Table 3.
Results(1).
| Source name | 0.3–10 keV rate | 0.3–1.0 keV rate | 0.3–10 keV X-ray flux (2) | X-ray luminosity (2) | BB Temp. | UVW2 (3, 4) | UVM2 (3) |
|---|---|---|---|---|---|---|---|
| (counts s−1) | (counts s−1) | (erg cm−2 s−1) | (erg s−1) | (105 K) | (mag) | (mag) | |
| 0616+2319 | < 2.0 × 10−3 | < 1.5 × 10−3 | < 1.00 × 10−13 | < 1.48 × 1031 | < 6.0 | – | 16.51 ± 0.04 |
| 1220+5841 | < 2.5 × 10−3 | < 2.5 × 10−3 | < 1.25 × 10−13 | < 7.17 × 1029 | < 4.2 | > 20.0 | – |
| 1313+4152 | < 1.6 × 10−3 | < 1.6 × 10−3 | < 8.00 × 10−14 | < 5.89 × 1029 | < 4.1 | > 21.5 | – |
| 1527+3536 | 1.2 ± 0.1 × 10−2 | 6.2 ± 0.7 × 10−3 | 5.20 ± 0.7 × 10−13 | 8.0 ± 1.0 × 1029 | – | – | 16.55 ± 0.04 |
| 1832–0119 | < 2.5 × 10−3 | < 1.6 × 10−3 | < 1.25 × 10−13 | < 4.90 × 1029 | < 4.0 | > 19.04 | – |
| 2128+3316 | < 1.9 × 10−3 | < 1.9 × 10−3 | < 9.50 × 10−14 | < 5.86 × 1029 | < 4.1 | > 20.5 | – |
Notes. (1)All errors and limits are quoted at 90% confidence level. (2)Flux and luminosity upper limits are calculated under the assumption of a power-law spectrum with index Γ = 2. (3)Vega system. (4)Observations of late-type stars with the UVW2 filter are affected by contamination from optical photons caused by the red tail of the filter passband. For a K2V type star, it is estimated that the UV portion is less than only 20% of the photons total flux Brown et al. (2010), and so any measured flux should be interpreted as an upper bound on the real flux.
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