adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries
Authors: Devarshi Choudhury, Anna L. Watts, Alexander J. Dittmann, M. Coleman Miller, Sharon M. Morsink, Tuomo Salmi, Serena Vinciguerra, Slavko Bogdanov, Sebastien Guillot, Michael T. Wolff, Zaven Arzoumanian
Figure caption: Simulated phase-energy-resolved X-ray pulse profiles, over 32 phase bins, and instrument channel range [30,300) generated by the different test configurations, as registered by NICER, using the 3C50 instrument response. These pulse profiles are generated by X-PSI using the ultra resolution settings.
Paper: Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries
Authors: Devarshi Choudhury, Anna L. Watts, Alexander J. Dittmann, M. Coleman Miller, Sharon M. Morsink, Tuomo Salmi, Serena Vinciguerra, Slavko Bogdanov, Sebastien Guillot, Michael T. Wolff, Zaven Arzoumanian
Figure caption: Energy-summed waveforms (left) and phase-summed spectra (right) generated by the different codes for the Ring-Polar configuration (top) and the corresponding fractional differences. For clarity, the Poisson bands are not shown in this figure since the fractional differences are far lower than the noise level.
Paper: Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries
Authors: Devarshi Choudhury, Anna L. Watts, Alexander J. Dittmann, M. Coleman Miller, Sharon M. Morsink, Tuomo Salmi, Serena Vinciguerra, Slavko Bogdanov, Sebastien Guillot, Michael T. Wolff, Zaven Arzoumanian
Figure caption: Energy-summed waveforms (left) and phase-summed spectra (right) generated by the different codes for the Crescent-Polar configuration (top) and the corresponding fractional differences.
Paper: Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries
Authors: Devarshi Choudhury, Anna L. Watts, Alexander J. Dittmann, M. Coleman Miller, Sharon M. Morsink, Tuomo Salmi, Serena Vinciguerra, Slavko Bogdanov, Sebastien Guillot, Michael T. Wolff, Zaven Arzoumanian
Figure caption: Total counts difference between the full phase-energy-resolved pulse profiles generated by the IM code and X-PSI (using the ultra resolution settings).
Paper: Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries
Authors: Devarshi Choudhury, Anna L. Watts, Alexander J. Dittmann, M. Coleman Miller, Sharon M. Morsink, Tuomo Salmi, Serena Vinciguerra, Slavko Bogdanov, Sebastien Guillot, Michael T. Wolff, Zaven Arzoumanian
Figure caption: Energy-summed waveforms (left) and phase-summed spectra (right) generated by the different codes for the Bithermal spot configuration (top) and the corresponding fractional differences. For clarity, the Poisson bands (at about 1.2%) are not shown in this figure.
Paper: Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries
Authors: Devarshi Choudhury, Anna L. Watts, Alexander J. Dittmann, M. Coleman Miller, Sharon M. Morsink, Tuomo Salmi, Serena Vinciguerra, Slavko Bogdanov, Sebastien Guillot, Michael T. Wolff, Zaven Arzoumanian
Figure caption: Energy-summed waveforms (left) and phase-summed spectra (right) generated by the different codes for the Crescent-Eq configuration (top) and the corresponding fractional differences.
Paper: Memory in the Burst Occurrence of Repeating Fast Radio Bursts
Authors: Ping Wang, Li-Ming Song, Shao-Lin Xiong, Xiao-Yun Zhao, Jin Wang, Shu-Min Zhao, Shuo Xiao, Ce Cai, Sheng-Lun Xie, Wang-Chen Xue, Chen-Wei Wang, Yue Wang, Wen-Long Zhang
Figure caption: The preconditioned distribution P(λ∣λ 0) characterizes the waiting times λ between successive FRBs that exceed specified thresholds for various sources. The preceding condition values λ 0 are taken from both the first (minimal) and last (maximum) quartiles, denoted as q 1 and q 4, respectively. For the sake of uniform notation, q 0 is used to represent the entire data set, implying that P(λ∣λ 0 ∈ q 0) = P(λ). (a) P(λ∣λ 0) for FRB 20121102A with fluence thresholds of 0.0 (square), 0.028 (circle), and 0.1 (right triangle) Jy ms; (b) P(λ∣λ 0) for FRB 20201124A(A) with fluence thresholds of 0.0 (square), 0.5 (circle), and 1.0 (right triangle) Jy s; (c) P(λ∣λ 0) for FRB 20220912A with fluence thresholds of 0.0 (square), 0.1 (circle), and 0.6 (right triangle) Jy ms; and (d) P(λ∣λ 0) for FRB 20201124A(B) with fluence thresholds of 0.0 (square), 0.1 (circle), and 0.5 (right triangle) Jy ms. For all subplots, the colors red, green, and blue correspond to λ 0 belonging to q 0, q 1, and q 4, respectively. The insets illustrate the behavior of the fitting curves near the point where ﹩\lambda /\bar{\lambda }=1﹩. The residuals between the data points and the best-fit values relative to the errors for all data are also displayed, with the color scheme corresponding to the different preconditions consistent with those in the preconditioned distribution P(λ∣λ 0).
Paper: Simultaneous X-Ray and Optical Polarization Observations of the Blazar Mrk 421
Authors: Athira M. Bharathan, C. S. Stalin, S. Sahayanathan, Kiran Wani, Amit Kumar Mandal, Rwitika Chatterjee, Santosh Joshi, Jeewan C. Pandey, Blesson Mathew, Vivek K. Agrawal
Figure caption: Results of the optical and X-ray polarization measurements on 2023 December 6. Top left-hand panel: Position of the 2−8 keV X-ray polarization in the ΠX–ΨX plane obtained using PCUBE (blue star) and XSPEC analysis (red star). Top right-hand panel: The normalized U/I and Q/I Stokes parameter in the total 2−8 keV (red circle), 2−3 keV (blue square), 3−5 keV (orange triangle), and 5−8 keV (green star). Bottom left-hand panel: The measured X-ray polarization in ΠX–ΨX plane. Here, the star represents 2−8 keV, the diamond represents 2−3 keV, a plus represents 3−5 keV, and the pentagon represents 5−8 keV. Bottom right-hand panel: The measured optical polarization (ΠO) in B band (star), V band (diamond) and R band (plus).
Paper: Simultaneous X-Ray and Optical Polarization Observations of the Blazar Mrk 421
Authors: Athira M. Bharathan, C. S. Stalin, S. Sahayanathan, Kiran Wani, Amit Kumar Mandal, Rwitika Chatterjee, Santosh Joshi, Jeewan C. Pandey, Blesson Mathew, Vivek K. Agrawal
Figure caption: The left-hand panel illustrates the emission regions characterized by different magnetic field configurations: an aligned magnetic field at position z 0, where X-ray emission originates, and a tangled magnetic field at position z  ν , which is the source of optical emission. The right-hand panel consists of two subplots: the top subplot shows the model fit (blue dotted line) to the observed optical and X-ray emissions, while the bottom subplot indicates the spatial extension of their respective emission regions (green dotted line).
Paper: Memory in the Burst Occurrence of Repeating Fast Radio Bursts
Authors: Ping Wang, Li-Ming Song, Shao-Lin Xiong, Xiao-Yun Zhao, Jin Wang, Shu-Min Zhao, Shuo Xiao, Ce Cai, Sheng-Lun Xie, Wang-Chen Xue, Chen-Wei Wang, Yue Wang, Wen-Long Zhang
Figure caption: The average values of the conditional probability of waiting time ﹩\hat{\lambda }({\lambda }_{0})/\bar{\lambda }﹩. They have a similar form as ﹩{\lambda }_{0}/\bar{\lambda }﹩, increasing with the same fluence thresholds shown in Figure 2. The plus symbols correspond to the shuffled sequences of waiting times that are fluctuating across ﹩\hat{\lambda }({\lambda }_{0})/\bar{\lambda }\approx 1﹩, indicative of a lack of memory in the data.
Paper: Memory in the Burst Occurrence of Repeating Fast Radio Bursts
Authors: Ping Wang, Li-Ming Song, Shao-Lin Xiong, Xiao-Yun Zhao, Jin Wang, Shu-Min Zhao, Shuo Xiao, Ce Cai, Sheng-Lun Xie, Wang-Chen Xue, Chen-Wei Wang, Yue Wang, Wen-Long Zhang
Figure caption: (a) The FAST telescope observed the sequence of FRB 121102 with a fluence greater than 0.2 Jy ms during continuous observation sessions. (b) Sequence of the waiting time above and below the median λ = 120 s (red line). (c) The same as (b), but for a shuffled sequence of original data.
Paper: Simultaneous X-Ray and Optical Polarization Observations of the Blazar Mrk 421
Authors: Athira M. Bharathan, C. S. Stalin, S. Sahayanathan, Kiran Wani, Amit Kumar Mandal, Rwitika Chatterjee, Santosh Joshi, Jeewan C. Pandey, Blesson Mathew, Vivek K. Agrawal
Figure caption: Left-hand panel: The measured mean optical polarization degree in B (star), V (plus), and R (square) filters, for all the epochs of observations (see Table 5). Right-hand panel: R-band measurements (n = 42) from 2023 December 7, demonstrating significant variability in the degree of polarization over the course of a single night.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Left: longitudinal magnetic fields at negative Galactic latitudes in the Sagittarius Arm, derived from pulsars at the displayed locations. The Sagittarius Arm center is delineated and labeled in purple, with its inner and outer boundaries shown by flanking black dotted lines. A CCW magnetic field (“positive” by our convention) is shown as a blue cross, while a CW magnetic field (“negative” by our convention) is indicated with a red diamond. The solar system is marked by the black cross at (x, y) = (0.0, 8.3) kpc. Outliers (listed in Table 3) are not shown. Right: same as the left panel, except at positive Galactic latitudes.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Left: the derived magnitudes and directions of the large-scale, planar magnetic field for negative Galactic latitudes. The magnetic field vectors are displayed atop the centers of the associated arms, except for the Sagittarius-to-Scutum Interarm field, which is shown between the Sagittarius and Scutum Arms. Arrow sizes are directly proportional to the magnitude of the magnetic field, while the arrow directions indicate whether the derived field is CW or CCW. Zones with derived magnetic field strengths less than their 1σ uncertainty are shown with crosses. See Table 1 for exact magnitudes and their uncertainties. Right: same as the left panel, but for positive Galactic latitudes.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Same as Figure 3, but for pulsars in the Perseus Arm. We truncate the right panel at δRMPers = [−500, 500] rad m−2, and hence two outliers at (δRMPers, δDMPers) = (735.79 rad m−2, 63.24 pc cm−3) and (−1267.22 rad m−2, 17.41 pc cm−3) are not shown. We also truncate the plot at δDMPers < 150 pc cm−3, with an outlier at (δRMPers, δDMPers) = (−307.25 rad m−2, 349.79 pc cm−3) not shown. All outlier information (including these two) is listed in Table 3.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Same as Figure 3, but for pulsars in the Sagittarius-to-Scutum Interarm.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Same as Figure 4, but for the Sagittarius-to-Scutum Interarm region. The dotted–dashed line represents the Galactic longitude limit below which the LOS would also sample the next inward region, the Scutum Arm.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Left: the geometrically corrected δRMScut as a function of Galactic longitude, for the Scutum Arm pulsars of Figure 11. Right: same as the left panel, except that the magnetic field B is displayed (positive is CCW) along the Scutum Arm. Pulsar LOSs at negative (nonnegative) Galactic latitudes are shown with red (blue) symbols. Outliers are denoted with a cross and listed in Table 4.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Same as Figure 2, but for the Scutum Arm. The dotted–dashed line represents the Galactic longitude limit below which the LOSs would also sample the next inward region.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Same as Figure 2, but for the Perseus Arm. The dotted–dashed line represents the Galactic longitude limit below which the LOS would also sample the Sagittarius-to-Perseus Interarm.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Same as Figure 3, but for pulsars in the Scutum Arm.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Picture of the anisotropic SN momentum injection scheme, as parameterized by the nominal anisotropy factor ζ. The star particle undergoing an SN event is shown in red, and the surrounding gas cells are shown as blue circles. The arrows indicate the magnitude and direction of the momentum injection. A low ζ value injects momentum primarily within the disk plane, and a high ζ injects momentum primarily out of the disk plane. ζ = 1 implies isotropic injection. Note that only the direction of injected momenta varies with ζ; the magnitude does not.
Paper: On the 3D Transport of Low-energy Galactic Cosmic-ray and Jovian Electrons in the Inner Heliosphere in the Presence of a Fisk-type Heliospheric Magnetic Field
Authors: N. E. Engelbrecht
Figure caption: Left panels, top to bottom: fluctuation energies, correlation scales, and normalized cross-helicities yielded by the S. Oughton et al. (2011) TTM along the trajectory of the Ulysses spacecraft, alongside observations of the same reported by B. Bavassano et al. (2000a, 2000b). Right panels, top to bottom: electron and proton temperatures, and resulting dissipation range onset wavenumbers, calculated from the TTM along Ulysses’ trajectory, alongside appropriate SWOOPs and B. Bavassano et al. (2000a, 2000b) observations. Bottom-right panels indicate the radial and colatitudinal positions of the Ulysses spacecraft, to guide the eye. Figure adapted from N. E. Engelbrecht & R. D. Strauss (2018). Note that the times given in the x-axes of the plots containing quantities calculated with the TTM serve only to indicate that those values correspond to the position of the spacecraft at that particular time, which can then be read off the bottom-right panels.
Paper: On the 3D Transport of Low-energy Galactic Cosmic-ray and Jovian Electrons in the Inner Heliosphere in the Presence of a Fisk-type Heliospheric Magnetic Field
Authors: N. E. Engelbrecht
Figure caption: Top-left panel: dissipation range onset wavenumber employed in this study (black line) compared with extrapolations of the same based on the results of R. J. Leamon et al. (2000) used in previous studies as a function of radial distance in the ecliptic plane. Top-right panel: parallel and perpendicular MFPs as a function of rigidity at Earth, alongside the I. D. Palmer (1982) consensus range and values reported by N. E. Engelbrecht et al. (2022a). Bottom-left panel: 6 MeV MFPs as a function of colatitude at 1 au, calculated assuming a Parker as well as a Schwadron–Parker HMF. Bottom-right panel: 6 MeV MFPs as a function of radial distance in the ecliptic, out to 84 au.
Paper: On the 3D Transport of Low-energy Galactic Cosmic-ray and Jovian Electrons in the Inner Heliosphere in the Presence of a Fisk-type Heliospheric Magnetic Field
Authors: N. E. Engelbrecht
Figure caption: Top panel: input spectra employed in this study, as a function of kinetic energy. Solid line represents the Jovian source spectrum constructed by A. Vogt et al. (2018), and dashed line represents the galactic cosmic-ray electron input spectrum constructed by N. E. Engelbrecht (2019). Bottom panel: Galactic electron and Jovian electron differential intensities at Earth, computed using a Schwadron–Parker hybrid field and a pure Parker field. Electron observations at 1 au, reported by J. L’heureux & P. Meyer (1976) and D. Moses (1987) are also shown, to guide the eye.
Paper: On the 3D Transport of Low-energy Galactic Cosmic-ray and Jovian Electrons in the Inner Heliosphere in the Presence of a Fisk-type Heliospheric Magnetic Field
Authors: N. E. Engelbrecht
Figure caption: Top panel: 6 MeV parallel and perpendicular MFPs along the trajectory of the Ulysses spacecraft. Middle panel: 6 MeV perpendicular MFP and drift scale along the same trajectory. Bottom panels: radial and colatitudinal trajectory of Ulysses as a function of time.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: SFR histories (top) and stellar mass formed (bottom) for runs with different weighting schemes: solid angle (red), volume (blue), and mass (green). The left and right panels correspond to isotropic momentum injection (γ ≈ 1) and out-of-disk favored momentum injection (γ > 1), respectively. In general isotropic injection results on more bursty SFR histories than out-of-disk favored ones. Solid-angle-based criteria assuming isotropic momentum injection maximizes the burstiness of star formation. The total stellar mass formed can vary by factors of 2–3 between runs with different numerical choices.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: In-disk, or radial (blue) and out-of-disk, or vertical (green), gas flow rate and associated SFR (red) for all eight robustness test runs, with respect to the same cylinder described in Figure 5. In all cases, the zeta1 runs have burstier SFRs and more violent gas flow patterns, whereas the zeta10 runs do not. This is the same behavior as observed in the main body of the paper, so changing the anisotropy affects the runs in this way regardless of these numerical choices explored here.
Paper: Discovery of MgS and NaS in the Interstellar Medium and Tentative Detection of CaO
Authors: Marta Rey-Montejo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Víctor M. Rivilla, Andrés Megías, David San Andrés, Miguel Sanz-Novo, Laura Colzi, Shaoshan Zeng, Álvaro López-Gallifa, Antonio Martínez-Henares, Sergio Martín, Belén Tercero, Pablo de Vicente, Miguel Requena-Torres
Figure caption: Column densities of metal-bearing molecules measured toward different astronomical sources (J. Cernicharo & M. Guelin 1987; B. E. Turner et al. 1994; J. L. Highberger et al. 2001, 2003; J. L. Highberger & L. M. Ziurys 2003; S. N. Milam et al. 2007; M. Agúndez et al. 2014; J. Cernicharo et al. 2019a, 2019b; J. R. Pardo et al. 2021). NaCl has also been observed toward Orion Source I and the IRAS 16547 binary system (see Section 1; A. Ginsburg et al. 2019; S. Tachibana et al. 2019; K. E. Tanaka et al. 2021), but no information is provided in these works about the derived column densities. Arrows denote upper limits.
Paper: Discovery of MgS and NaS in the Interstellar Medium and Tentative Detection of CaO
Authors: Marta Rey-Montejo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Víctor M. Rivilla, Andrés Megías, David San Andrés, Miguel Sanz-Novo, Laura Colzi, Shaoshan Zeng, Álvaro López-Gallifa, Antonio Martínez-Henares, Sergio Martín, Belén Tercero, Pablo de Vicente, Miguel Requena-Torres
Figure caption: Relative O/S ratio of detected molecules toward G+0.693 (CO/CS, H2CO/H2CS; M. Sanz-Novo et al. 2024a); (NO; V. M. Rivilla et al. 2022a); (NS M. Sanz-Novo et al. 2024b); (HNCO; S. Zeng et al. 2018); (HNCS; M. Sanz-Novo et al. 2024a); (HOCO+/HOCS+; M. Sanz-Novo et al. 2024b); (SiO/SiS; S. Massalkhi et al. 2023); (CH3OH/CH3SH, C2H5OH/C2H5SH, CH(O)OH/CH(O)SH; L. F. Rodríguez-Almeida et al. 2021a). CO/CS = 3500 ratio is not included since it is several orders of magnitude above the solar value (see M. Sanz-Novo et al. 2024a). The arrow pointing downward denotes an upper limit and the arrow pointing upward denotes a lower limit.
Paper: Discovery of MgS and NaS in the Interstellar Medium and Tentative Detection of CaO
Authors: Marta Rey-Montejo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Víctor M. Rivilla, Andrés Megías, David San Andrés, Miguel Sanz-Novo, Laura Colzi, Shaoshan Zeng, Álvaro López-Gallifa, Antonio Martínez-Henares, Sergio Martín, Belén Tercero, Pablo de Vicente, Miguel Requena-Torres
Figure caption: Transitions of CaO measured toward G+0.693, displayed in order of decreasing line intensity. Two of the observed transitions are unblended, while the other two appear heavily blended with other molecular species. The observed spectra are represented as gray histograms. The best LTE fit derived with MADCUBA is shown with a red line, while the blue line shows the expected molecular emission from all of the molecular species identified to date in our survey. The quantum numbers representing the J + 1 → J transitions are shown in the upper part of each panel.
Paper: Discovery of MgS and NaS in the Interstellar Medium and Tentative Detection of CaO
Authors: Marta Rey-Montejo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Víctor M. Rivilla, Andrés Megías, David San Andrés, Miguel Sanz-Novo, Laura Colzi, Shaoshan Zeng, Álvaro López-Gallifa, Antonio Martínez-Henares, Sergio Martín, Belén Tercero, Pablo de Vicente, Miguel Requena-Torres
Figure caption: Rotational diagram of MgS (red dots) using the transitions reported in Table 3 after subtracting the contribution from any blended species. The black dashed line corresponds to the best linear fit to the data points. The derived values for the molecular column density, N, and the excitation temperature, T ex, are shown in blue.
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption: (a) LS periodograms of Src2 in ﹩{g}^{{\prime} }﹩ and ﹩{r}^{{\prime} }﹩ filters using nterms = 1 and nterms = 2 with the window function generated using nterms = 1 overlaid on each periodogram. The dominant period in each is labeled. (b) Histograms of the most dominant signal power in ﹩{g}^{{\prime} }﹩ and ﹩{r}^{{\prime} }﹩ generated by randomizing the optical light curve of the source 500 times, using 1 or 2 nterms. The dashed vertical line selects the power resulting from the original light curve.
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption: Left: the joint fit for Chandra data from 0.5 to 7 keV and the NuSTAR data from 3 to 20 keV of Src2. The 0.5–20 keV X-ray spectrum can be fit assuming a simple power law with a photon index ΓX = 1.23 ± 0.19. The Chandra and NuSTAR data points are background subtracted. The background data are shown in gray for NuSTAR FPMA. The solid and dashed lines represent the source spectral models and components. Right: the residuals of the joint best fit. In both panels, the data are grouped to 20 counts per bin for easier visualization.