in this nuclear spectrum. We also include the MUSE spectrum of the same host at the smallest-resolution radius of MUSE (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2) corresponding to light within 88 pc of the SMBH, in blue. We label the locations of emission features (some not identified in any spectrum) with vertical lines, with [O III]  λλ4959,5007 in green; [Fe VII]  λ5276, [Fe XIV]  λ5303, and [Fe X]  λ6375 in brown; [N II]  λ5755 and [N II]  λλ6548,6583 in dark pink; and [S II]  λλ 6716, 6730 in red. Finally, we show the best-fit Gaussian to the [N II]  λ5755 and [Fe X]  λ6375 features, identified in all three spectra, in red overlays. These observations localize the high-ionization coronal lines to an emitting region closest to the host nucleus.
Paper: Resolving the Nuclear Environments of Tidal Disruption Event Host Galaxies within 45 pc
Authors: Megan Newsome, Iair Arcavi, K. Decker French, Curtis McCully, Ann Zabludoff, Nicholas Stone, Sjoert van Velzen, Tinggui Wang
Figure caption: Same as Figure 4, but with the estimated contribution from the central accretion disk (present at late times in ASASSN-14li, including at the time of our observations) removed from the nuclear spectrum. As in the prior figure, the calibration values (N0, N1, and N2) corresponding to the Chebyshev polynomial coefficients used to calibrate the flux have been omitted from the plot for visual clarity of the fits to physical parameters, but their best fits were centered at 1.10 ± 0.16, −0.17 ± 0.04, and 0.09 ± 0.02, respectively. The values found from this fit to the disk-subtracted spectrum are used as the results for the nuclear region throughout this work.
Paper: Resolving the Nuclear Environments of Tidal Disruption Event Host Galaxies within 45 pc
Authors: Megan Newsome, Iair Arcavi, K. Decker French, Curtis McCully, Ann Zabludoff, Nicholas Stone, Sjoert van Velzen, Tinggui Wang
Figure caption: Corner plot showing 2D projection of the fitted parameter space for the nuclear spectrum (light within a 44 pc radius from the nucleus) of ASASSN-14li’s host galaxy. The calibration values (N0, N1, and N2) corresponding to the Chebyshev polynomial coefficients used to calibrate the flux have been omitted from the plot for visual clarity of the fits to physical parameters, but their best fits were centered at 1.06 ± 0.15, 0.17 ± 0.04, and 0.02 ± 0.01, respectively.
Paper: Dynamical Properties and Velocity Dispersion–Mass Relation of z ∼ 1 Galaxy Clusters from the GOGREEN and GCLASS Surveys
Authors: Shrouk Abdulshafy, Mohamed H. Abdullah, Gillian Wilson, Michael L. Balogh, Raouf H. Mabrouk
Figure caption: The black points show offsets (αoff, δoff) from the cluster center for all spectroscopically confirmed galaxies (members and nonmembers) within a velocity gap of Δv ± 3500 km s−1 of each cluster redshift. The red points show spectroscopically confirmed members that satisfy these criteria and also lie within R200 (see also Figure 2, which shows the location of red and black galaxies in projected phase space). The contours were calculated using the two-dimensional adaptive kernel method (2DAKM) and show the density of (red and black) spectroscopically confirmed galaxies.
Paper: Resolving the Nuclear Environments of Tidal Disruption Event Host Galaxies within 45 pc
Authors: Megan Newsome, Iair Arcavi, K. Decker French, Curtis McCully, Ann Zabludoff, Nicholas Stone, Sjoert van Velzen, Tinggui Wang
Figure caption: Same as Figures 4 and 5, but for the offset spectrum (light centered at an 88 pc radius from the nucleus) of ASASSN-14li’s host galaxy.
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-reconstructed power spectrum multipoles of the DM fields with the truth is presented. Top: a comparison of the measured quadrupole (P2) of the DM halos in redshift space (red dashed), the UNet-reconstructed DM field (blue dashed), and the true value (black solid) in real space. The two mass-weighting schemes: “without Mhalo weighting” (left) and “with Mhalo weighting” (right) are chosen to illustrate the reconstructed performance. The shaded regions represent the 2σ confidence level, estimated from the test data set. Bottom: same as in the top panels, but for the higher-order multipole of hexadecapole (P4). As demonstrated, following the application of RSD corrections, the reconstructed multipoles of the quadrupole and hexadecapole exhibit good agreement with the true values at the 2σ level within the range of k ∈ [0.04, 0.4] h Mpc−1. Furthermore, the scheme of “with Mhalo weighting” is observed to provide a higher reconstruction accuracy and a smaller statistical uncertainty.
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-reconstructed momentum/velocity power spectra with the simulation truth for the two mass-weighting schemes. The specific field and the weighting scheme are clearly indicated in each panel. The bottom panels present the resulting relative deviations. In each plot, the shaded region represents the 2σ statistical uncertainty, estimated from a total of 25 boxes (each with a side length of 600 Mpc h−1) in the test data set. Based on Equations (2) and (3), the linear predictions are also provided for comparison, deviating increasingly from the true values as k increases. As seen, the relative deviations are in the range of R ∈ [−0.06, 0.06] at the scales of k ∈ [0.05, 0.1]. The average relative deviations of auto power spectrum are −0.013 ± 0.03, −0.011 ± 0.07, 0.033 ± 0.05, −0.004 ± 0.053 from left to right, respectively.
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 two-dimensional anisotropic 2PCFs, ξ(r⊥, r∥), of density fields between the prediction and the simulation truth in real space for “with Mhalos weighting” scheme. The results are based on a total of 25 boxes, each with a side length of 600 Mpc h−1. The contours were generated from the correlation values of [0.02, 0.06, 0.12], respectively. The gray shaded regions and blue dashed contours represent the derived ξ of the true and reconstructed fields in real space, respectively. The red dotted contours represent the redshift-space 2PCF of the DM halos. It is evident that despite the input being that of the DM halo density in redshift space, the reconstructed 2PCF is in good agreement with the true value. This suggests that UNet is capable of successfully recovering the real-space 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: Same as in Figure 11, but for the momentum/velocity divergence fields with two different mass-weighting schemes. The specific field and the weighting scheme are clearly indicated in each panel. The relative deviations fall within the range of [−0.1, 0.1] at the scale of k ∈ [0.05, 0.3], respectively, indicating a relatively accurate reconstruction. Compared to the linear predicted power spectra, the UNet model provides a more accurate reconstruction, especially when k > 0.1 h Mpc−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: The successes and failures of 3DBAROLO, FAT, and WKAPP for a sample of 100 idealized low-velocity galaxies generated by MCGSUITE. Circles and crosses indicate whether the models are accepted based only upon a visual inspection of their outputs. The colors of the symbols indicate whether (blue) or not (red) the models match the underlying MCGSUITE model for a particular mock cubelet. In other words, red circles would contaminate a final catalog. The panels in the upper row show the MCGSUITE size and inclination, with the size of the symbols mapping to the input H I mass, while the lower row shows ell_maj(the SOFIA-2 size estimate) and modeled inclination, with the size of the symbols mapping to the modeled ﹩{V}_{{\rm{\max }}}﹩. The 11 low-velocity WALLABY detections are shown in the bottom right panel.
Paper: First X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 17+2
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Alexandra J. Tetarenko, Pau Bosch-Cabot, Herman L. Marshall
Figure caption: First panel: Model fitted joint spectra of GX 17+2 as observed by IXPE DU1 (spring green), IXPE DU2 (green yellow), IXPE DU3 (dark green), NICER (orange), and NuSTAR (plum). The spectra are fitted with the tbnew∗(diskbb+nthcomp+relxillNS)∗polconst∗const model in the 1.5–30 keV energy band. The total model is shown with the dotted black (NICER, NuSTAR, and IXPE). The spectral components are consistent with the previously reported X-ray studies of the source. Second panel: The residuals between the data and the best-fit model. Third panel: The fraction of the different model components over the total model. The data for the IXPE, NICER, and NuSTAR spectra are rebinned only for plotting and representation purposes.
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 moment 0 and moment 1 maps for the 11 low-velocity WALLABY detections. The moment 1 map uses a custom color scheme from COSMOSCANVAS (J. English et al. 2024) designed so that the approaching blueshifted gas appears to come out from the page, while the redshifted gas goes into the page. The cyan circle in the moment 0 maps shows the size of the beam, and the magenta cross shows the location of the kinematic center listed in Table 1. The light gray grid illustrates lines of R.A.–decl. relative to the map coordinates. The moment 0 maps use a linear scale that causes them to appear to be smaller in size than the moment 1 maps, but the two do indeed cover the same parts of the sky. The panels are organized by optical type, with the top row containing the dwarf-like galaxies, the second row containing the irregular detections, the third row containing the face-on spirals, and the bottom row containing those detections not found in DECaLS.
Paper: First X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 17+2
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Alexandra J. Tetarenko, Pau Bosch-Cabot, Herman L. Marshall
Figure caption: Top: color–color diagram constructed from all NuSTAR observations of GX 17+2 (Observation IDs starting with 30101023, 30902026, and 91001339). Time bins of 128 are used. The CCD indicates that the source was in the NB branch of its Z-track during our IXPE observations (black data points; gray are all previous NuSTAR observations of GX 17+2). Bottom: hardness–intensity diagram constructed from the NICER observations simultaneous to our IXPE observation of GX 17+2. The NICER and NuSTAR CCDs indicate that the source was in the NB branch of its Z-track during the IXPE observations.
Paper: First X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 17+2
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Alexandra J. Tetarenko, Pau Bosch-Cabot, Herman L. Marshall
Figure caption: A comparison of the X-ray PA and radio jet position angle obtained from our study of GX 17+2. The X-ray polarization degree and angle are determined with the PCUBE algorithm, at the 68%, 95% and 99% confidence levels, in the 2–8 keV energy band (in blue). The PA (+1°) and thus potential radio jet/jet axis position angles (+1° if parallel or −89° if perpendicular) are shown in maroon and black, with the gray lines representing the uncertainties on the radio jet position angle (±5°). The lower limit (−5°) on the uncertainty of the jet axis position angle (−94°or 86°) goes beyond the plot. Our study shows the consistency between the X-ray PA and radio jet position angles in the case of GX 17+2.
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 rotation curves (top panel) and surface density profiles (bottom panel) for the 11 low-velocity kinematic models. In each panel, the gray lines show the entire suite of WALLABY PDR kinematic models.