adsabs/AstroCLIMB huggingface dataset:
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: NIRCam color composite of WLM. F090W was used as the blue channel, F150W as the green, and a combination of the two LW filters (F250M and F430M) as the red channel. The red and orange boxes highlight the a young star-forming complex (red) and a more typical region (orange) in WLM. The blue box shows the presence of member stars as well as several background galaxies. The central black bar is the intermodule gap, over which we opted not to dither.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: Comparisons between the photon-noise-based S/Ns from the DOLPHOT F090W and F150W photometry of M92 (gray shaded region) and the expected S/Ns from v2.0 of the NIRCam ETC (black lines). Over most of the dynamic ranges in magnitude the S/Ns reported by DOLPHOT and the ETC are consistent within the scatter (∼20%) of the data. Deviations at the bright end may be due to the presence of saturated pixels, while PSF shape, nonstellar objects (e.g., background galaxies), and incompleteness may contribute to a slight increase in the ratio at the faintest F150W magnitudes.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: Select NIRCam CMDs of WLM along with the deepest available HST/ACS optical CMD from Albers et al. (2019). Overplotted are isochrones from the PARSEC solar-scaled stellar models at a fixed metallicity of [Fe/H] = −1.2 dex for a variety of indicated ages. Panel (a) is the deepest CMD of an isolated dwarf galaxy to date, extending ∼1.5 mag below the oldest MSTO; it is deeper than the HST CMD despite ∼7000 s less integration time. The isochrones indicate the variety of stellar ages present in WLM. The LW CMD shown in panel (d) extends ∼2 mag below the red clump. Such deep CMDs show that JWST will provide for a variety of science at different cosmic epochs including exquisite lifetime SFHs, the study of evolved red stars, TRGB distances, and very young stars in galaxies outside the LG.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: Select NIRCam CMDs of Draco II along with the deepest optical CMD which is based on HST/ACS imaging (GO-14734; panel (b)). Overplotted are PARSEC stellar models at a fixed age (13 Gyr) for the same [Fe/H] values selected for M92. The SW CMD extends to the lowest-mass stellar model (M = 0.09 M ⊙), making it the deepest CMD of an MW satellite galaxy to date. The exquisite depth of our data indicates how JWST enables a variety of science, including constraining the low-mass IMF and quantifying low-mass star features (e.g,. the MS kink and objects near the hydrogen-burning limit) outside the MW.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: Peculiar motions of the YOCs (left) and O–B2-type stars (right) in the Galactic plane. The parallax uncertainties are smaller than 20% and the radial velocity uncertainties are smaller than 10 km s−1. The solid curved lines trace the centers of the spiral arms: from top to bottom are the Perseus, Local, and Carina Arms, respectively (Xu et al. 2023). The shadows and dashed lines are the 1σ and 2σ widths from the center of the spiral arms, respectively. The Sun (black Sun symbol) is at (0, 8.15) kpc (Reid et al. 2019). A 50 km s−1 scale vector is shown in the lower-left corner.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: Peculiar motions of the O (left) and B0–B2 (right) stars in Galactic plane. The others features are the same as in Figure 1.
Paper: Toward Model Compression for a Deep Learning–Based Solar Flare Forecast on Satellites
Authors: Kai Feng, Long Xu, Dong Zhao, Sixuan Liu, Xin Huang
Figure caption: ROC curves of the original ResNet18 quantized to 8-bit, 7-bit, 6-bit, 5-bit, and 4-bit.
Paper: Toward Model Compression for a Deep Learning–Based Solar Flare Forecast on Satellites
Authors: Kai Feng, Long Xu, Dong Zhao, Sixuan Liu, Xin Huang
Figure caption: Comparison of the ROC curves with and without fine-tuning after pruning.
Paper: Toward Model Compression for a Deep Learning–Based Solar Flare Forecast on Satellites
Authors: Kai Feng, Long Xu, Dong Zhao, Sixuan Liu, Xin Huang
Figure caption: The flow chart of model compression for solar flare forecast. The assembled compression model consists of a knowledge distillation, a pruning and a quantization module, compressing a pretraining deep-learning model progressively.
Paper: Toward Model Compression for a Deep Learning–Based Solar Flare Forecast on Satellites
Authors: Kai Feng, Long Xu, Dong Zhao, Sixuan Liu, Xin Huang
Figure caption: The pipeline of quantization.
Paper: Toward Model Compression for a Deep Learning–Based Solar Flare Forecast on Satellites
Authors: Kai Feng, Long Xu, Dong Zhao, Sixuan Liu, Xin Huang
Figure caption: The architecture of knowledge distillation.
Paper: Toward Model Compression for a Deep Learning–Based Solar Flare Forecast on Satellites
Authors: Kai Feng, Long Xu, Dong Zhao, Sixuan Liu, Xin Huang
Figure caption: The framework of pruning.
Paper: Toward Model Compression for a Deep Learning–Based Solar Flare Forecast on Satellites
Authors: Kai Feng, Long Xu, Dong Zhao, Sixuan Liu, Xin Huang
Figure caption: Visualization of saliency maps with almost the same region of interest. The first row gives the input magnetogram; the second and third rows provide saliency maps for the compressed and original models respectively; the highlighted regions are the region of interest that is highly relevant to solar flare forecasting.
Paper: Toward Model Compression for a Deep Learning–Based Solar Flare Forecast on Satellites
Authors: Kai Feng, Long Xu, Dong Zhao, Sixuan Liu, Xin Huang
Figure caption: ROC curves of the assembled compression framework (“KD” represents knowledge distillation).
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity maps of 3C 58, integrated over velocity ranges of −40 to −30 km s−1 (left) and −2.0 to +1.0 km s−1 (right). Minimum values of 12CO emission intensity shown in colorbars are at 3σ confidence level. Red tiny stars denote locations of broad lines at −2.5 km s−1 identified by full criteria. Red dashed circles denote the extent of the PWN. The black solid circle in the right panel delineates the CO shell, and black dashed ellipses delineate the H I bipolar shell found by Wallace et al. (1994).
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity maps of PWN candidate G32.64+0.53, at the +11.0 km s−1 velocity channel (left) and integrated over the velocity range of +88.9 to +101.8 km s−1 (right). Minimum values of 12CO emission intensity shown in colorbars are at 5σ confidence level. Red tiny stars denote locations of broad lines identified by full criteria. Red dashed circles denote the extent of the PWN. Black solid circles delineate the cavity edge (left) and the surrounding shell (right). The average 12CO (J = 1–0) spectrum of broad line emission from the surrounding shell is shown in the upper right corner of the right panel.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity map of PWN Eel, integrated over the velocity range of +6.0 to +20.8 km s−1. The minimum value of 12CO emission intensity shown in the colorbar is at 5σ level. Red tiny stars denote locations of broad lines identified by full criteria. The extent of the PWN is denoted by a red dashed circle. Two shell-like structures are sketched by two black dotted lines. The average 12CO (J = 1–0) spectrum of three broad line points on the western shell-like structure is shown in the upper right corner.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity maps of PWN CTB 87, at −55.9 km s−1 (left) and +5.4 km s−1 (right) velocity channels. Minimum values of 12CO emission intensity shown in colorbars are at 5σ confidence level. Red dashed circles denote the extent of the PWN. Black solid circles delineate the surrounding shell-like (left) and cavity-like (right) structures.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity maps of PWN candidate G36.01+0.06, at +34.9 km s−1 (left) and +51.7 km s−1 (right) velocity channels. Minimum values of 12CO emission intensity shown in colorbars are at 5σ confidence level. Red dashed circles denote the extent of the PWN. Black solid circles delineate edges of surrounding MCs.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity map of the Crab, at the +3.2 km s−1 velocity channel. The minimum value of 12CO emission intensity shown in the colorbar is at 5σ level. The extent of the PWN is denoted by a red dashed circle. The black solid circle delineates the diffuse shell-like structure.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity map of PWN candidate G63.7+1.1, at the +4.0 km s−1 velocity channel. The minimum value of 12CO emission intensity shown in the colorbar is at 5σ level. The extent of the PWN is denoted by a red dashed circle. Black solid circles delineate surrounding shell-like structures, with radii of 0.°74 and 1.°45.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity map of the Geminga, at the −10.8 km s−1 velocity channel. The minimum value of 12CO emission intensity as shown in the colorbar is at 3σ level. The extent of the PWN is denoted by a red dashed circle. The black solid circle delineates the shell-like structure.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The sky coverage for SAGES in the u  s /v  s  passband is shown on the top panel. About 87.8% of the fields in total have been observed for SAGES in both passbands, which uses the Bok 2.3 m telescope. For the gri passbands (which are shown in the bottom panel), we have finished the observations for the designed area with the NOWT, which can be combined with the SDSS data for the brighter part of the catalog. The gri-band data of NOWT will be released in subsequent papers.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The magnitude distribution of the SAGES u  s  and v  s  bands for all of the sources of the SAGES catalog in all observed fields, even including the sources fainter than the “limiting magnitude.” The y-axis represents the counts for the photometry magnitude number. It can be seen that the peaks are u  s  ∼ 21 mag and v  s  ∼ 20.5 mag for our SAGES photometry.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The photometry uncertainties (from Poisson statistics) vs. magnitude in the SAGES project in the u  s  band (top) and v  s  band (bottom) for a typical field. The limiting magnitude is ∼17 mag for both the u  s  band and the v  s  band of SAGES, with uncertainties of 0.01 mag, which corresponds to S/N ∼ 100.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The precision of astrometry in the SAGES project in the u  s  band (top) and v  s  band (bottom) for one typical image is shown. The external astrometric errors are estimated by comparing the difference between the coordinates from our catalog and those from reference catalog PPMX.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The observing area distribution of limiting magnitude in the SAGES u  s  passband for all fields for S/N = 100, corresponding to a photometry error of 0.01 mag.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The airmass distribution for SAGES observations, with a median value of 1.10. Clearly for most of the fields, the airmass is less than 1.2, which can ensure the quality of our images. This aspect has been incorporated in our survey strategy.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The color–magnitude of the M67 cluster with SAGES and Gaia DR2 photometry. The red dots are the giants, and the black dots are the dwarfs. The giants and dwarfs can be well separated in the color–color diagram (bottom right).
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: Shown here is the flow chart of the SIP for SAGES astrometry after two runs of SCAMP. In our work, we applied the pipeline based on SCAMP and our routine SIP.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The flow chart of photometric pipeline for SAGES data reduction.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The distribution of the complete magnitude (which is defined as the turnover in the magnitude histogram) of the SAGES u  s  passband for all fields, with a median value of u  s  = 20.4 mag.