adsabs/AstroCLIMB huggingface dataset:
Paper: A Comparative Analysis of the Solar Ultraviolet Spectral Irradiance Measured from Earth and Mars: Toward a General Empirical Model for the Study of Planetary Aeronomy
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Least-squares fits of the SEE irradiance between 30 and 31 nm and between 130 and 131 nm by using F10.7P as the solar proxy. Black dots: the SEE measurements. Red line: linear fits. Blue line: quadratic fits. (b) Same as (a) except that the Lyα flux is used as the solar proxy. (c)–(d) Time series of (red) the SEE irradiance and (blue) the modeled irradiance between 30 and 31 nm and between 130 and 131 nm, respectively. For the results shown in (c)–(d), both the F10.7P index and the Lyα flux are used as solar proxies to model the solar VUV irradiance. Note that the measurements of the irradiance between 130 and 131 nm in (a), (b), and (d) are linearly scaled up by four times and are then subtracted by 0.5 mW m−2 so they can be clearly displayed together with the 30–31 nm measurements.
Paper: A Comparative Analysis of the Solar Ultraviolet Spectral Irradiance Measured from Earth and Mars: Toward a General Empirical Model for the Study of Planetary Aeronomy
Authors: Zhen Xu, Jianqi Qin
Figure caption: Amplitudes of the solar irradiance and the F10.7P index in the frequency domain in arbitrary units. Period: the reciprocal of frequency. The periods of some salient features, e.g., ∼26, 41, 61, and 121 days, are marked with dashed rectangles. See text for details.
Paper: A Comparative Analysis of the Solar Ultraviolet Spectral Irradiance Measured from Earth and Mars: Toward a General Empirical Model for the Study of Planetary Aeronomy
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Time series of the integrated solar irradiance between 6 and 27 nm from 2010 April to 2014 May. Red: the irradiance measured by TIMED/SEE. Blue: the irradiance measured by SDO/EVE. (b) Uncertainties of the solar irradiance between 6 and 27 nm in model V3. (c) Time series of the integrated solar irradiance between 6 and 27 nm from 2014 October to 2016 December. Black: the irradiance at Earth predicted by model V3. Blue: the irradiance at Mars measured by MAVEN/EUVM. Magenta: the irradiance at Mars predicted by geometric extrapolation of model V3, denoted as EVEM.
Paper: A Comparative Analysis of the Solar Ultraviolet Spectral Irradiance Measured from Earth and Mars: Toward a General Empirical Model for the Study of Planetary Aeronomy
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Comparison of the solar VUV irradiance measured by SEE and predicted by the HEUVAC model on 2002 August 15 under solar maximum conditions. (b) Comparison of the solar VUV irradiance measured by SEE and predicted by the extended version of our empirical model on 2002 August 15. (c) Comparison of the percentage differences between the measured and the modeled irradiance shown in (a) and (b). (d)–(f) Same as (a)–(c), but for 2008 October 26 under solar minimum conditions.
Paper: A Comparative Analysis of the Solar Ultraviolet Spectral Irradiance Measured from Earth and Mars: Toward a General Empirical Model for the Study of Planetary Aeronomy
Authors: Zhen Xu, Jianqi Qin
Figure caption: The solar VUV irradiance received by Mars on (a) 2014 October 20 with F10.7 = 104 sfu at Mars (strong solar activity) and on (b) 2016 December 11 with F10.7 = 36 sfu at Mars (weak solar activity). Blue: the EUVM measurements. Red: the solar irradiance at Mars obtained through geometric extrapolation of the SEE measurements from Earth (SEEM).
Paper: A Comparative Analysis of the Solar Ultraviolet Spectral Irradiance Measured from Earth and Mars: Toward a General Empirical Model for the Study of Planetary Aeronomy
Authors: Zhen Xu, Jianqi Qin
Figure caption: Correlation coefficient of each 1 nm binned solar irradiance observed by TIMED/SEE in the (a) XUV–EUV and (b) FUV spectral ranges with the Lyα emission and the F10.7P index.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Comparison of the synthetic photometry based on the XP spectra with the corrected Gaia DR3 photometry. The left and right three columns plot the differences as a function of G and BP − RP, respectively. The first/fourth, second/fifth, and third/sixth columns depict, respectively, the results of synthetic photometry based on the original XP spectra, the corrected XP spectra, and the corrected XP spectra with absolute calibration. The color of the background indicates the number of sources. The red dots represent the sources from the CALSPEC. The horizontal red lines indicate zero differences.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Magnitude calibration curves, similar to the top panels of Figure 4 in Yang et al. (2021). The points represent the differences between the synthetic magnitudes derived from the CALSPEC spectra and the corresponding Gaia DR3 photometry. The blue and red points are sources of −0.3 < BP − RP < 0.5 and BP − RP > 0.5, respectively. The blue and red lines are absolute corrections of Yang et al. (2021) and our new ones for the BP band, respectively.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: A direct comparison between the corrected XP spectra and the test sample. The color of each point represents the BP − RP color of the corresponding source, and the solid red line denotes the median value of the differences at each wavelength.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Comparison of results between the nontruncated corrected XP spectra and MILES (shown as the red line), as well as the comparison between the four common sources of CALSPEC and MILES (depicted as the blue lines).
Paper: IRIS2+: A Comprehensive Database of Stratified Thermodynamic Models in the Low Solar Atmosphere
Authors: Alberto Sainz Dalda, Aaryan Agrawal, Bart De Pontieu, Milan Gošić
Figure caption: Same as Figure 4 for a multiline RP and RMA in the outer plage (marked with a white cross in the “Selected areas” panel). Both the inverted profile and the representative model atmosphere (RMA) are included in the IRIS2+, and they are both labeled as “plage” in the database.
Paper: IRIS2+: A Comprehensive Database of Stratified Thermodynamic Models in the Low Solar Atmosphere
Authors: Alberto Sainz Dalda, Aaryan Agrawal, Bart De Pontieu, Milan Gošić
Figure caption: Using IRIS2+ database to find and visualize the different models of umbra, penumbra, plage, and quiet Sun at a given interval of ﹩\mu =\cos (\theta )﹩, with θ being the heliocentric angle.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of our carbon stars in the H-R diagram. The black dashed line represents the dividing line between carbon dwarfs and carbon giants (i.e., M  G  = 5.0 mag). The orange and gray circles represent “UNKNOWN” stars and dC stars identified by Green (2013), respectively. The other symbols are the same as in Figure 10. The numbers in parentheses indicate the quantities of each subtype.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of our carbon stars in the J − H vs. H − K  s  diagram. The black solid line (see Equation (4)) is the dividing line between the warm carbon stars (C–H, C–R, Ba stars) and the cool carbon stars (C–N stars). The blue unfilled pentagon symbols represent the C–N stars, the red dendritic symbols toward the left represent the C–H stars, the dark magenta star symbols represent the Ba stars, and the green crosses display the C–R stars.
Paper: A Comparative Analysis of the Solar Ultraviolet Spectral Irradiance Measured from Earth and Mars: Toward a General Empirical Model for the Study of Planetary Aeronomy
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Solar VUV irradiance observed by TIMED/SEE under (red) solar maximum conditions with F10.7 = 216 sfu at Earth on 2002 August 15 and (blue) solar minimum conditions with F10.7 = 66 sfu at Earth on 2008 October 26. (b) Solar VUV irradiance observed by (red) TIMED/SEE and (blue) MAVEN/EUVM under moderate solar conditions with F10.7 = 95 sfu at Earth (corresponding to 40 sfu at Mars) on 2016 January 1. Note that SEE is orbiting Earth at 1 au whereas EUVM is orbiting Mars at ∼1.66 au on 2016 January 1.
Paper: A Comparative Analysis of the Solar Ultraviolet Spectral Irradiance Measured from Earth and Mars: Toward a General Empirical Model for the Study of Planetary Aeronomy
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a)–(d) Solar irradiance within 0.1–27, 27–120, and 120–190 nm and the solar Lyα emission measured by TIMED/SEE during 2002–2016. (e) The Mg II index during 2002–2016. (f) Gray: the daily F10.7 index. Black: the F10.7A index. Orange: the F10.7P index. These indices are scaled to a distance of 1 au from the Sun.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of S/Ns in the LAMOST g band. The blue solid and dashed lines represent the “UNKNOWN” and classified carbon stars, respectively. The red solid and dashed lines represent the dCs and carbon giants, respectively. The S/N distribution of all the carbon stars is also shown by the black dashed line.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Spatial distribution of the 3546 carbon stars reported in this paper in the Galactic coordinates. The black squares represent dC stars, the other symbols are the same as in Figure 10. The numbers in parentheses indicate the quantities of each subtype.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Normalized LAMOST spectra of five carbon stars classified as “UNKNOWN.” The red dashed lines represent the C2 bands in the blue part and the CN bands in the red part. The blue triangles represent the carbon features we are using to call these carbon stars.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Steps of the identification of carbon stars.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Fitting residuals for the nontruncated XP spectra. The top four rows show the residuals as a function of C2, G, C3, and E(B − V), respectively. The last row illustrates the comparison between the residuals and the original systematic errors, where the original systematic errors are subtracted by 1 to facilitate comparison. The red and blue points represent sources from the CALSPEC and NGSL, respectively.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: The correction of the nontruncated (red lines) and truncated (blue lines) XP spectra in C2, C3, and G terms. The green and yellow lines represent the additional correction in the G term for the nontruncated and truncated XP spectra, respectively.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Fitting residuals of the SCR method for the control sample. From top to bottom: T eff, [Fe/H], log g, BP − RP, G, and E(B − V), respectively. The green line indicates the median value of residuals.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Similar to Figure 9, the remaining differences to illustrate the systematic errors in the f 3(G) term. See more details in Section 4.1.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: The original systematic error (blue), dispersion of the fitting residuals (red), and typical observational error (green) of the training sample as a function of wavelength.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: The nontruncated XP spectra are used as an example to demonstrate the first iteration of the procedure. Red points represent sources from the CALSPEC, blue points correspond to sources from the NGSL, and magenta points depict the results of the fit at each step.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: The comparison between the original (blue lines) and corrected (red lines) nontruncated XP spectra for sources of different colors and magnitudes. The gray horizontal dashed lines indicate the positions where the flux of each spectrum is zero.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: The color–magnitude diagram of the test sample. Red points represent sources from MILES while blue points correspond to sources from LEMONY.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Same as Figure 6 but for the truncated XP spectra.
Paper: A Fast Second-order Solver for Stiff Multifluid Dust and Gas Hydrodynamics
Authors: Leonardo Krapp, Juan Garrido-Deutelmoser, Pablo Benítez-Llambay, Kaitlin M. Kratter
Figure caption: Numerical (open circles) and analytical (solid lines) solution of the five-fluid test described in Section 3.2 in Benítez-Llambay et al. (2019). The numerical solution was obtained at time t = 500, starting from the initial jump condition. The plot shows the density of the gas (blue) and dust (orange, green, red) species, respectively. In the large panel, to allow the quality of the asymptotic behavior far away from the shock to be assessed, the sampling rate for the open circles was reduced to 1:4 of the original data. We additionally plot as an inset a zoomed-in region about the shock showing the full sampling, where the unfilled circles correspond to the actual grid points. The code resolves the shock within a single cell, even when an increasing number of fluids is considered. The overall agreement between the numerical and analytical solutions is excellent.
Paper: A Fast Second-order Solver for Stiff Multifluid Dust and Gas Hydrodynamics
Authors: Leonardo Krapp, Juan Garrido-Deutelmoser, Pablo Benítez-Llambay, Kaitlin M. Kratter
Figure caption: Test resolution convergence for Jeans instability including drag forces. The dashed line denotes the analytic solution for only gas. The solid line shows the analytic solution for 128 fluids including gas and dust species with a linear distribution from t s = 10−4 to 10 and uniform density distribution with a total dust-to-gas ratio ϵ 0 = 0.01. The open circles indicate that the numerical solutions for different numbers of cells converge to the solid line. The vertical dotted line indicates ﹩k/{k}_{{\rm{J}}}=1/\sqrt{1+{\epsilon }^{0}}﹩.
Paper: A Fast Second-order Solver for Stiff Multifluid Dust and Gas Hydrodynamics
Authors: Leonardo Krapp, Juan Garrido-Deutelmoser, Pablo Benítez-Llambay, Kaitlin M. Kratter
Figure caption: Normalized CPU time vs. the number of fluids for the test described in Section 3.6. As expected, the complexity of MDIRK is ﹩{ \mathcal O }(N)﹩. For comparison, we also include the results of the multifluid second-order fully implicit method (RK2Im) from Huang & Bai (2022), which has complexity ﹩{ \mathcal O }({N}^{3})﹩.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of the 9,060,920 spectra and the known carbon stars in ﹩{\mathrm{EW}}_{\mathrm{CN}(\lambda \,7820\,{\rm{\mathring{\rm A} }})}﹩ vs. ﹩{\mathrm{EW}}_{\mathrm{CN}(\lambda \,7065\,{\rm{\mathring{\rm A} }})}﹩ plane. The solid dots indicate the density of 9,060,920 candidates with S/N(i) > 10. The red dashed lines indicate the cuts used to remove contaminants, and the magenta, orange, and green unfilled circles represent the carbon star samples from Li et al. (2018), Ji et al. (2016), and Alksnis et al. (2001), respectively. The numbers in brackets indicate the number of known carbon stars in each sample.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of the 609,702 candidates and the known carbon stars in the J − H vs. H − K  s  color–color diagram. The solid dots with marked density represent the candidates. The red dashed line (i.e., Equation (4)) divides the candidates and known carbon stars into two groups, the Warm Group and the Cool Group. The lower left of the dashed line is the Warm Group, while the upper right is the Cool Group. The other symbols are the same as in Figure 1.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Normalized spectra of four LAMOST carbon stars from this work, including a C–H star, a C–R star, a C–N star, and a Ba star. The G-branch, P-branch band, and Ba II lines are marked for the C–H star by red color. For the spectrum of a C–R star, we label the Ca I line. The weakening flux in the C–N spectrum is labeled in the blue part. The Ba II and Sr II lines are also marked by red color for the Ba star. The red dashed lines represent C2 bands in the blue part and CN bands in the red part.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of the 706,597 candidates and the known carbon stars in the J − H vs. J − K  s  color–color diagram. The solid dots indicate the density of the candidates. The other symbols are the same as in Figure 1.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of 23,629 cool candidates and known carbon stars in the EW﹩{}_{{{\rm{C}}}_{2}(\lambda 5635\,{\rm{\mathring{\rm A} }})}﹩ vs. ﹩{\mathrm{EW}}_{\mathrm{CN}(\lambda 7820\,{\rm{\mathring{\rm A} }})}﹩ plane. The red dashed line represents the cutting line (i.e., Equation (7)). The dots indicate the density of the candidates. The other symbols are the same as in Figure 1.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of the 586,073 warm candidates and the known carbon stars in the ﹩{\mathrm{EW}}_{{{\rm{C}}}_{2}(\lambda 5635\,{\rm{\mathring{\rm A} }})}﹩ vs. ﹩{\mathrm{EW}}_{{{\rm{C}}}_{2}(\lambda 4737\,{\rm{\mathring{\rm A} }})}﹩. The solid dots indicate the density of the warm candidates, the red dashed lines represent the cutting lines (i.e., Equation (5)), and other symbols are the same as in Figure 1.
Paper: Identification of Carbon Stars from LAMOST DR7
Authors: Linlin Li, Kecheng Zhang, Wenyuan Cui, Jianrong Shi, Wei Ji, Zhenyan Huo, Yawei Gao, Shuai Zhang, Mingxu Sun
Figure caption: Distribution of the 127,943 warm candidates and the known carbon stars in the EW ﹩{}_{{{\rm{C}}}_{2}(\lambda 5635\,{\rm{\mathring{\rm A} }})}﹩ vs. ﹩{\mathrm{EW}}_{\mathrm{CN}(\lambda 7065\,{\rm{\mathring{\rm A} }})}﹩ plane. The contours represent the density of the candidates. The red dashed lines are the cutting lines (i.e., Equation (6)). Other symbols are the same as in Figure 1.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Color–color diagrams of the training sample for BP − RP vs. C2 (upper left), BP − RP vs. C3 (upper right), and C2 vs. C3 (lower left). The lower right panel is identical to the lower left panel, but shows sources from the XpSampledMeanSpectrum_000000-003111.csv.gz data set (G < 15). The color in all panels represents the E(B − V) value.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Comparison of systematic errors between two pairs of sources from CALSPEC (top panel) and NGSL (bottom panel). The sources in each pair have similar BP − RP color and G magnitude, but very different E(B − V). The low-extinction and high-extinction sources are represented by blue and red lines, respectively.
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Systematic errors at 360 nm as a function of BP − RP. The truncated XP spectra are adopted here. In the left panel, the color of the points denotes the G magnitude, whereas in the right panel, it stands for the values of E(B − V).
Paper: A Comprehensive Correction of the Gaia DR3 XP Spectra
Authors: Bowen Huang, 博 闻 黄, Haibo Yuan, 海 波 苑, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Ruoyi Zhang, 若羿 张, Lin Yang, 琳 杨, Zexi Niu, 泽茜 牛, Hongrui Gu, 弘睿 顾
Figure caption: Color–magnitude diagram of the training sample. Red and blue points represent sources from the CALSPEC and NGSL, respectively.