adsabs/AstroCLIMB huggingface dataset:
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The pulse energy distributions for PSR J1945+1211 (upper plot), PSR J2323+1214 (middle plot), and PSR J1900–0134 (lower plot). All pulse energy is normalized by the respective mean on-pulse energy. The solid black lines represent the on-pulse regions, and dashed red lines indicate the off-pulse regions. The vertical dashed orange line represents the threshold energy value for Gaussian fitting to both null pulses and off-pulse regions. The representation of brown, green, and cyan lines is described in the main text and in Table 4. The x-axis is normalized by the mean on-pulse energy.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Integrated pulse profiles of PSR J1945+1211 (upper plot), PSR J2323+1214 (middle plot), and PSR J1900–0134 (lower plot), observed in different emission states: null (blue), burst (red), and overall (dashed black).
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The upper panels display the pulse energy sequences for PSR J1945+1211 (left plot) and PSR J2323+1214 (right plot), and the lower panels indicate their corresponding null and burst states. The pink rectangular boxes indicate transitional patterns.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The first 100 single pulses from PSR J1945+1211 (left plot), PSR J2323+1214 (middle plot), and PSR J1900–0134 (right plot), respectively.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The single-pulse sequence (upper panel) and the associated integrated pulse profile (lower panel) are shown for PSR J1945+1211 (left), PSR J2323+1214 (middle) and PSR J1900–0134 (right), respectively.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Similar to Figure 5, but for PSR J1900–0134.
Paper: Real-time Extrapolation of Nonlinear Force-free Fields from Photospheric Vector Magnetic Fields Using a Physics-informed Neural Operator
Authors: Mingyu Jeon, Hyun-Jin Jeong, Yong-Jae Moon, Jihye Kang, Kanya Kusano
Figure caption: EUV observations of AR 11158 and projected magnetic field lines from different extrapolation methods. The color of the field lines indicates the magnitude of the vertical current density in the photosphere. EUV observations in 171 and 94 Å are shown in (a) and (b), respectively. (c) Target magnetic field of the ISEE NLFFF database. (d) AI-generated magnetic field of our trained PINO model. (e) Magnetic field of the optimization method (T. Wiegelmann et al. 2012). (f) Magnetic field of the PINN method (λff/div = 0.1; R. Jarolim et al. 2023).
Paper: Real-time Extrapolation of Nonlinear Force-free Fields from Photospheric Vector Magnetic Fields Using a Physics-informed Neural Operator
Authors: Mingyu Jeon, Hyun-Jin Jeong, Yong-Jae Moon, Jihye Kang, Kanya Kusano
Figure caption: Time series of (top) total magnetic energy and (bottom) free magnetic energy calculated from NLFFFs of AR 11158. The dashed black vertical lines indicate flares ≥M1. We use SHARP data as the input data of the PINO model. The solid red line shows magnetic energy from the target fields of the ISEE NLFFF database, which covers the period from 12:00 UTC on 2011 February 13 to 12:00 UTC on 2011 February 15. The solid blue line is for our trained PINO, the dotted black line is for the optimization method (T. Wiegelmann et al. 2012), and the dashed green line is for the PINN method (R. Jarolim et al. 2023). The three lines correspond to the period from 00:00 UTC on 2011 February 12 to 00:00 UTC on 2011 February 17. The data for the black and green lines are obtained from R. Jarolim et al. (2023).
Paper: Real-time Extrapolation of Nonlinear Force-free Fields from Photospheric Vector Magnetic Fields Using a Physics-informed Neural Operator
Authors: Mingyu Jeon, Hyun-Jin Jeong, Yong-Jae Moon, Jihye Kang, Kanya Kusano
Figure caption: EUV observations of AR 12673 and projected magnetic field lines from different extrapolation methods. The format of the figure is the same as Figure 2.
Paper: Real-time Extrapolation of Nonlinear Force-free Fields from Photospheric Vector Magnetic Fields Using a Physics-informed Neural Operator
Authors: Mingyu Jeon, Hyun-Jin Jeong, Yong-Jae Moon, Jihye Kang, Kanya Kusano
Figure caption: EUV observations of AR 11158 and vertically integrated current density maps from different extrapolation methods. The format of the figure is the same as Figure 2.
Paper: Real-time Extrapolation of Nonlinear Force-free Fields from Photospheric Vector Magnetic Fields Using a Physics-informed Neural Operator
Authors: Mingyu Jeon, Hyun-Jin Jeong, Yong-Jae Moon, Jihye Kang, Kanya Kusano
Figure caption: EUV observations of AR 12673 and vertically integrated current density maps from different extrapolation methods. The format of the figure is the same as Figure 2.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Ratio of the relative error in the baryon mass, M  b  (as defined in Equation (23)), to the “proton mass,” M  p  (Equation (30)), for ∼5 ms of evolution of an M = 1.4 M ⊙ TOV star using the SFHo (A. W. Steiner et al. 2013) EOS.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Top: evolution of central rest-mass density of the static star A0 model with superposed poloidal magnetic field with WENOZ reconstruction. Bottom: integrated divergence of the magnetic field (Equation (18)) normalized by the maximum value of the magnetic field.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Top: convergence of the L 1 norm of the Hamiltonian constraint of static star model A0. Bottom: convergence of the L 1 norm of the momentum constraint of static star model A0. Data are evaluated at t = 2.96 ms. The modulus of the slopes, corresponding to the order of convergence in the Hamiltonian (momentum) constraint is 3.51 (4.41), 3.65 (5.46), and 3.64 (4.88) for PPM, WENOZ, and WENO5, respectively.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Temperature T (left) and electron fraction Y e (right) of the initial configuration (top) and after 0.5 ms of evolution (bottom) of an M = 1.4 M ⊙ TOV star using the SFHo (A. W. Steiner et al. 2013) EOS.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Convergence of the L 1[E(ρ)] norm of static star model A0 at t = 2.96 ms. Data refer to GRHD evolutions and various reconstruction schemes. The modulus of the slopes, corresponding to the order of convergence is 1.85, 1.76, and 1.87 for PPM, WENOZ, and WENO5, respectively.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Evolution of magnetic streamlines seeded in equatorial plane at radius 5.91 km. The gray isocontour shows the surface of ρ = 6.18 × 1014 g cm−3. Left: varicose instability at t = 4.93 ms. Middle: kink instability at t = 12.8 ms. Right: late-time nonlinear field arrangement at t = 44.3 ms.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Profiles of velocity component ﹩{\tilde{u}}^{y}﹩ and rest-mass density ρ along the x-direction at the initial time and after two rotational periods. Data refer to resolution N = 32 with PPM reconstruction. Note that velocity is plotted in geometric units.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Baryon mass conservation along the GRHD evolution of static star model A0. The mass conservation can be violated due to the artificial low-density atmosphere as the fluid expands beyond the computational domain.
Paper: GR-Athena++: General-relativistic Magnetohydrodynamics Simulations of Neutron Star Spacetimes
Authors: William Cook, Boris Daszuta, Jacob Fields, Peter Hammond, Simone Albanesi, Francesco Zappa, Sebastiano Bernuzzi, David Radice
Figure caption: Convergence of the L 1 norm of the error of the rest-mass density of rotating star AU4. Data refer to an evolution time of t = 3.06 ms (second rotational period). The modulus of the slopes, corresponding to the order of convergence is 0.75 and 0.86 for PPM and WENOZ, respectively.
Paper: A Catalog of 12,766 Carbon-enhanced Metal-poor Stars from LAMOST Data Release 8
Authors: Ziyu Fang, Xiangru Li, Haining Li
Figure caption: The performance of parameter estimation. The horizontal axis represents the reference values and the vertical axis represents the estimated values. These results are computed from the test set. The black dashed lines represent the reference line for theoretical consistency, while the red dashed lines represent the 3σ reference lines. The parameters μr and σr are, respectively, the mean and standard deviation of the difference between the parameter estimation and its corresponding reference on test spectra. The mean absolute error/difference between the parameter estimation and its corresponding reference on test spectra is calculated.
Paper: A Catalog of 12,766 Carbon-enhanced Metal-poor Stars from LAMOST Data Release 8
Authors: Ziyu Fang, Xiangru Li, Haining Li
Figure caption: The distribution of 12,766 CEMP candidates and the occurrence rate of CEMPs. In (b), proportions exceeding 150 are not displayed. [C/Fe] = [C/H] – [Fe/H].
Paper: An End-to-end Ensemble Machine Learning Approach for Predicting High-impact Solar Energetic Particle Events Using Multimodal Data
Authors: Pouya Hosseinzadeh, Soukaina Filali Boubrahimi, Shah Muhammad Hamdi
Figure caption: Performance results of TS-HOG-TB for balanced and imbalanced settings.
Paper: The 4–400 GHz Survey for the 32 Class II Disks in the Taurus Molecular Cloud
Authors: Chia-Ying Chung, An-Li Tsai, Melvyn Wright, Wenrui Xu, Feng Long, Mark A. Gurwell, Hauyu Baobab Liu
Figure caption: The Q-band 200 GHz spectral index (α44–200 GHz) vs. the submillimeter spectral index (α200–400 GHz) quoted from C.-Y. Chung et al. (2024). Color codes and symbols are the same as those in Figure 5. Gray vertical and horizontal dashed lines (and shaded areas) in the scatter plot represent the means (μα) (and standard deviations (σα)) of the α44–200 GHz and α200–400 GHz of all the sources, respectively, which are also labeled in the text. The dark blue dashed line shows where the two spectral indices are equal. Histograms of α200–400 GHz and α44–200 GHz for the radio-detected and non-detected sources are shown in the right and top panels.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Training losses of Cycle-StarNet as a function of epochs. The upper panel displays the losses in both the synthetic and observed domains for the within domain reconstructions (﹩{{ \mathcal X }}_{\mathrm{synth}\to \mathrm{synth}}﹩, ﹩{{ \mathcal X }}_{\mathrm{obs}{\to }\mathrm{obs}}﹩), cross-domain transferring (﹩{{ \mathcal X }}_{{\rm{synth}}\to {\rm{obs}}}﹩, ﹩{{ \mathcal X }}_{{\rm{obs}}\to {\rm{synth}}}﹩), and cycle reconstructions (﹩{{ \mathcal X }}_{{\rm{synth}}\to {\rm{obs}}\to {\rm{synth}}}﹩, ﹩{{ \mathcal X }}_{{\rm{obs}}\to {\rm{synth}}\to {\rm{obs}}}﹩). The left lower panel shows the evaluation of the adversarial losses on the training set for both the transfer loss (﹩{{ \mathcal X }}_{{\rm{synth}}\to {\rm{obs}}}﹩, ﹩{{ \mathcal X }}_{{\rm{obs}}\to {\rm{synth}}}﹩) and the adversarial loss (﹩{C}_{{\rm{synth}}/{\rm{obs}}}({{ \mathcal X }}_{{\rm{real}}/{\rm{fake}}})﹩. The right lower panel shows the validation scores for the latent spaces (﹩{{ \mathcal Z }}_{\mathrm{shared}/\mathrm{split}}﹩).
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: The t-SNE projections of 10,000 pairs of test spectra. The left panel highlights the disparity, referred to as the “synthetic gap,” between PHOENIX models and LAMOST spectra. The middle panel demonstrates that a shared representation for the latent spaces of the two domains has been achieved after model training. The right panel illustrates the transfer results in the observed domain, showcasing success in bridging the synthetic and observed domains through domain adaptation.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Comparison of residuals for 10,000 LAMOST spectra in the test set, showing the residuals between the best-fit and PHOENIX spectra both before and after transfer. After applying the domain adaptation model, the spectral residuals decreased from the mean intrinsic spectral error shown in the upper panel (over 2 times) to 1.68 times, as shown in the lower panel, with the fitting accuracy improved by around 20%.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Example of a LAMOST observed spectrum and its processing. From top to bottom: The original spectrum (black) with its pseudocontinuum fit (red); the flux uncertainty; the normalized spectrum after continuum division; and the normalized flux uncertainty. Gray shaded regions indicate masked wavelength ranges that are excluded from analysis. The wavelength range covers from 6000 to 8900 Å.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Evaluation of the reconstruction accuracy of the spectral emulator across the entire parameter space. Each point represents a synthetic spectrum from the model grid in the validation set, with points color coded by the reconstruction residuals, as calculated and described in Section 2.2.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Signal-to-noise ratio (S/N) distributions of M dwarf spectra classified by the LAMOST pipeline. The upper and lower panels show the distributions for the r band and i band, respectively, with black dashed lines indicating the sample selection thresholds of S/Nr = 5 and S/Ni = 5.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Comparison between Gaia RV and RV measurements from this study for approximately 100,000 homologous samples. The density map is color coded by the sample count. The red dashed line marks the reference line.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Galactic coordinate distribution of LAMOST DR10 M dwarf stars on the celestial sphere.
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: 5 GHz luminosity vs. redshift diagram. The transient sources from this work are marked with filled yellow (galaxies) and gray (quasar) circles. The open red circles (galaxies) and open black circles (quasars) indicate CSS and GPS sources taken from C. P. O’Dea (1998), I. A. G. Snellen et al. (1998a), W. H. de Vries et al. (1997), C. Stanghellini et al. (1998), and R. Fanti et al. (1990) as collected by M. A. Keim et al. (2019) into one sample. The red and black squares indicate galaxies and quasars, respectively, from the LLC sample (M. Kunert-Bajraszewska et al. 2010). The filled red circles (galaxies) and filled black circles (quasars) indicate radio transients discovered in the CNSS by A. Wołowska et al. (2021). The open blue triangles indicate transient quasars from K. Nyland et al. (2020).