Open Access
Table 4
2M1006 stellar parameters.
| Parameter | Value | Ref. |
|---|---|---|
| Unresolved stellar binary | ||
| RA(J2000) | 10:06:55.72 | Simbad |
| Dec(J2000) | −63:52:08.61 | Simbad |
| B | 11.812 ± 0.014 | APASS/DR9 |
| V | 11.015 | this work |
| g′ | 11.368 ± 0.054 | APASS/DR9 |
| r′ | 10.690 ± 0.060 | APASS/DR9 |
| i′ | 10.385 ± 0.033 | APASS/DR9 |
| GBp | 11.227 ± 0.008 | GaiaEDR3 |
| G | 10.744 ± 0.004 | GaiaEDR3 |
| GRp | 10.085 ± 0.006 | GaiaEDR3 |
| GBp − G | 0.482880 | GaiaEDR3 |
| GBp − GRp | 1.141988 | GaiaEDR3 |
| G − GRp | 0.659108 | GaiaEDR3 |
| J | 9.262 ± 0.028 | 2MASS |
| H | 8.744 ± 0.061 | 2MASS |
| Ks | 8.580 ± 0.024 | 2MASS |
| W1 | 8.530 ± 0.023 | allWISE |
| W2 | 8.541 ± 0.020 | allWISE |
| W3 | 8.455 ± 0.018 | allWISE |
| W4 | 8.236 ± 0.149 | allWISE |
| EW(Li I λ6707) (mÅ) | 350 ± 10 | (1) |
| EW(Hα)(Å) | 0.00 ± 0.01 | (1) |
| vsini (km s−1) | 77.0 ± 7.7 | (1) |
| AV (mag) | <0.13 | This work |
| Primary (A) | ||
| SpT | G8V − K0V | (1) and This work |
| Teff (K) | ![$\[5196_{-96}^{+162}\]$](/articles/aa/full_html/2025/07/aa49582-24/aa49582-24-eq16.png) |
This work |
| log(L/L⊙) (dex) | −0.1 ± 0.05 | This work |
| Age (Myr) | ![$\[25_{-6}^{+3}\]$](/articles/aa/full_html/2025/07/aa49582-24/aa49582-24-eq17.png) |
This work |
| Mass (M⊙) | 1.03 ± 0.05 | This work |
| G | 10.82 ± 0.01 | This work |
| MagAO − X/z′ | 9.94 ± 0.01 | This work |
| S PHERE/J2 | 9.56 ± 0.01 | This work |
| S PHERE/J3 | 9.40 ± 0.01 | This work |
| S PHERE/H | 9.05 ± 0.01 | This work |
| S PHERE/KS | 8.96 ± 0.02 | This work |
| Fainter star (B) | ||
| Teff (K) | ![$\[3458_{-91}^{+110}\]$](/articles/aa/full_html/2025/07/aa49582-24/aa49582-24-eq18.png) |
This work |
| log(L/L⊙) (dex) | −0.90 ± 0.04 | This work |
| G | 13.67 ± 0.13 | this work |
| MagAO − X/z′ | 11.80 ± 0.06 | This work |
| S PHERE/J2 | 11.04 ± 0.05 | This work |
| S PHERE/J3 | 10.83 ± 0.04 | This work |
| S PHERE/H | 10.30 ± 0.04 | This work |
| S PHERE/KS | 10.04 ± 0.03 | This work |
Notes. The magnitudes of the primary star and fainter star between G and S PHERE/KS are calculated by synthetic photometry on the fitted spectra with SPECIES. Their uncertainties are likely underestimated.
References. (1) Torres et al. (2006).
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