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Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Histogram of the RFe II distribution in SDSS quasar spectra based on Y. Shen et al. (2011) (blue) and S. Rakshit et al. (2020) (green).
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Observed composite spectrum of RM 102. The regions between the vertical black and brown dashed lines represent the broad UV and optical wavelength ranges, respectively, considered in this work. The shaded blue and red regions denote the blue and red parts in the corresponding regions. Top panel: the observed spectrum is in gray, the dashed red and the blue lines correspond to the best fit of the emission lines and the continuum, respectively. Bottom panel: the red line depicts the Fe II pseudocontinuum. For reference, we also show the semiempirical UV (dotted line) and optical (dashed line) templates implemented in PyQSOfit in dark red.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: A comparison of the observed Fe II emission in RM 102 (gray curve) with separate theoretical templates for UV and optical parts (see the text). The red curve denotes the Fe II flux in the wavelength range 1989–4000 Å for ﹩\mathrm{log}\,{\Phi }_{{\rm{H}}}\,({\mathrm{cm}}^{-2}\,{{\rm{s}}}^{-1})=20﹩ and a covering factor of 30%, while the black curve represents the Fe II emission in the wavelength range 4000–5530 Å for ﹩\mathrm{log}\,{\Phi }_{{\rm{H}}}\,({\mathrm{cm}}^{-2}\,{{\rm{s}}}^{-1})=19﹩ and a covering factor of 50%. The gas density is fixed at 1010 cm−3 and the microturbulence velocity is 100 km s−1.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Contour plots for RFe II, i.e., the ratio of Fe II 4434–4684 Å to Hβ (λ4861.32) fluxes for microturbulence velocity Vturb = 100 km s−1 and different metallicities. The shaded region represents the model parameter space reproducing the strength of optical blue Fe II emission, assuming a covering factor of 100%, consistent with the observed value for the test object RM 102. The red-dashed contour denotes the observed value (0.95) for source RM 102.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: A comparison of observed and model-predicted Fe II spectra over a wavelength range of 1989–5530 Å for different models. Plots in the left column are for microturbulence 50 km s−1, while those in the right column are for the same models but for microturbulence 100 km s−1.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: The exemplary fits to the SALT spectrum with the Fe II template phi19.0-nH12.0-m50.dat, FWHM = 5400 km s−1 (upper panel), phi18.25-nH12.0-m50.dat, FWHM = 5400 km s−1 (middle panel), and phi18.0-nH12.0-m50.dat, FWHM = 5800 km s−1 (lower panel). The middle panel shows the best fit.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: A comparison of the potential Fe II contribution from RM 102 using the power-law (blue curve) and disk continuum (orange curve) fitting methods. For reference, we also plotted the semiempirical UV (dotted line) and optical (dashed line) templates implemented in PyQSOfit in dark red.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Plot showing Fe II emission (in arbitrary units) over a wavelength range of 2650–2850 Å around the UV Mg II line to justify the choice of a 2 Å bin size. The larger bin size (5 Å) already shows a visible departure in the smoothed shape from the denser grid.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Contour plots for the ratio of red (5150–5350 Å) to blue (4434–4684 Å) part of the optical Fe II spectra for microturbulence velocity Vturb = 100 km s−1 and different metallicities. The shaded region denotes the model parameter space that predicts the strength of optical blue Fe II emission consistent with the observed value for a covering factor of 100%. The red-dashed contour denotes the observed value (0.68) for source RM 102.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Contour plots for the ratio of red (2800–3090 Å) to blue (2650–2800 Å) part of the UV Fe II spectra for microturbulence velocity Vturb = 100 km s−1 and different metallicities. The shaded region denotes the model parameter space that predicts the EW of UV red Fe II wing consistent with the observed value for a 100% covering factor.
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Example trajectories for different models of charged particles in magnetic turbulence, colored by the curvature of the gyrocenter motion. Cases (a), (c), and (d) are obtained by solving the Newton–Lorentz equations in a turbulent magnetohydrodynamics (MHD) snapshot, a multifractal continuous cascade (CC) field, and a structured Lagrangian mapping (LM) field. Case (b) is generated by our generative diffusion model (DM).
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Distributions of curvature of gyrocenter trajectory, by averaging the velocity signals V(t) with a window of 1.5 Tg. The gyrocenter motion exhibits an asymptotic tail with slope −2.5, and, for large α, an intermediate regime with slope −1.5. The low-curvature tails scale with slope 1. The distributions are compensated with κ for visualization purposes; the indicated slopes take this compensation into account.
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Schematic illustration of the diffusion model (DM) process.
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Distribution of field-line curvature in turbulent vector fields. The −2.5 asymptotic scaling is only present in the MHD case, while the CC case is characterized by a −4 slope. All low-curvature tails scale also with slope 1. The distributions are again compensated with κ, which is taken into account by the indicated slopes.
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Distributions of normalized increments ﹩{\delta }_{\tau }V/{\sigma }_{{\delta }_{\tau }V}﹩ for different time lags τ. Shown are the MHD and DM cases with α = 512. Power-law tails for small τ with strong non-Gaussianity, and confined sub-Gaussian behavior for large τ due to Vi ∈ [ −1, 1].
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Mean-squared displacement as an indicator for the transport properties of charged particles. Compensated by the time τ to distinguish between ballistic and diffusive behavior.
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Fourth-order velocity flatness ﹩{F}_{\tau }^{(4)}﹩ of particle trajectories, indicating the deviation from the Gaussian case ﹩{F}_{\tau }^{(4)}=3﹩.
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Second-order velocity structure functions ﹩{S}_{\tau }^{(2)}﹩ of particle trajectories, compensated by the MHD case to highlight differences.
Paper: Generation of Cosmic-Ray Trajectories by a Diffusion Model Trained on Test Particles in 3D Magnetohydrodynamic Turbulence
Authors: Johannes Martin, Jeremiah Lübke, Tianyi Li, Michele Buzzicotti, Rainer Grauer, Luca Biferale
Figure caption: Example of a mirror event in a DM-generated trajectory. The event is characterized by high curvature and a change of the handedness of the helix, as indicated by the sign of the torsion. The curvature and torsion are computed for the gyrocenter motion.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: (GBP − GRP, G) CMD of the SMC region excluding foreground sources. The area above the magenta line is the region occupied by massive stars in the CMD, defined in the Section 2.1. In the left panel, stars in the SMC region are plotted excluding foreground objects. The green shadow represents the range of variation in the massive star selection region for a distance modulus of ±5 kpc, which corresponds to distances of 60 and 70 kpc. In the right panel, only massive star candidates are plotted. The red line, yellow dotted line, and blue dashed line are PARSEC isochrones for ages of 1.0, 10.0, and 36.5 Myr, respectively, with a reddening correction of AV = 0.15 mag added, as noted in the text. The black cross represents the median value (−0.2809, 15.67) of the massive star candidates. The white arrow extending from the black cross is the reddening vector corresponding to AV = 0.15 mag, illustrating the amount of reddening required to move from the median position (−0.2809, 15.67) across the magenta line.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: Stellar density distribution around SMC obtained from Gaia data. Foreground objects are excluded by the limitation of the annual parallax ϖ > 0.1 mas and cuts around two globular clusters NGC 362 and NGC 104.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: The internal PMs of the clipped samples determined by subtracting the mean PM of the clipped samples within 3∘ of the H I dynamical center. To account for the effects of coordinate distortion during this subtraction, a coordinate transformation used by Gaia Collaboration et al. (2018) is applied, and the proper motion is subtracted using the transformed coordinates. The color of the PM vectors represents the direction of the PM vector, and the angle is defined counterclockwise from north (0°) in the (x, y) coordinates based on the orthographic projection defined in Section 4.1. The legends indicate the magnitudes of PM vectors corresponding to 200 and 85 km s−1, assuming a distance of 65 kpc, with the latter representing the minimum escape velocity derived under the assumption of H I rotation (S. Stanimirović et al. 2004; N. M. McClure-Griffiths et al. 2018).
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: (Upper left) The spatial distribution of spectroscopically identified massive stars around the SMC from the B10 catalog. The background shows 0–600 deciRayleighs (dR) of Hα emission by SHASSA. E04 stars, which are part of the 4073 objects in the B10 catalog, are represented by red circles, while the remaining 1251 objects are represented by green crosses. (Upper right) The spatial distribution of stars classified as B0-type and O-type from the B10 catalog around the SMC. The background is the same as in the upper left panel. Stars classified as B0-type (181 objects) are represented by purple crosses, and O-type stars (281 objects) are represented by light blue circles. Since there is a range of type classifications, stars that may be later than B3, including B3 itself, are excluded. Stars that are classified as both O-type and B0-type are included in the O-type category. (Lower left) Similar to the upper left panel, but showing B10 catalog stars successfully crossmatched in Gaia DR3 data. Among the 4073 E04 stars, 1323 successfully crossmatched stars are represented by red circles, while, among the 1251 stars identified through other observations, 1142 successfully crossmatched stars are represented by green crosses. (Lower right) Similar to the upper right panel, but showing B10 catalog stars successfully crossmatched in Gaia DR3 data. The purple crosses represent 130 crossmatched B0-type stars, and the light blue circles represent 188 crossmatched O-type stars.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: KDE map of our massive star candidates. The contours show [0.01, 0.1, 0.3, 0.5, 0.7, 0.9, 1.0] levels, normalized to the maximum value. The background shows Hα emission by SHASSA in the range of 0–600 deciRayleighs (dR; J. E. Gaustad et al. 2001). Three distinct peaks located at the boundaries of the bar structure and wing structure in the northern region are highlighted with dashed lines. Note that the contours are elongated in the east–west direction due to the influence of coordinate distortion.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: Comparison of the spatial distribution of massive star candidates with that of the ISM around the SMC. The background is a color multiwavelength montage of the Hα emission by MCELS (red; 0–300 × 10−17 erg cm−2 s−1; R. C. Smith & MCELS Team 1999) with the Herschel 350 μm image (green; 0–25 MJy sr−1; M. Meixner et al. 2013) and the H I with ASKAP and Parkes integrated over the LSRK velocity range 130–170 km s−1 (blue; 1000–3000 K km s−1; N. M. McClure-Griffiths et al. 2018). The resolution varies by color. Massive star candidates are overplotted as yellow circles. The three regions indicated by white dotted lines correspond to the three overdensities in the northern part, which are highlighted in Figure 5.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: (Left) The spatial distribution of 7261 massive star candidates with PM in both R.A. and decl. directions contained within 2σ (the clipped samples). The white cross represents the mean position of all the 7426 massive star candidates. The red circle represents the dynamical center of the H I gas (S. Stanimirović et al. 2004), the green triangle represents the optical center (G. de Vaucouleurs & K. C. Freeman 1972), and the blue square represents the center of the classical Cepheids distribution (V. Ripepi et al. 2017). (Right) The PM vectors of the clipped samples. The legend indicates the magnitude of the PM vector corresponding to 400 km s−1, assuming a distance of 65 kpc. The white dashed circle represents a radius of 3∘ centered on the dynamical center of the H I gas, which is used for calculating the systemic PM of the massive star candidates.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: Comparison of the RVs of the clipped samples with the three velocity components of H I. The overplotted circles represent the 491 objects within the clipped samples for which RVs are available. The color of the circles indicates the magnitude of the RVs. The background is a color multivelocity montage of the H I emission with ASKAP and Parkes (N. M. McClure-Griffiths et al. 2018), with red representing the integrated intensity for the 179–187 km s−1 range, green for the 144–152 km s−1 range, and the blue for the 105–113 km s−1 range, all on a common scale of 10–800 K km s−1 (log scale). Note that these velocity components are consistent with those shown in Figure 2 of N. M. McClure-Griffiths et al. (2018). The line-of-sight velocities of both H I and the clipped samples are referenced to the LSRK.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: (Left) The spatial distribution of the reddened OB0 stars in the B10 catalog. The background shows the Herschel 350 μm emission ranging from 0 to 25 MJy sr−1. The red crosses represent the 31 stars located below the magenta line in Figure 7. The white square indicates the NGC 346 region, which is enlarged in the right panel. (Right) An enlarged view of the NGC 346 region indicated by the white square in the left panel. The contours represent the peak temperature map of CO (J = 2–1) obtained with ALMA (K. Tokuda et al. 2021; T. Ohno et al. 2023). The contour levels are 3σ for cyan and 10σ for magenta. The red crosses again represent the 31 stars located below the magenta line in Figure 7, while the green circles represent the 287 OB stars from the B10 catalog that are positioned above the magenta line. The small yellow circles represent our massive star candidates. Note that the massive star candidates plotted in this figure include many stars of later types than B0-type listed in the B10 catalog, as well as several newly detected as massive stars.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: (Left) The CMD of crossmatched B0-type and O-type stars in the B10 catalog, plotted as (GBP − GRP, G). The 130 B0-type stars are represented by purple crosses, and the 187 O-type stars are represented by light blue circles. The black circles represents the 7426 massive star candidates identified by us. Below the magenta line delineating the boundary of massive stars, 18 B0-type stars and 13 O-type stars are plotted. The red arrow represents the reddening vector corresponding to AV = 0.30 mag. (Right) Similar to the left panel, but for the CMD of stars with ϖ > 0.1 mas, which were excluded from our data as foreground objects. Four B0-type stars and 13 O-type stars are plotted. Below the magenta line indicating the boundary of massive stars, there is one O-type star.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: The spatial distribution of the massive star candidates selected in Section 2.1. On the background of Figure 1, the massive star candidates are overplotted as dark yellow circles.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: (Left) An enlarged view of the spatial distribution of the massive star candidates in the northwest of the SMC. The dark yellow circles represent massive star candidates. The superstructures are distinguished by circles of different colors. The white arrows highlight the lines of massive star candidates extending from the superstructure 7. The background is a color multiwavelength montage, showing the Hα emission by MCELS (red; 5–100 × 10−17 erg cm−2 s−1; R. C. Smith & MCELS Team 1999) and the H I emission with ASKAP and Parkes (green and blue; integrated over the LSRK velocity range 144–152 km s−1 and 105–113 km s−1, respectively; 10–1200 K km s−1; N. M. McClure-Griffiths et al. 2018), all in log scale. The green and blue H I velocity components are the same as those shown in Figure 11. (Right) The internal PM vectors of the clipped samples in the region shown in the left panel. The background is the same as in the left panel. The legends indicate the magnitudes of PM vectors corresponding to 85 km s−1, representing the minimum escape velocity derived under the assumption of H I rotation.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: (Left) Stellar density distribution of the newly defined SMC region, contained within a circle of radius 3∘ centered at l = 302﹩\mathop{.}\limits^{\unicode{x000B0}}﹩8084, b = −44﹩\mathop{.}\limits^{\unicode{x000B0}}﹩3277. Foreground objects are excluded using the restriction ϖ ≤ 0.1 mas and cuts around the two globular clusters NGC 362 and NGC 104. Positions are shown in the (x, y) coordinates based on the orthographic projection defined in Section 4.1. The overplotted dark yellow circles represent the stars plotted above the magenta line in Figure 16. The newly defined circular SMC region contains 6828 dark yellow circles. (Right) Stellar density distribution of the region symmetric to the SMC region relative to the Galactic plane, contained within a circle of radius 3∘ centered at l = 302﹩\mathop{.}\limits^{\unicode{x000B0}}﹩8084, b = +44﹩\mathop{.}\limits^{\unicode{x000B0}}﹩3277. Foreground objects are excluded using the restriction ϖ ≤ 0.1 mas. Positions are shown in the (x, y) coordinates based on the orthographic projection defined in Section 4.1. The overplotted dark yellow circles represent the stars plotted above the magenta line in Figure 16. The symmetric region contains 38 dark yellow circles. The dark yellow circles in the symmetric region are enlarged for visibility.