adsabs/AstroCLIMB huggingface dataset:
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: All the information obtained in one line of sight. (a) The variation of extinction with distance. Blue points represent E(B − V)LAMOST, orange points represent E(B − V)XP, and gray points represent data that are not within the resolution but included with a certain weight. To avoid overlapping error bars, only 50% of the blue points, 25% of the orange points, and 10% of the gray points have their error bars plotted. “×”-shaped points in different colors represent data removed after 3σ clipping. The red line is the best-fit function for this line of sight, and the brown dashed line represents the contribution from diffuse dust. The other dashed lines represent the contributions from different molecular clouds. (b) The variation of dust density with distance. The red line is the derivative of the best-fit line from panel (a), the brown dashed line represents the contribution from diffuse dust, and the shaded regions represent different molecular cloud components. The width of the shading indicates the size of the defined molecular clouds ﹩{{\rm{\Lambda }}}_{i}^{\mathrm{MC}}﹩, and the dashed lines mark the distances to the molecular clouds. (c) The residual distribution of the fit is shown in panel (a). Only the residuals of the colored points are shown, with blue shading indicating the 3σ range for different distance bins. The gray dashed line represents a residual of zero. (d), (e), (f) Histograms of the residuals for the distance bins 0–2 kpc, 1–4 kpc, and >2 kpc, respectively. The red line represents a normal distribution fit, with the σ value indicated in the panel. (g) The total residual histogram for this line of sight, with the red line representing a normal distribution fit and the sigma value indicated. (h) The position of this line of sight in Galactic coordinates, shown as a red square. The resolution of 6﹩\mathop{.}\limits{^{\prime} }﹩6 is marked in the lower right corner. Three parameter values, which are not easily discernible, are also indicated in the lower right corner.
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: A comparison of the E(B − V) derived from the extinction integral at the maximum reliable distance in this work and those from the SFD is shown. The black points represent the median values within each bin, and the black line is the linear fit to these points. LMC, SMC, and ∣b∣ < 20° regions were excluded. The upper left subplot displays a histogram of the differences between the extinction from this work at the maximum reliable distance and those from the SFD, along with a normal distribution function fit.
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: Dust density in the XY plane containing the Sun, with the Sun located at a distance of 8.34 kpc from the Galactic center (marked by the black “×” symbol). The directions of Galactic longitude l = 0° and l = 90° are also indicated. The solid black and dashed curved lines represent the center and ±1σ widths of the spiral arm models, from left to right: Perseus arm, Local arm, Local arm spur, and Sagittarius–Carina arm, as taken from M. J. Reid et al. (2019) cantilever position obtained using proper motions of molecular masers. Top: dust density in the XZ plane. Right: dust density in the YZ plane.
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: Sky distribution and variation with cumulative extinction of the fitted residual standard deviation (σ) along different lines of sight. The upper panels show sky maps of σ calculated using both LAMOST and XP sources, as well as σLAMOST calculated using only LAMOST sources. The lower panels present the variation of these σ values with cumulative extinction. For comparison, the lower panels also include σ values directly calculated from the extinction curves provided by G. M. Green et al. (2019).
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: Comparison to the 2D extinction map of D. J. Schlegel et al. (1998). Top panel: our 3D extinction map at the maximum reliable distance, with E(B − V) shown at a resolution of 3﹩\mathop{.}\limits{^{\prime} }﹩3, corresponding to Nside = 1024. Middle panel: the extinction map from D. J. Schlegel et al. (1998) is scaled by a factor of 0.834, also shown at a resolution of 3﹩\mathop{.}\limits{^{\prime} }﹩4 (Nside = 1024). Bottom panel: the difference between the extinction map in the middle panel and the map in the top panel.
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: Cumulative reddening in the Galactic Mollweide projection at different distances: 0–0.5, 0.5–1, 1–2, and 2–5 kpc. The left side of the figure shows the results from our work, while the right side displays the results from G. M. Green et al. (2019). All subplots are plotted with a resolution of 3﹩\mathop{.}\limits{^{\prime} }﹩3, corresponding to Nside = 1024.
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: The difference with the D. J. Schlegel et al. (1998), after scaling by a factor of 0.834, is shown in the 2D histogram of the Galactic latitude. The black points represent the mean values calculated after a 3σ clipping within each Galactic latitude bin, and the error bars indicate the standard deviation.
Paper: A Deep Learning–Based Multimodal F10.7 Prediction with Mamba
Authors: Dong Zhao, Fengping Dou, Xueshang Feng, Xin Huang, Sai Ma, Long Xu
Figure caption: Dissensions on the data selections. Top: the table details the prediction results of the models under different types of data. Bottom: to enable a clearer comparative analysis, we used bar charts to display the performance of each multimodal model on evaluation metrics. In these bar charts, different colored bars represent groups composed of different numbers of image types, while the wider bars with a translucent background represent the average of the evaluation metrics for the corresponding groups.
Paper: A Deep Learning–Based Multimodal F10.7 Prediction with Mamba
Authors: Dong Zhao, Fengping Dou, Xueshang Feng, Xin Huang, Sai Ma, Long Xu
Figure caption: Predicted results of MaFI in 2013, which was trained on the F10.7 data from 1957 to 2008. Note that the prediction delay problem still exists.
Paper: A Deep Learning–Based Multimodal F10.7 Prediction with Mamba
Authors: Dong Zhao, Fengping Dou, Xueshang Feng, Xin Huang, Sai Ma, Long Xu
Figure caption: The comparisons between our single-modal (MaFI) and multimodal (MaFI+MaSI) F10.7 predictions. The data used in this experiment are similar to those in Figures 2 and 4.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Comparison of GALEX, SBC, and COS fluxes. The top left panel shows the bandpass-corrected SBC F150LP fluxes extracted in a 6″ radius aperture, similar to the GALEX one. The two other top panels show the fluxes from COS synthetic photometry, corrected using F150LP photometry (due to the small sizes of the apertures) to match the value that would be measured in the GALEX aperture. The middle top panel shows what would be measured with an aperture combining the COS vignetting profile and LzLCS spectral extraction window (aperture 1), and the right top panel, the circular 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 diameter aperture value (aperture 2). Blue lines show linear fits to the data. The bottom panels show, from left to right, the normalized bandpass response of GALEX FUV and SBC F150LP overlaid on the spectrum for J172010 spectra, and the two apertures used to correct the COS synthetic FUV photometry, overlaid on the Lyα image of J172010.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Optical RGB composite (top panels) and Lyα images (bottom panels) for galaxies with optical extent exceeding 20 kpc on the side. The data are the same as shown in Figures 3 and 4, but on scales that showcase the emission visible across all filters. The white bar at the bottom of the RGB composite panels indicates the 20 kpc scale. These galaxies all have very tenuous Lyα emission, which is the reason why it is barely visible in the lower panels.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Line-of-sight LyC escape fraction measured in the COS aperture as a function of observables extracted in a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩12 aperture centered around the brightest UV continuum pixel in each galaxy. The first top row of panels shows the position of the aperture on the UV continuum (left), Lyα (middle), and F850LP (right) images of galaxy J172010 as an example. The panels below show on their x-axis, from top to bottom and left to right, the Lyα luminosity, EW, the UV continuum flux density, and the spatial offset between the brightest UV continuum pixel and the brightest Lyα pixel as a function of ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩. We show the Kendall τ and associated p-value assessing the degree of correlation between variables in the top corners of the plots. In general, there is a high degree of correlation between the Lyα observables within the aperture and the LyC escape fraction.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Global photometric Lyα observables vs. ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩. From left to right, the x-axis shows the Lyα luminosity, EW, and Lyα escape fraction. Black filled circles show galaxies confidently detected in LyC, while gray arrows show galaxies with LyC escape fraction upper limits. Kendall τ and p-values assessing the degree of correlation between the x- and y-axes variables are shown on the top right corner of each panel. The escape fraction shows the same trends with photometric Lyα observables as those identified with the spectroscopic values (S. R. Flury et al. 2022b), but the correlation with Lyα luminosity and escape fraction is weaker, while ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩ shows a slightly larger degree of correlation with the photometric Lyα EW.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Comparison between Lyα observables obtained via COS spectroscopy and global photometry. From left to right, the panels show comparisons for the Lyα luminosity (LLyα), rest-frame equivalent width (EWLyα), and escape fraction (﹩{f}_{{\rm{esc}}}^{{\rm{Ly}}\alpha }﹩). The solid line shows the 1:1 relation. The global values from photometry are in broad agreement with the spectral values, indicating the galaxies are compact.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Comparison between UV half-light radius calculated using COS acquisition images and SBC photometry. A solid black line indicates the 1:1 relation. The r50 values obtained with SBC are slightly larger, but in agreement with COS measurements, except for galaxy J095700.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Top panel: LyC escape fraction as a function of r50 obtained from F165LP SBC images. Bottom panel: LyC escape fraction as a function of ΣSFR. The trends with ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩ are the same as those measured with spectroscopy, but the correlations are weaker.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Rest-frame Lyα EW maps of the LaCOS galaxies. The panels display a physical scale of 20 kpc × 20 kpc, and are ordered by increasing LyC escape fraction, displayed in the lower right corner of each panel.
Paper: The Lyα and Continuum Origins Survey. I. Survey Description and Lyα Imaging
Authors: Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Jens Melinder, Alberto Saldana-Lopez, Aaron Smith, Axel Runnholm, Yu-Heng Lin, Ricardo O. Amorín, Hakim Atek, Sanchayeeta Borthakur, Cody A. Carr, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Alaina Henry, Anne E. Jaskot, Zhiyuan Ji, Intae Jung, Floriane Leclercq, Rui Marques-Chaves, Stephan R. McCandliss, M. S. Oey, Göran Östlin, Swara Ravindranath, Daniel Schaerer, Trinh X. Thuan, Xinfeng Xu
Figure caption: Comparison between LaCOS (top panels) and LaXs (bottom panels) Lyα and UV continuum maps for J092532 (left set of panels) and J124835 (right set of panels).
Paper: A JWST Study of Polycyclic Aromatic Hydrocarbon Emission in a Region of 30 Doradus
Authors: Congcong Zhang, Joelene Hales, Els Peeters, Jan Cami, Ameek Sidhu, Junfeng Zhen
Figure caption: JWST/NIRCam F335M image of 30 Dor. The blue box represents the field of view of MIRI/MRS Channel 1. The inset shows the spectroscopic fields of view (FOVs): NIRSpec (green, 4﹩\mathop{.}\limits^{\unicode{x02033}}﹩56 × 4﹩\mathop{.}\limits^{\unicode{x02033}}﹩24, 1.17 pc × 1.09 pc), MIRI/MRS Channel 1 (blue, 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩80 × 4﹩\mathop{.}\limits^{\unicode{x02033}}﹩82, 0.98 pc × 1.24 pc), MIRI/MRS Channel 2 (pink, 4﹩\mathop{.}\limits^{\unicode{x02033}}﹩57 × 5﹩\mathop{.}\limits^{\unicode{x02033}}﹩91, 1.17 pc × 1.52 pc), and MIRI/MRS Channel 3 (yellow, 5﹩\mathop{.}\limits^{\unicode{x02033}}﹩93 × 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩43, 1.52 pc × 1.91 pc). For 30 Dor, 1″ corresponds roughly to 0.257 pc.
Paper: A JWST Study of Polycyclic Aromatic Hydrocarbon Emission in a Region of 30 Doradus
Authors: Congcong Zhang, Joelene Hales, Els Peeters, Jan Cami, Ameek Sidhu, Junfeng Zhen
Figure caption: JWST/NIRCam images of the spectroscopic FOV in the F187N (left) and F335M (right) filters, tracing ionized gas and PAH emission, respectively. The white contour lines represent the F187N surface brightness in both panels. The direction of radiation from R136 is indicated by blue arrows.
Paper: A JWST Study of Polycyclic Aromatic Hydrocarbon Emission in a Region of 30 Doradus
Authors: Congcong Zhang, Joelene Hales, Els Peeters, Jan Cami, Ameek Sidhu, Junfeng Zhen
Figure caption: Extraction apertures plotted on the NIRCam image in the filter F335M tracing PAH emission.
Paper: A JWST Study of Polycyclic Aromatic Hydrocarbon Emission in a Region of 30 Doradus
Authors: Congcong Zhang, Joelene Hales, Els Peeters, Jan Cami, Ameek Sidhu, Junfeng Zhen
Figure caption: PAH ratios observed in 30 Dor and the Orion Bar on the charge–size grid for a radiation field with 〈Eabs〉 = 8 eV from A. Maragkoudakis et al. (2020). We adjusted the observed 11.2 μm/3.3 μm ratios by 0.66 to correct for the overestimation of the 3.3 μm intensity in the theoretical calculations. The neutral–cation relative contributions are labeled: 75%–25% (N75C25), 50%–50% (N50C50), 25%–75% (N25C75), etc. NC in the figure is the number of carbon atoms making up the PAH molecule.
Paper: A JWST Study of Polycyclic Aromatic Hydrocarbon Emission in a Region of 30 Doradus
Authors: Congcong Zhang, Joelene Hales, Els Peeters, Jan Cami, Ameek Sidhu, Junfeng Zhen
Figure caption: PAH ratios observed in 30 Dor and the Orion Bar on the charge–size grid from B. T. Draine et al. (2021) for three radiation fields: a 3 Myr old starburst (〈Eabs〉 = 8.6 eV, blue grid), a typical interstellar radiation field in the diffuse ISM (mMMP, 〈Eabs〉 = 4.5 eV, black grid), and the M31 bulge radiation field 〈Eabs〉 = 2.7 eV, red grid; for details, see B. T. Draine et al. 2021).
Paper: A JWST Study of Polycyclic Aromatic Hydrocarbon Emission in a Region of 30 Doradus
Authors: Congcong Zhang, Joelene Hales, Els Peeters, Jan Cami, Ameek Sidhu, Junfeng Zhen
Figure caption: Comparison of the PAH emission in A6 of 30 Dor with the three Orion Bar templates (the atomic PDR, DF2, and DF3; E. Peeters et al. 2024; R. Chown et al. 2024) shown in the black, blue, green, and red curves, respectively. All spectra are normalized to the 11.2 μm band peak surface brightness.
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: An example of the results for a target star using the standard-pair algorithm. The top three panels show the distribution of control stars in the parameter space, with the colors encoding the intrinsic colors of the control stars. The bottom three panels display the residuals from the linear fit, with the blue shading and red dashed lines indicating the 3σ range and the mean (μ) of the residuals, respectively. The gray dashed line marks the zero level.
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: The 2D histogram of the residual standard deviation from the linear fit to the target stars, derived using the standard-pair algorithm, as a function of Teff,LAMOST, with color encoding representing the stellar number density.
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: Mean and standard deviation of the differences between the two independent measurements of extinction (E(B − V)LAMOST − E(B − V)SFD).
Paper: An All-sky 3D Dust Map Based on Gaia and LAMOST
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Maosheng Xiang, 茂盛 向, Ruoyi Zhang, 若羿 张, Bowen Huang, 博闻 黄, Hongrui Gu, 弘睿 顾, Shuaicong Wang, 帅聪 王, Jiawei Li, 佳伟 李
Figure caption: Teff,LAMOST vs. ﹩{\mathrm{log}}\,{g}_{\mathrm{LAMOST}}﹩ (left panel) and Teff,LAMOST vs. [Fe/H]LAMOST (right panel) distributions of the target and control samples. The blue dots represent the control sample stars, and the density contours represent the target sample.
Paper: Imaging the Solar Corona from “Within”: A Cutting-edge Approach to Enhance PSP/WISPR Imagery
Authors: Guillermo Stenborg, Angelos Vourlidas, Russell A. Howard
Figure caption: Background-removed versions of a WISPR-I image acquired on 2023 September 28 at 08:00 UT in E17. Left panel: LW-processed. Middle panel: L3-processed. Right panel: LT-processed. The corresponding background model has been removed from the image by taking the ratio of the image to the background in the LW- and LT- processed frames; whereas for the L3 processing, the background was removed by subtracting it from the image. The colored symbols point out features of interest discussed in the text.
Paper: Imaging the Solar Corona from “Within”: A Cutting-edge Approach to Enhance PSP/WISPR Imagery
Authors: Guillermo Stenborg, Angelos Vourlidas, Russell A. Howard
Figure caption: Comparison of the LX (top row), L3 (middle row), and LT (bottom row) techniques as applied to a set of WISPR-I images acquired during E18. The background models for the LX-processed samples were computed with Equation (2) (i.e., Case II). The corresponding background models in the LX- and LT-processed frames have been removed from the images by taking the ratio; whereas for the L3 processing, the background was removed by subtracting it from the image. The colored symbols point out features of interest discussed in the text.