Table 6.
Accretion noise values as a function of SpT and Teff.
| SpT | Teff [K] | log(Lacc, noise/L⋆) |
|---|---|---|
| G8.0 | 5180 | −1.3 |
| G8.5 | 5102 | −1.3 |
| G9.0 | 5025 | −1.3 |
| G9.5 | 4947 | −1.3 |
| K0.0 | 4870 | −1.4 |
| K0.5 | 4830 | −1.4 |
| K1.0 | 4790 | −1.4 |
| K1.5 | 4750 | −1.5 |
| K2.0 | 4710 | −1.5 |
| K2.5 | 4625 | −1.5 |
| K3.0 | 4540 | −1.5 |
| K3.5 | 4457 | −1.5 |
| K4.0 | 4375 | −1.5 |
| K4.5 | 4292 | −1.6 |
| K5.0 | 4210 | −1.7 |
| K5.5 | 4162 | −1.7 |
| K6.0 | 4115 | −1.8 |
| K6.5 | 4067 | −1.9 |
| K7.0 | 4020 | −1.9 |
| K7.5 | 3960 | −1.9 |
| M0.0 | 3900 | −2.0 |
| M0.5 | 3810 | −2.0 |
| M1.0 | 3720 | −2.0 |
| M1.5 | 3640 | −2.0 |
| M2.0 | 3560 | −2.1 |
| M2.5 | 3485 | −2.2 |
| M3.0 | 3410 | −2.3 |
| M3.5 | 3300 | −2.3 |
| M4.0 | 3190 | −2.5 |
| M4.5 | 3085 | −2.6 |
| M5.0 | 2980 | −2.7 |
| M5.5 | 2920 | −2.7 |
Notes. The accretion noise values are obtained from interpreting the 1σ level of uncertainty on the Balmer and Paschen continua (< 500 nm) on our interpolated class III spectra at a given spectral type as accretion luminosity. Teff obtained from the relationship from HH14 are also listed for convenience.
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