MMM6V Kirkpatrick(in GrayCorbally09) call Gl 406 (= Wolf 359) the primary M6V standard. Boeshaar76 standard: GJ 406 (=Wolf 359) - M6e (plate III standard) Boeshaar76 standard: GJ 65AB - M6-e (plate IV standard) Turnshek85 standard: GJ 406 (=Wolf 359) - dM6e Boeshaar85 standard: GJ 4037 (=LHS 3339) - dM6 (in text, not Table II) Kirkpatrick91 standards: GJ 1245B - M6V (pri. stan.) GJ 65B - M6V (pri. stan.) GJ 406 (=Wolf 359) - M6V (pri. stan.) LHS 5142 - M6V (sec. stan.) Kirkpatrick97 standard: GJ 406 (=Wolf 359) - M6V Hawley02 standard: 2MASS J0435+1537 - M6V Henry02 standards: GJ 65B - M6V GJ 283B - M6V GJ 406 (=Wolf 359) - M6V GJ 1245B - M6V Henry04 standard: GJ 406 (=Wolf 359) - M6.0V (pri. stan.) Kirkpatrick(GrayCorbally09): Gl 406 (=Wolf 359) - M6V (pri. stan.) Kirkpatrick10 standard: GJ 3146 (LHS 1375) - M6V (opt.,near-IR stan.) Pecaut13 standard: GJ 406 (=Wolf 359) - M6V Newton14 standard: GJ 406 - M6V Kirkpatrick16 standard: GJ 406 (=Wolf 359) - M6V RECONS shows GJ 406 (=Wolf 359; J1056+0700) as the nearest M6V star, followed by GJ 65B (J0139-1757), & GJ 1245B (J1953+4424). (M6V) = 1.64 ; Fitzgerald70 (M6V) = 1.72 ; Johnson66 (B-V)(M6V) = 1.73 ; SchmidtKaler82 (B-V)(M6V) = 1.83 ; sec. stan. GJ 283B (B-V)(M6V) = 1.95 ; Leggett92 "young disk" (B-V)(M6V) = 1.98 ; sec. stan. GJ 1245B (B-V)(M6V) = 1.98 ; ter. stan. GJ 3146 (B-V)(M6V) = 1.99 ; prim. stan. GJ 406 (Kilkenny98) (M6V) = 2.0+ ; Bessell79 (B-V)(M6V) = 2.034 +- 0.0069 ; prim. stan. GJ 406 (Landolt09) (B-V)(M6V) = 2.06 ; Bessell91 "old disk" => adopt (B-V)(M6V) = 2.00 (M6V) = 1.27 ; Johnson66 (U-B)(M6V) = 1.26 ; U-B vs. B-V trend from Landolt09 for B-V=2.00 (very few points) (U-B)(M6V) = 1.165 +- 0.0346 ; pri. stan. GJ 406; Landolt09 => adopt (U-B)(M6V) = 1.3 (V-Rc)(M6V) = 1.823 +- 0.0073 ; pri. stan. GJ 406 (Landolt09) (V-Rc)(M6V) = 1.91 ; Bessell91 "old disk" (M6V) = 1.93 ; Johnson66 (V-Rc)(M6V) = 1.95 ; adopting V-I=4.10, R-I=2.15 (see below) (V-Rc)(M6V) = 2.25 ; non-standard LHS 2026 => adopt (V-Rc) = 1.95 (V-Ic)(M6V) = 4.62 ; non-standard LHS 2026 (V-Ic)(M6V) = 4.45 ; non-standard LHS 2471 (V-Ic)(M6V) = 4.22 ; non-standard LHS 1604 (V-Ic)(M6V) = 4.20 ; non-standard LHS 2314 (V-Ic)(M6V) = 4.14 ; non-standard GJ 316.1 (V-Ic)(M6V) = 4.13 ; Bessell91 "old disk" (V-Ic)(M6V) = 4.11 ; sec. stan. GJ 283B (V-Ic)(M6V) = 4.000 +- 0.0062 ; pri. stan. GJ 406 (Landolt09) (V-Ic)(M6V) = 4.0 ; Hawley96 (M6V) = 3.76 ; Johnson66 (V-Ic)(M6V) = 3.75 ; Leggett92 "young disk" (V-Ic)(M6V) = 3.740 ; sec. stan. GJ 1245B (M6V) = 3.58 ; Bessell79 => adopt (V-Ic)(M6V) = 4.10 (R-I)(M6V) = 2.152 ; N=4 M6Vs in Liebert06 (+-0.045 sem, +-0.090 rms) (R-I)(M6V) = 2.174 +-0.0025 ; pri. stan. GJ 406 (Landolt09) (M6V) = 2.18 ; Bessell79 (R-I)(M6V) = 2.22 ; Bessell91 "old disk" => adopt (V-Rc)(M6V) = 2.16 (M6V) = 4.63 ; Johnson66 (M6V) = 6.204 +-0.167 (sem) (stdev = 0.334) (N=4 stans) (M6V) = 5.58 ; Johnson66 (V-Ks)(M6V) = 6.54 ; exemplar LSPM J0011+5908 (V-Ks)(M6V) = 6.603 ; sec. stan. GJ 1245B (M6V) = 6.65 ; Beuermann06 (V-K_CIT)(M6V) = 6.65 ; Leggett92 "young disk" (V-Ks)(M6V) = 6.809 ; ter. stan. GJ 3146 (V-Ks)(M6V) = 6.90 ; exemplar SCR J0630-7643 AB (V-K)(M6V) = 7.0 ; Hawley96 (V-Ks)(M6V) = 7.259 ; ter. stan. GJ 283B (V-Ks)(M6V) = 7.34 ; ter. stan. LHS 5142 (V-K)(M6V) = 7.37 ; Bessell91 "old disk" (V-Ks)(M6V) = 7.445 ; prim. stan. GJ 406 (V-Ks)(M6V) = 7.514 ; exemplar LHS 2314 (V-Ks)(M6V) = 7.788 ; non-standard LHS 1604 (V-Ks)(M6V) = 7.798 ; exemplar LHS 2026 => adopt (V-Ks)(M6V) = 7.10 *** [updated 10/3/2019] [note that GJ 406 appears to be redder than the other M6V standards, but not so red compared to non-standard M6Vs] => adopt (V-J)(M6V) = 6.343 => adopt (V-H)(M6V) = 6.948 => adopt (I-Ks)(M6V) = 3.186 (J-H)(M6V) = 0.648 (+-0.012 sem,+-0.033 stdev) ; N=7 M6V Cruz03 (J-H)(M6V) = 0.605 ; color-color-trend for V-K=7.30 => adopt (J-H)(M6V) = 0.605 (M6V) = 0.89 ; Beuermann06 (J-Ks)(M6V) = 0.957 ; color-color trend for V-K=7.30 (J-Ks)(M6V) = 1.028 (+-0.017 sem,+-0.036 stdev) ; N=7 M6V Cruz03 => adopt (J-Ks)(M6V) = 0.957 (M6V) = 0.33 ; Beuermann06 (H-Ks)(M6V) = 0.352 ; color-color trend for V-K=7.30 (H-Ks)(M6V) = 0.391 (+-0.013 sem,+-0.029 stdev) ; N=7 M6V Cruz03 (Ks-L')(M6V) = 0.320 ; Dupuy12 polynomial (Bp-Rp)(M6V) = 3.6899 ; G_234-45 M6V (Bp-Rp)(M6V) = 3.8419 ; GJ_1245B sec. stan. (Bp-Rp)(M6V) = 3.9546 ; GJ_3146 ter. stan. (Bp-Rp)(M6V) = 3.9546 ; GJ_65B ter. stan. (Bp-Rp)(M6V) = 4.4215 ; LHS_2090 M6V (Bp-Rp)(M6V) = 4.3916 ; GJ_283B ter. stan. (Bp-Rp)(M6V) = 4.4644 ; LHS_5142 ter. stan. => adopt (Bp-Rp)(M6V) = 3.95 [updated 3/1/2019] (G-Rp)(M6V) = 1.3850 ; G_234-45 M6V (G-Rp)(M6V) = 1.4076 ; GJ_1245B sec. stan. (G-Rp)(M6V) = 1.4208 ; GJ_3146 ter. stan. (G-Rp)(M6V) = 1.4568 ; GJ_65B ter. stan. (G-Rp)(M6V) = 1.4724 ; GJ_283B ter. stan. (G-Rp)(M6V) = 1.4850 ; LHS_2090 M6V (G-Rp)(M6V) = 1.5009 ; LHS_5142 ter. stan. => adopt (G-Rp)(M6V) = 1.45 [updated 3/1/2019] => adopt (Bp-G)(M6V) = 2.50 [updated 3/1/2019; Bp-Rp=3.95, G-Rp=1.45] (Bp-G)(M6V) = 2.4343 ; GJ_1245B (Bp-G)(M6V) = 2.4978 ; GJ_65B (Bp-G)(M6V) = 2.5337 ; GJ_3146 (Bp-G)(M6V) = 2.9192 ; GJ_283B (Bp-G)(M6V) = 2.9635 ; LHS_5142 (G-V)(M6V) = -2.7111 ; GJ_283B (G-V)(M6V) = -2.2106 ; GJ_3146 (G-V)(M6V) = -2.071 ; GJ_1245B (G-V)(M5V) = -1.826 ; median M5V d<60pc (N=39) (likely biased blue) (G-V)(M6V) = -1.6859 ; GJ_65B => adopt (G-V)(M6V) = -2.14 [updated 3/4/2019] Teff(M6V) = 3190 K ; Bertone04[NextGen] Teff(M6V) = 3050 K ; Schmidt-Kaler82 Teff(M6V) = 2967 K ; Rajpurohit18 (mean for N=3 M6Vs) Teff(M6V) = 2950 K ; Johnson66 Teff(M6V) = 2950 K ; ter. stan. GJ 65 Teff(M6V) = 2920 K ; exemplar LSPM J0011+5908 Teff(M6V) = 2900 K ; ter. stan. GJ 3146 Teff(M6V) = 2883 K ; RojasAyala12(mean N=13 M6V stars) Teff(M6V) = 2881 K ; sec. stan. GJ 1245B (median Teff) Teff(M6V) = 2857 K ; pri. stan. GJ 406 (median Teff) Teff(M6V) = 2846 K ; Golimowski04 Teff(M6V) = 2800 K ; Bessell91 "old disk" Teff(M6V) = 2800 K ; Rajpurohit13(N=2) Teff(M6V) = 2750 K ; Bessell79 (Blackbody Teffs from Veeder74) Teff(M6V) = 2758 K ; EEM N=34 Teffs Teff(M6V) = 2520 K ; ter. stan. GJ 283B (single Teff calculated from V-K) => adopt Teff(M6V) = 2850 K (logT = 3.455) [last updated 10/3/2019] BCv(M6V) = -2.32 mag ; Bertone04[NextGen] BCv(M6V) = -3.007 mag ; Casagrande08 for Teff=2850K BCv(M6V) = -3.08 mag ; Schmidt-Kaler82(BCv=-3.21 + 0.13 offset) BCv(M6V) = -3.753 mag ; sec. stan. GJ 1245B (calc using Mann15) BCv(M6V) = -4.136 mag ; consensus trend for Teff=2850K BCv(M6V) = -4.305 mag ; Mann15(V-J=6.343) BCv(M6V) = -4.36 mag ; BC_K=2.94, V-K=7.30 BCv(M6V) = -4.413 mag ; pri. stan. GJ 406, using Mann15 BCv(M6V) = -4.43 mag ; Bessell91("old disk"; BCv = (V-I)-BC_I) BCv(M6V) = -4.438 mag ; pri. stan. GJ 406/LHS 36 (Golimowski04; using BC_Ks & calc. Mv) BCv(M6V) = -4.487 mag ; pri. stan. GJ 406, using Pavlenko06 below => adopt BCv(M6V) = -4.36 mag [last updated 3/8/2018; BC_Ks=2.98, V-Ks=7.30] BC_K(M6V) = 3.034 mag ; Golimowski04(SpT function) BC_K(M6V) = 3.01 mag ; pri. stan. Wolf359/LHS 36 (Golimowski04) BC_K(M6V) = 3.010 mag ; pri. stan. Wolf359 (calc. using Mann15) BC_K(M6V) = 2.994 mag ; Mann15(V-J=6.343) BC_K(M6V) = 2.97 mag ; LHS 36 (Leggett01) BC_K(M6V) = 2.946 mag ; Leggett01 polynomial for I-K=3.186 BC_K(M6V) = 2.936 mag ; pri. stan. Wolf359 (calc using Pavlenko06) BC_K(M6V) = 2.921 mag ; smoothed trend over M0V-M9V for M6V BC_K(M6V) = 2.870 mag ; sec. stan. GJ 1245B (calc using Mann15) BC_K(M6V) = 2.855 mag ; Leggett01 polynomial for J-K=0.957 => adopt BC_Ks(M6V) = 2.94 mag [last updated 3/8/2018] Mv(M6V) = 11.47 ; Wegner07 (clearly in error, or biased somehow!) Mv(M6V) = 13.5 ; Schmidt-Kaler82 Mv(M6V) = 15.70 ; sec. stan. GJ 1245B Mv(M6V) = 16.17 ; Henry94 Mv(M6V) = 16.49 ; Kirkpatrick94 Mv(M6V) = 16.60 ; Dieterich14 calibration for V-Ks=7.30 Mv(M6V) = 16.62 ; pri. stan. GJ 406 Mv(M6V) = 16.7 ; Reid04 Mv(M6V) = 16.80 ; sec. stan. GJ 283B Mv(M6V) = 16.88 ; exemplar LHS 2314 Mv(M6V) = 16.88 ; EEM fit to Reid CNS3 data for V-K=7.30) => adopt Mv(M6V) = 16.62 mag [for V-Ks=7.30, M_Ks=9.32; and ident. to Mv for GJ 406; 3/8/2018] M_Ks(M6V) = 9.10 ; sec. stan. GJ1245B M_Ks(M6V) = 9.15 ; ter. stan. GJ3146 M_Ks(M6V) = 9.20 ; pri. stan. GJ406/Wolf359 M_Ks(M6V) = 9.30 ; Dieterich14 calibration for V-Ks=7.30 M_Ks(M6V) = 9.31 ; Dupuy12 mean M_Ks(M6V) = 9.32 ; V-K=7.30, Mv=16.62 M_Ks(M6V) = 9.34 ; Finch14 calibration for V-Ks=7.30 M_Ks(M6V) = 9.36 ; exemplar LHS 2314 M_Ks(M6V) = 9.388 ; Dupuy12 polynomial M_Ks(M6V) = 9.55 ; ter. stan. GJ 283B M_Ks(M6V) = 9.58 ; EEM fit to Reid CNS3 data for V-K=7.30 M_Ks(M6V) = 9.60 ; exemplar LHS 2026 M_Ks(M6V) = 9.66 ; ter. stan. LHS 5142 => adopt M_Ks(M6V) = 9.32 mag [last updated 3/8/2018; V-Ks=7.30, Mv=16.62] logL(M6V) = -3.018 dex ; Mv=16.62, BCv=-4.32 => Mbol = 12.300 logL(M6V) = -3.018 dex ; M_Ks=9.32, BC_Ks=2.98 => Mbol = 12.300 logL(M6V) = -2.97+-0.02 dex ; non stan. LHS 36 (Golimowski04) logL(M6V) = -2.97 dex ; LHS 36 (Leggett01) logL(M6V) = -2.82 dex ; sec. stan. GJ 1245B (see below) => adopt logL(M6V) = -3.018 dex => adopt Mbol(M6V) = 12.300 mag Mass(M6V) = 0.098 Msun ; Mv=16.88 => Delfosse10 calibration Mass(M6V) = 0.099 Msun ; M_Ks=9.30 => Delfosse10 calibration Mass(M6V) = 0.101 Msun ; M_Ks=9.32 => Mann18 calib. Mass(M6V) = 0.101 Msun ; pri. stan. GJ 406 (Jenkins09) Mass(M6V) = 0.105 Msun ; M_Ks=9.32 => Benedict16 calibration Mass(M6V) = 0.108 Msun ; sec. stan. GJ 1245B (Jenkins09) Mass(M6V) = 0.1195 Msun ; GJ 65B (dynamical) => adopt Mass(M6V) = 0.101 Msun [last updated 8/2/2018] # No Standards Houk75, Boeshaar85, Keenan85 do not list M6V standards # Primary Standard GJ 406 = Wolf 359 = LHS 36 = CN Leo = StKM 2-681 (J1056+0700) M5.5V: Hawley97 M5.9: Mann15 *M6.0V: Boeshaar76,Turnshek85(stan;dM6e),Bidelman85(M6),Bessell91(M6Ve),Kirkpatrick91(pri),Kirkpatrick93,Kirkpatrick94,Kirkpatrick97(stan),Henry02,Geballe02,Henry04(M6.0Ve),Kirkpatrick(GrayCorbally09),Newton14(stan) M6.5Ve: Joy74,Mukai90(M6.5) M8:e: : Stephenson86 Undoubtedly the most agreed upon M6V standard. V=13.529+-0.025(Mermilliod91), V=13.53(Kilkenny98), V=13.507+-0.006(Landolt09), V=13.52(Bessell83), B-V=2.013+-0.018(Mermilliod91), B-V=2.034+-0.0069(Landolt09), B-V=2.00(Bessell83), U-B=1.268+-0.131(Mermilliod91), U-B=1.165+-0.0346(Landolt09), V-I=5.12(Morel78), V-Ic=4.037(Bessell83), V-Ic=4.000+-0.0062 (Landolt09), V-Ic=4.032(Kilkenny98), V-Rc=1.856(Kilkenny98), V-Rc=1.860(Bessell83), R-Ic=2.177(Bessell83), R-I=2.46(Morel78), R-Ic=2.174+-0.0025(Landolt09), R-Ic=2.176(Kilkenny98), J=7.085+-0.024(2MASS), H=6.482+-0.042(2MASS), Ks=6.084+-0.017(2MASS), V-J=6.444(Mermilliod91 & 2MASS), (V-Ks)=7.445(Mermilliod91 & 2MASS), plx = 418.9+-2.4 mas (Harrington93). Mbol=12.18+-0.08(Golimowski04), BC_Ks=3.01+-0.07(Golimowski04), log(L/Lsun)=-2.97+-0.02 dex(Golimowski04). Mv = 16.618+-0.012 mag, M_Ks = 9.20+-0.02 mag. Hence BCv = Mbol - Mv = 12.18 - 16.618 = -4.438. Mass: 0.101Msun(Jenkins09). Teffs: 2500K(Casagrande08), 2520K(Jenkins09), 2600K(Leggett00), 2700K(Dieterich14), 2800K(Pavlenko06), 2808+-27K(Mann15#2), 2818+-60K(Mann15#1), 2857+-112K(Newton14), 2865+-60K(Gaidos14), 2887+-20K(RojasAyala12), 2900K(Golimowski04), 2900K(Rajpurohit18), 2911K(Rice10), 3000+-100K(Jones02,[Fe/H]=-0.5+-0.5), 3185K(Terrien15#1), 3356K(Terrien15#2) => Adopt Teff = 2857K. Rojas-Ayala12 estimates [Fe/H] ~ 0.18+-0.17, and Newton15 [Fe/H] ~ 0.31 or 0.30. Yes, systematic error among several modern Teff estimates for arguably the best studied M6V star is at the +-250K level! Jone's IR spectroscopy was compatible with Teff=2900K for [Fe/H]=-1.0 and Teff=3100K for [Fe/H]=0.0. mbol = 9.02(Pavlenko06; assumes MbolSun = 4.75, Lsun=3.86e26), mbol = 9.07(Leggett00). The Pavlenko06 mbol is approximately consistent with BCv = mbol - V = 9.02 - 13.507 = -4.487, BC_Ks = 9.02 - 6.084 = 2.936. Mann15 estimates fbol = (0.57980+-0.00690)e-11 W/m2, on IAU2015 scale mbol = 9.094+-0.013, hence BC_Ks = 9.094 - 6.084 = 3.01, BCv = 9.094 - 13.507 = -4.413. # Secondary Standard GJ 1245B = G 208-45 = LHS 3495 = NLTT 48415 *M6V: Rodono80,McCarthy88,Kirkpatrick91(pri),Kirkpatrick93,Kirkpatrick94,Geballe02,CNS4 M5.5V: Boeshaar85(dM5.5),Reid04 7" away from G208-44 = GJ 1245AC, and *not* G 208-44, which is considered a M5.5V standard, even though Reid04 classify "C" as a M7V. V=13.990(Mermilliod91), V=14.01(CNS4,Henry04), B-V=1.980(Mermilliod91), B-V=1.97(CNS4), Rc=12.36(Henry04), R-I=2.07(Delfosse98,CNS4), V-Rc = 1.65(Henry04), Ic=10.27(Henry04), V-Ic=3.74(Reid04,Henry04), J=8.275+-0.026(2MASS), H=7.728+-0.031(2MASS), Ks=7.387+-0.018(2MASS), V-J=5.715(Mermilliod91 & 2MASS), (V-Ks)=6.603(Mermilliod91 & 2MASS). Plx = 220.2+-1.5mas(Harrington93). Mv = 15.70+-0.01 mag, M_Ks = 9.10 +- 0.02 mag. Mass: 0.108Msun(Jenkins09). Using Casagrande10 relations, I estimate mbol=10.085+-0.025 mag, hence for Harrington93 parallax => Mbol=11.80mag, logL=-2.82. Mann15 estimates fbol = (0.1986+-0.0032)e-11 W/m2, on IAU2015 scale mbol = 10.257+-0.017. Hence BC_Ks = mbol - Ks = 10.257 - 7.387 = 2.87, BCv = 10.257 - 14.01 = -3.753. Teffs: 2673K(Jenkins09), 2859K(Mann15#1), 2881K(RojasAyala12), 2919+-34K(Mann15#2), 2944+-60K(Gaidos14) => median Teff = 2881K. # Tertiary Standard GJ 283B = L 745-46B = LFT 544 = LHS 234 *M6.0V: Bessell91(M6e),Henry94,Hawley97,Henry02,Reid04 M6.5V: Dieterich Star does not appear to be as well studied as the other standards, and has only one published Teff estimate. No type listed in Hawley97. Note that Bessell type is for "GJ 283" or "LHS 234"? GJ 283A is DA3 or DC or DZ6 white dwarf 21" away. V=14.47(Salim03, bad value?), V=16.42(Gliese91,Reid04), V=16.55(vanAltena95), V=16.54(Bessell91), V=16.67(Hawley97) [I adopt value from vanAltena95], B-V=1.83(Gliese91), Ic=12.43(Bessell91), V-I=4.110(Casagrande08), Rc=14.68(Bessell91), V-R=1.860(Casagrande08), V-J=4.31(Salim03) J=10.155+-0.022(2MASS), H=9.628+-0.023(2MASS), Ks=9.291+-0.022(2MASS), V-J=6.395(vanAltena95 & 2MASS), (V-Ks)=7.259(vanAltena95 & 2MASS), V-K=7.40(Hosey15). Plx = 112.4+-2.7 mas (vanAltena95). M_Ks = 9.55+-0.06 mag, Mv = 16.80+-0.05 mag. Using Casagrande08 relations, I estimate m_bol = 12.11+-0.02 mag (the JHK m_bols agree within 0.03 mag). Teffs: 2520K(V-K=>Casagrande08), 2900K(Rajpurohit18). [Fe/H]=+0.2(Rajpurohit18). LHS 5142 = LP 606-35 *M6V: Kirkpatrick91(sec),Kirkpatrick95,Kirkpatrick11 M6.5: Kirkpatrick93 M7: West08(M7e),Burgasser15 M8e: West11 DwarfArchives cites Kirkpatrick91. V=18.50(Lepine05), I=14.527+-0.03(DENIS), J=12.106+-0.024(2MASS), H=11.538+-0.023(2MASS), Ks=11.161+-0.021(2MASS) V-J=6.39(Lepine05 & 2MASS), (V-Ks)=7.34(Lepine05 & 2MASS). plx = 50.1+-3.8mas(Dittman14) => M_Ks=9.66+-0.17(2MASS,Dittman14), Mv=17.00(Lepine05,Dittman14). Per = 1.663d(Newton16). No published Teff estimates. GJ 65B = UV Ceti = L 726-8B = LHS 10 *M6.0V: Joy74,Kirkpatrick91(pri),Kirkpatrick94,Henry94,Henry02,Dieterich12 M6-e: Boeshaar76(stan,GJ65AB) M5.5: Cruz02,Reid04 Washington Double Star catalog lists GJ 65 (WDS 01388-1758 = LDS 838) as a 2.1" binary as of epoch 2010, with V mags of 12.7(A) and 13.2(B). GJ 65B (LHS 10) is the infamous star "UV Ceti". Kervella16 conducts comprehensive interferometric and dynamical study of this system. Joy74, Kirkpatrick91, and Henry02 call consider the pair of stars A & B to be M5.5V and M6.0V, respectively. Reid04 lists GJ 65AB as M5.5V, but lists B as a M5.5V also. Boeshaar76 and Boeshaar94 call the unresolved pair M6-V, while Reid04 calls the unresolved pair M5.5V. So most experts consider A & B to be ~0.5 subtype different, and they are ~0.5 mag different in V magnitude. It's not obvious that such a system is optimal for use as a standard star(s), especially if one is not blessed with <1" seeing. plx = 375+-4 mas(Geyer88), 373.7+-2.7mas(vanAltena95). The 2MASS JHK and Mermilliod91 UBV photometry for GJ 65AB is unresolved: J=6.283+-0.019, H=5.690+-0.029, Ks=5.343+-0.021. Teffs: 2900K(Kochukhov17), ~2900K(Kervella16,evol.track), ~3000K(Kervella16,adopted for limb darkening), 3167+-12K(Kovaleva12), => adopt = 2950K. Kervella16 lists: M=0.1195+-0.0043 Msun, logg=5.113+-0.015, [Fe/H]=-0.12+-0.20 (A is -0.03+-0.20), R=0.159+-0.006 Rsun, Radius inflacted ~13% in both stars, presumably due to inhibition of convection by magnetic fields. vsini = 30.6+-2 km/s. GJ 3146 = LHS 1375 = 2MASS J02162977+1335136 *M6V: Henry04,Kirkpatrick10(opt.,near-IR),Rojas-Ayala12,Newton14(near-IR) M6.1: Mann15 M6.39: Newton14(from Terrien15) M5.5V: Reid04,Dieterich12,Stelzer13,Cortes-Contreras17 V=15.790(Mermilliod91), B-V=1.980(Mermilliod91), J=9.871+-0.021(2MASS), H=9.314+-0.022(2MASS), Ks=8.981+-0.017(2MASS). V-Ks=6.809(Mermilliod91,2MASS). plx = 108.3+-5.0mas(Dittman14) => Mv=15.96, M_Ks=9.15. Teff = 2829+-60K(Mann15), 2868+-21K(Rojas-Ayala12), 2899+-48K(Mann15#2), 2936K(Stelzer13), 3181K(Terrien15#1), 3312K(Terrien15#2) => adopt Teff=2900K # Deprecated Standards GJ 4037 = LHS 3339 = LP 102-320 = NLTT 45700 *M5.5V: Kirkpatrick91(sec) M6V: Boeshaar85(stan),Hawley97,Geballe02,Basri06 M5V: Reid04 Depricated as a standard as it appears to have been little used since Kirkpatrick91. plx=61.10+-3.90mas(Dittman14), but see Dahn02. Not in Washington Double Star Catalog. Dahn02 derives: plx=46.4+-1.1 mas ((m-M)=1.67+-0.05), V=17.98+-0.02, R=16.20+-0.020, I=14.03+-0.01, K=10.78+-0.03, M_J = 10.05, BC_J = 2.02, Mbol = 12.07, R = 0.1308 Rsun, Teff = 2957+-70K. Hence, mbol = 13.74, and BCv = 13.74 - 17.98 = -4.24, BC_K = 13.74 - 10.875 = 2.87. V=17.90(Lepine05), V=17.98(Gliese91, vanAltena95), V=17.43(Salim03), J=11.819+-0.023(2MASS), H = 11.227+-0.023(2MASS), Ks=10.875+-0.016(2MASS). V-Ks=17.98-10.875=7.105. Teffs: 4100K(Morales08). # Exemplars LHS 2314 = 2MASS J10490338+0502227 *M6.0V: Henry04 M6Ve: Bessell91 M6: Reid95 Everyone agrees on M6 subtype. V=19.11(Henry04), Ic=14.91(Henry04), V-Ic=4.20(Henry04), J=12.535+-0.024(2M), H=11.970+-0.024(2M), Ks=11.596+-0.019(2M). V-Ks = 19.11 - 11.596 = 7.514. plx = 35.7616+-0.1279mas(GaiaDR2). Mv = 16.88, M_Ks=9.36. LHS 2026 = L 605-23 *M6.0Ve: Bessell91(M6Ve),Henry04(M6.0V) V=18.94(Henry04), Rc=16.69(Henry04), Ic=14.32(Henry04), V-Rc=2.25(Henry04), V-Ic=4.62(Henry04), J = 12.035+-0.023(2M), H=11.477+-0.021(2M), Ks=11.142+-0.023(2M). V-Ks = 18.94 - 11.142 = 7.798. plx = 49.0900+-0.1212mas(GaiaDR2). Mv=17.40, M_Ks=9.60. SCR J0630-7643 AB = SIPS J0630-7643 M5.0: Henry18 *M6Ve: Henry04,Reid07(M6.0),Stelzer13(M6.0),Gaidos14(M6) 1.2" binary, WDS lists magnitudes 15.5 and 15.7, so probably similar types. Resolved in Gaia DR2 (plx: 112.4936+-0.1222, 112.6759+-0.1105 mas; GaiaDR2). G=13.2069+-0.0019 & 13.4197+-0.0025. delta(G) = 0.2128. V=14.816(Henden16), V=14.82(Winters11), B-V=1.778(Henden16), R=13.08(Winters11), I=11.00(Winters11), Ks=7.923+-0.027(2MASS). V-Ks(AB)=14.82 - 7.923 = 6.897. Teffs: 2860K(Stelzer13), 2881+-67K(Muirhead18), 2892K(Stassun18), 2980+-60K(Gaidos14) => = 2886K. LSPM J0011+5908 = LSR J0011+5908 = 2MASS J00113182+5908400 M5.5V: Lepine03,AlonsoFloriano15 M6: RojasAyala12(near-IR) *M6.1: Mann15 M6.5V(e): Lepine09 V=15.611+-0.040(Mann15), V=15.63(Winters11), J=9.945+-0.023(2MASS), H=9.393+-0.026(2MASS), Ks=9.093+-0.021(2MASS). V-Ks = 15.63 - 9.093 = 6.537. plx = 107.4214+-0.0651mas(GaiaDR2). Mv = 15.79. M_Ks=9.25+-0.02. Teffs: 2805+-87K(Muirhead18), 2864+-60K(Mann15), 2898K(Houdebine19), 2918+-18K(RojasAyala12), 2921+-32K(Mann15#2), 2936K(Stelzer13), 3211K(Terrien15#1), 3347K(Terrien15#2) => = 2920K. # Other Stars GJ 1245C = G 208-44B M6.0V: Kirkpatrick91,Henry02 M5.5V: Hawley97,Reid04 binary with GJ 1245 AC (M5.5V+M7.0V) GJ 316.1 = LHS 2034 = AZ Cnc M6.0V: Bessell91,Henry04,Shkolnik09 *M6.5Ve: Dahn85 M7.0V: Newton14(M7V,near-IR),Bardalez14(M7.0) Literature values ~M6.5+-0.5. B-V=2.02(Dahn85), V=17.59(Henry04), V=17.68(Dahn85), Ic=13.45(Henry04), V-Ic=4.14(Henry04), V-I=4.34(Dahn85; "Kron-Mayall system"), J=11.053+-0.022(2M), H=10.419+-0.023(2M), Ks=10.046+-0.018(2M). V-Ks = 17.59 - 10.046 = 7.544. plx = 71.1+-1.0 mas (Henry04). GCVS lists variability with max 14.1, min 20.5! LHS 2471 = GJ 3693 M6.0V: Henry04,Hawley97(M6) M6.5V: Bessell91 *M7V: Newton14(near-IR),Bardalez14(near-IR) M8: Bardalez14(optical) Wide dispersion - appears to be ~M7+-1, earlier in optical. V=18.11(Henry04), Ic=13.66(Henry04), V-Ic=4.45(Henry04), J=11.256+-0.022(2M), H=10.660+-0.027(2M), Ks=10.262+-0.022(2M). V-Ks = 18.11 - 10.262 = 7.848. GJ 3512 = LHS 252 = G 234-45 M6V: Rojas-Ayala12(M6;K-band),Newton14(near-IR) *M5.70: Terrien15 M5.5: Reid95,Morales19(no ref.) Adopt M5.7 or M6-V, following Keenan's notation. Clearly bluer than M6V standards. B-V=1.93(vanAltena95), V=15.05(vanAltena95). J=9.615+-0.023(2MASS), H=8.996+-0.028(2MASS), Ks=8.668+-0.021(2MASS). V-Ks = 15.05 - 8.668 = 6.382. Morales19 reports 0.46 Mjup planet - huge for star of this mass. LHS 1604 = DENIS J0351000-005244 = SDSS J035100.03-005245.9 = LP 593-68 M6.0V: Cruz02,Henry04 M7e: West11 M7.5: Cruz03 M8e: West08 M5.5/7.0e: Crifo05 Not good agreement on types, probably ~M7+-1. V=18.02(Henry04), Ic=13.80(Henry04), V-Ic = 4.22(Henry04), J=11.302+-0.024(2MASS), H=10.609+-0.022(2MASS), Ks=10.232+-0.024(2MASS). V-Ks = 18.02 - 10.232 = 7.788. 2MASS J0435+1537 = 2MASS J04354898+1537198 = 2MASSW J0435489+153719 M6V: Gizis99(M6e),Hawley02(stan) Only 6 SIMBAD references - 1999-2008. Discovered by Gizis99. Not used as a standard anywhere else besides Hawley02. Poorly studied.