adsabs/AstroCLIMB huggingface dataset:
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: A plot of the balloon altitude as a function of time for the 2023 FB2 flight. Dashed horizontal lines show the nominal and minimum altitude requirements for FB2 observations at 138,000 and 105,000 feet, respectively. Dashed vertical lines show the onset of night hours and the minimum flight requirement for night observation time. The shaded region shows the combined altitude and time minimum requirement for the FB2 science observation window.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: The FB2 gondola suspended from a mobile crane for a preflight on-sky pointing test. The gondola is lifted off the ground and allowed to move freely under the rotator connected to the crane with lifting straps. The gondola doors are open to allow light into the telescope, and the instrument and support systems are installed in the instrument bay.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: The back surface of the FB2 1 m primary mirror. Pairs of bond pads are visible arrayed around the surface, with two damaged areas indicated in the boxed regions.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: A cross-sectional CAD rendering of the FB2 calibration system cap from J. S. Li et al. (2024), which delivers the UV calibration sources to the instrument. Eight fibers illuminate the reflective underside of an actuatable shutter, which then scatters the light into the instrument.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: Notional FB2 2023 flight plan. The altitude and air mass of each target field throughout the evening is shown, with the bolded part of each track representing the time that the field is observed in the FB2 flight planning. The elevation limit of the gondola is added using transparency.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: A comparison of the balloon flight altitude as a function of time for the 2023 FB2 flight (solid curve) and 2018 FB2 flight (dashed curve). The FB2 precampaign nominal and minimum float altitudes are plotted as horizontal dashed lines.
Paper: Exoplanets in the Antarctic Sky. V. The Second Data Release of AST3-II/CHESPA and Newly Found Variables within the Southern Continuous Viewing Zone of TESS
Authors: Bixuan Zhao, 碧轩 赵, Hui Zhang, 辉 张, Michael C. B. Ashley, Jiapeng Zhu, Huigen Liu, Zhouyi Yu, Dan Zhou, Bin Ma, Jeremy Mould, Robert A Wittenmyer, Xiangyan Yuan, Zhengyang Li, Xiaoyan Li, Jianning Fu, Jilin Zhou, Lifan Wang
Figure caption: Model fitting to the EMI pulses. (a) The overscan region is not exposed to light and contains only bias, dark noise, and EMI stripes. (b) Flux of each row within the small part of the overscan region. The EMI stripes can be decomposed into chains of EMI pulses with various amplitudes, intervals, and frequencies. (c) EMI pulses can be fitted by a complicated model.
Paper: Exoplanets in the Antarctic Sky. V. The Second Data Release of AST3-II/CHESPA and Newly Found Variables within the Southern Continuous Viewing Zone of TESS
Authors: Bixuan Zhao, 碧轩 赵, Hui Zhang, 辉 张, Michael C. B. Ashley, Jiapeng Zhu, Huigen Liu, Zhouyi Yu, Dan Zhou, Bin Ma, Jeremy Mould, Robert A Wittenmyer, Xiangyan Yuan, Zhengyang Li, Xiaoyan Li, Jianning Fu, Jilin Zhou, Lifan Wang
Figure caption: Steps to remove the EMI stripes. (a) A small part of the first readout channel with obvious EMI stripes and stars. (b) A binary map of all stars identified and marked. (c) EMI stripe pattern extracted from the median combination of 16 star-masked channels. (d) The same part image of panel (a), with the EMI stripe pattern subtracted.
Paper: Exoplanets in the Antarctic Sky. V. The Second Data Release of AST3-II/CHESPA and Newly Found Variables within the Southern Continuous Viewing Zone of TESS
Authors: Bixuan Zhao, 碧轩 赵, Hui Zhang, 辉 张, Michael C. B. Ashley, Jiapeng Zhu, Huigen Liu, Zhouyi Yu, Dan Zhou, Bin Ma, Jeremy Mould, Robert A Wittenmyer, Xiangyan Yuan, Zhengyang Li, Xiaoyan Li, Jianning Fu, Jilin Zhou, Lifan Wang
Figure caption: Light-curve rms vs. magnitude of stars from DR2. Light-curve rms is expressed in relative flux units. Each point represents the overall rms of a detrended light curve spanning the entire observation campaign.
Paper: Exoplanets in the Antarctic Sky. V. The Second Data Release of AST3-II/CHESPA and Newly Found Variables within the Southern Continuous Viewing Zone of TESS
Authors: Bixuan Zhao, 碧轩 赵, Hui Zhang, 辉 张, Michael C. B. Ashley, Jiapeng Zhu, Huigen Liu, Zhouyi Yu, Dan Zhou, Bin Ma, Jeremy Mould, Robert A Wittenmyer, Xiangyan Yuan, Zhengyang Li, Xiaoyan Li, Jianning Fu, Jilin Zhou, Lifan Wang
Figure caption: Statistics of the image quality parameters. Images within the shadowed regions were dropped to maintain high data quality.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Top panel: the distribution of half of the BHB stars in GCs in the ﹩{M}_{g}^{{\rm{dis}}}﹩ vs. (g − i)0 plane with a color-coded [Fe/H]. (The [Fe/H] is sourced from W. E. Harris 1996.) The colored lines are four different [Fe/H] fitted to the points using Equation (3). The black line is the linear model fitted to the points (Equation (4)). Bottom panel: the residuals of the calculated first-order 2D polynomial fitting results (pink triangles) and linear model fitting results (gray dots).
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Top panel: the distribution of stars of the parent sample in (u − v)0 vs. (g − i)0 plane. Bottom panel: this panel magnifies the green box (0.8 ≤ (u − v)0 ≤ 1.9 and −0.50 ≤ (g − i)0 ≤ −0.08) of the top panel to show the distinct difference in the distribution of BHB and BS. Orange and blue dots represent BS stars and BHB stars, which come from X. X. Xue et al. (2008) and X.-X. Xue et al. (2011), respectively.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Top panel: BHB stars in NGC 5139 (Δα and Δδ represent the relative positions of these stars to the cluster center taken from W. E. Harris 1996, 2010 revision). The black cross marks the center coordinates of the NGC 5139, and the brown ring denotes its 15rh (rh is the half-light radius of GC). Bottom panel: proper motion distribution of BHB stars in NGC 5139. The black cross marks the μα* and μδ of the NGC 5139, and the brown ring denotes its 8σ in proper motion. The gray dots represent the distribution of field stars.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: The distribution of (u − v)0 of stars with ∣b∣ > 65∘. The blue and orange lines represent the Gaussian distribution of BHB and BS stars, respectively. The black lines are the sum of two Gaussian distributions. The red dashed lines represent the intersection of two Gaussians distributions, delineating the boundary between the BHB and BS stars.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: The completeness (top panel) and purity (bottom panel) of BHB stars as a function of stellar color (g − i)0. The hollow symbols represent the X.-X. Xue et al. (2011) samples, and the dots are our samples. In each panel, different colors represent different ∣b∣ intervals, with darker colors indicating higher ∣b∣.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: The comparison of ﹩{M}_{g}^{{\rm{dis}}}﹩ obtained using GC distances and ﹩{M}_{g}^{{\rm{fit}}}﹩, which is obtained by the relationship between (g − i)0 and the g-band absolute magnitude (Equation (4)).
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: The network architecture of the DBCTNet. DwConv denotes depth-wise convolution, while W-attention represents window self-attention. GAB stands for global attention block, and projection refers to the projection operation. Channel interaction and spatial interaction are used to realize information fusion between branches. In the parallel branches, relationships captured both within and across windows are concatenated and then sent to the feed-forward network (FFN). Additionally, GAP indicates global average pooling.
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: The basic architecture of an SR model based on GANs. We could select or design “Basic Blocks” (e.g., residual block (K. He et al. 2016), residual-in-residual dense block (X. Wang et al. 2018), and residual Swin Transformer block (J. Liang et al. 2021) for better performance. “Conv” refers to the convolutional layer.
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: Randomly drawn objects. The top row is the SDSS images and the bottom row is GC DR1 images for the same objects.
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: The loss function curves during two training stages. (a) The L1 loss of the first stage. (b) The generator total loss and the discriminator real and fake losses of the second stage.
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: Examples of galaxy images from each of the four classes in the interacting galaxy classification data set.
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: Visual comparison for SR results (×2) of different models in the first stage.
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: Visual comparison for SR results (×2) of different models in the second stage.
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: Illustration of the difference between the SR images and the HR images. From left to right are the absolute residual maps of GAN-based SR models (Real-ESRGAN, SwinIR, HAT, EDAT, and DBCTGAN) reconstruction images and HR images.
Paper: Astronomical Image Superresolution Reconstruction with Deep Learning for Better Identification of Interacting Galaxies
Authors: Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao
Figure caption: The evaluation metrics calculated on the test samples as a function of iterations. (a) The first training stage and (b) the second training stage.
Paper: A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. I. The “Winged” Radio Galaxies
Authors: Soumen Kumar Bera, Taotao Fang, Tapan K. Sasmal, M. Kunert-Bajraszewska, Xuelei Chen, Soumen Mondal
Figure caption: Distribution of radio power vs. redshift at 144 MHz (left panel) and 1.4 GHz (right panel) for the newly identified winged sources and the FIRST sample. The curved lines represent the fitted power trends for XRGs (violet line), ZRGs (green line), and the FIRST sample (orange line). Horizontal lines indicate the median or mean power values (as described in the text) for FR I sources (blue dashed–dotted line) and FR II sources (red dashed line).
Paper: A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. I. The “Winged” Radio Galaxies
Authors: Soumen Kumar Bera, Taotao Fang, Tapan K. Sasmal, M. Kunert-Bajraszewska, Xuelei Chen, Soumen Mondal
Figure caption: Spectral index distribution of the newly identified winged radio sources (left panel) and the FIRST and LoTSS samples (right panel). The vertical red dashed line (α = –0.50) marks the boundary between steep spectra (left of the line) and flat spectra (right of the line). The bin size for both plots is set to 0.1.
Paper: A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. I. The “Winged” Radio Galaxies
Authors: Soumen Kumar Bera, Taotao Fang, Tapan K. Sasmal, M. Kunert-Bajraszewska, Xuelei Chen, Soumen Mondal
Figure caption: The FR classification of newly identified winged sources, divided into XRGs and ZRGs (left panel), along with the FR classification of winged sources from the FIRST and LoTSS samples (right panel).
Paper: A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. I. The “Winged” Radio Galaxies
Authors: Soumen Kumar Bera, Taotao Fang, Tapan K. Sasmal, M. Kunert-Bajraszewska, Xuelei Chen, Soumen Mondal
Figure caption: Distribution of linear sizes among the identified winged sources and candidates. The vertical red dashed line at 0.7 Mpc marks the threshold for GRG candidates, which are located to the right of this line. The bin size is set to 0.1 Mpc.
Paper: A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. I. The “Winged” Radio Galaxies
Authors: Soumen Kumar Bera, Taotao Fang, Tapan K. Sasmal, M. Kunert-Bajraszewska, Xuelei Chen, Soumen Mondal
Figure caption: Example sets of three XRG (top), ZRG (middle), and WRG candidates (bottom) from our identification. The LOFAR full-resolution 6″ radio images are displayed. Radio contours, plotted in ﹩\sqrt{2}﹩ intervals, are overlaid on SDSS r-band images shown in color scale. The contours start at three times (or more) their respective Isl_rms, increasing by a factor of 2. A star marks the optical host position, while a circle indicates the radio position when optical information is unavailable.
Paper: A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. I. The “Winged” Radio Galaxies
Authors: Soumen Kumar Bera, Taotao Fang, Tapan K. Sasmal, M. Kunert-Bajraszewska, Xuelei Chen, Soumen Mondal
Figure caption: Examples of radio images of sources classified as (from left to right): FR I (J0908+5342), FR II (J0959+4146), and those for which no classification was made (J0830+5532).
Paper: A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. I. The “Winged” Radio Galaxies
Authors: Soumen Kumar Bera, Taotao Fang, Tapan K. Sasmal, M. Kunert-Bajraszewska, Xuelei Chen, Soumen Mondal
Figure caption: Radio power distribution at 1.4 GHz for winged sources from FIRST and LoTSS samples. The bin size is set to 0.5.
Paper: SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy
Authors: Haopeng Wang, Liping Yang, Stefaan Poedts, Andrea Lani, Yuhao Zhou, Yuhang Gao, Luis Linan, Jiakun Lv, Tinatin Baratashvili, Jinhan Guo, Rong Lin, Zhan Su, Caixia Li, Man Zhang, Wenwen Wei, Yun Yang, Yucong Li, Xinyi Ma, Edin Husidic, Hyun-Jin Jeong, Mahdi Najafi-Ziyazi, Juan Wang, Brigitte Schmieder
Figure caption: Synoptic maps of the EUV observations from the 193 Å channel of AIA on board SDO (top) for CRs 2110 (left) and 2111 (right), alongside the distributions of open- and closed-field regions modeled by the time-evolving SIP-IFVM coronal model (middle and bottom), all shown in a corotating coordinate system. In the middle and bottom panels, the white and black patches represent open-field regions with magnetic field lines pointing outward and inward relative to the Sun, respectively, while the gray patches indicate closed-field regions.
Paper: SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy
Authors: Haopeng Wang, Liping Yang, Stefaan Poedts, Andrea Lani, Yuhao Zhou, Yuhang Gao, Luis Linan, Jiakun Lv, Tinatin Baratashvili, Jinhan Guo, Rong Lin, Zhan Su, Caixia Li, Man Zhang, Wenwen Wei, Yun Yang, Yucong Li, Xinyi Ma, Edin Husidic, Hyun-Jin Jeong, Mahdi Najafi-Ziyazi, Juan Wang, Brigitte Schmieder
Figure caption: Evolution of physical time vs. computational time in the time-evolving coronal simulation for CRs 2110 and 2111 (left), with close-up views of the profile during the first 1.2 hr (middle) and between 10.24 and 10.65 hr of computational time (right).
Paper: SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy
Authors: Haopeng Wang, Liping Yang, Stefaan Poedts, Andrea Lani, Yuhao Zhou, Yuhang Gao, Luis Linan, Jiakun Lv, Tinatin Baratashvili, Jinhan Guo, Rong Lin, Zhan Su, Caixia Li, Man Zhang, Wenwen Wei, Yun Yang, Yucong Li, Xinyi Ma, Edin Husidic, Hyun-Jin Jeong, Mahdi Najafi-Ziyazi, Juan Wang, Brigitte Schmieder
Figure caption: Synoptic maps of the EUV images derived from the time-evolving simulation results at four different moments.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Top left panel: the log g distribution of BHB. Top right panel: the log g distribution of BS. Bottom panel: simulations of the real distributions of BHB and BS stars in the (NUV − u)0 vs. (g − i)0 plane.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Similar to Figure 2 but for the stars with 55∘ < ∣b∣ < 65∘.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Sensitivity of color to log g of stars from CSST photometry in the (NUV − u)0 vs. (g − i)0 plane, color coded by log g, as shown by the right color bar. The values of log g range from 2 to 5 dex.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Top panel: the Galactic sky coverage of our BHB sample in the celestial equator coordinate system. Bottom panel: the spatial distribution of our BHB samples in the R–Z plane.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: The distribution of apparent magnitudes for BHB of this work (blue), X.-X. Xue et al. (2011; green), and J. Ju et al. (2024; pink).