No. . | Object . | Other name . | p (ms)* . | F 3.4(mag)† . | M 3.4(mag)‡ . | T eff § . | log fbol‖ . | log L/L⊙|$^\#$| . | R/R⊙** . | K †† . | M K ‡‡ . | M/M⊙§§ . |
---|---|---|---|---|---|---|---|---|---|---|---|---|
1 | GJ 406 | Wolf 359 | 419.1 | 5.807 | 8.92 | 2800. | − 8.221 | −2.975 | 0.139 | 6.08 | 9.19 | 0.103 |
2 | GJ 644C | vB 8 | 148.92 | 8.619 | 9.48 | 2640. | − 9.329 | −3.184 | 0.123 | 8.82 | 9.69 | 0.090 |
3 | GJ 752B | vB 10 | 170.36 | 8.317 | 9.47 | 2250. | − 9.422 | −3.394 | 0.133 | 8.80 | 9.96 | 0.088 |
4 | GJ 3849 | LHS 2924 | 95.0 | 10.428 | 10.32 | 2130. | − 10.210 | −3.675 | 0.107 | 10.67 | 10.56 | 0.080 |
No. . | Object . | Other name . | p (ms)* . | F 3.4(mag)† . | M 3.4(mag)‡ . | T eff § . | log fbol‖ . | log L/L⊙|$^\#$| . | R/R⊙** . | K †† . | M K ‡‡ . | M/M⊙§§ . |
---|---|---|---|---|---|---|---|---|---|---|---|---|
1 | GJ 406 | Wolf 359 | 419.1 | 5.807 | 8.92 | 2800. | − 8.221 | −2.975 | 0.139 | 6.08 | 9.19 | 0.103 |
2 | GJ 644C | vB 8 | 148.92 | 8.619 | 9.48 | 2640. | − 9.329 | −3.184 | 0.123 | 8.82 | 9.69 | 0.090 |
3 | GJ 752B | vB 10 | 170.36 | 8.317 | 9.47 | 2250. | − 9.422 | −3.394 | 0.133 | 8.80 | 9.96 | 0.088 |
4 | GJ 3849 | LHS 2924 | 95.0 | 10.428 | 10.32 | 2130. | − 10.210 | −3.675 | 0.107 | 10.67 | 10.56 | 0.080 |
*Parallax by RECONS for GJ 406 and GJ 644C, by Hipparcos (van Leeuwen 2007) for GJ 752B, and by Gliese and Jahreiss (1991) for GJ 3849.
† W1 band flux centered at 3.4 μm from the WISE All-Sky Release for F3.4 < 8.0 mag and from the AllWISE catalog for F3.4 > 8.0 mag (Wright et al. 2010).
‡Absolute magnitude at 3.4 μm based on F3.4.
§Based on the infrared flux method (Tsuji et al. 1996a).
‖Observed bolometric flux based on the integration of SED (Tsuji et al. 1996a).
|$^\#$|Bolometric luminosity based on the fourth and eighth columns.
**Based on L/L⊙ and Teff.
††Observed K magnitude (Leggett 1992).
‡‡Absolute magnitude at K.
§§Based on MK–M/M⊙ of Delfosse et al. (2000) extended by the use of MK–M/M⊙ from the evolutionary models of Baraffe et al. (1998). See figure 2.
No. . | Object . | Other name . | p (ms)* . | F 3.4(mag)† . | M 3.4(mag)‡ . | T eff § . | log fbol‖ . | log L/L⊙|$^\#$| . | R/R⊙** . | K †† . | M K ‡‡ . | M/M⊙§§ . |
---|---|---|---|---|---|---|---|---|---|---|---|---|
1 | GJ 406 | Wolf 359 | 419.1 | 5.807 | 8.92 | 2800. | − 8.221 | −2.975 | 0.139 | 6.08 | 9.19 | 0.103 |
2 | GJ 644C | vB 8 | 148.92 | 8.619 | 9.48 | 2640. | − 9.329 | −3.184 | 0.123 | 8.82 | 9.69 | 0.090 |
3 | GJ 752B | vB 10 | 170.36 | 8.317 | 9.47 | 2250. | − 9.422 | −3.394 | 0.133 | 8.80 | 9.96 | 0.088 |
4 | GJ 3849 | LHS 2924 | 95.0 | 10.428 | 10.32 | 2130. | − 10.210 | −3.675 | 0.107 | 10.67 | 10.56 | 0.080 |
No. . | Object . | Other name . | p (ms)* . | F 3.4(mag)† . | M 3.4(mag)‡ . | T eff § . | log fbol‖ . | log L/L⊙|$^\#$| . | R/R⊙** . | K †† . | M K ‡‡ . | M/M⊙§§ . |
---|---|---|---|---|---|---|---|---|---|---|---|---|
1 | GJ 406 | Wolf 359 | 419.1 | 5.807 | 8.92 | 2800. | − 8.221 | −2.975 | 0.139 | 6.08 | 9.19 | 0.103 |
2 | GJ 644C | vB 8 | 148.92 | 8.619 | 9.48 | 2640. | − 9.329 | −3.184 | 0.123 | 8.82 | 9.69 | 0.090 |
3 | GJ 752B | vB 10 | 170.36 | 8.317 | 9.47 | 2250. | − 9.422 | −3.394 | 0.133 | 8.80 | 9.96 | 0.088 |
4 | GJ 3849 | LHS 2924 | 95.0 | 10.428 | 10.32 | 2130. | − 10.210 | −3.675 | 0.107 | 10.67 | 10.56 | 0.080 |
*Parallax by RECONS for GJ 406 and GJ 644C, by Hipparcos (van Leeuwen 2007) for GJ 752B, and by Gliese and Jahreiss (1991) for GJ 3849.
† W1 band flux centered at 3.4 μm from the WISE All-Sky Release for F3.4 < 8.0 mag and from the AllWISE catalog for F3.4 > 8.0 mag (Wright et al. 2010).
‡Absolute magnitude at 3.4 μm based on F3.4.
§Based on the infrared flux method (Tsuji et al. 1996a).
‖Observed bolometric flux based on the integration of SED (Tsuji et al. 1996a).
|$^\#$|Bolometric luminosity based on the fourth and eighth columns.
**Based on L/L⊙ and Teff.
††Observed K magnitude (Leggett 1992).
‡‡Absolute magnitude at K.
§§Based on MK–M/M⊙ of Delfosse et al. (2000) extended by the use of MK–M/M⊙ from the evolutionary models of Baraffe et al. (1998). See figure 2.
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