adsabs/AstroCLIMB huggingface dataset:
Paper: Spectral Observations and Modeling of a Solar White-light Flare Observed by CHASE
Authors: De-Chao Song, Jun Tian, Y. Li, M. D. Ding, Yang Su, Sijie Yu, Jie Hong, Ye Qiu, Shihao Rao, Xiaofeng Liu, Qiao Li, Xingyao Chen, Chuan Li, Cheng Fang
Figure caption: (a) Construction of 18 flare loops based on the GOES SXR 1–8 Å time derivative plus Fermi HXR 30–300 keV emission, with the heating episodes indicated by the red vertical lines. The green curve represents the area of CHASE Hα brightenings after a cubic spline interpolation. (b) Electron-beam parameters including the energy flux, low-energy cutoff, and spectral index used in the simulations for 18 loops (L1–L18). Note that the fitting uncertainties of low-energy cutoff and spectral index are plotted in error bars, which are quite small mostly. (c) and (d) Fermi HXR spectral fitting with a thermal component (cyan) plus a nonthermal component (magenta) for two time intervals corresponding to the heating episodes of L6 (c) and L11 (d) in principle. The fitting parameters including low-energy cutoff (E  c ) and spectral index (δ) for the nonthermal component are shown in the panels.
Paper: Spectral Observations and Modeling of a Solar White-light Flare Observed by CHASE
Authors: De-Chao Song, Jun Tian, Y. Li, M. D. Ding, Yang Su, Sijie Yu, Jie Hong, Ye Qiu, Shihao Rao, Xiaofeng Liu, Qiao Li, Xingyao Chen, Chuan Li, Cheng Fang
Figure caption: (a)–(c) Temporal evolution of the relative enhancements of HMI continuum, CHASE continuum, Fe I line, and Hα line for kernels K1–K3 summed over an area of 3″ × 3″, together with the SXR 1–8 Å flux and its time derivative. The uncertainties of continuum and line intensity enhancements are plotted in error bars. Note that the uncertainty in Hα is quite small compared with its enhancement. The continuum intensity is from the wavelength at 6568.2 Å as indicated by the magenta vertical line in panels (d)–(f) and the Fe I and Hα line intensities are integrated over the wavelengths of ±0.5 Å and ±2.3 Å, respectively. The black dashed vertical line denotes the peak time of the three intensity curves from CHASE. (d)–(f) Temporal evolution of the Fe I and Hα line profiles (averaged over an area of 3″ × 3″) at K1–K3. The line centers of Fe I and Hα are marked by two black dotted vertical lines in each panel.
Paper: Spectral Observations and Modeling of a Solar White-light Flare Observed by CHASE
Authors: De-Chao Song, Jun Tian, Y. Li, M. D. Ding, Yang Su, Sijie Yu, Jie Hong, Ye Qiu, Shihao Rao, Xiaofeng Liu, Qiao Li, Xingyao Chen, Chuan Li, Cheng Fang
Figure caption: (a) Light curves of GOES SXR 1–8 Å, its time derivative, Fermi HXR 30–300 keV, and EOVSA microwave 6–18 GHz for the flare. (b) HMI continuum (near 6173 Å), CHASE continuum (at 6568.2 Å), Fe I (integrated over ±0.5 Å), and Hα (integrated over ±2.3 Å) intensity curves summed over the field of view of the images as shown in panels (c)–(g), together with the SXR 1–8 Å flux and its time derivative. The gray and blue vertical lines in panels (a) and (b) denote the peak times of the SXR flux and its time derivative, respectively. (c)–(h) CHASE continuum, HMI continuum (base difference), CHASE Fe I (base difference), CHASE Hα, and AIA 131 Å images for the flare. Three white-light brightening kernels (K1–K3) are indicated by three arrows in panels (c)–(f). The white and blue contours in panel (c) mark the sunspot umbra and penumbra, respectively. The magenta and orange contours in panel (d) denote the magnetic polarities at +400 and −400 G, respectively. The yellow and red contours in panels (d)–(h) show the microwave sources at 15.2 and 17.8 GHz, respectively.
Paper: Spectral Observations and Modeling of a Solar White-light Flare Observed by CHASE
Authors: De-Chao Song, Jun Tian, Y. Li, M. D. Ding, Yang Su, Sijie Yu, Jie Hong, Ye Qiu, Shihao Rao, Xiaofeng Liu, Qiao Li, Xingyao Chen, Chuan Li, Cheng Fang
Figure caption: The line profiles of Fe I (a)–(c) and Hα (d)–(f) selected from a single pixel at kernels K1–K3. The gray and black curves refer to the preflare profile and the profile at the peak time, respectively, while the blue curve represents the contrast profile (difference between them). A single Gaussian fitting and a bisector method are used to derive the Doppler velocities for Fe I and Hα, respectively, based on the contrast profiles. The Doppler velocity plus an uncertainty is shown in each panel, together with the relative enhancements of the continuum and Fe I and Hα lines. Note that for Hα, the velocity value represents the median of the velocities at different intensity levels from bisector. The black and green vertical lines in each panel indicate the line center and the median Doppler velocity, respectively.
Paper: Spectral Observations and Modeling of a Solar White-light Flare Observed by CHASE
Authors: De-Chao Song, Jun Tian, Y. Li, M. D. Ding, Yang Su, Sijie Yu, Jie Hong, Ye Qiu, Shihao Rao, Xiaofeng Liu, Qiao Li, Xingyao Chen, Chuan Li, Cheng Fang
Figure caption: Synthetic Fe I (a)–(c) and Hα (d)–(f) line profiles varying with time for three loops (L6, L11, and L4) in different initial atmospheres. The maximum enhancements of the continuum and Fe I and Hα lines are shown for each loop from the simulations.
Paper: Thermal Effects in Binary Neutron Star Mergers
Authors: Jacob Fields, Aviral Prakash, Matteo Breschi, David Radice, Sebastiano Bernuzzi, André da Silva Schneider
Figure caption: The reconstructed GW spectrum of the ℓ = 2, m = 2 mode using the NRPMw model. The colored solid lines represent the median waveform and the colored shaded regions represent the 90% credible intervals on the posterior distribution of the spectra computed from the recovered parameter space of NRPMw. The colored dashed limes represent the injected spectra at an S/N of 15. Additionally, shown are the postmerger peak frequencies f 2 (in vertical dashed lines) and the 90% credible intervals (in gray) on the posterior distribution of f 2 from the reconstructed waveforms.
Paper: Thermal Effects in Binary Neutron Star Mergers
Authors: Jacob Fields, Aviral Prakash, Matteo Breschi, David Radice, Sebastiano Bernuzzi, André da Silva Schneider
Figure caption: The maximum rest-mass density of the SR simulations (top) and the the gravitational wave strain of the ℓ = 2, m = 2 mode (top).
Paper: Thermal Effects in Binary Neutron Star Mergers
Authors: Jacob Fields, Aviral Prakash, Matteo Breschi, David Radice, Sebastiano Bernuzzi, André da Silva Schneider
Figure caption: The average temperature as a function of density at t ≈ 5 ms postmerger for the M0 (left) and M1 (right) SR simulations. Each average was calculated by constructing two-dimensional histograms in temperature and density, then averaging over the temperature with a weight corresponding to the mass of each density-temperature bin. To reduce noise in the data, five equally spaced time steps (with Δt ≈ 0.05 ms) centered on t ≈ 5 ms were averaged together.
Paper: Thermal Effects in Binary Neutron Star Mergers
Authors: Jacob Fields, Aviral Prakash, Matteo Breschi, David Radice, Sebastiano Bernuzzi, André da Silva Schneider
Figure caption: Temperature and rest-mass density slices in the x–y plane of the m* = 0.55 and m* = 0.95 SR simulations at approximately 5 ms postmerger (top) and average temperature as a function of density (bottom). Contour lines correspond to rest-mass densities ρ = {1012, 1013, 1014, 5 × 1014} g cm−3. For visual clarity, the m* = 0.75 model is not shown in the slice plot.
Paper: Thermal Effects in Binary Neutron Star Mergers
Authors: Jacob Fields, Aviral Prakash, Matteo Breschi, David Radice, Sebastiano Bernuzzi, André da Silva Schneider
Figure caption: The deviation from weak equilibrium ﹩{\rm{\Delta }}{\mu }_{{\nu }_{e}}/T﹩ between M0 (left) and M1 (right) for m* = 0.55 (top), m* = 0.75 (middle), and m* = 0.95 (bottom) at t ≈ 5 ms. The contour lines correspond to the rest-mass densities ρ = {1012, 1013, 1014, 5 × 1014} g cm−3.
Paper: Thermal Effects in Binary Neutron Star Mergers
Authors: Jacob Fields, Aviral Prakash, Matteo Breschi, David Radice, Sebastiano Bernuzzi, André da Silva Schneider
Figure caption: The GW strain of the ℓ = 2, m = 2 mode at D  L  = 40 Mpc for both the M1 (solid lines) and M0 (dashed lines) SR simulations.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Disk-integrated spectra (left) and the spectrum at the position of the NE Blob extracted from a single beam (right) for SO, SiS, and 13CO. The vertical dashed line indicates the systemic velocity of 6.9 km s−1. For the individual spectrum, the rms is computed as the standard deviation of line-free channels and is shown in the upper right of each panel. The shaded regions in the SO and SiS spectra show the velocity regions used to compute the column densities in Table 2. A non-Keplerian, compact emission counterpart to the planet location is labeled in the 13CO spectrum.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Selected channel maps and spectra extracted from a single beam at the position of the point-source-like emission in 12CO J = 3 − 2 (upper row; red border) and 13CO J = 3 − 2 (lower row; blue border). The middle row shows the 12CO channels for reference, with the border color corresponding to each set of channels. Several channels (gray border) between 3.50 and 4.94 km s−1 have been omitted for the sake of visual clarity. The orange contours show the millimeter dust rings. The colorscale shows the line emission and has been intentionally saturated to highlight the faint emission associated with a point source at a projected distance of 340–400 mas and PA ≈ 38°. Contours in pink show rms × [2.5, 3, 3.5]. The synthesized beam is shown in the lower left corner of each panel. We show the JvM-uncorrected images here to provide the most conservative estimate of the S/N of the compact 12CO and 13CO emission. A comprehensive analysis of both JvM- and non-JvM-corrected images is provided in Appendix B.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Deprojected radial intensity profiles of SO and SiS for the HD 169142 disk (left, middle columns). Shaded regions show the 1σ uncertainty. Solid lines mark rings and dotted lines denote gaps. The major axis of the synthesized beam is shown in the lower left corner. SO and SiS emission profiles are extracted from narrow wedges over the labeled PA range, measured east of north in the sky frame. These wedges are illustrated in the associated zeroth-moment maps (right column).
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: A gallery of chemical signatures related to the HD 169142 b planet. The peak intensities of 12CO (pink), 13CO (blue), SiS (peach), and SO (teal) are shown in contours, and the millimeter dust is in the colorscale. The planet location is indicated by a white circle (Gratton et al. 2019; Hammond et al. 2023). A scale bar showing 10 au is in the lower right corner.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Gallery of selected 12CO and 13CO channels (3.22 and 4.96 km s−1, respectively), which show the peak intensity of the emission counterparts. Images were generated with a range of Briggs robust values from 0.0 to 2.0 (left to right) and without (top) and with (bottom) the JvM correction. The locations of the compact emission counterparts and the expected Keplerian rotation are marked in the upper rightmost panel. Contours show rms ×[2.5,3,4] and ×[2.5,3,4,5] for 12CO and 13CO, respectively. The disk center is marked by a “+” and the synthesized beam is shown in the lower left corner of each panel.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Gallery of SO peak intensity maps generated from images with a range of Briggs robust values from 0.0 to 2.0. The location of the NE Blob and the two SO rings are labeled in the rightmost panel. Contours show rms×[3,4,5,6]. The synthesized beam is shown in the lower left corner of each panel.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Radial column densities of SO and SiS derived with a constant T rot = 100 K. The SO radially resolved profile is shown in black, and the disk-averaged SO value is marked by a horizontal red line. The column densities of the NE Blob for SO and SiS are shown as teal and orange rectangles, respectively.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Channel maps of the SO J = 88–77 emission of the HD 169142 disk. A representative Keplerian mask is shown in light gray. Contours show rms×[3,4,5,6]. The synthesized beam is shown in the lower left corner of each panel, and the LSRK velocity in km s−1 is printed in the upper right.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Channel maps of the SiS J = 19−18 emission of the HD 169142 disk. Contours show rms×[3,4,5]. The hand-drawn masks are marked in orange. Otherwise, as in Figure 9.
Paper: Multiscale Stamps for Real-time Classification of Alert Streams
Authors: Ignacio Reyes-Jainaga, Francisco Förster, Alejandra M. Muñoz Arancibia, Guillermo Cabrera-Vives, Amelia Bayo, Franz E. Bauer, Javier Arredondo, Esteban Reyes, Giuliano Pignata, A. M. Mourão, Javier Silva-Farfán, Lluís Galbany, Alex Álvarez, Nicolás Astorga, Pablo Castellanos, Pedro Gallardo, Alberto Moya, Diego Rodríguez
Figure caption: Visualization of the proposed multiscale stamps. The original stamp shows a stamp from an alert of ZTF, and the small square in the middle represents the size of an LSST stamp. The multiscale stamp on the upper right side shows the same stamp from ZTF but represented as four images of 8 by 8 pixels of different scales. The four images are presented in the lower part of the figure with their corresponding FoV.
Paper: Multiscale Stamps for Real-time Classification of Alert Streams
Authors: Ignacio Reyes-Jainaga, Francisco Förster, Alejandra M. Muñoz Arancibia, Guillermo Cabrera-Vives, Amelia Bayo, Franz E. Bauer, Javier Arredondo, Esteban Reyes, Giuliano Pignata, A. M. Mourão, Javier Silva-Farfán, Lluís Galbany, Alex Álvarez, Nicolás Astorga, Pablo Castellanos, Pedro Gallardo, Alberto Moya, Diego Rodríguez
Figure caption: Confusion matrices for the four scenarios, all of them evaluated over the same test set. Each row is normalized to sum 100. AGN means active galactic nuclei, SN means supernovae, and VS means variable stars.
Paper: Multiscale Stamps for Real-time Classification of Alert Streams
Authors: Ignacio Reyes-Jainaga, Francisco Förster, Alejandra M. Muñoz Arancibia, Guillermo Cabrera-Vives, Amelia Bayo, Franz E. Bauer, Javier Arredondo, Esteban Reyes, Giuliano Pignata, A. M. Mourão, Javier Silva-Farfán, Lluís Galbany, Alex Álvarez, Nicolás Astorga, Pablo Castellanos, Pedro Gallardo, Alberto Moya, Diego Rodríguez
Figure caption: Spatial distribution of a set of unlabeled sources. The sources are separated according to the classification given by the multiscale stamp classifier. The yellow/orange line corresponds to the Galactic plane, and the red line corresponds to the ecliptic plane.
Paper: Multiscale Stamps for Real-time Classification of Alert Streams
Authors: Ignacio Reyes-Jainaga, Francisco Förster, Alejandra M. Muñoz Arancibia, Guillermo Cabrera-Vives, Amelia Bayo, Franz E. Bauer, Javier Arredondo, Esteban Reyes, Giuliano Pignata, A. M. Mourão, Javier Silva-Farfán, Lluís Galbany, Alex Álvarez, Nicolás Astorga, Pablo Castellanos, Pedro Gallardo, Alberto Moya, Diego Rodríguez
Figure caption: Alerts classified as satellite by the multiscale stamp classifier. This is a selection of the alerts classified as satellite with the highest confidence. For each alert we show its difference image, object ID, and the probability of being a satellite according to the model.
Paper: Multiscale Stamps for Real-time Classification of Alert Streams
Authors: Ignacio Reyes-Jainaga, Francisco Förster, Alejandra M. Muñoz Arancibia, Guillermo Cabrera-Vives, Amelia Bayo, Franz E. Bauer, Javier Arredondo, Esteban Reyes, Giuliano Pignata, A. M. Mourão, Javier Silva-Farfán, Lluís Galbany, Alex Álvarez, Nicolás Astorga, Pablo Castellanos, Pedro Gallardo, Alberto Moya, Diego Rodríguez
Figure caption: Altitude–azimuth spatial distribution of the sources shown in Figure 3. The numbers in the color bar represent the object density, i.e., the number of sources per squared radian (steradian).
Paper: Multiscale Stamps for Real-time Classification of Alert Streams
Authors: Ignacio Reyes-Jainaga, Francisco Förster, Alejandra M. Muñoz Arancibia, Guillermo Cabrera-Vives, Amelia Bayo, Franz E. Bauer, Javier Arredondo, Esteban Reyes, Giuliano Pignata, A. M. Mourão, Javier Silva-Farfán, Lluís Galbany, Alex Álvarez, Nicolás Astorga, Pablo Castellanos, Pedro Gallardo, Alberto Moya, Diego Rodríguez
Figure caption: 500″ × 500″ images for ZTF alerts ZTF21abklvrx and ZTF20achpliw.
Paper: A Tight Correlation between Millimeter and X-Ray Emission in Accreting Massive Black Holes from <100 mas Resolution ALMA Observations
Authors: Claudio Ricci, Chin-Shin Chang, Taiki Kawamuro, George C. Privon, Richard Mushotzky, Benny Trakhtenbrot, Ari Laor, Michael J. Koss, Krista L. Smith, Kriti K. Gupta, Georgios Dimopoulos, Susanne Aalto, Eduardo Ros
Figure caption: The ratio between the observed fluxes in the 2–10 keV and in the 100 GHz bands vs. the column density for the objects in our sample. The horizontal black dashed line marks the median value of the ratio obtained using the intrinsic 2–10 keV fluxes (see Section 4). The dashed red line represents the best fit to the data in the ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})=22-24.5﹩ range (see Equation (5)). The green dot-dotted–dashed line shows the expected decrease of the flux ratio with N H by considering the RXTORUSD model.
Paper: A Tight Correlation between Millimeter and X-Ray Emission in Accreting Massive Black Holes from <100 mas Resolution ALMA Observations
Authors: Claudio Ricci, Chin-Shin Chang, Taiki Kawamuro, George C. Privon, Richard Mushotzky, Benny Trakhtenbrot, Ari Laor, Michael J. Koss, Krista L. Smith, Kriti K. Gupta, Georgios Dimopoulos, Susanne Aalto, Eduardo Ros
Figure caption: The ratio between 100 GHz and intrinsic 14–150 keV luminosities vs. the column density (top left panel), Eddington ratio (top right panel), black hole mass (bottom left panel), and star formation rate (bottom right panel). The horizontal dashed green lines represent the median value of ﹩\mathrm{log}({L}_{100\,\mathrm{GHz}}/{L}_{14-150\,\mathrm{keV}})﹩.
Paper: A Tight Correlation between Millimeter and X-Ray Emission in Accreting Massive Black Holes from <100 mas Resolution ALMA Observations
Authors: Claudio Ricci, Chin-Shin Chang, Taiki Kawamuro, George C. Privon, Richard Mushotzky, Benny Trakhtenbrot, Ari Laor, Michael J. Koss, Krista L. Smith, Kriti K. Gupta, Georgios Dimopoulos, Susanne Aalto, Eduardo Ros
Figure caption: Left panel: 100 GHz continuum luminosity vs. the intrinsic 14–150 keV luminosity for the sources in our sample. The solid red line represents the best fit to the data (Equation (1)), while the dashed red lines show the 1σ scatter (0.22 dex). Right panel: same but for the corresponding fluxes (best-fit relation given in Equation (2)). Uncertainties on the ALMA 100 GHz fluxes and luminosities are 5%.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Top two rows: zeroth-moment maps of 12CO J = 3 − 2, 13CO J = 3 − 2, SO J = 88 − 77, SiS J = 19 − 18 for the HD 169142 disk. The synthesized beam and a scale bar indicating 20 au are shown in the lower left and right corner, respectively, of each panel. Bottom row: composite image of the 0.9 mm continuum emission (colorscale) with contours showing the integrated (left) and peak intensity (right) of SO and SiS. The rms for the integrated intensities represents the zeroth-moment map uncertainty. For the peak intensities, the rms is the channel map noise. The planet location from Gratton et al. (2019) and Hammond et al. (2023) is marked by a white circle. The synthesized beams for the continuum (orange), SO (teal), and SiS (peach) are shown in the lower left corners. The disk rotation is clockwise.
Paper: Statistical Study of Anisotropic Proton Heating in Interplanetary Magnetic Switchbacks Measured by Parker Solar Probe
Authors: Qiaowen Luo, Die Duan, Jiansen He, Xingyu Zhu, Daniel Verscharen, Jun Cui, Hairong Lai
Figure caption: (a) and (d) Averaged temperatures of the switchback intervals (blue) and their ambient background intervals (red) in the parallel direction (see panel (a)) and the perpendicular direction (see panel (d)). (b) and (e) Statistical comparison of the parallel and perpendicular proton temperatures inside and outside the switchbacks.. (c) and (f) Statistical distribution histogram of the parallel temperature ratios inside and outside the switchbacks, and the perpendicular temperature ratios. (g) Thermal anisotropy (T ⊥2/T ∥) of the switchback intervals (blue) and their ambient intervals (red). (h) Statistical comparison of the thermal anisotropy inside and outside the switchbacks. (i) Statistical histogram of the thermal anisotropy ratio, A in/A out, where A = T ⊥2/T ∥.
Paper: Statistical Study of Anisotropic Proton Heating in Interplanetary Magnetic Switchbacks Measured by Parker Solar Probe
Authors: Qiaowen Luo, Die Duan, Jiansen He, Xingyu Zhu, Daniel Verscharen, Jun Cui, Hairong Lai
Figure caption: Proton core temperatures in the parallel and perpendicular directions as obtained from the GA fitting method. (a) and (d) Averaged Proton core temperatures in the parallel and perpendicular directions for the switchback intervals (blue) and the background intervals (red). (b) and (e) Statistical comparison of the parallel and perpendicular proton core temperatures inside and outside the switchback intervals. (c) and (f) Statistical histogram of the parallel temperature ratios inside and outside the switchbacks, and the perpendicular temperature ratios. (g) Proton core thermal anisotropy (T  c,⊥2/T  c,∥) of the switchback intervals (blue) and their ambient intervals (red). (h) Statistical comparison of the proton core thermal anisotropy inside and outside the switchbacks. (i) Statistical histogram of the proton core thermal anisotropy ratio, A c,in/A c,out, where A = T  c,⊥2/T  c,∥.