| Title | Mapping the emission line strengths and kinematics of supernova remnant S147 with extensive LAMOST spectroscopic observations |
| Authors | Ren, Juan-Juan Liu, Xiao-Wei Chen, Bing-Qiu Xiang, Mao-Sheng Yuan, Hai-Bo Huang, Yang Zhang, Hua-Wei Wang, Chun Tian, Zhi-Jia Liu, Gao-Chao Wu, Hong |
| Affiliation | Peking Univ, Dept Astron, Beijing 100871, Peoples R China. Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100101, Peoples R China. Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China. Yunnan Univ, South Western Inst Astron Res, Kunming 650091, Yunnan, Peoples R China. China Three Gorges Univ, Coll Sci, Yichang 443002, Peoples R China. Peking Univ, Dept Astron, Beijing 100871, Peoples R China. Ren, JJ (reprint author), Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100101, Peoples R China. |
| Keywords | ISM: supernova remnants ISM: kinematics and dynamics ISM: general NOVA REMNANTS DATA RELEASE GALACTIC ANTICENTRE ABUNDANCE GRADIENT OPTICAL-EMISSION SKY SURVEY EXTINCTION CALIBRATION CATALOG CLOUD |
| Issue Date | 2018 |
| Publisher | RESEARCH IN ASTRONOMY AND ASTROPHYSICS |
| Citation | RESEARCH IN ASTRONOMY AND ASTROPHYSICS. 2018, 18(9). |
| Abstract | We present extensive spectroscopic observations of supernova remnant (SNR) S147 collected with the Large sky AreaMulti-Object fiber Spectroscopic Telescope (LAMOST). The spectra were carefully sky-subtracted taking into account the complex filamentary structure of S147. We have utilized all available LAMOST spectra toward S147, including sky and stellar spectra. By measuring the prominent optical emission lines including H alpha, [N II] lambda 6584 and [S II] lambda lambda 6717, 6731, we present maps of radial velocity and line intensity ratio covering the whole nebula of S147 with unprecedented detail. The maps spatially correlate well with the complex filamentary structure of S147. For the central 2 degrees of S147, the radial velocity varies from -100 to 100 km s(-1) and has peaks between similar to 0 and 10 km s(-1). The intensity ratios of H alpha/[S II] lambda lambda 6717, 6731, [S II] lambda 6717/lambda 6731 and H alpha/[NII] lambda 6584 peak at about 0.77, 1.35 and 1.48, respectively, with a scatter of 0.17, 0.19 and 0.37, respectively. The intensity ratios are consistent with the literature values. However, the range of variations of line intensity ratios estimated here, which are representative of the whole nebula, is larger than previously estimated. |
| URI | http://hdl.handle.net/20.500.11897/522988 |
| ISSN | 1674-4527 |
| DOI | 10.1088/1674-4527/18/9/111 |
| Indexed | SCI(E) |
| Appears in Collections: | 物理学院 科维理天文与天体物理研究所 |
