adsabs/AstroCLIMB huggingface dataset:
Paper: Effects of Coronal Magnetic Field Configuration on Particle Acceleration and Release during the Ground Level Enhancement Events in Solar Cycle 24
Authors: Wenlong Liu, Xiangliang Kong, Fan Guo, Lulu Zhao, Shiwei Feng, Feiyu Yu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: (a) Schematics of the locations of Earth (green), STA (red), and STB (blue) in the ecliptic plane as seen from the north of the Sun for the GLE 71 event on 2017 September 10. Communications with STB were lost. (b) Composite running-difference image observed by GOES-16/SUVI in 195 Å and LASCO C2 at 16:00 UT, when the CME first appeared in the FOV of LASCO C2. (c) EUV running-difference image observed by AIA 193 Å at GLE particle release time 16:03 UT, with closed field lines in magenta indicating the streamer belt located to the northeast of the AR12673. (d) Composite image of GOES-16/SUVI in 195 Å and LASCO C2 shows the CME at 16:12 UT.
Paper: Effects of Coronal Magnetic Field Configuration on Particle Acceleration and Release during the Ground Level Enhancement Events in Solar Cycle 24
Authors: Wenlong Liu, Xiangliang Kong, Fan Guo, Lulu Zhao, Shiwei Feng, Feiyu Yu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: (a)–(b) Temporal evolution of the 10 minute integrated proton energy spectra within the first 2 hr after the GLE onset time. Data are taken from EPEAD and HEPAD on board GOES 15. (c)–(d) Temporal evolution of the spectral indexes at 2 minute cadence obtained by fitting the proton energy spectra above 100 MeV with a single power-law function, F(E) ∝ E −δ . The vertical solid lines indicate the GLE onset time.
Paper: Effects of Coronal Magnetic Field Configuration on Particle Acceleration and Release during the Ground Level Enhancement Events in Solar Cycle 24
Authors: Wenlong Liu, Xiangliang Kong, Fan Guo, Lulu Zhao, Shiwei Feng, Feiyu Yu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: Reconstructed 3D shock fronts using the ellipsoid model are overplotted on the running-difference images of LASCO C2 and STA/COR1 for the GLE 71 (a)–(c) and GLE 72 (d)–(f) events.
Paper: Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear
Authors: D. J. Yu, 대중 유
Figure caption: Phase speeds  v  + vs. k z R for the forward sausage modes under photospheric conditions, where  v  se = 1.5v si, v Ai = 2.0 v  si,  v  Ae = 0.5 v  si,  v  ci ≈ 0.8944v si, and  v  ce ≈ 0.4743 v  si: fast surface sausage mode (fss), slow body sausage modes (sbs 1–3), and slow surface sausage mode (sss). These parameter values are used throughout the figures.
Paper: The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis
Authors: William Jeffrey Surgent, Enrique Lopez-Rodriguez, Susan E. Clark
Figure caption:  B-field orientation of our sample of spiral galaxies. Polarization measurements are shown with constant length to illustrate the inferred B-field orientations at 154 μm (black lines) and 6 cm (white lines) overlaid on the 154 μm total intensity (color scale). All figures share the same color scale as shown in the color bar of NGC 6946. The contours are in fractions of 0.2, 0.4, 0.6, 0.8, 0.9, and 0.98 of the peak intensity. Polarization measurements per beam (red circle) with PI/σ PI ≥ 3.0 are shown, where PI and σ PI are the polarized intensity and its uncertainty, respectively. A legend with the spatial scale of 1 kpc is shown in each panel.
Paper: The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis
Authors: William Jeffrey Surgent, Enrique Lopez-Rodriguez, Susan E. Clark
Figure caption: Example of the B-field decomposition of a galaxy. The composition of the m = 2 mode with β 2 = −i and the m = 0 mode with β 0 = −i is shown. Additionally, the relationship between the averaged pointwise rotation of the B-field orientation, ∠β 2, and the magnetic pitch angle, Ψ2, is illustrated at the top of the m = 2 mode on the left.
Paper: The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis
Authors: William Jeffrey Surgent, Enrique Lopez-Rodriguez, Susan E. Clark
Figure caption: Examples of the decomposition of the linear polarization fields in a ring. The morphology of the linear polarization field corresponding to 0 ≤ m ≤ 3 modes with different values of the β  m  coefficient is presented.
Paper: The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis
Authors: William Jeffrey Surgent, Enrique Lopez-Rodriguez, Susan E. Clark
Figure caption: Linear decomposition results of the FIR and radio B-fields for M51 and M83. The titles of each galaxy show the intensity map at FIR wavelengths to guide the reader with the morphological structure of the galaxy. We show the FIR and radio magnetic pitch angles, Ψ2, as a function of the galactocentric radius with the middle solid line corresponding to the mean values and the width of the line corresponding to ±1σ (left). Note that for M51, we have included ∠β 0, which is the angle associated with the m = 0 mode. The center panel shows the relative amplitude of each mode as a function of distance from the galactic center at FIR wavelengths with the width of each band corresponding to the value of the mode’s relative amplitude. Additionally, on the top of each band for each mode are error bars, showing ±1σ. The right panel shows the same but at radio wavelengths.
Paper: The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis
Authors: William Jeffrey Surgent, Enrique Lopez-Rodriguez, Susan E. Clark
Figure caption: As in Figure 4 with NGC 3627, NGC 4736, and NGC 6946.
Paper: The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis
Authors: William Jeffrey Surgent, Enrique Lopez-Rodriguez, Susan E. Clark
Figure caption: Statistical significance of ∣β  m ∣ per B-field mode for each galaxy. Each panel shows ﹩{\sigma }_{| {\beta }_{m}| }﹩ at FIR (top) and radio (bottom) for each mode with their error bars estimated as the propagated statistical errors of the full galaxy. ﹩\pm {\sigma }_{| {\beta }_{| m| \gt 10}| }﹩ (red shaded region) and ﹩3{\sigma }_{| {\beta }_{| m| \gt 10}| }﹩ (black solid line) are shown. For reference, m = 2 (black dashed line) and m = [–3, 3] (grey shaded region) are shown.
Paper: The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis
Authors: William Jeffrey Surgent, Enrique Lopez-Rodriguez, Susan E. Clark
Figure caption: Mean relative amplitudes of the B-field modes of a composited spiral galaxy. FIR (red) and radio (blue) relative amplitudes for modes −3 ≤ m ≤ 3 are shown. The B-field pattern associated with each mode is shown at the top.
Paper: The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis
Authors: William Jeffrey Surgent, Enrique Lopez-Rodriguez, Susan E. Clark
Figure caption: Comparison of measurements of magnetic pitch angle, Ψ2, between methods at FIR and radio wavelengths. Our method and the pitch angles by Borlaff et al. (2021) are shown.
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Top panel: Chandra/ACIS true color image of NGC 4214, obtained from a stack of all four data sets and then adaptively smoothed. Red = 0.3–1.0 keV, green = 1.0–2.0 keV, blue = 2.0–7.0 keV. X-1 is the subject of this study. SNR1, SNR2, SNR3, SNR5, SNR6, and SNR7 are the X-ray counterparts of the optical SNRs identified by Dopita et al. (2010); their estimated X-ray luminosities are listed in the Appendix. Bottom panel: HST/WFC3 UVIS true color image on the same scale as the Chandra image. Red = F814W (≈I), green = F547M (≈V), blue = F336W (≈U). Chandra flux contours of the strongest X-ray sources are overplotted in green (0.3–7.0 keV band).
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Chandra/ACIS light curves of X-1 in the 0.3–8 keV band. Top left: ObsID 2030; top right: ObsID 4743; bottom left: ObsID 5197; bottom right: ObsID 22372. Each light curve has been rebinned to 250 s (blue histogram) and 500 s (red histogram). Dashed black lines mark the 250 s bins corresponding to eclipse ingresses. The last dashed line in ObsID 2030 and the first dashed line in ObsID 5197 represent predicted eclipse times. In each plot, the reference time T 0 is the observation start time in Table 2. We have omitted the error bars for clarity.
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Chandra/ACIS-S spectra of X-1 in the four epochs of observations, with best-fitting power-law model and data/model ratios. Black data points and model histogram are for ObsID 2030; red for ObsID 4743; green for ObsID 5197; blue for ObsID 22372. See Table 4 for the fit parameters. The spectra were fitted with the Cash statistics; the data points have been rebinned to a signal-to-noise ratio >3 for plotting purposes only. The decreasing count rates below 1 keV from the black to the green and blue spectra are the result of the decrease of ACIS-S sensitivity from 2001–2020, for the same absorbing column density.
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Combined Chandra/ACIS-S spectrum of X-1 from ObsIDs 2030, 5197, and 22372, with best-fitting diskbb model and data/model ratios. See Table 5 for the fit parameters. The spectra were fitted with the Cash statistics; the data points have been rebinned to a signal-to-noise ratio >3 for plotting purposes only.
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Average Chandra light curve of X-1 in the 0.3–8 keV band, folded on three alternative and statistically equivalent binary periods, and rebinned to 35 phase intervals per period. Top panel: folding period of 13,020.24 s; middle panel: folding period of 12,953.12 s; bottom panel: folding period of 12,937.86 s.
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Details of the central region of NGC 4214, adapted from an HST/WFC3 image processed and published by the Hubble Heritage Team (images from the GO-11360 program; PI: R. O’Connell). The red color comes from a combination of the F657N and F814W filters; the green color is from F502N and F547M; the blue color is from F225W, F336W, F438W, and F487N. The optical counterpart of X-1 is marked by an arrow near the bottom right of the image. It is at the outskirts of the current starburst region. Credit: NASA, ESA, and the Hubble Heritage (STScI/AURA)-ESA/ Hubble Collaboration.
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Top panel: zoomed-in view of the field around X-1 in the near-UV band (HST/WFC3 UVIS filter F225W). The circle has a radius of 0.″2, approximately corresponding to the positional uncertainty of the X-ray source on the HST image. The image has been smoothed with a Gaussian kernel of radius 2 pixels. Middle panel: HST/WFC3 UVIS true color image of the same field, also smoothed with a 2 pixel Gaussian. Red = F814W, green = F547M, blue = F336W. Bottom panel: (unsmoothed) HST/WFC3 IR image of the same field (F160W filter).
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Unfolded Chandra/ACIS-S spectra of X-1 in the four epochs of observations, based on a power-law model (Table 4). Color coding and re-binning are as in Figure 6. The unfolded spectra highlight that X-1 was in a different state in ObsID 4743, compared with the other three epochs.
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Left panel: Chandra/ACIS-S spectra above (blue data points) and below (red data points) a threshold corresponding to an equivalent count rate of 0.01 ct s−1 in ObsID 2030. The spectra were simultaneously fitted with the Cash statistics; the data points have been rebinned to a signal-to-noise ratio >2.7 for plotting purposes. The fitted model is tbabs Gal×tbabs int×pcfabs×diskbb, with all parameters locked between the two spectra except for the covering fraction in pcfabs. The best-fitting covering fraction in the low-flux spectrum is (91 ± 2)% (C-stat =658.4/786). A formally identical fit is obtained with the pure Compton scattering model cabs, which implies a column density of the scattering medium N H = (3.0 ± 0.3) × 1024 cm−2 in front of the low-flux spectrum. Right panel: as in the left panel, for a threshold corresponding to an equivalent count rate of 0.03 ct s−1 in ObsID 2030. The best-fitting partial-covering fraction is (76 ± 2)% for the low-flux spectrum. Alternatively, a Compton scattering model implies N H = (1.8 ± 0.1) × 1024 cm−2 (C-stat =825.7/874 in both models).
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: SED plot showing that the optical data require two blackbody components: one at a characteristic temperature of ≈(90,000 ± 30,000) K and radius ≈(2.1 ± 0.3)R ⊙ (strongly dependent on the poorly constrained reddening); the other at T ≈ (2700 ± 300) K and R ≈ (420 ± 50)R ⊙. Blue data points are from Chandra and from the broadband and medium-band filters of HST/WFC3 (Table 3). In addition, we have plotted (green data points) the flux density measured in the two narrow-band HST/WFC3 filters with the highest signal-to-noise ratio (F657N and F673N).
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. IV. Development of SPECIAL BLEND: A New Public Analysis Code for Supernova Neutrinos
Authors: Akira Harada, Yudai Suwa, Masayuki Harada, Yusuke Koshio, Masamitsu Mori, Fumi Nakanishi, Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Roger A. Wendell
Figure caption: Distance dependence of parameter best fits and 68%/95% CIs. The average PDFs of 100 realizations are used to determine best fits and CIs. The top, middle, and bottom panels correspond to the mass, radius, and energy, respectively. The upper and lower portions for each panel indicate the parameter ranges and 68% relative uncertainties, respectively. The true values are indicated by cyan lines.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. IV. Development of SPECIAL BLEND: A New Public Analysis Code for Supernova Neutrinos
Authors: Akira Harada, Yudai Suwa, Masayuki Harada, Yusuke Koshio, Masamitsu Mori, Fumi Nakanishi, Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Roger A. Wendell
Figure caption: The simplified likelihood to see the symmetrization. The lower panels show the single likelihooddefined in Equation (A4), while the upper panels display the likelihood in Equation (A3). The left, middle, and right panels are the likelihoods as functions of the normalized mass m, radius r, and energy e, respectively. To draw this graph, the event time and energy are fixed as (t, ϵ) = (30 s, 6.8 MeV). The event energy is the mean positron energy at the event time.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. IV. Development of SPECIAL BLEND: A New Public Analysis Code for Supernova Neutrinos
Authors: Akira Harada, Yudai Suwa, Masayuki Harada, Yusuke Koshio, Masamitsu Mori, Fumi Nakanishi, Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Roger A. Wendell
Figure caption: The parameter PDFs at various distances. PDFs for each realization are indicated by thin gray lines, while the thick black line shows the average. The left, middle, and right columns correspond to the mass, radius, and energy, respectively. The distances are indicated at the upper-right corner of each panel; they are in ascending order from top to bottom. The analysis mode BLH or UBLH is selected according to the neutrino event number; see text for detail. The vertical dashed lines presented in each panel indicate the true values.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. IV. Development of SPECIAL BLEND: A New Public Analysis Code for Supernova Neutrinos
Authors: Akira Harada, Yudai Suwa, Masayuki Harada, Yusuke Koshio, Masamitsu Mori, Fumi Nakanishi, Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Roger A. Wendell
Figure caption: Triangle plot for the mass, radius, and energy estimation. For the 2D likelihood, the best-fit values and 68%/95% CIs are shown. The different colors indicate different likelihoods: red, UBLH; green, BLH; and blue, GALH. Black crosses and vertical dashed lines indicate the true values.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. IV. Development of SPECIAL BLEND: A New Public Analysis Code for Supernova Neutrinos
Authors: Akira Harada, Yudai Suwa, Masayuki Harada, Yusuke Koshio, Masamitsu Mori, Fumi Nakanishi, Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Roger A. Wendell
Figure caption: One-dimensional marginalized likelihoods for different realizations of mock observational data. The top (UBLH) and middle (BLH) rows show the parameter estimation results of all realizations (thin lines with lighter colors) and their averages (thick lines with darker colors). The bottom row compares the averages of the UBLH, BLH, and GALH. For each panel, true values are indicated by vertical dashed lines.
Paper: On the Short-period Eclipsing High-mass X-Ray Binary in NGC 4214
Authors: Zikun Lin, Roberto Soria, Douglas A. Swartz
Figure caption: Chandra/ACIS-S spectrum of X-1 from ObsID 4743, with best-fitting pow + apec model and data/model ratios. See Table 6 for the fit parameters. The spectra were fitted with the Cash statistics; the data points have been rebinned to a signal-to-noise ratio >3 for plotting purposes only. The green histogram shows the contribution of the apec component; the magenta histogram represents the power-law component; the red histogram shows the combined model.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. IV. Development of SPECIAL BLEND: A New Public Analysis Code for Supernova Neutrinos
Authors: Akira Harada, Yudai Suwa, Masayuki Harada, Yusuke Koshio, Masamitsu Mori, Fumi Nakanishi, Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Roger A. Wendell
Figure caption: Distance dependence of the parameter estimation similar to Figure 4. The differences are that the red and blue lines correspond to the results using ﹩{w}_{\mathrm{log}}(\theta )﹩ and w lin(θ), respectively, and the 95% CIs are omitted.
Paper: Searching for the Sources of Excess Extragalactic Dispersion of FRBs
Authors: Sunil Simha, Khee-Gan Lee, J. Xavier Prochaska, Ilya S. Khrykin, Yuxin Huang, Nicolas Tejos, Lachlan Marnoch, Metin Ata, Lucas Bernales, Shivani Bhandari, Jeff Cooke, Adam T. Deller, Stuart D. Ryder, Jielai Zhang
Figure caption: An updated Macquart relation plot including published well-localized FRBs from CRAFT at z ≲ 1. The solid line is the mean 〈DMcosmic〉 from a universe with a ΛCDM cosmology, aka the Macquart relation. The blue shading represents p(DMcosmic∣z), the probability distribution function (PDF) of DMcosmic at each redshift given the variance in the matter density along a random sight line in the Universe from intervening halos and the gas in the cosmic web filaments. Note the median of the distribution (dashed line) lies lower than the mean, implying that most sight lines are expected to have few intervening foreground halos that contribute significantly to DMcosmic. The data points are estimates ﹩{\mathrm{DM}}_{\mathrm{cosmic}}^{\mathrm{est}}﹩ for FRBs from the CRAFT survey. These are the observed DMFRB corrected for the Milky Way contribution and an assumed host contribution of ﹩\overline{{\mathrm{DM}}_{\mathrm{host}}}=186\,\mathrm{pc}\,{\mathrm{cm}}^{-3}﹩ in the rest frame. The sight lines examined in this work are marked in red, all of which have ﹩{\mathrm{DM}}_{\mathrm{cosmic}}^{\mathrm{est}}\gt \langle {\mathrm{DM}}_{\mathrm{cosmic}}\rangle ﹩. Of the other notably high ﹩{\mathrm{DM}}_{\mathrm{cosmic}}^{\mathrm{est}}﹩ sources, FRB20190520B (z FRB ∼ 0.23) at ∼1000 pc cm−3 will be analyzed in a future work.
Paper: Searching for the Sources of Excess Extragalactic Dispersion of FRBs
Authors: Sunil Simha, Khee-Gan Lee, J. Xavier Prochaska, Ilya S. Khrykin, Yuxin Huang, Nicolas Tejos, Lachlan Marnoch, Metin Ata, Lucas Bernales, Shivani Bhandari, Jeff Cooke, Adam T. Deller, Stuart D. Ryder, Jielai Zhang
Figure caption: Empirical evaluation of DMhalos for the FRB sight lines as a function of redshift. The blue curve presents the cumulative estimation of DMhalos from z = 0, which increases monotonically as foreground halos are encountered along the sight line. The blue shading represents 68% confidence limits on the DMhalos estimate, which is the running quadrature sum of the individual 1σ limits of the DM distributions for the individual galaxies. The black dashed lines represent estimates for 〈DMhalos〉 assuming the adopted HMF (up to M halo = 1016  M ⊙) and the adopted halo gas distribution model used to calculate DMhalos. While the FRB20190714A sight line clearly exceeds the average expectation, both FRB20210117A and FRB20200906A are barely in excess of DMhalos = 0 pc cm−3. FRB20200430A exhibits a DMhalos value consistent with 〈DMhalos〉.
Paper: Searching for the Sources of Excess Extragalactic Dispersion of FRBs
Authors: Sunil Simha, Khee-Gan Lee, J. Xavier Prochaska, Ilya S. Khrykin, Yuxin Huang, Nicolas Tejos, Lachlan Marnoch, Metin Ata, Lucas Bernales, Shivani Bhandari, Jeff Cooke, Adam T. Deller, Stuart D. Ryder, Jielai Zhang
Figure caption: Estimates of DMcosmic for the FRB sight lines as a function of redshift. The solid, teal curve is ﹩{\mathrm{DM}}_{\mathrm{cosmic}}^{\mathrm{model}}﹩, the sum of DMhalos, i.e., the solid blue curve from Figure 5 and an estimate of the average IGM contribution to DMcosmic (see Equation (7)). The dotted line shows 〈DMcosmic〉 at z FRB in each subplot. The shading around the solid curve represents a 68% confidence limit which includes an assumed 20% uncertainty for 〈DMIGM〉 in quadrature with the uncertainties from Figure 5. The red point is an estimate of DMcosmic for each FRB taken from Figure 1, i.e., by subtracting the assumed host and Milky Way contributions.
Paper: Searching for the Sources of Excess Extragalactic Dispersion of FRBs
Authors: Sunil Simha, Khee-Gan Lee, J. Xavier Prochaska, Ilya S. Khrykin, Yuxin Huang, Nicolas Tejos, Lachlan Marnoch, Metin Ata, Lucas Bernales, Shivani Bhandari, Jeff Cooke, Adam T. Deller, Stuart D. Ryder, Jielai Zhang
Figure caption: Zoomed-in (﹩5^{\prime} \times 5^{\prime} ﹩) illustration of the fields and results for the four FRB sight lines: (a) FRB20190714A, (b) FRB20200430A, (c) FRB20200906A, and (d) FRB20210117A. The background shows Pan-STARRS r-band images. In each image, the red cross marks the location of the FRB, the green triangles mark background galaxies, and the yellow stars mark the point sources that were ignored from spectroscopic targeting. The blue circles mark foreground galaxies, which are color scaled according to the estimated DMhalo value.
Paper: Searching for the Sources of Excess Extragalactic Dispersion of FRBs
Authors: Sunil Simha, Khee-Gan Lee, J. Xavier Prochaska, Ilya S. Khrykin, Yuxin Huang, Nicolas Tejos, Lachlan Marnoch, Metin Ata, Lucas Bernales, Shivani Bhandari, Jeff Cooke, Adam T. Deller, Stuart D. Ryder, Jielai Zhang
Figure caption: Histogram of galaxy redshifts obtained from the AAOmega spectrograph in the four fields. The full 1.°1 radius sample is shown in blue and the subset of galaxies within 10′ is shown in orange. The FRB redshift is marked by the dashed red line, and the shaded regions represent background galaxies that are not relevant to this study.