adsabs/AstroCLIMB huggingface dataset:
Paper: ALMASOP. The Localized and Chemically Rich Features near the Bases of the Protostellar Jet in HOPS 87
Authors: Shih-Ying Hsu, Chin-Fei Lee, Sheng-Yuan Liu, Doug Johnstone, Tie Liu, Satoko Takahashi, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Neal J. Evans, Naomi Hirano, Mika Juvela, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Xunchuan Liu, Qiuyi Luo, Sheng-Li Qin, Dipen Sahu, Patricio Sanhueza, Hsien Shang, 賢 尚, Kenichi Tatematsu, Yao-Lun Yang
Figure caption: The velocity widths vs. upper energy for the molecular transitions in the two chemically rich regions. Only molecular species having multiple transitions are included. The blue and red markers represent the measurement at the blueshifted (northern) and redshifted (southern) lobes, respectively. The error bars are referred from the spectral channel widths (∼1.4 km s−1.) The velocity widths seem to be anticorrelated with the upper energies of the molecular transitions, possibly due to the different populations of each transition state.
Paper: ALMASOP. The Localized and Chemically Rich Features near the Bases of the Protostellar Jet in HOPS 87
Authors: Shih-Ying Hsu, Chin-Fei Lee, Sheng-Yuan Liu, Doug Johnstone, Tie Liu, Satoko Takahashi, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Neal J. Evans, Naomi Hirano, Mika Juvela, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Xunchuan Liu, Qiuyi Luo, Sheng-Li Qin, Dipen Sahu, Patricio Sanhueza, Hsien Shang, 賢 尚, Kenichi Tatematsu, Yao-Lun Yang
Figure caption: The PV diagrams of ratios between flux densities. The label in each panel denotes the molecular transitions for the numerator and denominator. The pixels having flux density smaller than 5σ are excluded.
Paper: ALMASOP. The Localized and Chemically Rich Features near the Bases of the Protostellar Jet in HOPS 87
Authors: Shih-Ying Hsu, Chin-Fei Lee, Sheng-Yuan Liu, Doug Johnstone, Tie Liu, Satoko Takahashi, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Neal J. Evans, Naomi Hirano, Mika Juvela, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Xunchuan Liu, Qiuyi Luo, Sheng-Li Qin, Dipen Sahu, Patricio Sanhueza, Hsien Shang, 賢 尚, Kenichi Tatematsu, Yao-Lun Yang
Figure caption: Integrated-intensity images of all transitions listed in Table A1. The other captions follow Figure 1. Note that some panels are repeated from Figure 1 but may be labeled differently. The black and the green contours depict the 1.3 mm continuum and the SiO integrated-intensity map, respectively.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: A detailed view of the average flare spectrum (black line) from the IRIS FUV bandpasses with line identifications. Fitted H2 Lyman band lines are identified in blue with the (J, v) quantum numbers of the upper level. Fitted atomic lines are noted in red, while atomic lines that were not fitted are labeled in magenta. Fitted lines with unknown identifications are labeled in gray. The composite fitted profiles for H2, unknown, and weak atomic lines are shown by the dark-blue, gray, and red lines, respectively, where the continuum level of each is given an arbitrary offset from zero. The FALC × 100 synthetic H2 spectrum is shown in cyan. The background 2D spectrum has a reversed logarithmic color scale and comes from the time and slit position indicated in Figures 1 and 2.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: An example of how the spectral radiance for the H2 pumping line was derived from the spatially resolved flare spectra. For each H2 pumping wavelength considered (pink dashed line), we reversed the H2 line wavelength with respect to the rest wavelength of the transition region line that provides the pumping photons and interpolated the spectral radiance at this location (red dashed line). The line profiles shown here come from the position indicated by the plus sign in Figure 2.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: Maps of line amplitude (left), Doppler velocity (middle), and FWHM (right) derived from line-fitting analysis of the mid-chromospheric O I line at 1355.598 Å (top), the two brightest H2 lines in the IRIS FUV (middle panels), and the photospheric Fe I line from the NUV (bottom). The H2 velocity maps share some features in common with both the photospheric and chromospheric lines, but they also have unique features, indicating that H2 probes a unique height between the photosphere and chromosphere. The color scales are specific to each plot grouping.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: An example of the chromospheric O I and photospheric Fe I line fits performed on the spatially resolved flare spectrum. The line profiles shown here come from the position indicated by the plus sign in Figure 2.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: Selected lines of H2, neutral atomic species, and Fe II were used to determine the approximate local rest frame for the 1D flare spectrum in the IRIS FUV 1 (top) and FUV 2 (bottom) channels. The error bars plotted for each point represent the 1σ errors in the fitted wavelength.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: An example of H2 line fits performed on the spatially resolved flare spectrum. The line profiles shown here come from the position indicated by the plus sign in Figure 2.
Paper: Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Shu-Qing Zhong, Long Li, Biao Zhang, Zi-Gao Dai
Figure caption: Upper panel: illustration of the coordinate systems in which the polarization vector relevant to synchrotron emission is calculated. Here, the local bulk velocity direction is ﹩\hat{{\boldsymbol{\beta }}}=\hat{{\boldsymbol{r}}}﹩ and the uniform magnetic field direction is transverse to that with azimuthal angle ϕ  B . The inclination angle Θ in the lab frame is between the directions of the local bulk velocity and observed photon (the LOS ﹩\hat{{\boldsymbol{n}}}﹩), with ﹩\cos {\rm{\Theta }}=\hat{{\boldsymbol{n}}}\cdot \hat{{\boldsymbol{\beta }}}﹩. Lower panel: the observer sees the projection of the ordered magnetic field (blue arrow) and polarization vector (red arrow) on the plane of the sky (shaded yellow region; orthogonal to the observed photon direction with wavevector ﹩\hat{{\boldsymbol{k}}}=\hat{{\boldsymbol{n}}}﹩, which points out of the page). For an ordered magnetic field, the PA α is measured from the ordered field direction (solid arrow); otherwise, α is measured from the projection of the ejecta axis (dashed arrow).
Paper: Estimating the Spin of MAXI J1348–630 from Intermediate and Soft States Using Insight-HXMT Data
Authors: J. Guan, R. C. Ma, L. Tao, A. C. Fabian, J. A. Tomsick, S. N. Zhang, L. Zhang, J. L. Qu, S. Zhang
Figure caption: Top panel: Spin measurements are shown with different hardening factors f col. The blue and red represent the results of the kerrbb model with f col fixed at 1.6 and the kerrbb2 model with a free f col, respectively. Bottom panel: The evolution of the hardening factor f col over time is depicted. The blue and red represent the results of the kerrbb model with a fixed spin at 0.8 and the kerrbb2 model with a freely fitted spin, respectively.
Paper: Estimating the Spin of MAXI J1348–630 from Intermediate and Soft States Using Insight-HXMT Data
Authors: J. Guan, R. C. Ma, L. Tao, A. C. Fabian, J. A. Tomsick, S. N. Zhang, L. Zhang, J. L. Qu, S. Zhang
Figure caption: Evolution of the spectral parameters of model const∗Tbabs∗(kerrbb2+NthComp+relconv* reflionx_hd_Nthcomp). a * is the spin; ﹩\dot{M}﹩ is the mass accretion rate in units of 1018 g s−1; N nthC is the normalization of NthComp; ξ is the ionization of the accretion disk; A Fe is the iron abundance; Γ is the photon index; kT bb is the seed photon temperature; N Refl is the normalization of reflionx_hd_Nthcomp. The vertical line represents the transition from SIMS to SS on approximately MJD 58258.
Paper: Estimating the Spin of MAXI J1348–630 from Intermediate and Soft States Using Insight-HXMT Data
Authors: J. Guan, R. C. Ma, L. Tao, A. C. Fabian, J. A. Tomsick, S. N. Zhang, L. Zhang, J. L. Qu, S. Zhang
Figure caption: Comparison of the spin derived from different data and models. Red: Insight-HXMT spectra fitted with const∗Tbabs∗(kerrbb2+NthComp+relconv*reflionx_hd_Nthcomp) model; green: Insight-HXMT spectra fitted with const∗Tbabs∗(kerrbb2+NthComp+relconv∗relxillD model; black: NuSTAR spectrum fitted with const∗Tbabs∗(kerrbb2+NthComp+relconv*reflionx_hd_Nthcomp) model. The vertical line represents the transition from SIMS to SS.
Paper: Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Shu-Qing Zhong, Long Li, Biao Zhang, Zi-Gao Dai
Figure caption: Top: the best spectral modeling for the FXRB associated with FRB 20200428. Middle: time-sliced and averaged PDs in the energy range of 1− 300 keV. Bottom: energy-sliced and averaged PDs in the time range of 10−3−0.5 s since t 0 − 0.220 s, in which t 0 = 14:34:24.447 UT is the trigger time (A. Ridnaia et al. 2021).
Paper: Estimating the Spin of MAXI J1348–630 from Intermediate and Soft States Using Insight-HXMT Data
Authors: J. Guan, R. C. Ma, L. Tao, A. C. Fabian, J. A. Tomsick, S. N. Zhang, L. Zhang, J. L. Qu, S. Zhang
Figure caption: Representative spectrum (ObsID P021400203601) of MAXI J1348 fitted with const∗Tbabs∗(kerrbb2+NthComp+relconv* reflionx_hd_Nthcomp). The red, blue, green, and black dashed lines represent the thermal, Compton, reflection, and total components, respectively.
Paper: Estimating the Spin of MAXI J1348–630 from Intermediate and Soft States Using Insight-HXMT Data
Authors: J. Guan, R. C. Ma, L. Tao, A. C. Fabian, J. A. Tomsick, S. N. Zhang, L. Zhang, J. L. Qu, S. Zhang
Figure caption:  R ISCO-scaled inner disk radius, simply derived from the formula of spin vs. ISCO radius, as a function of the Eddington-scaled luminosity. R ISCO is calculated assuming the spin value to be 0.8, while the Eddington luminosity is computed assuming M = 11 M ⊙.
Paper: Estimating the Spin of MAXI J1348–630 from Intermediate and Soft States Using Insight-HXMT Data
Authors: J. Guan, R. C. Ma, L. Tao, A. C. Fabian, J. A. Tomsick, S. N. Zhang, L. Zhang, J. L. Qu, S. Zhang
Figure caption: Representative spectrum (ObsID P021400203601) of MAXI J1348 fitted with constant∗TBabs∗(diskbb+powerlaw). The red, blue, and black dashed lines represent diskbb, powerlaw, and the total component, respectively.
Paper: Mildly Super-Eddington Accretion onto Slowly Spinning Black Holes Explains the X-Ray Weakness of the Little Red Dots
Authors: Fabio Pacucci, Ramesh Narayan
Figure caption: In the plane ﹩{\mathrm{log}}_{10}{L}_{\mathrm{bol}}﹩ vs. X-ray bolometric correction (in the observed 2–10 keV range, for z = 6), we compare the X-ray weakness of our super-Eddington SEDs with that of high-z LRD populations, and some well-known low-z samples. Teal dots represent the bolometric corrections derived in this study from super-Eddington SEDs at z = 6 (i.e., the median redshift from LRDs catalogs). Note that the bolometric luminosities of our SEDs are compatible with those observed. Orange circles indicate LRD populations at 4 < z < 11 from R. Maiolino et al. (2024) and M. Yue et al. (2024), with arrows showing lower limits, while the red star marks the stacked data point (for sources at z > 4) from the work of R. Maiolino et al. (2024), which provides the most robust constraint. The dark orange circle displays the location of GN-28074, which is the most X-ray weak among all AGNs discovered by JWST (z = 2.26; I. Juodžbalis et al. 2024a). Note that each data point has been shifted to the observed 2–10 keV range, to be comparable to our SEDs. The solid black line (with its spread) represents the rest-frame k X(L bol) relation from F. Duras et al. (2020). The gray distribution in the background shows low-z Type-1 AGN data from E. Lusso et al. (2020).
Paper: Mildly Super-Eddington Accretion onto Slowly Spinning Black Holes Explains the X-Ray Weakness of the Little Red Dots
Authors: Fabio Pacucci, Ramesh Narayan
Figure caption: Comparison between accretion structures in the poloidal plane (the black hole is at (0, 0) and the jets are oriented in the vertical direction) for our reference cases of X-ray-weak (left) and X-ray-strong (right) SEDs (see Section 4.4). The rows are, from top to bottom: temperature, gas density, scattering optical depth, and β γ. X-ray-strong accretion structures are significantly hotter and more relativistic.
Paper: Photospheric Hot Spots at Solar Coronal Loop Footpoints Revealed by Hyperspectral Imaging Observations
Authors: L. P. Chitta, M. van Noort, H. N. Smitha, E. R. Priest, L. H. M. Rouppe van der Voort
Figure caption: Coronal evolution. Panels (a) and (b) show the coronal EUV emission maps recorded by the AIA 193 Å and 211 Å filters. The green box outlines the MiHI FOV (see Figure 1). The white dashed box marks the area over which we detected hot spots in our MiHI Hα data. The black contours represent the locations where these hot spots were detected over the course of ∼65 minutes of observations. In panel (c) we plot the EUV emission light curves from the two filters (brown- and purple-colored curves). These light curves are mean EUV emission from the respective white dashed box. The gray vertical lines mark the instances when we detected hot spots. In this case, a vertical line is drawn if a given MiHI snapshot has at least one hot spot in the FOV. See Sections 2 and 4 for details.
Paper: Photospheric Hot Spots at Solar Coronal Loop Footpoints Revealed by Hyperspectral Imaging Observations
Authors: L. P. Chitta, M. van Noort, H. N. Smitha, E. R. Priest, L. H. M. Rouppe van der Voort
Figure caption: Observed and inverted Hα line profiles. The symbols around Δλ = 0 Å in each panel are the observed Hα Stokes I profiles, normalized to the quiet-Sun continuum, of four different features as labeled. Continuum points are assumed to be on both blue and red wings of the observed line profile between 55 and 60 Å away from the nominal line core position (i.e., 6562.817 Å). We note that the observed continuum point is actually around 6468 Å (i.e., about 95 Å away from the line core on the blue-wing side). The observed Hα Stokes I profiles including the assumed continuum points are normalized to the observed local continuum and further scaled with respect to the quiet-Sun continuum intensity. The solid black curves represent the best-fit inverted Hα Stokes I profiles. Insets in each panel zoom into the ±2 Å about the core region of the respective Hα profiles. See Section 3.2 for details.
Paper: Photospheric Hot Spots at Solar Coronal Loop Footpoints Revealed by Hyperspectral Imaging Observations
Authors: L. P. Chitta, M. van Noort, H. N. Smitha, E. R. Priest, L. H. M. Rouppe van der Voort
Figure caption: Thermal diagnostics. Temperature stratification on optical depth scale of the inverted atmospheres corresponding to the various analyzed features as labeled. Four selected hot-spot atmospheres are shown in red and are labeled by their event number. See Section 3.2 for details.
Paper: Photospheric Hot Spots at Solar Coronal Loop Footpoints Revealed by Hyperspectral Imaging Observations
Authors: L. P. Chitta, M. van Noort, H. N. Smitha, E. R. Priest, L. H. M. Rouppe van der Voort
Figure caption: Statistical properties of hot spots. Histograms of lifetimes detected events (panel (a)) and the size of individual events at every instance throughout their lifetime (panel (b)) are shown. See Section 3 for details.
Paper: Photospheric Hot Spots at Solar Coronal Loop Footpoints Revealed by Hyperspectral Imaging Observations
Authors: L. P. Chitta, M. van Noort, H. N. Smitha, E. R. Priest, L. H. M. Rouppe van der Voort
Figure caption: Examples of hot spots. Same as Figure 2, but showing additional examples.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: Luminosity vs. redshift plot showing all unresolved radio sources as circle markers from this work. The detections and deep limits obtained from VLA observations are plotted as light green inverted triangles and colored circles. The markers with red-colored marker edges are estimated with z spec while others are estimated using ﹩{z}_{\max }﹩. The luminosities shown in circles for these detections except the ones with red marker edges are considered upper limits since they were estimated using ﹩{z}_{\max }﹩. In addition to the PRS of FRB 20121102A, 20190520B, and a potential PRS of FRB 20201124A (all light blue stars), we also show limits for FRB 20180916B (diamonds), and FRB 20200120E (hexagons). M19 and K20 represent B. Marcote et al. (2019) and F. Kirsten et al. (2020), respectively. The blue dotted line is the luminosity of the PRS of FRB 20121102A. Upper limits on PRSs from VLASS (small purple and white inverted triangles for first and second epochs) are also plotted, and two VLASS detections are shown as purple circles. The purple and orange dashed lines are the VLASS and LoTSS 5σ sensitivity limit as a function of redshift. The two potential PRSs from this work are shown as bigger circles with black-lettered labels: 20181030A-1 and 20190417A-1. 3σ and 5σ luminosity upper limits on the presence of a PRS are shown as inverted light green triangles for FRBs fields observed with VLA for FRBs having subarcsecond and baseband localizations respectively.
Paper: Multi-Observatory Research of Young Stellar Energetic Flares (MORYSEF): X-Ray-flare-related Phenomena and Multi-epoch Behavior
Authors: Konstantin V. Getman, Eric D. Feigelson, Abygail R. Waggoner, L. Ilsedore Cleeves, Jan Forbrich, Joe P. Ninan, Oleg Kochukhov, Vladimir S. Airapetian, Sergio A. Dzib, Charles J. Law, Christian Rab
Figure caption: (a)–(f) Comparison of Chandra ACIS-I apparent X-ray MEs across different epochs. The red lines represent the unity reference, while the green lines show linear regression fits derived using the Major Axis algorithm, which treats variables symmetrically (D. I. Warton et al. 2006), from R’s lmodel2 function (P. Legendre & L. Legendre 1998). The figure legends display the intercept, slope, and 68% confidence interval half-widths from the lmodel2 results. Panels (a)–(c) include only characteristic light-curve segments (i.e., “c” in Column (9) of Table 3), while panels (d)–(f) encompass all light-curve segments (i.e., large flares “f,” mild variability “n,” and characteristic “c”). (g-i) ECDFs of fractional differences (MEepoch − ME2003)/ME2003 across different energy ranges, epochs, and light-curve segments. Energy ranges: (g) all stars, (h) stars with ME2003 < 3 keV, and (i) stars with ME2003 ≥ 3 keV. Epochs: 2012 (cyan), 2016 (purple), and 2023 (blue). Light-curve segments: solid curves represent only characteristic segments, while dashed curves represent all segments.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: Gemini North spectra for the plausible host galaxies of radio sources 20190110C-S (top panel), 20190117A-S (middle panel), and 20190417A-S1 (bottom panel). In the top panel, the spectrum exhibits a bright emission line, possibly H α , which is also clearly visible in the 2D spectra. In the middle panel, there are no prominent emission or absorption lines, making it unsuitable for estimating the redshift of the likely host galaxy of 20190117A-S. In the bottom panel, the spectrum of the likely host galaxy of 20190417A-S1 displays distinct emission line features, indicated by dashed gray lines. These lines were used to derive a redshift of z spec = 0.12817(2) and other properties of the galaxy as discussed in Section A.9.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: VLA images capturing the six FRB fields featuring detected radio sources (unresolved, resolved, and extended). The 90% confidence level baseband error regions of the FRBs are depicted as red ellipses. For some fields, the white crosshair marks the location of the sources, while others have the sources labeled with “S” corresponding to the number of radio sources in the field. The beam of each image is represented by a small cyan-colored ellipse at the lower left corner of each image.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: Spectral energy distribution of the unresolved radio sources shown as colored circles while the colored stars are known PRSs (FRB 20121102A, FRB 20190520B) and a potential third PRS. In general, most of the sources have nonpositive spectral shapes similar to that seen for FRB 20121102A and FRB 20190520B. 20181119A-S (brown) is the only source with a positive spectra shape among the radio sources but similar to that of the potential PRS of FRB 20201124A. Solid lines connect contemporaneous flux periods.