adsabs/AstroCLIMB huggingface dataset:
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Absorption lines of Mg IIλλ2796 (top panels), Mg IIλ2803 (middle panels), and O Iλ1302 (bottom panels) in our reanalysis of the J1342 NIRSpec spectrum. The orange lines and shaded regions highlight the region used to fit the continuum and the 1σ noise, respectively. The blue shaded regions show the pixels used to measure the line equivalent widths.
Paper: Detailed Radial Scale Height Profile of Dust Grains as Probed by Dust Self-scattering in HL Tau
Authors: Haifeng Yang, 海峰 杨, Ian W. Stephens, Zhe-Yu Daniel Lin, Manuel Fernández-López, Zhi-Yun Li, Leslie W. Looney, Rachel Harrison
Figure caption: The constraints on scale heights and the scale height profiles for various models. The gray shaded regions represent the suggested regions from our modeling on the polarization from dust self-scattering. The dashed curves show two models with constant turbulence α. The dotted–dashed curves show one model with varying turbulence α. The blue shaded region and the blue dot with a rough error bar represent the constraints from O. M. Guerra-Alvarado et al. (2024) and C. Pinte et al. (2016), respectively.
Paper: Prediction of Time-evolving Radial Magnetic Fields on the Solar Surface Using Deep Learning
Authors: Hyun-Jin Jeong, Stefaan Poedts, Haopeng Wang, Ekatarina Dineva, Panagiotis Gonidakis, Francesco Carella, George Miloshevich, Luis Linan, Harim Lee
Figure caption: Three examples of target data and prediction results from our Model A (blue boxes), Model B (green boxes), the classical SFT model (brown boxes), and the persistence model (gray boxes), for predictions at (a) 1 day, (b) 3 days, and (c) 24 days after 2014 December 17. The right panel of each model output shows the absolute difference map between the predicted and target magnetic fields, where darker regions indicate larger differences. Yellow arrows indicate emerging magnetic flux regions obtained on 2014 December 20, and yellow boxes highlight cases where our models yield results that are more consistent with the target data than those of the other models. The color map and coordinate system of the magnetic field data are the same as in Figure 1.
Paper: Detailed Radial Scale Height Profile of Dust Grains as Probed by Dust Self-scattering in HL Tau
Authors: Haifeng Yang, 海峰 杨, Ian W. Stephens, Zhe-Yu Daniel Lin, Manuel Fernández-López, Zhi-Yun Li, Leslie W. Looney, Rachel Harrison
Figure caption: Panels (a)–(e): the ﹩{Q}^{{\prime} }﹩ in the first ring. Panel (a): the data. Panels (b)–(e): models with H/R = 0.01,  0.05, 0.1, and 0.15, respectively. The white contours represent the four regions for averaging the ﹩{Q}^{{\prime} }﹩. Panel (f): averaged ﹩{Q}^{{\prime} }﹩ at the first ring.
Paper: Detailed Radial Scale Height Profile of Dust Grains as Probed by Dust Self-scattering in HL Tau
Authors: Haifeng Yang, 海峰 杨, Ian W. Stephens, Zhe-Yu Daniel Lin, Manuel Fernández-López, Zhi-Yun Li, Leslie W. Looney, Rachel Harrison
Figure caption: Comparison between our final model and the data. Upper panels: the Stokes ﹩{Q}^{{\prime} }﹩ and ﹩{U}^{{\prime} }﹩ of the model. Note that the inner disk is saturated. Lower panels: the difference between the Stokes parameters of the model and the data. The contours show the ±3σIp contours. All panels share the same colormap, which is shown on the right of the figure. The colormap is the same as the lower panels of Figure 1.
Paper: Prediction of Time-evolving Radial Magnetic Fields on the Solar Surface Using Deep Learning
Authors: Hyun-Jin Jeong, Stefaan Poedts, Haopeng Wang, Ekatarina Dineva, Panagiotis Gonidakis, Francesco Carella, George Miloshevich, Luis Linan, Harim Lee
Figure caption: Comparison of average pixel-to-pixel CC (a) and RMSE (b) for our Models A (blue) and B (green), the classical SFT model (brown), and the persistence model (black), at various prediction times, with a longitudinal resolution of 1°. Vertical error bars represent the standard deviations of the CC and RMSE values.
Paper: Detailed Radial Scale Height Profile of Dust Grains as Probed by Dust Self-scattering in HL Tau
Authors: Haifeng Yang, 海峰 杨, Ian W. Stephens, Zhe-Yu Daniel Lin, Manuel Fernández-López, Zhi-Yun Li, Leslie W. Looney, Rachel Harrison
Figure caption: The difference of ﹩{Q}^{{\prime} }﹩ between the nearside and the farside along the minor axis at each ring. Blue (red) dots represent model (data). The shades from the darkest to the lightest in the right panels represent (1, 2, 3) × σPI, respectively.
Paper: Spectral Hardening Reveals Afterglow Emergence in Long-duration Fast X-Ray Transients: A Case Study of GRB 250404A/EP250404a
Authors: Yi-Han Iris Yin, Yuan Fang, Bin-Bin Zhang, Chen Deng, Jun Yang, Run-Chao Chen, Yuan Liu, Yehao Cheng, Dong Xu, Xiaofeng Wang, Rongfeng Shen, Rui-Zhi Li, Jirong Mao, Wen-Xiong Li, Alberto Javier Castro-Tirado, Weihua Lei, Shao-Yu Fu, Yuan-Pei Yang, Shuai-Qing Jiang, Jie An, Chun Chen, Zhong-Nan Dong, Guowang Du, Ali Esamdin, Zhou Fan, Haicheng Feng, Lu Feng, Emilio Fernández-García, Xing Gao, Maria Gritsevich, Wei-Jian Guo, Jingwei Hu, You-Dong Hu, Yanlong Hua, Abdusamatjan Iskandar, Junjie Jin, Niu Li, Xia Li, Ziwei Li, Jia-Qi Lin, Dezi Liu, Jinzhong Liu, Qichun Liu, Xiaowei Liu, Xing Liu, Daniele B. Malesani, Ignacio Pérez-García, Hui Sun, Xue-Feng Wu, Yun-Ao Xiao, Ding-Rong Xiong, Shengyu Yan, Beibei Zhang, Jinghua Zhang, Haichang Zhu, Zipei Zhu, Hu Zou, Weimin Yuan, Bing Zhang
Figure caption: Left: the observed light curve of EP250404a detected by EP/WXT in the energy range of 0.5–4.0 keV, the observed light curve of GRB 250404A detected by Fermi/GBM in the energy range of 10–1000 keV and the accumulated counts, and the spectral evolution based on the best-fit parameters of the CPL, PL, and SBPL models. The gray block marks the time interval where the source was outside the field of view of the detector. The dashed curve in the WXT light curve indicates a significant slew of the WXT telescope during the main emission phase, during which flux measurements may be affected. The blue dashed vertical lines represent the T90 interval, and the purple dashed vertical lines in the GBM light curve denote T100, with solid (dashed) gray horizontal lines indicating the 0% (5%) and 100% (95%) levels, respectively. The dark blue dashed vertical lines in the FXT (fourth) panel correspond to the time interval where the spectra start to harden and reach a plateau. Right: the evolution of the SEDs. The SEDs are derived from the spectral fittings at different time intervals listed in Tables A1 and A2. All error bars mark the 1σ confidence level.
Paper: Spectral Hardening Reveals Afterglow Emergence in Long-duration Fast X-Ray Transients: A Case Study of GRB 250404A/EP250404a
Authors: Yi-Han Iris Yin, Yuan Fang, Bin-Bin Zhang, Chen Deng, Jun Yang, Run-Chao Chen, Yuan Liu, Yehao Cheng, Dong Xu, Xiaofeng Wang, Rongfeng Shen, Rui-Zhi Li, Jirong Mao, Wen-Xiong Li, Alberto Javier Castro-Tirado, Weihua Lei, Shao-Yu Fu, Yuan-Pei Yang, Shuai-Qing Jiang, Jie An, Chun Chen, Zhong-Nan Dong, Guowang Du, Ali Esamdin, Zhou Fan, Haicheng Feng, Lu Feng, Emilio Fernández-García, Xing Gao, Maria Gritsevich, Wei-Jian Guo, Jingwei Hu, You-Dong Hu, Yanlong Hua, Abdusamatjan Iskandar, Junjie Jin, Niu Li, Xia Li, Ziwei Li, Jia-Qi Lin, Dezi Liu, Jinzhong Liu, Qichun Liu, Xiaowei Liu, Xing Liu, Daniele B. Malesani, Ignacio Pérez-García, Hui Sun, Xue-Feng Wu, Yun-Ao Xiao, Ding-Rong Xiong, Shengyu Yan, Beibei Zhang, Jinghua Zhang, Haichang Zhu, Zipei Zhu, Hu Zou, Weimin Yuan, Bing Zhang
Figure caption: Multiwavelength observations of GRB 250404A/EP250404a and afterglow modeling with the best-fit parameters from the FS+RS model with u-, v-, and g-band correction factors. The multiwavelength data utilized in the afterglow fitting are marked with filled points, while the optical observations on clear filters that are not included in the afterglow fitting are marked with open points. The optical and near-infrared data have been corrected for Galactic extinction, which is E(B − V) = 0.073 mag (E. F. Schlafly & D. P. Finkbeiner 2011). We assume a total to selective extinction ratio of RV = 3.1 according to the extinction law from E. L. Fitzpatrick (1999). The inverted triangle points signify upper limits. The best-fit FS+RS, FS, and RS models are shown with solid, dashed–dotted, and dotted lines, respectively. The dark blue dashed vertical lines correspond to the same time interval where the spectra start to harden and reach a plateau.
Paper: Prediction of Time-evolving Radial Magnetic Fields on the Solar Surface Using Deep Learning
Authors: Hyun-Jin Jeong, Stefaan Poedts, Haopeng Wang, Ekatarina Dineva, Panagiotis Gonidakis, Francesco Carella, George Miloshevich, Luis Linan, Harim Lee
Figure caption: Comparisons of the input, output, and target data from the prediction models starting on 2024 May 7 at 20:00 (red solid vertical line in panel (c)) and ending on June 3 at 14:00. The prediction start time in Figure 5 (2024 May 7 at 02:00) is indicated by the red dashed vertical line in panel (c). The target data in panels (a) and (b) correspond to the same date and time as those in Figures 5(a) and (b). The figure layout is also the same as that in Figure 5.
Paper: Spectral Hardening Reveals Afterglow Emergence in Long-duration Fast X-Ray Transients: A Case Study of GRB 250404A/EP250404a
Authors: Yi-Han Iris Yin, Yuan Fang, Bin-Bin Zhang, Chen Deng, Jun Yang, Run-Chao Chen, Yuan Liu, Yehao Cheng, Dong Xu, Xiaofeng Wang, Rongfeng Shen, Rui-Zhi Li, Jirong Mao, Wen-Xiong Li, Alberto Javier Castro-Tirado, Weihua Lei, Shao-Yu Fu, Yuan-Pei Yang, Shuai-Qing Jiang, Jie An, Chun Chen, Zhong-Nan Dong, Guowang Du, Ali Esamdin, Zhou Fan, Haicheng Feng, Lu Feng, Emilio Fernández-García, Xing Gao, Maria Gritsevich, Wei-Jian Guo, Jingwei Hu, You-Dong Hu, Yanlong Hua, Abdusamatjan Iskandar, Junjie Jin, Niu Li, Xia Li, Ziwei Li, Jia-Qi Lin, Dezi Liu, Jinzhong Liu, Qichun Liu, Xiaowei Liu, Xing Liu, Daniele B. Malesani, Ignacio Pérez-García, Hui Sun, Xue-Feng Wu, Yun-Ao Xiao, Ding-Rong Xiong, Shengyu Yan, Beibei Zhang, Jinghua Zhang, Haichang Zhu, Zipei Zhu, Hu Zou, Weimin Yuan, Bing Zhang
Figure caption: X-ray/optical/near-infrared afterglow specific flux density spectra of GRB 250404A/EP250404a in different time intervals. The best-fit afterglow model is indicated by dashed–dotted gray lines. The red curves correspond to the partial host galaxy extinction curve derived from the best-fit correction factors from the afterglow modeling. For comparison, the yellow, blue, and green curves show the average extinction laws of the MW, SMC, and LMC, respectively, assuming a reddening value of E(B − V) = 0.1 mag.
Paper: Spectral Hardening Reveals Afterglow Emergence in Long-duration Fast X-Ray Transients: A Case Study of GRB 250404A/EP250404a
Authors: Yi-Han Iris Yin, Yuan Fang, Bin-Bin Zhang, Chen Deng, Jun Yang, Run-Chao Chen, Yuan Liu, Yehao Cheng, Dong Xu, Xiaofeng Wang, Rongfeng Shen, Rui-Zhi Li, Jirong Mao, Wen-Xiong Li, Alberto Javier Castro-Tirado, Weihua Lei, Shao-Yu Fu, Yuan-Pei Yang, Shuai-Qing Jiang, Jie An, Chun Chen, Zhong-Nan Dong, Guowang Du, Ali Esamdin, Zhou Fan, Haicheng Feng, Lu Feng, Emilio Fernández-García, Xing Gao, Maria Gritsevich, Wei-Jian Guo, Jingwei Hu, You-Dong Hu, Yanlong Hua, Abdusamatjan Iskandar, Junjie Jin, Niu Li, Xia Li, Ziwei Li, Jia-Qi Lin, Dezi Liu, Jinzhong Liu, Qichun Liu, Xiaowei Liu, Xing Liu, Daniele B. Malesani, Ignacio Pérez-García, Hui Sun, Xue-Feng Wu, Yun-Ao Xiao, Ding-Rong Xiong, Shengyu Yan, Beibei Zhang, Jinghua Zhang, Haichang Zhu, Zipei Zhu, Hu Zou, Weimin Yuan, Bing Zhang
Figure caption: The evolution of spectral index αX and intrinsic absorption column density NH,int. The blue (yellow) points in the upper panel represent the best-fit spectral indices in the time-resolved spectral fittings with fixed (free) NH,int. The yellow points in the lower panels correspond to the best-fit NH,int. The two blue dotted–dashed horizontal lines mark the best-fit intrinsic absorption column density NH,int1 and NH,int2 obtained from time-integrated spectral fittings, respectively. The red dotted–dashed horizontal line denotes the Galactic absorption column density NH,gal. All error bars on data points represent their 1σ confidence level.
Paper: Extending the Short Gamma-Ray Burst Population from Subthreshold Triggers in Fermi/GBM and GECAM Data and Its Implications
Authors: Ce Cai, Shao-Lin Xiong, Yan-Qiu Zhang, Jin-Peng Zhang, Ping Wang, Yao-Guang Zheng, Shi-Jie Zheng, Shuo Xiao, Hao-Xuan Guo, Jia-Cong Liu, Yang-Zhao Ren, Wen-Jun Tan, Chen-Wei Wang, Yue Wang, Sheng-Lun Xie, Wang-Chen Xue, Zheng-Hang Yu, Peng Zhang, Wen-Long Zhang, Chao Zheng, Jia-Wei Luo, Shuai Zhang, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Light curves of a representative burst detected jointly by GBM, GECAM-B, and GECAM-C. The event occurred at T0 = 2023-03-06T16:09:01.44 (UTC). Count rates are shown in 50 ms bins. The shaded region indicates the time bin that maximizes the joint signal significance (approximately 12σ).
Paper: Extending the Short Gamma-Ray Burst Population from Subthreshold Triggers in Fermi/GBM and GECAM Data and Its Implications
Authors: Ce Cai, Shao-Lin Xiong, Yan-Qiu Zhang, Jin-Peng Zhang, Ping Wang, Yao-Guang Zheng, Shi-Jie Zheng, Shuo Xiao, Hao-Xuan Guo, Jia-Cong Liu, Yang-Zhao Ren, Wen-Jun Tan, Chen-Wei Wang, Yue Wang, Sheng-Lun Xie, Wang-Chen Xue, Zheng-Hang Yu, Peng Zhang, Wen-Long Zhang, Chao Zheng, Jia-Wei Luo, Shuai Zhang, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Distribution of the likelihood ratio (LR) for the 49 validated events, separated by GBM reliability score. Events with a reliability score of 5 are shown in yellow, while those with a score of 8 are shown in blue.
Paper: Extending the Short Gamma-Ray Burst Population from Subthreshold Triggers in Fermi/GBM and GECAM Data and Its Implications
Authors: Ce Cai, Shao-Lin Xiong, Yan-Qiu Zhang, Jin-Peng Zhang, Ping Wang, Yao-Guang Zheng, Shi-Jie Zheng, Shuo Xiao, Hao-Xuan Guo, Jia-Cong Liu, Yang-Zhao Ren, Wen-Jun Tan, Chen-Wei Wang, Yue Wang, Sheng-Lun Xie, Wang-Chen Xue, Zheng-Hang Yu, Peng Zhang, Wen-Long Zhang, Chao Zheng, Jia-Wei Luo, Shuai Zhang, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Light curves of a subthreshold burst detected jointly by GBM and GECAM-C. The event occurred at T0 = 2023-02-04T03:06:30.391 (UTC). Count rates are shown with 50 ms bins. The shaded region indicates the time bin that maximizes the joint signal significance (approximately 17σ).
Paper: Extending the Short Gamma-Ray Burst Population from Subthreshold Triggers in Fermi/GBM and GECAM Data and Its Implications
Authors: Ce Cai, Shao-Lin Xiong, Yan-Qiu Zhang, Jin-Peng Zhang, Ping Wang, Yao-Guang Zheng, Shi-Jie Zheng, Shuo Xiao, Hao-Xuan Guo, Jia-Cong Liu, Yang-Zhao Ren, Wen-Jun Tan, Chen-Wei Wang, Yue Wang, Sheng-Lun Xie, Wang-Chen Xue, Zheng-Hang Yu, Peng Zhang, Wen-Long Zhang, Chao Zheng, Jia-Wei Luo, Shuai Zhang, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Light curves of a subthreshold burst detected by GBM and GECAM-B. The event occurred at T0 = 2021-08-22T15:32:13.83 (UTC). Count rates are plotted with 50 ms resolution. The shaded region indicates the time bin that maximizes the joint signal significance (approximately 12σ).
Paper: Extending the Short Gamma-Ray Burst Population from Subthreshold Triggers in Fermi/GBM and GECAM Data and Its Implications
Authors: Ce Cai, Shao-Lin Xiong, Yan-Qiu Zhang, Jin-Peng Zhang, Ping Wang, Yao-Guang Zheng, Shi-Jie Zheng, Shuo Xiao, Hao-Xuan Guo, Jia-Cong Liu, Yang-Zhao Ren, Wen-Jun Tan, Chen-Wei Wang, Yue Wang, Sheng-Lun Xie, Wang-Chen Xue, Zheng-Hang Yu, Peng Zhang, Wen-Long Zhang, Chao Zheng, Jia-Wei Luo, Shuai Zhang, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Distribution of the joint likelihood ratio (LR) values for the 116 candidates exceeding the LR thresholds (marked in gray). The blue bars represent all events exceeding the predefined LR thresholds that were not confirmed by manual inspection, while the orange bars indicate those further confirmed through visual inspection.
Paper: Extending the Short Gamma-Ray Burst Population from Subthreshold Triggers in Fermi/GBM and GECAM Data and Its Implications
Authors: Ce Cai, Shao-Lin Xiong, Yan-Qiu Zhang, Jin-Peng Zhang, Ping Wang, Yao-Guang Zheng, Shi-Jie Zheng, Shuo Xiao, Hao-Xuan Guo, Jia-Cong Liu, Yang-Zhao Ren, Wen-Jun Tan, Chen-Wei Wang, Yue Wang, Sheng-Lun Xie, Wang-Chen Xue, Zheng-Hang Yu, Peng Zhang, Wen-Long Zhang, Chao Zheng, Jia-Wei Luo, Shuai Zhang, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Joint light curves of a subthreshold burst detected on 2022 December 15 at T0 = 08:23:07.50 (UTC). The left panels show the summed counts from all detectors in GBM , GECAM-B, and GECAM-C. The right panels present the optimized light curves, where counts from all detectors are summed with different weight factors. The shaded region indicates the time bin that maximizes the joint signal significance (approximately 10σ).
Paper: Extending the Short Gamma-Ray Burst Population from Subthreshold Triggers in Fermi/GBM and GECAM Data and Its Implications
Authors: Ce Cai, Shao-Lin Xiong, Yan-Qiu Zhang, Jin-Peng Zhang, Ping Wang, Yao-Guang Zheng, Shi-Jie Zheng, Shuo Xiao, Hao-Xuan Guo, Jia-Cong Liu, Yang-Zhao Ren, Wen-Jun Tan, Chen-Wei Wang, Yue Wang, Sheng-Lun Xie, Wang-Chen Xue, Zheng-Hang Yu, Peng Zhang, Wen-Long Zhang, Chao Zheng, Jia-Wei Luo, Shuai Zhang, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Likelihood ratio vs. the time offset (Δt) between the GBM trigger time and the center of the detection window that resulted in the highest signal significance for the burst in our sample. Events are separated by duration: short-duration bursts (<2 s, blue circles) and long-duration bursts (≥2 s, yellow triangles). Error bars represent the width of the detection window.
Paper: Extending the Short Gamma-Ray Burst Population from Subthreshold Triggers in Fermi/GBM and GECAM Data and Its Implications
Authors: Ce Cai, Shao-Lin Xiong, Yan-Qiu Zhang, Jin-Peng Zhang, Ping Wang, Yao-Guang Zheng, Shi-Jie Zheng, Shuo Xiao, Hao-Xuan Guo, Jia-Cong Liu, Yang-Zhao Ren, Wen-Jun Tan, Chen-Wei Wang, Yue Wang, Sheng-Lun Xie, Wang-Chen Xue, Zheng-Hang Yu, Peng Zhang, Wen-Long Zhang, Chao Zheng, Jia-Wei Luo, Shuai Zhang, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Distribution of burst durations for the 49 subthreshold events. Orange bars represent short-duration bursts (<2 s), and blue bars represent long-duration bursts (≥2 s).
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: Diagram illustrating the transit geometry with corresponding morning (blue), evening (red), and combined (gray) limb signals in the transit light curve.
Paper: Discovery of an [Fe/H] ∼ −4.8 Star in Gaia XP Spectra 
Authors: Guilherme Limberg, Vinicius M. Placco, Alexander P. Ji, Yupeng Yao, Anirudh Chiti, Mohammad K. Mardini, Anna Frebel, Silvia Rossi
Figure caption: Upper left: (LZ, Etot); see text for discussion. Upper right: (LX, LY). Gray and yellow dots are distant (≥35 kpc) low-metallicity ([Fe/H] < −2.5) halo stars (G. Limberg et al. 2023), where the latter are presumably associated with the Sagittarius stellar stream (B. D. Johnson et al. 2020). Purple circles are outer-halo extremely metal-poor stars ([Fe/H] < −3) from the MAGIC survey (V. M. Placco et al. 2025). Green diamonds are the LMC (filled) and SMC (empty) based on phase-space information compiled by A. B. Pace (2024; github.com/apace7/local_volume_database). Green dashed lines in (LX, LY) space delineate plausible association with the proposed Magellanic stellar stream (V. Chandra et al. 2023). In both upper panels, GDR3_526285 is represented by the blue square. Bottom left: 200 realizations of GDR3_526285’s orbit (thin blue lines, with mean trajectory as the dotted one) in a time-varying model potential that includes both the Milky Way and the infalling LMC (E. Vasiliev et al. 2021). This panel depicts GDR3_526285’s distance to the LMC (rLMC) as a function of lookback time (backward orbit). Bottom right: on-sky location of GDR3_526285, SMC, and LMC in Galactic coordinates. The distribution of E(B − V) values from the D. J. Schlegel et al. (1998) dust map is displayed as the grayscale background, with darker regions depicting higher reddening. The Magellanic gas stream (D. L. Nidever et al. 2010) is overlaid in transparent green.
Paper: Discovery of an [Fe/H] ∼ −4.8 Star in Gaia XP Spectra 
Authors: Guilherme Limberg, Vinicius M. Placco, Alexander P. Ji, Yupeng Yao, Anirudh Chiti, Mohammad K. Mardini, Anna Frebel, Silvia Rossi
Figure caption: Left: normalized spectra of GDR3_526285. The medium-resolution GMOS spectrum (﹩{ \mathcal R }\sim 1500﹩; see text) is shown in the upper portion of this panel. Red and blue insets highlight spectral features of interest in our high-resolution MIKE spectrum (﹩{ \mathcal R }\sim 35k﹩; Section 2.2), namely Ca II K and H (3920 ≲ λ/Å ≲ 3980) and CH G band (∼4300 Å), respectively. Right: 12 Gyr, α-enhanced Y2 isochrones (S. Yi et al. 2001; P. Demarque et al. 2004) in Teff vs. ﹩{\mathrm{log}}\,g﹩ space at, from right to left, [Fe/H] = −2 (black), −2.5 (yellow), −3 (orange), and −3.5 (green). The inset panel shows the quadratic ﹩{\mathrm{log}}\,g﹩–ξ relation from P. S. Barklem et al. (2005; fit by A. P. Ji et al. 2023, gray line). Star GDR3_526285 is plotted as the blue square.
Paper: Discovery of an [Fe/H] ∼ −4.8 Star in Gaia XP Spectra 
Authors: Guilherme Limberg, Vinicius M. Placco, Alexander P. Ji, Yupeng Yao, Anirudh Chiti, Mohammad K. Mardini, Anna Frebel, Silvia Rossi
Figure caption: Top panel: MIKE spectrum of GDR3_526285 around the CH G band (blue squares); 4300 ≤ λ/Å ≤ 4316. Our final A(C) = 4.11 upper limit is represented by the solid magenta line. The difference between our A(C) upper limit and the no-carbon case is shown as the red region within magenta and black lines. Panels (a), (b), (c), and (d) illustrate different λ windows used in our χ2 minimization method to derive the carbon-abundance upper limit (Section 3.2). Bottom panels: key elemental abundance ratios that characterize UMP stars: A(C)cor, [C/Fe]cor, [Mg/Fe], and [Ca/Fe] as a function of [Fe/H], where the subscript “cor” indicates carbon abundances with applied evolutionary corrections (V. M. Placco et al. 2014). Small dots are non-UMP stars ([Fe/H] > −4) compiled from the SAGA database and JINAbase (T. Suda et al. 2008; A. Abohalima & A. Frebel 2018), while the UMP stars are shown with larger circles. Symbols are colored according to stellar [C/Fe] ratios: subsolar in gray, 0 ≤ [C/Fe] < +0.7 in black, and CEMP stars in red. Upper/lower limits are plotted with arrows. In the carbon-abundance panels on the left, the red dashed lines mark this [C/Fe] = +0.7 boundary for CEMP classification. Black dashed lines denote solar levels in all panels. GDR3_526285 is the blue square (Table 2).
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: The scale height normalized 1D forward model grid for morning and evening limbs, as shown in the top left panel of Figure 8. The plotted spectra sample the temperature range by every 100 K from 700 to 1900 K.