adsabs/AstroCLIMB huggingface dataset:
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Fe XI] λ7892 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Fe VII] λ5276 and [Fe VI] λ5176 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Ca V] λ5309 and [Fe XIV] λ5303 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Fe VII] λ5159 and [Fe VI] λ5146 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [S XII] λ7609 and [Fe X] λ6374 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Ar X] λ5533 and [Fe VI] λ5335 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Fe VII] λ λ 5720, 6087 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: The direct and the indirect orbits for two example locations in the Earth’s orbit, defined by the DOYs 305 and 37. Solid lines correspond to the orbits preferred for observations on the given DOYs: the indirect orbit for DOY 305, and the direct orbit for DOY 37, as on IBEX. The dashed–dotted lines are the complementary orbits for the two selected locations. The indirect orbits are drawn in blue, and the direct ones in purple. The arrows mark the directions of the solar-inertial velocity vectors of the atoms. The dots on the trajectories mark time intervals corresponding to the Carrington period. The ☉ symbol marks the Sun, the black Sun-centered circle marks the Earth’s orbit, and the dotted lines the radius-vectors of the observer for the selected DOYs. The colored broken arcs mark the angles swept by atoms following the direct and the indirect orbits: Δθ dir305 the angle swept by the atom on the direct orbit, Δθ ndir305 that for the indirect orbit for this DOY, and Δθ dir037 the angle swept by an atom in a direct orbit for DOY 37.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Kinetic energy of ISN He atoms from the direct (purple) and indirect beams (blue) relative to the detector traveling with the Earth, shown as functions of DOY. The two horizontal lines connect extreme DOY pairs for the direct and indirect beams for which the atom energy at the detector are identical between the direct and indirect beams (the first and last rows of Table 1). The calculations were made using the cold-model approximation.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Projection of the direct and indirect orbits on the ecliptic plane for a (indirect, direct) DOY pair (case (5) in Table 1), drawn with the solid lines. The dashed–dotted lines mark the corresponding indirect (blue) and direct (purple) orbits for the two selected DOYs. The format of this figure is identical to that of Figure 2. Note that the direct and indirect beams drawn with solid lines overlap before entering inside Earth’s orbit.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: The radial modulation function ﹩{\hat{\beta }}_{\mathrm{el}}(r)﹩ of the electron-impact ionization rate, defined in Equation (2), as a function of distance from the Sun.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Heat maps for comparing similarity between different flare intensities by using the Bhattacharyya distance from the radial magnetic field magnetograms. The histogram on top of each column shows how flares are distributed within each category.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Mean and standard deviation scatter plots of three features (i.e., number of PILs, PIL size, and masked unsigned flux of PIL) derived from the radial magnetic field magnetograms over the entire flaring active region time series in regard to their relationships with the number of associated flares per day.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Box plots of means between selected PIL features prior to flaring and nonflaring instances based on Geostationary Operational Environmental Satellite (GOES) flare intensity level for 6, 12, and 24 hr time intervals from the radial magnetic field magnetograms.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Box plots of standard deviations between selected PIL features prior to flaring and nonflaring instances based on GOES flare intensity level for 6, 12, and 24 hr time intervals from the radial magnetic field magnetograms.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Binary masks overlaying the HMI magnetogram patch of NOAA Active Region 11158 (HARP 377) on 2011 February 14 at 04:24:00 UT. The left three figures show the original magnetogram patches with the zoomed-in area, while the right three show the zoomed-in detailed patches. In panel (a), the green area indicates the RoPI binary mask. In panel (b), the red area shows the binary mask of the convex hull of the PIL network in the AR. In panel (c), the pink line represents the detected PIL binary mask.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Mean and standard deviation scatter plots of three features (i.e., number of PILs, PIL size, and masked unsigned flux of PIL) derived from the entire flaring active region time series in regard to their relationships with number of associated flares per day.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Box plots of standard deviations between selected PIL features prior to flaring and nonflaring instances based on GOES flare intensity level for 6, 12, and 24 hr time intervals.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Box plots of means between selected PIL features prior to flaring and nonflaring instances based on GOES flare intensity level for 6, 12, and 24 hr time intervals.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Heat maps for comparing similarity between different flare intensities by using the Bhattacharyya distance. The histogram on top of each column shows how flares are distributed within each category.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Box plots of standard deviations between selected PIL features prior to flaring and nonflaring instances based on GOES flare intensity level for 6, 12, and 24 hr time intervals with largest flare from each active region in the radial magnetic field magnetograms.
Paper: A Systematic Magnetic Polarity Inversion Line Data Set from SDO/HMI Magnetograms
Authors: Anli Ji, Xumin Cai, Nigar Khasayeva, Manolis K. Georgoulis, Petrus C. Martens, Rafal A. Angryk, Berkay Aydin
Figure caption: Box plots of means between selected PIL features prior to flaring and nonflaring instances based on GOES flare intensity level for 6, 12, and 24 hr time intervals with the largest flare from each active region in the radial magnetic field magnetograms.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: The black histogram shows the distribution of the angular separation θ ow between the mid-IR counterpart, assigned in the G4Jy catalog, and the optical one for all those G4Jy-3CRE radio sources having IDF = 1.0, which, according to our analysis, implies that both counterparts are coincident. Two dashed black lines mark the location for θ ow equal to 0.″2, and 3″, respectively, while the red one corresponds to 1″. The red histogram includes also those radio sources with IDF = 2.2 for which our optical analysis helped to identify the mid-IR counterpart (see Section 3.2 for more details). As a comparison, we also report here the typical range of positional uncertainties of the NVSS and the SUMSS catalogs (Vollmer et al. 2005), mainly used in the G4Jy catalog to compute brightness-weighted radio centroids.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: Top panels: same as Figure 3, but for G4Jy 1846. As shown in the right panel, the optical counterpart of the radio nucleus is too faint to be detected in the images available from the Pan-STARRS, DES, and DSS databases; however, it is clear from the left panel that the radio source has an infrared counterpart. These cases are indicated with IDF = 4.1. Middle panels: same images for G4Jy 1057, but in this case, despite the lack of a plausible optical counterpart, the radio map available indicates that the assigned mid-IR counterpart appears to be incorrect, thus marked in our analysis with IDF = 4.2. Bottom panels: same as the middle panels, but for sources such as G4Jy 1587 that lack both a mid-IR and an optical counterpart of its radio core. G4Jy 1587 has IDF = 4.3. These are radio sources for which we also visually inspected other optical images available in the Pan-STARRS and in the DES databases in the g, i, z, and y bands searching for signatures of their host galaxies.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: Top panels: same as Figure 2, but for the case of G4Jy 524, a radio source for which the mid-IR counterpart identified in the G4Jy catalog is different from the optical one that corresponds to the position of the radio core detected in the VLASS radio map at 3 GHz. Sources showing the same behavior were marked with an IDF = 2.1 in our analysis. Bottom panels: same as Figure 2, but for G4Jy 593. This radio source, having IDF = 2.2, is an example of those cases for which there is a clear optical counterpart but they lack an assigned mid-IR source in the G4Jy catalog.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: Same as Figure 2, but for G4Jy 934. The lack of a high angular resolution radio map (in this case the one from which radio contours are computed was collected from the SUMSS archive) prevented us from clearly identifying the host galaxy of the radio source. These cases are flagged as “confused” in our analysis and have IDF = 3.0.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: Same as the right panel of Figure 3, but for G4Jy 122. The dashed blue circle, having 10″ radius, is centered on the location of the potential optical counterpart identified here since (i) it lies between the two radio lobes of G4Jy 122 showing a classical FR II radio morphology and (ii) there are no other optical sources within this area.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: The sky distribution, shown in the Hammer–Aitoff projection, of the 3CR sources located in the Northern Hemisphere (black circles) in comparison with those belonging to the G4Jy-3CRE catalog (red squares), equivalent to the 3CR but located in the Southern Hemisphere. It is clear how footprints of both surveys are complementary, and the region of the Galactic plane was excluded to select the G4Jy-3CRE catalog.
Paper: Observational Properties of 155 O- and B-type Massive Pulsating Stars 
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Li-ying Zhu, 俐颖 朱, Liang Liu, 亮 刘, Lin-jia Li, 临甲 李, Lei Zang, 蕾 臧
Figure caption: The H-R diagram of these OB-type pulsating stars. The red solid circles, the black open circles, and the black open circles with dots refer to these SPB, BCEP, and BCEP/SPB stars, respectively. The orange crosses represent those SPB stars with pure low frequency. Meanwhile, the candidate targets are shown as cyan solid triangles. The black solid and dotted lines are the theoretical zero-age main sequence and the evolutionary tracks for the different masses with Z = 0.02. The blue and magenta dotted line shows the instability regions of the SPB and BCEP stars for Z = 0.02 and a spherical harmonic degree l ≤ 3 from Miglio et al. (2007), respectively.
Paper: Observational Properties of 155 O- and B-type Massive Pulsating Stars 
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Li-ying Zhu, 俐颖 朱, Liang Liu, 亮 刘, Lin-jia Li, 临甲 李, Lei Zang, 蕾 臧
Figure caption: The P-L diagram of these OB-type pulsating stars. The horizontal dashed lines represent a frequency = 3 cycles day−1. Symbols are the same as those in Figure 5. The red solid line, the red dashed line, and the black solid line refer to the relation derived by the least-square method for all SPB stars, those SPB stars with pure LF, and those BCEP stars.
Paper: Observational Properties of 155 O- and B-type Massive Pulsating Stars 
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Li-ying Zhu, 俐颖 朱, Liang Liu, 亮 刘, Lin-jia Li, 临甲 李, Lei Zang, 蕾 臧
Figure caption: The dominant pulsating period and the effective temperature relation diagram of these OB-type pulsating stars. The horizontal dashed lines represent a frequency = 3 cycles day−1. Symbols are similar to those in Figure 5, but the size of the circles indicates their pulsation amplitude of the dominant frequency.