HiFAST: an HI data calibration and imaging pipeline for FAST
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2024
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| author | Jing, Yingjie Wang, Jie Xu, Chen Liu, Ziming Chen, Qingze Liang, Tiantian Xu, Jinlong Cao, Yixian Wang, Jing Hu, Huijie Zhang, Chuan-Peng Guo, Qi Gao, Liang Ai, Mei Gan, Hengqian Gao, Xuyang Han, Jinlin Hou, Ligang Hou, Zhipeng Jiang, Peng Kong, Xu Li, Fujia Liu, Zerui Shao, Li Pan, Hengxing Pan, Jun Qian, Lei Sun, Jinghai Tang, Ningyu Yang, Qingliang Zhang, Bo Zhang, Zhiyu Zhu, Ming |
| author_facet | Jing, Yingjie Wang, Jie Xu, Chen Liu, Ziming Chen, Qingze Liang, Tiantian Xu, Jinlong Cao, Yixian Wang, Jing Hu, Huijie Zhang, Chuan-Peng Guo, Qi Gao, Liang Ai, Mei Gan, Hengqian Gao, Xuyang Han, Jinlin Hou, Ligang Hou, Zhipeng Jiang, Peng Kong, Xu Li, Fujia Liu, Zerui Shao, Li Pan, Hengxing Pan, Jun Qian, Lei Sun, Jinghai Tang, Ningyu Yang, Qingliang Zhang, Bo Zhang, Zhiyu Zhu, Ming |
| contents | The Five-hundred-meter Aperture Spherical radio Telescope (FAST) has the largest aperture and a 19-beam L-band receiver, making it powerful for investigating the neutral hydrogen atomic gas (HI) in the universe. We present HiFAST (https://hifast.readthedocs.io), a dedicated, modular, and self-contained calibration and imaging pipeline for processing the HI data of FAST. The pipeline consists of frequency-dependent noise diode calibration, baseline fitting, standing wave removal using an FFT-based method, flux density calibration, stray radiation correction, and gridding to produce data cubes. These modules can be combined as needed to process the data from most FAST observation modes: tracking, drift scanning, On-The-Fly mapping, and most of their variants. With HiFAST, the RMS noises of the calibrated spectra from all 19 beams were only slightly (~ 5%) higher than the theoretical expectation. The results for the extended source M33 and the point sources are consistent with the results from Arecibo. The moment maps (0,1 and 2) of M33 agree well with the results from the Arecibo Galaxy Environment Survey (AGES) with a fractional difference of less than 10%. For a common sample of 221 sources with signal-to-noise ratio S/N >10 from the Arecibo Legacy Fast ALFA (ALFALFA) survey, the mean value of fractional difference in the integrated flux density, $S_{\mathrm{int}}$, between the two datasets is approximately 0.005 %, with a dispersion of 15.4%. Further checks on the integrated flux density of 23 sources with seven observations indicate that the variance in the flux density of the source with luminous objects ($S_\mathrm{int}$ $ > 2.5$ Jy km s$^{-1}$) is less than 5%. Our tests suggest that the FAST telescope, with the efficient, precise, and user-friendly pipeline HiFAST, will yield numerous significant scientific findings in the investigation of the HI in the universe. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_17364 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | HiFAST: an HI data calibration and imaging pipeline for FAST Jing, Yingjie Wang, Jie Xu, Chen Liu, Ziming Chen, Qingze Liang, Tiantian Xu, Jinlong Cao, Yixian Wang, Jing Hu, Huijie Zhang, Chuan-Peng Guo, Qi Gao, Liang Ai, Mei Gan, Hengqian Gao, Xuyang Han, Jinlin Hou, Ligang Hou, Zhipeng Jiang, Peng Kong, Xu Li, Fujia Liu, Zerui Shao, Li Pan, Hengxing Pan, Jun Qian, Lei Sun, Jinghai Tang, Ningyu Yang, Qingliang Zhang, Bo Zhang, Zhiyu Zhu, Ming Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics Instrumentation and Methods for Astrophysics The Five-hundred-meter Aperture Spherical radio Telescope (FAST) has the largest aperture and a 19-beam L-band receiver, making it powerful for investigating the neutral hydrogen atomic gas (HI) in the universe. We present HiFAST (https://hifast.readthedocs.io), a dedicated, modular, and self-contained calibration and imaging pipeline for processing the HI data of FAST. The pipeline consists of frequency-dependent noise diode calibration, baseline fitting, standing wave removal using an FFT-based method, flux density calibration, stray radiation correction, and gridding to produce data cubes. These modules can be combined as needed to process the data from most FAST observation modes: tracking, drift scanning, On-The-Fly mapping, and most of their variants. With HiFAST, the RMS noises of the calibrated spectra from all 19 beams were only slightly (~ 5%) higher than the theoretical expectation. The results for the extended source M33 and the point sources are consistent with the results from Arecibo. The moment maps (0,1 and 2) of M33 agree well with the results from the Arecibo Galaxy Environment Survey (AGES) with a fractional difference of less than 10%. For a common sample of 221 sources with signal-to-noise ratio S/N >10 from the Arecibo Legacy Fast ALFA (ALFALFA) survey, the mean value of fractional difference in the integrated flux density, $S_{\mathrm{int}}$, between the two datasets is approximately 0.005 %, with a dispersion of 15.4%. Further checks on the integrated flux density of 23 sources with seven observations indicate that the variance in the flux density of the source with luminous objects ($S_\mathrm{int}$ $ > 2.5$ Jy km s$^{-1}$) is less than 5%. Our tests suggest that the FAST telescope, with the efficient, precise, and user-friendly pipeline HiFAST, will yield numerous significant scientific findings in the investigation of the HI in the universe. |
| title | HiFAST: an HI data calibration and imaging pipeline for FAST |
| topic | Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2401.17364 |