adsabs/AstroCLIMB huggingface dataset:
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the DM–peak flux plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the RM–pulse width plane for FRB 20180301A and FRB 20201124A. All bursts are detected by FAST. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the RM–peak flux plane for FRB 20180301A and FRB 20201124A. All bursts are detected by FAST. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the pulse width–waiting time plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the bandwidth–waiting time plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the bandwidth–pulse width plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the DM–waiting time plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the DM–fluence plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the RM–waiting time plane for FRB 20180301A and FRB 20201124A. All bursts are detected by FAST. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the DM–bandwidth plane for FRB 20121102A and FRB 20201124A. All bursts are detected by FAST. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the RM–bandwidth plane for FRB 20201124A. All bursts are detected by FAST. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the RM–fluence plane for FRB 20201124A. All bursts are detected by FAST. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the bandwidth bound–waiting time plane for FRB 20121102A. All bursts are detected by Arecibo. Here f High and f Low stand for the upper and lower bounds of the observed bandwidth, respectively. The horizontal and vertical dashed lines mark the average values of the two parameters.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the bandwidth bound–pulse width plane for FRB 20121102A. All bursts are detected by Arecibo. Here f High and f Low stand for the upper and lower bounds of the observed bandwidth, respectively. The horizontal and vertical dashed lines mark the average values of the two parameters.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the bandwidth bound–fluence plane for FRB 20121102A. All bursts are detected by Arecibo. Here f High and f Low stand for the upper and lower bounds of the observed bandwidth, respectively. The horizontal and vertical dashed lines mark the average values of the two parameters.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the peak flux–waiting time plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the fluence–waiting time plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the bandwidth–peak flux plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the bandwidth–fluence plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Observed center frequency plotted vs. flux density for FRB 20121102A. All bursts are detected by Arecibo. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Observed center frequency plotted vs. pulse width for FRB 20121102A. All bursts are detected by Arecibo. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of observed bursts on the DM–RM plane for FRB 20180301A and FRB 20201124A. All bursts are detected by FAST. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Observed center frequency plotted vs. fluence for FRB 20121102A. All bursts are detected by Arecibo. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: Summary of the elongation settings to maximize science opportunities for ISN gas studies with IMAP-Lo, to accomplish within 2 yr of operations. The upper and lower panels represent the settings for the first and second years, respectively. The colors mark the ISN observation campaigns discussed in the text; the corresponding legends are displayed next to the panels. To provide a wider context, the background in both panels is adapted from the upper panel of Figure 15 in Sokół et al. (2019b).
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: Combinations of elongations and DOYs for which the maxima of the fluxes of ISN species and their populations are expected. The gray grid marks the (ε, DOY) combinations available in the simulation pool. The colored lines mark the progression of the positions of ISN beam peaks of the species/populations. The large colored asterisks mark the (DOY, ε) combinations for which the fluxes of the respective ISN populations are the largest during the year (see the species legend). The red (blue) dots connected with the solid horizontal and vertical lines in respective colors correspond to two alternative sections in the (DOY, ε) space with either a fixed DOY or ε that offer almost identical fluxes of the ISN species (see text). The evolution of the peak maxima for the blue cross for individual atom populations are presented in Figure 3. The blue dots represent the days for which we show the fluxes in Figure 4. Note that all of the lines shown in the figure appear to be broken because of the overlaid simulation grid.
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: Expected fluxes of ISN species for the two perpendicular cuts through the (DOY, ε) space, displayed Figure 2 as the blue cross. The upper row presents the fluxes for a number of elongations for a fixed DOY = 105 (the dots in the vertical bar of the cross). The lower row shows the fluxes for a number of DOYs for a fixed elongation ε = 120° (the dots in the horizontal bar of the cross). The figure demonstrates that, even though the two rows correspond to different loci in the (DOY, ε) space, the fluxes are very similar to each other within the panel columns.
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: Illustration of the separation of the He signal from that of H. The first panel shows a (DOY, ε) combination for which a mixture of signals from both He and H populations is expected. In the second panel, the contribution from ISN H is several orders of magnitude smaller than that from He, including the far wings of the peak, where pure secondary He is visible. In the third panel, there is no visible contribution from ISN H because the impact energy is below the detection threshold, and due to a small size of the scanning circle the count statistics of He, Ne, and O is expected to be very good. The fourth panel presents an opportunity to see a mixture of indirect beams of the primary and secondary He without H and any other species.
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: Sample illustration of (DOY, ε) combinations facilitating observations of the primary population of ISN He with a negligible contribution from the secondary population (first and second panels) and of the secondary population with a negligible contribution from the primary (third and fourth panels). The second panel shows a dominating primary indirect beam, with small contribution from the secondary indirect population. The third panel represents a viewing geometry where the direct beam of the secondary population is observed, and the primary population has not risen enough yet. The fourth panel represents a viewing geometry for the indirect beam of the secondary population.
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: Expected fluxes and impact energies of ISN He, Ne, and O for two viewing geometries when the spacecraft is close to the upwind direction. The upper portions of the two panels present the fluxes, and the lower portions the corresponding impact energies. The left panel presents detection in the ram viewing geometry, with the energies of all species above the detection threshold of 20 eV. The right panel corresponds to a situation when the spacecraft has already passed the upwind direction and the atoms are chasing the spacecraft, i.e., to the anti-ram geometry. Only the O and Ne components exceed the energy detection threshold and feature a flux sufficiently high to expect their detection. The flux of ISN He is high but its energy for the primary population barely exceeds the detection threshold, and that of the secondary He is below it.
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: First panel: magnitudes of the spin-angle maxima of the flux as a function of the elongation angle ε for a fixed DOY 105 and various elongations, i.e., for the vertical bar of the blue cross in Figure 2. Second panel: magnitudes of the spin-angle maxima of the flux as a function of DOY for a fixed elongation ε = 120°, i.e., for the horizontal bar of the blue cross shown in Figure 2.
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: Simulated flux of the primary populations of ISN Ne and O and of the primary and secondary ISN He populations for a line-of-sight passage across the ISN beams with the elongation fixed at ε = 136° (left and middle panels) and for ε = 148° (right panel). The left panel represents a viewing geometry where the beam is observed before reaching the maximum magnitude. The other two panels show viewing the beam for the elongation angles resulting in the maximum possible flux for the given DOYs.
Paper: Science Opportunities for IMAP-Lo Observations of Interstellar Neutral Helium, Neon, and Oxygen during a Maximum of Solar Activity
Authors: M. A. Kubiak, M. Bzowski, P. Swaczyna, E. Möbius, N. A. Schwadron, D. J. McComas
Figure caption: Opportunities for separating Ne and O. The panels show the expected fluxes for the primary O and Ne, as well as those for the primary and secondary He. From left to right, they show the following conditions: Ne > O, Ne = O, and Ne < O (the O flux larger than that of Ne by ∼70%.)
Paper: BASS. XXXIV. A Catalog of the Nuclear Millimeter-wave Continuum Emission Properties of AGNs Constrained on Scales ≤ 100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Richard F. Mushotzky, Masatoshi Imanishi, Franz E. Bauer, Federica Ricci, Michael J. Koss, George C. Privon, Benny Trakhtenbrot, Takuma Izumi, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: ALMA Band 6 images of the 28 objects that showed both or one of largely extended or blob-like components. North is up and east is to the left. Beam sizes are shown by the white ellipses in the bottom-left corners. Each central black cross indicates the peak of the nuclear mm-wave emission. Black solid contours indicate where flux densities per beam are 5σ mm, 10σ mm, 20σ mm, 40σ mm, 80σ mm, and 160σ mm, while red dotted ones are drawn where flux densities per beam are −5σ mm. For three objects (NGC 5506, Mrk 520, and NGC 7172), flux densities per beam at 3σ mm are indicated by black dotted contours. The individual values of σ mm are listed in Table 3. The annotations in blue are used for the discussions in Appendix C.
Paper: BASS. XXXIV. A Catalog of the Nuclear Millimeter-wave Continuum Emission Properties of AGNs Constrained on Scales ≤ 100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Richard F. Mushotzky, Masatoshi Imanishi, Franz E. Bauer, Federica Ricci, Michael J. Koss, George C. Privon, Benny Trakhtenbrot, Takuma Izumi, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Left: cumulative detection-significance distribution of the objects showing both or one of extended (e) or blob-like (b) components (blue) and the others without such nonnuclear components (yellow). The p-value obtained from the K-S test is indicated in the parenthesis. The small p-value suggests the significant difference in the distributions and the trend that the objects without nonnuclear components were detected at lower significance. Right: same as the left, but for the beam size in units of parsecs. The distributions and p-value suggest the trend that the objects without nonnuclear components were observed at coarser physical resolutions.
Paper: BASS. XXXIV. A Catalog of the Nuclear Millimeter-wave Continuum Emission Properties of AGNs Constrained on Scales ≤ 100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Richard F. Mushotzky, Masatoshi Imanishi, Franz E. Bauer, Federica Ricci, Michael J. Koss, George C. Privon, Benny Trakhtenbrot, Takuma Izumi, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Spectral index as a function of the signal-to-noise ratio of the nuclear emission (left panel) and the density derived by the kernel density estimation (right panel). The black dashed lines correspond to 0.5, the mean for the BAT AGNs, while the yellow dotted lines indicate α mm = −3.5, expected for thermal dust emission.
Paper: Infrared Spectral Fingerprint of Neutral and Charged Endo- and Exohedral Metallofullerenes
Authors: R. Barzaga, D. A. García-Hernández, S. Díaz-Tendero, SeyedAbdolreza Sadjadi, A. Manchado, M. Alcami, M. A. Gómez-Muñoz, T. Huertas-Roldán
Figure caption: Total (black) and individual spectra of neutral metalloendofullerenes [M@C60] in the 5–25 μm range for seven different metals (Li, Na, K, Ca, Mg, Ti, and Fe). In the case of Ti ([Ti@C60]), an intensity offset has been applied to facilitate the visualization. The legend plot shows the color code we used to represent the individual neutral metalloendofullerene spectra. The dashed vertical gray lines and shaded peaks indicate the four strongest IR features of pristine C60 at the DFT B3LYP/6-31G level of theory. In addition, binding energies (eV) concerning the metal-C60 bond are also added for each metal. The full range (5–50 μm) of the mid-IR spectra can be found in the corresponding appended data.
Paper: Infrared Spectral Fingerprint of Neutral and Charged Endo- and Exohedral Metallofullerenes
Authors: R. Barzaga, D. A. García-Hernández, S. Díaz-Tendero, SeyedAbdolreza Sadjadi, A. Manchado, M. Alcami, M. A. Gómez-Muñoz, T. Huertas-Roldán
Figure caption: Total (black) and individual spectra of charged metalloendofullerenes [M@C60]+ in the 5–25 μm range for seven different metals (Li, Na, K, Ca, Mg, Ti, and Fe). As in Figure 1, the legend plot shows the color code we used to represent the individual charged metalloendofullerene spectra, and the binding energies (eV), while the pristine C60 features are marked with vertical gray lines and shaded peaks. Note that this time, the intensities are multiplied by a factor of 4.5 in order to match Figure 1. Again, the full range (5–50 μm) of the mid-IR spectra can be found in the corresponding appended data.
Paper: DESI z ≳ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ∼ 4.7–6.6
Authors: Jinyi Yang, Xiaohui Fan, Ansh Gupta, Adam D. Myers, Nathalie Palanque-Delabrouille, Feige Wang, Christophe Yèche, Jessica Nicole Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Kyle Dawson, Axel de la Macorra, Arjun Dey, Govinda Dhungana, Kevin Fanning, Andreu Font-Ribera, Satya Gontcho, Julien Guy, Klaus Honscheid, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Laurent Le Guillou, Michael Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Edward Schlafly, Gregory Tarlé, Mariana Vargas Magana, Benjamin Alan Weaver, Risa Wechsler, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: The example spectra of contaminants from our quasar survey, rebinned with 7 pixels. The first two are M dwarfs and the other two are galaxies. They all have red colors and thus contaminate the quasar selection.