adsabs/AstroCLIMB huggingface dataset:
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: Fraction of pixels (F < Fcont − 2σflux). The x-axis represents the fraction of pixels whose flux is at least two flux errors below the pseudocontinuum in a given spectrum. The y-axis indicates the number of spectra. The vertical dashed line represents x ≈ 0.05.
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: Schematic diagram of the Spec-Unet processing for the C IV pseudocontinuum autofitting. The input spectral segment has 410 sampling points. After modeling, the output is a pseudocontinuum with 410 data points.
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: Schematic diagrams of the fitted pseudocontinua of the different methods. From the top, the six panels are pseudocontinua fitted by Spec-Unet with HUANG23, QUIDER11, and ZHU13, respectively. The gray dashed line represents the ±1σflux.
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: Example of absorption-line measurement results. Three subfigures in the first row are based on HUANG23’s pseudocontinuum measurement, and the subfigures in the second row are based on Spec-Unet’s pseudocontinuum measurement. (a) Spectra are selected based on EW differences. (b) Spectra selected are based on FWHM1548 differences. (c) Spectra selected are based on FWHM1551 differences.
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: χ2 distribution diagrams between (a) Spec-Unet and ZHU13, (b) Spec-Unet and QUIDER11, and (c) Spec-Unet and HUANG23. The x-axis is χ2. To make the figure easier to observe, the y-axis is presented in a logarithmic scale.
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: Examples of three types of C IV spectra (fitting in 1475 Å < λrest < 1621 Å). From top to bottom: an NAL spectrum, a BAL spectrum, and a spectrum without absorption features.
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 EW of optical Fe II blends for microturbulence Vturb = 50 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 the EW of UV Fe II blends for microturbulence Vturb = 20 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 the EW of optical Fe II blends for microturbulence Vturb = 20 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 the EW of UV Fe II blends for microturbulence Vturb = 50 km s−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: (a) Training loss function against epochs. (b) Fourth-order flatness ﹩{F}_{\tau }^{(4)}﹩ of the particle trajectories generated by the diffusion model at five different training times (A–E, highlighted in the training loss function), 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: Distribution of the cosine similarity of the closest training trajectory for a generated sample (red) and training trajectory (black) for α = 128.
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 diagram of the employed UNet architecture with five layers. The upper row corresponds to the encoder, the lower row to the decoder, and the vertical part to the bottleneck. The dashed lines represent the connecting paths where the data is concatenated.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: The angle separation between the targeted-search location (TL) of bursts and the true position of SGR J1935+2154.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: The targeted-search location (TL) of bursts. The red star marks the accurate position of SGR J1935+2154 (R.A. = 293﹩\mathop{.}\limits^{\unicode{x000b0}}﹩73, decl. = 21﹩\mathop{.}\limits^{\unicode{x000b0}}﹩90).
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Temporal evolutions of the abundances of NH2CH2CH2OH, CH3NH2, CH3OH, and C2H5OH in the warm-up model with the final temperature ﹩{T}_{{\rm{\max }}}﹩ = 200 K. The cyan dashed line shows the time-varying temperature. The horizontal red, green, and blue areas show the observed abundances of CH3NH2, CH3OH, and C2H5OH with an uncertainty factor of 3 relative to the total hydrogen density N(H) = 2.0 × 1024 cm−2 (L. Pagani et al. 2017), respectively. The horizontal red dotted line presents the observational upper limit abundance of CH3NH2 relative to the total hydrogen density N(H) = 2.0 × 1024 cm−2 (J. R. Rizzo et al. 2017). The vertical black area supplies the consistent timescale between the modeled abundances of CH3NH2, CH3OH, and C2H5OH and their observed values.
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Main formation mechanism of s-NH2CH2CH2OH in the best-fitting shock-wave model (the combination of isothermal model I5 and C-shock model S5). If all the species in a reaction are the ice-phase species, which are labeled “s-,” the reaction includes both its grain-surface reaction and its grain-mantle reaction. Otherwise, the reaction is only its grain-surface reaction. The reactions with “-J-H” or “-s-H” are the cosmic-ray-induced photodissociation reactions. Except for them, all the reactions are addition reactions. The reactions in blue are proposed by V. M. Rivilla et al. (2021b) and the references therein.
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Geometries of CH2CH2OH and HOCCNH at the level of B3LYP/May-cc-PVTZ using the D3 version of Grimme's dispersion with Becke–Johnson damping. Distances are given in angstroms and angles in degrees.
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Potential energy surface intersection for s-OCHCNH + s-H → s-NHCHCHO at the level of M062X/Aug-cc-PVTZ using the D3 version of Grimme's dispersion with the original D3 damping function. Based on the intersection point, the barrier is estimated to be 973 K. Distance is given in angstroms.
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Potential energy surface for s-CH2CHNH2 + s-H → s-NH2CH2CH2 at the level of CCSD(T)/Jun-cc-PVQZ//B2PLYPD3/May-cc-PVTZ. Distances are given in angstroms and angles in degrees.
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Temporal evolutions of the abundances of CH2CH2OH, NH2CH2CH2O, and HOCCNH toward G+0.693. The vertical gray area supplies the “consistent timescale.”
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Potential energy surface for s-NHCHCH2OH + s-H → s-NHCH2CH2OH at the level of CCSD(T)/Jun-cc-PVQZ//B2PLYPD3/May-cc-PVTZ. Distances are given in angstroms and angles in degrees.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: CMD for A2061 with g − r [MAG_ISO] color and r [MAG_AUTO] from SExtractor. Red circles represent the spectroscopically confirmed cluster member galaxies within z ± 0.03 of the cluster redshift. The green dashed box highlights the photometrically selected sample of cluster member candidates based on a linear fit to the red sequence. Background galaxies (blue circles) are selected following the criteria described in Section 3.4. A red selection of source galaxies is included for A2061 because of its low redshift (z = 0.08).
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A2061 PSF distortion. Top: measured ellipticity of a selection of stars from the mosaic coadded image. The lines represent the direction and magnitude of the ellipticity of stars. Outliers have not been removed and clearly do not follow the general trend of the PSF. Bottom: ellipticity of the model PSFs at each star location. Models are designed in each component frame and stacked to a coadded PSF. Comparing the top and bottom panels shows that the measured stellar shape is well reproduced by the PSF model.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: Photometric zero-point calibration of A2061 (left panel). The SDSS catalog is used as a reference. Stars (red circles) are selected from the size–magnitude plot (right panel) and matched with stars in the reference catalog. The magnitude offset as a function of SDSS r-band magnitude is plotted, and a linear fit to the stars is made to determine the zero-point. The same stars are utilized in PSF modeling.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A2061 PSF model correction. Red circles denote the observed ellipticity of stars. Black circles are the corrected ellipticities where the PSF model ellipticities have been subtracted from the observed ellipticities of their respective stars. The figure demonstrates that the ellipticity is being corrected. The goal is to tighten the dispersion and shift the centroid to zero. As the legend shows, the dispersion is decreased by ~2, and the centroid is corrected to the 10−4 level.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: The Subaru color image of the galaxy cluster A2061 provides an example of the quality of the imaging (blue = g band, green = r band, red = i band). The rotation and dithering technique of the observations is noticeable at the perimeter of the image and is beneficial to WL analysis because it minimizes the diffraction spikes caused by stars and allows for a better sampling of the PSF.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: Foreground contamination percentage as a function of upper-limit color constraint from the photometry and redshifts of the COSMOS2020 catalog (J. R. Weaver et al. 2022). The rainbow color gradient signifies curves of a range of redshifts that demarcate foreground and background galaxies (i.e., a cluster redshift). Light, solid curves are for all galaxies, and dark, dashed curves are for HSC-r > 22 (top) and HSC-i > 22 (bottom) galaxies. The combination of a magnitude and color constraint are effective at removing contamination by foreground galaxies.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: 1RXSJ0603. A dissociative merger with an extremely large radio relic. Top left: WL convergence S/N (white contours) of the Toothbrush cluster over Subaru color image. Contours start at 2σ and increase in intervals of 1σ. The dashed blue circles are centered on the local BCG of the subcluster and have a radius of R3000. Top right: WL convergence S/N contours over X-ray emission with radio relic plotted as green contours. Bottom left: WL convergence S/N over galaxy luminosity density. Bottom right: WL convergence S/N over galaxy number density. The red circles in the galaxy panels are the FWHM of the Gaussian used to smooth the galaxy maps.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A521. A three-subcluster system with a cool core, a radio halo, and two radio relics. The NW radio relic is faint and marked with a green crescent. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: Galaxy number density by magnitude for the constrained (by color) GOODS-S reference catalog and A2061 source galaxy catalog. The GOODS-S observations are much deeper, which gives rise to the large difference in source density at faint magnitudes. To make up for the difference in depth, the GOODS-S catalog is weighted by the ratio of the bins when used as a reference catalog.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A523. A collision between two subclusters with radio emission in the middle. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A781. A large-scale structure of clusters comprised of Main, Middle, and North. East is at a higher redshift. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A746. A complex cluster merger with four diffuse radio sources. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A1240. A head-on collision, dissociative merger with double radio relics. WL contours increase in steps of 1σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A115. A merger with peculiar ram-pressure-stripped gas that suggests a large impact parameter. WL contours increase in steps of 0.5σ.
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 different microturbulence velocities. The shaded region represents 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 (0.95) 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 spectra in the wavelength range 2200–2700 Å. Both spectra are scaled to 1 at their maximum values. (a) Spikes are seen at around 2400 and 2600 Å in the model-predicted spectra without including microturbulence. Blue-shaded regions denote the wavelength range for spikes, while the cyan-shaded region shows that for the gap. (b) Observed spectrum of RM 102 indicating no such spikes.
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: Variation of UV Fe II peak wavelength with the smear velocity for ﹩\mathrm{log}\,{\Phi }_{{\rm{H}}}\,({\mathrm{cm}}^{-2}{{\rm{s}}}^{-1})=20.5,\mathrm{log}\,{n}_{{\rm{H}}}\,({\mathrm{cm}}^{-3})=12﹩, and different microturbulence velocities. Top panel: UV peak in units of angstroms. Bottom panel: UV peak in velocity space. Here, a negative peak value represents an outflow, while a positive value denotes an inflow.
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 spike-to-gap ratio for different microturbulence velocities. The shaded region represents the model parameter space that predicts the EW of broadband UV Fe II consistent with the observed value, assuming a covering factor of 100%, for the test object RM 102. The red-dashed contour denotes the observed value (1.58) of the ratio 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 UV Fe II to optical Fe II emission for microturbulence velocity Vturb = 100 km s−1 and different metallicities. The shaded region represents the parameter space reproducing the optical broadband Fe II emission strength, assuming a covering factor of 100%, in test object 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 UV-to-optical broadband Fe II emission for different microturbulence velocities. The shaded region represents the parameter space reproducing the optical broadband Fe II emission strength in test object RM 102 for a covering factor of 100%. However, the observed value (2.54) of the ratio in this object, shown by the red contour, is barely reproduced in the case of low microturbulence, and it is never consistent with the model for high microturbulence.
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 different microturbulence velocities. The shaded region denotes the model parameter space that predicts the EW of the UV red Fe II wing consistent with the observed value for a 100% covering factor. The red-dashed contour denotes the observed value (2.02) 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 (5150–5350 Å) to blue (4434–4684 Å) part of the optical Fe II spectra for different microturbulence velocities. The shaded region indicates the model parameter space that predicts the strength of optical blue Fe II emission, assuming a covering factor of 100%, consistent with the observed value. The red-dashed contour denotes the observed value (0.68) for source RM 102.