adsabs/AstroCLIMB huggingface dataset:
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: Background-subtracted 0.3–9 keV NICER spectra of IM Peg during the intervals a0−a4 (panel (a), ObsID 6203900101) and b0−b4 (panel (b), ObsID 6203900102). The best-fit models using the three-temperature CIE components (vapec) are shown by the solid black line, composed of 92 MK (red dashed), 15 MK (green dashed–dotted), and 0.92 MK (blue dotted) for panel (a) and 64 MK (red dashed), 13 MK (green dashed–dotted), and 0.92 MK (blue dotted) for panel (b). The navy solid lines show the background spectra calculated with the 3C50 model. The right upper inset panels show the enlarged spectra around the iron emission lines. The lower panels in (a) and (b) are the ratio of the observed data relative to the best-fit model.
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: (a) The interval b1 spectrum fitted with a phenomenological model (powerlaw+Gauss+Gauss). The vertical green and blue dashed–dotted lines indicate the line center of Heα and Lyα emission lines at the rest frame in the CIE model, respectively. The green and blue shaded areas show the 90% error range of the line center of the two Gaussians. (b) Theoretically expected CIE spectrum during the interval b1 at the electron temperature of ﹩{T}_{e}^{{\rm{b}}1}\sim 76﹩ MK calculated with PyAtomDB. (c) Same spectrum as panel (b) folded by the NICER response function.
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: (a) 64 s binned 0.3–4 keV count rate (cps; counts s−1) during all NICER observations of IM Peg. The time zero of MJD 60148.5 corresponds to 12:00 UT 2023 July 23. The one standard deviation statistical error bars are smaller than the symbol size. The navy vertical dashed–dotted line indicates the time when MAXI detected the flare (∼ −0.05 day). (b) Enlarged light curve during the first two ObsIDs 6203900101 (blue) and 6203900102 (green). Interval numbers in our spectral analysis are shown above the inset panel.
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: Comparison of spectral fittings using different plasma models around the iron emission lines during the interval b1: the CIE (apec, panel (a)); ionizing (nei, panel (b)); and recombining (rnei, panel (c)) plasma models with the velocity fixed at v = 0. The lower panels show the fitting residuals. Panels (d), (e), and (f) are the same as panels (a), (b), and (c), respectively, but letting the velocity of the plasma free.
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: Same as Figure 2 but during the intervals a0, b1, and b4 for panels (a), (b), and (c), respectively. The temperatures of the three components are 101, 15, and 1 MK for panel (a); 65, 13, and 1 MK for panel (b); and 49, 13, and 1 MK for panel (c).
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: (a)−(c) Examples of NICER Cas A spectra fitted with the phenomenological model of powerlaw+Gauss, whose exposure times are (a) ∼500 s, (b) ∼1000 s, and (c) ∼1500 s, respectively. Orange and green dashed lines indicate powerlaw and Gauss components, respectively. (d) The distribution of the line center of the Gaussian function (ΔE = E − E med). The upper panel shows the histogram of the distribution for all data (N = 605) and the Gaussian fitting (black dashed–dotted line). The color map shows the distribution at each range of the exposure time. The right panel shows the histogram of the distribution at each exposure time.
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: Doppler velocity of the blueshifted components of the Fe XXV Heα line (see, e.g., Figure E1) overlaid on that of the line center of the Fe XXV Heα line shown in Figure 4(g). Navy and red dashed lines indicate the Doppler velocity of the blueshifted components of the Fe XXV Heα line with the 90% error range during the combined intervals a0−a4 and b0−b4, respectively, when we fit the spectra with powerlaw+Gauss∗3 model. Green and orange dashed–dotted lines indicate the Doppler velocity of the line center of the Fe XXV Heα line with the 90% error range during the combined intervals a0−a4 and b0−b4, respectively, when we fit the spectra with the powerlaw+Gauss∗2 model.
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: Background-subtracted 5−9 keV spectra of IM Peg fitted with a phenomenological model (powerlaw+Gauss∗3) during the intervals a0−a4 and b0−b4 for panels (a) and (b), respectively. Green dashed–dotted and blue dashed lines correspond to the Fe XXV Heα and the Fe XXVI Lyα lines, respectively, whose line centers are fixed to the values in the laboratory frame. Navy dotted lines indicate the blueshifted components of the Fe XXV Heα line.
Paper: Extended Emission-line Regions in Poststarburst Galaxies Hosting Tidal Disruption Events
Authors: Thomas Wevers, K. Decker French
Figure caption: Composite color image and emission-line contour map. Left: three-color composite image combining the continuum emission (7200–7500 Å, in red), Hα (green hues), and [O III] (blue hues) emission. These maps reveal spatially EELRs far beyond the stellar continuum. Note that this panel does not cover the full MUSE field of view, only the regions of interest. Right: emission-line contour maps of [O III] overlaid on a continuum image. A red cross marks the center of the continuum emission for reference. Several regions identified by colored circles are used for detailed spectral analysis. The contours in the right panel represent an [O III] flux level of 60 (outer), 150 (middle), and 300 (inner) × 10−20 AA−1 erg cm−2 s−1 Å. The lowest flux contour is also shown in the left panel.
Paper: Extended Emission-line Regions in Poststarburst Galaxies Hosting Tidal Disruption Events
Authors: Thomas Wevers, K. Decker French
Figure caption: Spectra and diagnostic diagrams. Top: spectra extracted from the regions indicated in Figure 1, illustrating the lack of continuum emission and the emission lines in regions C, D, and E. The nuclear spectrum (red) has been rescaled by a factor of 20 for clarity. Bottom: BPT (left) and WHAN (right) diagnostic diagrams of these aperture spectra. A hard/nonstellar ionizing continuum is required to power the extended emission although the nucleus does not currently host a powerful AGN (red cross in the LINER-like region).
Paper: Extended Emission-line Regions in Poststarburst Galaxies Hosting Tidal Disruption Events
Authors: Thomas Wevers, K. Decker French
Figure caption: Stellar and gas kinematics. Top: stellar velocity (left) and velocity dispersion (right). Stellar rotation is evident, and the stellar velocity dispersion peaks in the nucleus. Bottom: gas velocity (left) and velocity dispersion. The velocity of the gas is consistently blueshifted irrespective of the stellar motions, indicating that the gas is decoupled from the stars. The gas-velocity dispersion peaks at a higher value than the stellar dispersion in the nucleus, while it is very low across the EELR.
Paper: Extended Emission-line Regions in Poststarburst Galaxies Hosting Tidal Disruption Events
Authors: Thomas Wevers, K. Decker French
Figure caption: Constraints on the ionizing luminosity. Estimate of the nuclear ionizing luminosity required to power the recombination H Balmer lines in the EELR. The upper envelope traces the lower limit of ﹩{L}_{\mathrm{ion},\min }﹩ (marked by an orange line). We have removed low S/N spaxels with line fluxes <25 × 10−20 erg cm−2 s−1.
Paper: The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201
Authors: Tianjun Gan, Sharon X. Wang, Fei Dai, Joshua N. Winn, Shude Mao, Siyi Xu, Enric Pallé, Jacob L. Bean, Madison Brady, Nina Brown, Cicero Lu, Rafael Luque, Teo Mocnik, Andreas Seifahrt, Guđmundur K. Stefánsson
Figure caption: Top panel: projected stellar obliquity λ of giant-planet systems (M  p  ≥ 0.3 M  J ) versus host star effective temperature. Obliquity results are from RM measurements. The red dots are hot Jupiters (defined as having a/R ⋆ < 15), and the blue dots are warm Jupiters (a/R > 15). The position of TOI-4201b is marked with an black arrow. Bottom panel: same but for planets with M  p  < 0.3 M  J . In both panels, the vertical black line marks the Kraft break. The gray shaded region highlights the stars with T eff ≤ 4000 K. Results were retrieved from the NASA Exoplanet Archive (Akeson et al. 2013).
Paper: The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201
Authors: Tianjun Gan, Sharon X. Wang, Fei Dai, Joshua N. Winn, Shude Mao, Siyi Xu, Enric Pallé, Jacob L. Bean, Madison Brady, Nina Brown, Cicero Lu, Rafael Luque, Teo Mocnik, Andreas Seifahrt, Guđmundur K. Stefánsson
Figure caption: Projected stellar obliquity λ versus planet-to-star mass ratio, for four planet groups. Obliquity results are from RM measurements. Different colors represent planets with different scaled semimajor axes a/R *. Giant-planet systems with mass ratio M  p /M * over 3 × 10−3 (black vertical line) tend to be aligned, while small planets have a broad range of λ across mass ratio between 2 × 10−5 and 3 × 10−4. The position of TOI-4201b is marked with a black arrow.
Paper: The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201
Authors: Tianjun Gan, Sharon X. Wang, Fei Dai, Joshua N. Winn, Shude Mao, Siyi Xu, Enric Pallé, Jacob L. Bean, Madison Brady, Nina Brown, Cicero Lu, Rafael Luque, Teo Mocnik, Andreas Seifahrt, Guđmundur K. Stefánsson
Figure caption: TESS transit photometry of TOI-4201 from Sectors 06 and 33 (left), out-of-transit RVs (middle), and RM measurements after subtracting the best-fit Keplerian model (right). The excess scatter in the RVs after egress is probably due to the degraded seeing. In each case, the black curve illustrates the best-fit model. The plotted error bars are the quadrature sums of the formal measurement uncertainties and the fitted “jitter” parameters. Residuals are shown in the bottom panels.
Paper: The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201
Authors: Tianjun Gan, Sharon X. Wang, Fei Dai, Joshua N. Winn, Shude Mao, Siyi Xu, Enric Pallé, Jacob L. Bean, Madison Brady, Nina Brown, Cicero Lu, Rafael Luque, Teo Mocnik, Andreas Seifahrt, Guđmundur K. Stefánsson
Figure caption: Dimensionless, phase-folded, ground-based transit observations of TOI-4201 with maximum phase of 1. The instrument name and observation filter are shown at the top of each panel. The red solid lines represent the best-fit transit models from the joint-fit analysis.
Paper: The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201
Authors: Tianjun Gan, Sharon X. Wang, Fei Dai, Joshua N. Winn, Shude Mao, Siyi Xu, Enric Pallé, Jacob L. Bean, Madison Brady, Nina Brown, Cicero Lu, Rafael Luque, Teo Mocnik, Andreas Seifahrt, Guđmundur K. Stefánsson
Figure caption: The posterior distributions of key parameters in the joint fit (see Section 3). The red solid lines mark the median values of each distribution.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Burst profile and RM (RM = ∂PA/∂λ 2) in FRB 20210912A (left) and FRB 20181112A (right). The frequency-averaged Stokes I profiles of the FRBs are shown in red at a time resolution of 3.8 μs (in normalized flux density units not shown in the plots). The horizontal error bars represent the time range for the corresponding RM measurements. The absolute difference between the RMs of the sub-bursts is ≈15 rad m−2 for both FRBs (in the observer frame). See Sections 3 and 4 for details.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Short-timescale variation of RM (=∂PA/∂λ 2; top panel( and κ (=∂(V/I)/∂λ 2; bottom panel) in FRB 20210912A for sub-bursts A (left) and B (right). The frequency-averaged Stokes I profile is shown in red at a time resolution of 3.8 μs (in normalized flux density units not shown in the plots). The uncertainties in the abscissa are the time range for the corresponding measurements. The cyan dashed lines show best-fit Gaussian profiles to the RM variation (see Appendix C for details).
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Time-resolved polarization of FRB 20210912A. (a) The frequency-averaged normalized total intensity (I) and linearly (L) and circularly (V) polarized intensity at a time resolution of ≈3.8 μs. (b) PA of linear polarization. Corrections for the average RM (RMavg = 4.55 rad m−2) have been applied. The dashed curve shows the PA profile corresponding to an RVM with inclination of α = 76.°2 and magnetic obliquity of Θ = 59.°1. See text for details.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Short-timescale variation of RM (=∂PA/∂λ 2; top panel) and κ (=∂(V/I)/∂λ 2; bottom panel) in FRB 20181112A for sub-bursts A. The frequency-averaged Stokes I profile is shown in red at a time resolution of 3.8 μs (in normalized flux density units not shown in the plots). The horizontal error bars represent the time range for the corresponding measurements. The cyan dashed line shows the best-fit Gaussian profile to the RM variation.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Decomposition of the two sub-bursts A (left panel) and B (right panel) of FRB 20181112A into multiple exponentially scattered Gaussian components. The top panels show the intensity profiles in solid red curves, best-fit models in solid black curves, and individual components in dotted blue curves. The bottom panels show the residuals (normalized by the rms noise in the intensity profile). A faint emission component at t ≈ 1.2 ms remains unmodeled with the optimum number of components for sub-burst B.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Scaled burst profiles of FRB 20181112A and FRB 20210912A. The frequency-averaged Stokes I (total intensity) profiles of FRB 20210912A (blue) and FRB 20181112A (red) are plotted against time normalized by the separation between the two sub-bursts (ΔT) for each FRB, at a time resolution of ≈9.5 μs. Flux densities are normalized by the peak of the profile.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Total intensity time profiles of FRB 20210912A in four sub-bands within the observing frequency band. The central frequency of each sub-band is mentioned in the upper right corner. The flux densities have been normalized by the peak of the full-band profile. All profiles have a time resolution of 3.8 μs.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Full Stokes time profile and dynamic spectra (I, Q, U, V) of FRB 20210912A at a time resolution of 3.8 μs. The flux densities have been normalized by the peak of the total intensity profile. Q and U have been corrected for RMavg = 4.55 rad m−2.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Time-resolved polarization of FRB 20181112A. (a) The frequency-averaged normalized total intensity (I) and linearly (L) and circularly (V) polarized intensity at a time resolution of ≈3.8 μs. (b) PA of linear polarization. Corrections for the average RM (RMavg = 13.15 rad m−2) have been applied.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Decomposition of the two sub-bursts A (left panel) and B (right panel) of FRB 20210912A into multiple exponentially scattered Gaussian components. The top panels show the intensity profiles in solid red curves, best-fit models in solid black curves, and individual components in dotted blue curves. The bottom panels show the residuals (normalized by the rms noise in the intensity profile).
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Polarization spectra of FRB 20210912A integrated over the entire burst (left), sub-burst A (middle), and sub-burst B (right) before correcting for the average RM. The time ranges for averaging are mentioned in each panel. Polarization fractions weakly vary with frequency. Slope of the V/I vs. λ 2 curve, κ, is mentioned in the upper right corner of each panel. Frequency dependence of PA, especially in sub-burst A, shows hints of deviation from the Faraday law. Reduced χ 2 (﹩{\chi }_{r}^{2}﹩) of the fits are mentioned in the bottom panels. Data points are plotted after averaging two adjacent channels of the 64-channel spectra on which the fits were performed.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Time-resolved polarization spectra of FRB 20210912A in sub-burst A before correcting for the average RM. The time ranges for averaging and the slope of the V/I vs. λ 2 curve, κ, are mentioned in each panel. Frequency dependence of PA shows hints of deviation from the Faraday law in time bins close to the intensity peak. Reduced χ 2 (﹩{\chi }_{r}^{2}﹩) of the fits are mentioned in the bottom panels. Data points are plotted after averaging two adjacent channels of the 64-channel spectra on which the fits were performed.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Time-resolved polarization spectra of FRB 20210912A in sub-burst B before correcting for the average RM. The time ranges for averaging and the slope of the V/I vs. λ 2 curve, κ, are mentioned in each panel. Reduced χ 2 (﹩{\chi }_{r}^{2}﹩) of the corresponding fits are mentioned in the bottom panels. See Appendix B for details. Data points are plotted after averaging two adjacent channels of the 64-channel spectra on which the fits were performed.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: Polarization spectra of FRB 20181112A integrated over the entire burst (left), sub-burst A (middle), and sub-burst B (right) before correcting for the average RM. The time ranges for averaging and the slope of the V/I vs. λ 2 curve, κ, are mentioned in each panel. Data points are plotted after averaging two adjacent channels of the 64-channel spectra on which the fits were performed.
Paper: The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?
Authors: Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, Tyson Dial
Figure caption: RM of FRB 20210912A estimated using the RM synthesis method, in sub-bursts A (left) and B (right). The frequency-averaged Stokes I profile of the FRB is shown in red at a time resolution of 3.8 μs (in normalized flux density units not shown in the plots). The horizontal error bars represent the time range for the corresponding measurements. The bottom panels show the corresponding PA at infinite frequency, assuming that PA has a linear dependence on λ 2. See Appendix B for details.