Table 4
Observation ID and coronal properties of our sample of ultra-fast rotating low mass stars.
| Star | Obs. ID | T | log EM |
|
|
|
||||||
| MK | 1053 cm-3 | |||||||||||
|
|
||||||||||||
| AB Dor | 0602240201 | 11.49 |
10.18 |
0.23 ± 0.02 | 5.01 ± 0.81 | 0.44 ± 0.06 | ||||||
| BO Mic | 0400460301 | 11.78 |
8.11 |
0.21 ± 0.07 | 5.69 ± 1.14 | 0.39 ± 0.06 | ||||||
| HK Aqr | 0202360101 | 8.42 |
0.93 |
0.17 ± 0.08 | 5.47 ± 0.73 | 0.36 ± 0.04 | ||||||
| YY Gem | 0123710101 | 10.20 |
3.38 |
0.29 ± 0.05 | 5.35 ± 0.67 | 0.33 ± 0.05 | ||||||
| PZ Tel | 0203060201 | 11.15 |
16.32 |
0.27 ± 0.03 | 2.03 ± 0.41 | 0.76 ± 0.13 | ||||||
| LO Peg | This work | 9.98 |
4.51 |
0.23 ± 0.02 | 5.85 ± 0.70 | 0.54 ± 0.07 | ||||||
Notes. For consistency we carried out a detailed analysis of each of the target and obtained the X-ray coronal properties using similar APEC models. The abundance ratios 
are relative to the solar photosphere, while we obtain the 
ratio using the method described by Drake & Testa 2005, i.e., the ratio is coronal.
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