X-ray loud M dwarfs are a major source of by-products （contamination） in the X-ray band of the multiwavelength quasar survey. As a by-product, the low dispersion spectra of 22 M dwarfs are obtained in which the spec...X-ray loud M dwarfs are a major source of by-products （contamination） in the X-ray band of the multiwavelength quasar survey. As a by-product, the low dispersion spectra of 22 M dwarfs are obtained in which the spectra of 16 sources are taken for the first time. The spectral types and distances of the sample are given based on spectral indices CaH2, CaH3, and TiO5. The parameter ζ TiO/CaH is calculated to separate the different metallicity classes among dwarfs, subdwarfs and extreme subdwarfs. We also discuss the distributions in the diagrams of log（L x /L bol ）, the ratio between X-ray and bolometric luminosity versus spectral type and infrared colors.展开更多
基金supported by the Scientific Research Foundation of Beijing Normal Universitythe National Natural Science Foundation of China (Grant No.10778717)supported by the Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
文摘X-ray loud M dwarfs are a major source of by-products （contamination） in the X-ray band of the multiwavelength quasar survey. As a by-product, the low dispersion spectra of 22 M dwarfs are obtained in which the spectra of 16 sources are taken for the first time. The spectral types and distances of the sample are given based on spectral indices CaH2, CaH3, and TiO5. The parameter ζ TiO/CaH is calculated to separate the different metallicity classes among dwarfs, subdwarfs and extreme subdwarfs. We also discuss the distributions in the diagrams of log（L x /L bol ）, the ratio between X-ray and bolometric luminosity versus spectral type and infrared colors.
