adsabs/AstroCLIMB huggingface dataset:
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Demonstrating the necessity of using multiple channels of data to derive class memberships. The left panel shows r vs. r − z as in the right panel of Figure 1, but using the third PC as in Figure 2. The right panel shows the reverse case, i.e., r − i vs. i − z as in Figure 2, but using class probabilities derived using the second PC as in Figure 1.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Likelihood generation for X-ray colors. Left: histogram of X-ray colors filtered on hardness ratios for a well-measured subsample, with the histogram for the full sample shown as the dashed black/yellow line normalized to the same number of objects and overplotted. Middle: the likelihoods generated by square-root transformation of the Gaussian components, with the tails modified to be linearly decreasing. Right: class assignments with points color coded as RGB tuples as in Figure 1.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Separating Cygnus OB2 sources using extinction, A  v  (based on F96; see Figure B1 for the FM case). The observed histogram (left) is modeled as a mixture of three Gaussians, with the components that predominate at low, medium, and high A  v  assumed to represent the foreground (red), member (green), and background (blue) objects, respectively. These Gaussian components, after removal of the population size effect and renormalization, are identified with the corresponding likelihoods (middle). A scatter plot showing the difference in estimated A  v  when using the extinction laws of F96 and FM is shown in the right panel, with the points color coded as RGB tuples as in Figure 1.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Set of diagrams showing colors and magnitudes of all the sources of our OIR catalog with good photometry in the involved bands (gray circles), candidate OIR+X-ray foreground sources (red diamonds), Cygnus OB2 members (green circles), and background sources (blue crosses). We also show the extinction vectors and the 2.5 Myr isochrone from Siess et al. (2000; solid lines) and the MIST database (dashed line), assuming a distance of 1400 pc and A  V  = 3.5 m  with corresponding mass values labeled with a horizontal displacement. In the top right panel the solid lines are instead ZAMS at increasing E  B−V  (0, 1, 2, 3).
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: As in the first two panels of Figure 4, but for extinctions derived from FM.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Left: distributions of the median energy of the detected photons for all the X-ray sources detected in our survey (gray), for those matched with OIR counterparts (blue), and for the X-ray sources without an OIR counterpart (red). Right: distribution of the ACIS Extract parameter prob-no-source for the X-ray sources with no OIR counterpart separated according to their median photon energies, with soft (0.5–1 keV; red), medium (1–2.5 keV; blue), hard (2.5–7.5 keV; green), and all (black).
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Spatial distribution of background (left), association member (middle), and foreground (right) sources with OIR matches. The contours mark continuum emission levels at [8.0] μm Spitzer band, denoting the presence of dust and high A  v . The position of Cyg X-3 is marked in red. The filled blue stars denote O stars.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Left: distribution of the individual extinctions of the sources in the catalog. Right: map of stellar extinction across the area of the survey. The red contours mark the continuum emission levels at 8.0 μm. The blue stars mark the positions of known O stars.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Waiting time plotted vs. MJD time for the most active repeating FRBs. The horizontal dashed line corresponds to the average value of the waiting time for each source. The solid line is the best linear fit to the data points. The distribution of the waiting time is also illustrated via histogram. The inset shows the observational data points from each telescope.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between various parameters concerning the waiting time for repeating FRBs. Here μ and σ are the two parameters derived by fitting the waiting time through a lognormal distribution for each FRB, characterizing the typical waiting time and the dispersion range, respectively. The red dots represent the high-value waiting time, while the blue dots are the low-value waiting time. “Average” indicates the mean value. “Peak” indicates the value observed most frequently. The FRBs annotated in black are not used for parametric analysis due to the small sample size but are shown here for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between redshift, SFR, and pulse width for repeating FRBs. (a) μ Width vs. redshift. (b) μ Width vs. SFR. Note that μ Width is derived using a lognormal function to fit the observed pulse width distribution for each source and thus represents the typical pulse width. The FRB 20180916B is not used for statistical analysis due to the small number of bursts with pulse width measurements but is also shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Relation between the redshift, SFR, and typical waiting time for repeating FRB sources. (a) μ WaitingTime(High−Value) vs. redshift. (b) μ WaitingTime(High−Value) vs. SFR. Here μ WaitingTime(High−Value) refers to the typical waiting time of the right peak in the bimodal distribution, derived by using a lognormal function to fit the peak for each FRB. The FRBs 201800301A and 20181030A are not used for statistical analysis due to the small number of bursts that can be used for calculating the waiting time but are shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Pulse width plotted vs. time for repeating FRBs. The horizontal dashed line corresponds to the average of the pulse width for each source. The solid line is our linear fit to the data points. The distribution of the data points is also illustrated via histogram. The inset shows the observational data points from each telescope.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between various statistical parameters derived by fitting the pulse width distribution with a lognormal function for repeating FRBs. Here μ and σ characterize the typical width and the dispersion range, respectively. “Average” indicates the mean value of the pulse width. “Peak” indicates the width value observed most frequently. The FRB 20180916B is not used for statistical analysis due to the small number of bursts with pulse width measurements but is shown in the figure for completeness.
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 bandwidth of FRBs plotted vs. time for the active repeating FRBs. The horizontal dashed line corresponds to the average of the bandwidth for each FRB. The solid line is our linear fit to the data points. For the FRBs detected by different telescopes, the distribution of the bandwidth is illustrated via histogram. Here f High and f Low stand for the upper and lower frequency of the observed bandwidth, 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: Correlation between the statistical parameters of bandwidth for repeating FRBs. Here μ and σ represent the two parameters derived from the normal distribution fitting of the bandwidth for each source, characterizing the typical bandwidth and the dispersion range, respectively. “Average” indicates the mean value. “Peak” represents the value observed most frequently.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between the redshift and the characteristic bandwidth for repeating FRBs. Here μ Bandwidth is the characteristic bandwidth derived from the normal distribution fitting, which could represent the average bandwidth.
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: Apparent motion of the beam of ISN He in the spacecraft-inertial frame for ∼2 months during the year, presented in heliographic coordinates. The color-coded flux magnitude images can be regarded as daily snapshots of the energy-integrated, spatially resolved differential flux of ISN He for DOYs 69, 105, and 133, from left to right. The lines represent portions of Sun-centered scanning circles, with the angular radii (elongation angles ε) listed in the second panel. The selected DOYs are identical to those represented as blue dots in Figure 2 and used in the three bottom-rightmost columns of panels in Figure 4.
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 for NGC 526A, NGC 3281, NGC 3393, and IC 5063. The beam sizes are indicated by the white ellipses in the bottom-left corners. In each panel, the identification number, assigned in this study (Table 1) and Paper I, is presented along with the object name. The frequency is the rest-frame central frequency of the collapsed spectral window adopted, after removing any emission line flux. The central black cross indicates the peak of the nuclear mm-wave emission, expected to be the AGN position. A morphological parameter, which can consist of e and b, is also presented below the frequency. As detailed in Section 4, e and b indicate the presence of extended emission connected with the central unresolved component and the presence of isolated blob-like emission, respectively. Colors are assigned according to flux density per beam following the color bar on the right side. The orange contours indicate where flux densities per beam are 5σ mm, 10σ mm, 20σ mm, 40σ mm, 80σ mm, and 160σ mm. For NGC 526A, NGC 3281, NGC 3393, and IC 5063, σ mm = 0.016 mJy beam−1, σ mm = 0.022 mJy beam−1, σ mm = 0.025 mJy beam−1, σ mm = 0.059 mJy beam−1, respectively. ALMA images for all 98 objects are summarized in Appendix B.
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 studies of ISN Ne using small elongation angles. The upper portions of the panels present the fluxes, the lower portions the respective impact energies (color-coded). The left panel illustrates an opportunity to view ISN Ne with no contribution from ISN O. Both the direct and indirect beams are in the instrument visibility strip, and the O atoms are missing because they suffered much larger ionization losses than the Ne atoms. Also, the primary and secondary populations of ISN He are visible, but in their case a clear separation between the direct and indirect beams is not easy because of the larger thermal spread of He. The second panel presents the same DOY but a larger elongation angle (76° vs. 60°). This scenario corresponds to a viewing geometry where both the He and Ne beams have merged but the expected Ne signal is close to the adopted flux-detection threshold. The third panel shows a (DOY, ε) combination for which only the direct beam is in the visibility strip and both ISN O and Ne are visible. A combination of the viewing geometries represented in the first and last panels can be used to verify the calibration of the instrument for O and Ne atoms.
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: Radial surface-brightness profiles for NGC 526A, NGC 3281, NGC 3393, and IC 5063. The radius is in units of the averaged beam size (﹩{\theta }_{\mathrm{beam}}^{\mathrm{ave}}﹩). In each panel, observed values are indicated with black error bars, but particularly those detected at significances more than 3 times the SEs with respect to an unresolved component (blue dots and lines) are shown in orange. The dashed gray line indicates the MRS. The ALMA images of the four objects are presented in Figure 1. The radial profiles for all 98 AGNs are summarized in Figure 6.
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 fluxes of the primary and secondary ISN O and of the primary Ne for (DOY, ε) combinations well suited for observations of the secondary O. Four cases of hypothetical parameters of the secondary O populations are displayed. The simulations for the two hypothetical densities are presented with solid (for the density of 50% of that of the primary) or broken lines (for 22%). The green vs. magenta colors differentiate between the flow parameters from Park et al. (2019) and Kubiak et al. (2016). The two panels at the left side show the times when the primary O and Ne are not yet visible. The third panel represents an example when the secondary population is well visible at the wings of the ISN O peak. The extreme-right panel illustrates a situation wherein the primary populations have already disappeared from the field of view, but the secondary populations are still well visible.
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 viewing the secondary population of ISN O. The figure is in a similar format to that used in Figure 7 by Sokół et al. (2019b). Dark green dots (Opri) represent the combinations of (DOY, ε) for the primary population of ISN O. The light green dots represent the secondary population of ISN O with the inflow parameters from Park et al. (2019; O﹩{}_{\sec }﹩ P19 in the figure) and the density equal to 50% of that of the primary assumed. The cyan (Opri Peak) and red dots (O﹩{}_{\sec }﹩ Peak) mark the positions of the maximum of the flux for the primary and secondary populations, respectively. To qualify for this map, the flux must be larger than 10 atoms cm−2 s−1 for at least three spin-angle bins.
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: A pie chart of the observation times for ISN Ne over the calendar year. See text for details.
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 metalloexofullerenes [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 metalloexofullerene 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 1.3 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: 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 metalloexofullerenes [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 neutral metalloexofullerene 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 0.4 (i.e., the feature intensities are higher than in Figure 1) 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: 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: Comparison of the continuum-subtracted Spitzer Space Telescope (top) and representative metallofullerene simulated IR spectra (bottom) for two fullerene-rich objects showing very different C60 17.4 μm/18.9 μm band ratios and chemical abundances: the PN LMC 99, and the RCB star DY Cen. The guidelines show the features of pristine C60 at 7.09, 8.53, 17.34, and 18.91 μm, according to our calculations. The representative metallofullerene simulated spectra correspond to the simulations by Barzaga et al. (2023), which consider the metal abundances, ionization level, and endo and exo concentration (see Barzaga et al. 2023, for more details), and reproduce the observed 17.4 μm/18.9 μm band ratios. The intensity has been normalized according to the 17.4 μm/18.9 μm band ratio under the assumption that metallofullerenes are the only emitters causing the 17.4 μm/18.9 μm anomaly in the spectra; i.e., the more intense feature of the 17.4 μm/18.9 μm pair has been used to establish the reference in the normalization.
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: Charge-density difference maps of the simulated metalloendofullerenes obtained for an isovalue of 0.02 atomic units. Light red regions indicate electron depletion, while light blue regions indicate electron accumulation. In each case, the ∣V∣/G ratio is displayed in the top left corner of the model.
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: Charge-density difference maps of the simulated metalloexofullerenes. The notation is the same as in Figure 5.