M1V Kirkpatrick(in GrayCorbally09) calls Gl 229A the primary M1V standard. GJ 908 is the only star that I find that both Henry and Hawley agree upon as M1V. KeenanMcNeil76 standard: Gl 229 - M1V Keenan80 standard: Gl 191 (= Kapteyn's star) - M1pVI Gl 617A (=HD 147379) - M1-V Keenan83 standard: Gl 191 (= Kapteyn's star) - M1pVI HD 197481 (=AU Mic) - M1Ve Ba1 Keenan85 standard: Gl 191 (= Kapteyn's star) - M1pVI Keenan88 standard: Gl 191 (= Kapteyn's star) - M1pVI Gl 617A (=HD 147379) - M1-Ve Keenan89 standard: Gl 191 (= Kapteyn's star) - M1pVI Gl 617A (=HD 147379) - M1-eV Kirkpatrick91 standard: Gl 229A - M1V Hawley02 standard: GJ 1141B - M1V (from Reid95) Henry02 standards: Gl 229A - M1V (from Kirkpatrick91) GJ 908 - M1V (from Henry94) GJ 412A - M1V (from Henry94) GJ 514 - M1V (from Henry94) GJ 570BC - M1.0VJ (from Henry94) Kirkpatrick(in GrayCorbally09): Gl 229A - M1V primary standard Kirkpatrick10 standard: GJ 424 - M1V (pri. standard, opt. & near-IR) Pecaut13 standard: GJ 229A - M1.0V (from Henry02) Kirkpatrick16 standard: GJ 229A (=HD 42581) - M1V Keenan89 lists no M1V standards, but does list a non-standard "normal" M1V star (Gl 825), and some M1V variants: GJ 908 (M1V Fe-1), GJ 617A (M1-Ve), AU Mic (M1Ve Ba1). Joy74 M1V stars appear to be M0.5V(+-1.0 subtype) on the Kirkpatrick91 system. RECONS list shows GJ 887 is the nearest M1.0V star, and the only 5 M1.0V stars within the nearest 100 systems are: GJ 887 (B-V=1.476; Mermilliod91), GJ 412A (standard; B-V=1.491), GJ 526 (B-V=1.435; HIP), GJ 205 (B-V=1.474; HIP), GJ 908 (B-V=1.460; HIP). The Kirkpatrick12 sample of d<8pc stars lists the following M1V stars: GJ 412A (standard; B-V=1.491), GJ 229A (B-V=1.491), GJ 908 (B-V=1.464), GJ 514 (B-V=1.497). Mean color B-V = 1.488+-0.009. Note that the primary standard GJ 229A and two secondary standards GJ 514 & 412A - which are M1V standards according to Henry02 (and at least GJ 229A is a primary standard in Kirkpatrick's works), are all classified M0.5 by Hawley97. The Kirkpatrick12 sample of d<8pc stars lists the following M1V stars: GJ 412A (standard; B-V=1.491), GJ 229A (B-V=1.491), GJ 908 (B-V=1.464), GJ 514 (B-V=1.497). Mean color B-V = 1.488+-0.009. (B-V)(M1V) = 1.419 ; ter. stan. GJ 424 (metal poor) (M1V) = 1.438 ; 18 Gray03/06 stars (+-0.011 sem, +-0.035 stdev) (B-V)(M1V) = 1.46 ; SchmidtKaler82 (M1V) = 1.47 ; Fitzgerald70 (M1V) = 1.47 ; ShayaOlling11 (B-V)(M1V) = 1.473 ; exemplar GJ 212 (B-V)(M1V) = 1.474 ; median SIMBAD M1V d<25pc (N=85) (B-V)(M1V) = 1.476 ; non-stan. GJ 887 (M1V) = 1.48 ; Vyssotsky63 (B-V)(M1V) = 1.48 ; JohnsonMorgan53, Johnson66, KenyonHartmann95 (B-V)(M1V) = 1.48 ; Bessell91 "old disk" (B-V)(M1V) = 1.484 (+-0.010 sem,+-0.041 stdev); med. for 14 ARICNS M1V stars (B-V)(M1V) = 1.484 ; prim. stan. GJ 229A ; d<8 pc sample (B-V)(M1V) = 1.488 ; mean of 4 M1V stars within 8 pc from Kirkpatrick12 (B-V)(M1V) = 1.491 ; sec. stan. GJ 412A ; d<8 pc sample (B-V)(M1V) = 1.493 ; sec. stan. GJ 514 ; d<8 pc sample (U-B)(M1V) = 1.22 ; Johnson66 (U-B)(M1V) = 1.21 ; JohnsonMorgan53 (U-B)(M1V) = 1.08 ; ter. stan. GJ 424 (metal poor) (V-I)(M1V) = 1.70 ; ter. stan. GJ 424 (metal poor) (M1V) = 1.841 (+-0.032 sem, +-0.117 stdev; Gray01/03/06 N=18) (V-Ic)(M1V) = 1.96 ; Bessell91 "old disk" (M1V) = 2.020 (+-0.010 sem, +-0.017 stdev; N=3 standards) (V-Ic)(M1V) = 2.08 ; Hawley96 (M1V) = 2.45 ; Johnson66 (V-R)(M1V) = 0.94 ; Bessell91 "old disk" (R-I)(M1V) = 1.02 ; Bessell91 "old disk" (G-J)(M1V) = 2.227 ; Bentley18 (G-Ks)(M1V) = 3.077 ; Bentley18 (Ks-W2)(M1V) = 0.193 ; Bentley18 (W1-W2)(M1V) = 0.057 ; Bentley18 (Ks-W1)(M1V) = 0.137 ; fit to Winters15 data for V-Ks=4.02 (Ks-W1)(M1V) = 0.136 ; Bentley18 (Ks-W1)(M1V) = 0.105 ; Best18 (Ks-W1)(M1V) = 0.093 ; Avenhaus12 for V-Ks=4.02 => adopt (Ks-W1)(M1V) = 0.13 [updated 12/29/2019] (M1V) = 3.06 ; Johnson66 (M1V) = 3.159 (+-0.068 sem, +-0.118 stdev; N=3 standards) (M1V) = 3.19 (+-0.18 stdev) ; Lepine12 (M1V) = 3.76 ; Beuermann06 (V-K)(M1V) = 3.780 ; ter. stan. GJ 424 (metal poor) (V-K)(M1V) = 3.854 ; pri. stan. GJ 229A (predicted from V-J color) (V-K)(M1V) = 3.86 ; Bessell91 "old disk" (V-K)(M1V) = 3.932 ; exemplar GJ 809 = HD 199305 (M1V) = 3.95 ; Johnson66 (V-K)(M1V) = 4.0 ; Hawley96 (V-K)(M1V) = 4.010 ; pri. stan. GJ 229A (predicted from V-I color) (V-K)(M1V) = 4.014 ; sec. stan. GJ 514 (V-Ks)(M1V) = 4.02 ; exemplar GJ 212 (V-K)(M1V) = 4.051 ; sec. stan. GJ 412A (V-K)(M1V) = 4.10 ; pri. stan. GJ 229A (predicted from B-V color) (V-K)(M1V) = 4.25 ; pri. stan. GJ 229A => adopt (V-Ks)(M1V) = 4.00 [last updated (all) 4/9/2020] => adopt (B-V)(M1V) = 1.473 => adopt (U-B)(M1V) = 1.172 => adopt (V-I)(M1V) = 2.005 => adopt (V-R)(M1V) = 0.956 => adopt (R-I)(M1V) = 1.049 => adopt (V-J)(M1V) = 3.164 => adopt (V-H)(M1V) = 3.778 => adopt (H-Ks)(M1V) = 0.222 => adopt (J-H)(M1V) = 0.614 => adopt (K-W1)(M1V) = 0.136 (M1V) = 0.85 ; Beuermann06 (M1V) = 0.18 ; Beuermann06 (Bp-Rp)(M1V) = 1.8470 ; V*_AX_Mic (Bp-Rp)(M1V) = 1.9583 ; GJ_424 ter. stan. (Bp-Rp)(M1V) = 2.0490 ; HD_199305 (Bp-Rp)(M1V) = 2.0822 ; GJ_229A pri. stan. (Bp-Rp)(M1V) = 2.0888 ; GJ_514 sec. stan. (Bp-Rp)(M1V) = 2.1049 ; V*_BR_Psc M1V_Fe-1 (Bp-Rp)(M1V) = 2.1275 ; HD_165222 (Bp-Rp)(M1V) = 2.1689 ; GJ_412A sec. stan. => adopt (Bp-Rp)(M1V) = 2.09 [updated 3/1/2019] (G-Rp)(M1V) = 0.9218 ; V*_AX_Mic M1V (G-Rp)(M1V) = 0.9623 ; GJ_424 ter. stan. (G-Rp)(M1V) = 0.9918 ; HD_199305 M1V (G-Rp)(M1V) = 1.0032 ; GJ_229A pri. stan. (G-Rp)(M1V) = 1.0105 ; GJ_514 sec. stan. (G-Rp)(M1V) = 1.0170 ; V*_BR_Psc M1V_Fe-1 (G-Rp)(M1V) = 1.0224 ; HD_165222 M1V (G-Rp)(M1V) = 1.0901 ; GJ_412A sec. stan. => adopt (G-Rp)(M1V) = 1.01 [updated 3/1/2019] => adopt (Bp-G)(M1V) = 1.08 [last updated 3/1/2019; Bp-Rp=2.09, G-Rp=1.01] (G-V)(M1V) = -0.8516 ; GJ_412A (G-V)(M1V) = -0.8228 ; GJ_514 (G-V)(M1V) = -0.8178 ; GJ_229A (G-V)(M1V) = -0.796 ; median M1V d<60pc (N=182) (G-V)(M1V) = -0.79 ; GJ_424 => adopt (G-V)(M1V) = -0.82 [updated 12/10/2018] => adopt (G-Ks)(M1V) = 4.02 + -0.82 = 3.18 [updated 4/9/2020] => adopt M_G(M1V) = 8.82 = Mv + (G-V) = 9.64 + -0.82 [updated 4/9/2020] Teff(M1V) = 3497 +- 39 K ; Boyajian12b (N=1) Teff(M1V) = 3506 K ; deprecated stan. GJ 570BC Teff(M1V) = 3539 K ; Pecaut13 (sec. stan. GJ 412A) Teff(M1V) = 3565 +- 44 K ; Lepine12 Teff(M1V) = 3580 K ; Morrell19 for stars w/i +-0.05 mag of M_Ks=5.67 Teff(M1V) = 3596 K ; median of 33 published Teffs for M1V stars (EEM) Teff(M1V) = 3600 K ; Johnson66 Teff(M1V) = 3640 K ; ter. stan. GJ 424 Teff(M1V) = 3650 K ; Bessell91 "old disk" Teff(M1V) = 3652 K ; Boyajian12 calibration for V-K=4.099,[Fe/H]=0.0 Teff(M1V) = 3660 K ; Rad=0.4996Rsun & Mann15 calib for M_Ks=5.64, [Fe/H]=0.0 Teff(M1V) = 3664 K ; sec. stan. GJ 412A (median Teff) Teff(M1V) = 3670 K ; ter. stan. GJ 514 (median Teff) Teff(M1V) = 3677 K ; mean photometric Teff Teff(M1V) = 3690 K ; non-stan. GJ 887 Teff(M1V) = 3690 K ; empirical L-R relation for logL=-1.404 Teff(M1V) = 3700 K ; pri. stan. GJ 229A (median Teff) Teff(M1V) = 3700 K ; Rajpurohit13 (N=1; HD 42581a) Teff(M1V) = 3720 K ; Schmidt-Kaler82 Teff(M1V) = 3730 K ; smooth Teff(SpT) trend Teff(M1V) = 3735 K ; RojasAyala12(mean N=10 M1V stars) Teff(M1V) = 3765 K ; candidate standard GJ 212 Teff(M1V) = 3860 K ; Bertone04(NextGen) Teff(M1V) = 3890 K ; Bertone04(ATLAS) => adopt Teff(M1V) = 3660 K (logT = 3.563) [updated 4/9/2020] BCv(M1V) = -1.697 mag ; Flower96(Teff=3700K) [but unreliable, see Torres10] BCv(M1V) = -1.62 mag ; pri. stan. GJ 229A (see notes, but dependent on Golimowski04) BCv(M1V) = -1.54 mag ; sec. stan. GJ 412A (calc from mbol via JHK and Casagrande08 calib.) BCv(M1V) = -1.51 mag ; sec. stan. GJ 514 (calc from mbol via JHK and Casagrande08 calib.) BCv(M1V) = -1.49 mag ; Schmidt-Kaler82(BCv=-1.62 + 0.13 offset) BCv(M1V) = -1.487 mag ; Pecaut13(V-K=4.099) BCv(M1V) = -1.450 mag ; exemplar GJ 887 = Lacaille 9352 BCv(M1V) = -1.440 mag ; Casagrande18(Teff=3700K,logg=4.5) BCv(M1V) = -1.434 +- 0.020 ; sec. stan. GJ 412A (Pecaut13) BCv(M1V) = -1.425 mag ; Mann15(V-J=3.164) BCv(M1V) = -1.424 mag ; Morrell19 for G-Ks=3.18 and adopting V-Ks=4.00 BCv(M1V) = -1.39 mag ; Bessell91("old disk"; BCv = (V-I)-BC_I) BCv(M1V) = -1.325 mag ; Bessell98(ATLAS9,logg=4.5,Teff=3700K) BCv(M1V) = -1.275 mag ; Casagrande08(Teff=3700K) => adopt BCv(M1V) = -1.42 mag [updated 4/9/2020; BC_K=2.58, V-Ks=4.00] BC_K(M1V) = 2.43 mag ; sec. stan. GJ 412A (calculated from JHK via Casagrande08) BC_K(M1V) = 2.50 mag ; sec. stan. GJ 514 (calculated from JHK via Casagrande08) BC_K(M1V) = 2.536 mag ; smoothed trend over M0V-M9V for M1V BC_K(M1V) = 2.539 +- 0.024 ; sec. stan. GJ 412A (Pecaut13) [mbol = 7.308+-0.014, Ks=4.769+-0.020] BC_Ks(M1V)= 2.576 mag ; Morrell19 trend for G-Ks=3.18 BC_K(M1V) = 2.578 mag ; Mann15 calibration for V-J=3.164 BC_K(M1V) = 2.61 mag ; Pecaut13(V-K=4.099) BC_K(M1V) = 2.63 mag ; Leggett01 (J-K=0.835) BC_K(M1V) = 2.63 +- 0.07 mag ; pri. stan. GJ 229A (Golimowski04) => adopt BC_K(M1V) = 2.58 mag [updated 4/9/2020; BC_K=2.58, BCv=-1.42, V-Ks=4.00] Mv(M1V) = 9.3 mag ; Schmidt-Kaler82 Mv(M1V) = 9.33 mag ; pri. standard GJ 229A Mv(M1V) = 9.33 mag ; Kirkpatrick94 Mv(M1V) = 9.42 mag ; median SIMBAD M1V d<25pc (N=85) Mv(M1V) = 9.51 mag ; ter. stan GJ 424 Mv(M1V) = 9.55 mag ; Wegner07 Mv(M1V) = 9.63 mag ; sec. standard GJ 514 Mv(M1V) = 9.64 mag ; V-K=4.00, M_Ks=5.64 Mv(M1V) = 9.66 mag ; Henry94 Mv(M1V) = 9.8 mag ; Reid04 Mv(M1V) = 10.39 mag ; sec. standard GJ 412 A => adopt Mv(M1V) = 9.64 mag [updated 4/9/2020, V-K=4.00, M_Ks=5.64] M_Ks(M1V) = 6.34 ; sec. standard GJ 412 A M_Ks(M1V) = 5.78 ; V-Ks=4.0 => Henry04 M_Ks(M1V) = 5.734 ; ter. stan. GJ 424 M_Ks(M1V) = 5.66 ; V-Ks=4.0 => EEM fit M_Ks(M1V) = 5.69 ; V-Ks=4.0 => JohnsonApps09 for [Fe/H]=0 M_Ks(M1V) = 5.64 ; V-Ks=4.0 => Finsh14 calib M_Ks(M1V) = 5.62 ; sec. standard GJ 514 M_Ks(M1V) = 5.57 ; V-Ks=4.0 => Schlaufman10 for [Fe/H]=0 M_Ks(M1V) = 5.56 ; V-Ks=4.0 => EEM fit to Jao16 M_Ks(M1V) = 5.47 ; V-Ks=4.0 => EEM fit to Reid CNS3 data M_Ks(M1V) = 5.10 ; pri. standard GJ 229A => adopt M_Ks(M1V) = 5.64 mag [updated 4/9/2020] logL(M1V) = -1.29 dex ; pri. stan. GJ 229 A logL(M1V) = -1.35 dex ; sec. stan. GJ 514 logL(M1V) = -1.392 dex ; M_Ks=5.64, BC_Ks=2.58, Mbol=8.220 logL(M1V) = -1.408 dex ; Morrell19 trend for logL for M_Ks=5.67 logL(M1V) = -1.61 dex ; sec. stan. GJ 412A (calculated via JHK and Casagrande08 calib.) => adopt logL(M1V) = -1.392 dex [updated 4/9/2020] => adopt Mbol(M1V) = 8.220 mag [updated 4/9/2020] Mass(M1V) = 0.495 Msun ; M_Ks=5.64 => Mann18 calib Mass(M1V) = 0.503 Msun ; Mv=9.64 => Benedict16 calibration Mass(M1V) = 0.515 Msun ; Eker15 calibration for logL=-1.422 Mass(M1V) = 0.523 Msun ; M_Ks=5.64 => Delfosse00 calibration Mass(M1V) = 0.53 Msun ; Mv=9.77 => HenryMcCarthy93 calibration Mass(M1V) = 0.558 Msun ; M_Ks=5.64 => Benedict16 calibration Mass(M1V) = 0.599+-0.005 Msun ; GJ 278C (Benedict16) Mass(M1V) = 0.62 Msun ; EEM Mv vs. Mass fit for binaries (Mv=9.80) Mass(M1V) = 0.626 Msun ; Mv=9.64 => Torres10 calibration => adopt Mass(M1V) = 0.50 Msun [updated 4/9/2020] Rad(M1V) = 0.547+-0.007 Rsun ; non-stan. GJ 809 Rad(M1V) = 0.506 Rsun ; Rabus19 trend for Teff=3690K Rad(M1V) = 0.5008 Rsun ; Teff=3660K, logL=-1.392 Rad(M1V) = 0.4996 Rsun ; Mann15 trend M_Ks=5.64, [Fe/H]=0.0 Rad(M1V) = 0.483+-0.016 Rsun ; sec. stan. GJ 514 (Yee17) Rad(M1V) = 0.470+-0.001 Rsun ; exemplar GJ 887 = Lacaille 9352 Rad(M1V) = 0.3982+-0.0091 Rsun ; Boyajian12 (N=1) *** (see below) Rad(M1V) = 0.3982 Rsun ; pri. stan. GJ 412A Rad(M1V) = 0.398+-0.009 Rsun ; pri. stan. GJ 412A (Yee17) => adopt Rad(M1V) = 0.501 Rsun [updated 4/9/2020] *** note that N(star) = 1, and for M1.5V, they derive =0.4979+-0.0026 Rsun (presumably GJ 412A) So their M1.5V point appears to be much better constrained. # No Standard JM53, Houk75, Keenan85, Boeshaar85, Corbally86 do not list a M1V standard. # Primary Standard GJ 229A = HD 42581 = LHS 1827 = HIP 29295 (J0610-2151) *M1V: Boeshaar76,KeenanMcNeil76(stan),Kirkpatrick91(pri),Henry02,Kirkpatrick(GrayCorbally09)(pri) M1/M2V: Houk88 M0.5V: Hawley97,Reid04 Secondary is famous first T dwarf GJ229B 36" away. V=8.15(HIP), V=8.129+-0.008(Kilkenny98), B-V=1.487+-0.008(HIP), B-V=1.484+-0.004(Kilkenny98),U-B=1.227+-0.004(Mermilliod91), U-B=1.196+-0.008(Kilkenny98),V-I=2.012+-0.006(Kilkenny98), V-I=2.01+-0.02(HIP), J=5.104+-0.037(2MASS,but flag "E"), K=3.90(Matthews96). 2MASS H & K are saturated. V-J=8.129-5.104=3.025(Kilkenny98 & 2MASS), (V-Ks)=4.25(HIP & Matthews96). Plx=173.81+-0.99(vanLeeuwen07). Mv = 9.33+-0.02 (Kilkenny98,vanLeeuwen07). M_Ks = 5.10 (Matthews96,vanLeeuwen07). Mbol = 7.97+-0.09(Golimowski04), BC_K=2.63+-0.07(Golimowski04), logL=-1.29+-0.02(Golimowski04). Combining the Matthews96 Kmag, Kilkenny98 Vmag, and Golimowski04 BC_K, I estimate BCv = -1.62. The star seems a bit overluminous for its color. Teffs: 3522K(Houdebine10), 3571K(Jenkins09), 3700K(Rajpurohit13), 3700K(Leggett02), 3700K(Morales08), 3720K(Cesetti13), 3755K(Golimowski04), 3790+-90K(Gaidos14), 3814K(Alonso96) => adopt Teff = 3700K. Rad = 0.695+-0.024Rsun(Houdebine10). # Secondary Standards GJ 412A = Lal 21258 = G 176-11 = LHS 38 = LFT 757 = HIP 54211 M0V: Stephenson86 M0.5V: Morgan38,Bidelman85(M0.5),Reid95/Hawley97 *M1V: Henry94,Henry02,Geballe02,RojasAyala12,Lepine13(M1),Gaidos14(M1),Alonso-Floriano15,Mann15 M2V: Adams26,Vyssotsky43,Roman55,Joy74,Terrien15(M2) M3: Lee47 Remarkably poor agreement on type for a standard before the '90s, then agreement since Henry94. 28" binary with M8Ve star. V=8.82(HIP), V=8.742+-0.015(Mermilliod91), B-V=1.491(HIP), B-V=1.532+-0.019(Mermilliod91), U-B=1.175+-0.010(Mermilliod91), V-I=2.01(HIP), J=5.538+-0.019(2MASS), H=5.002+-0.021(2MASS), Ks=4.769+-0.020(2MASS), V-J=3.282(HIP & 2MASS), (V-Ks)=4.051(HIP & 2MASS). Plx=206.27+-1.00 mas(HIP2). Mv = 10.39(HIP,vanLeeuwen07), M_Ks = 6.34+-0.02(2MASS,vanLeeuwen07). mbol = 7.203+-0.029 (JHK=>Casagrande08) => BCv = -1.539, BC_K = 2.434, Mbol = 8.77(w/vanLeeuwen07 plx), logL = -1.61(w/vanLeeuwen07 plx). Teffs: 3512K(Houdebine10), 3537+-41K(Newton15#1), 3544K(Cenarro01,Valdes04), 3600+-30K(Woolf05), 3619+-60K(Mann15#1), 3649+-32K(Mann15#2), 3650K(Prugniel07#1), 3650K(Frasca09), 3664+-227K(Newton15#2), 3664K(Koleva12), 3684K(RojasAyala12), 3687K(Soubiran08), 3696K(Alonso96,Katz11), 3730K(Morales08), 3761+-58K(Ramirez05), 3762K(Schiavon07), 3788K(Prugniel07#2), 3948K(Wu11) => median Teff = 3664K. Inexplicably, Katz11 lists [Fe/H]=0.93 - perhaps a typo. logg=4.85(Prugniel07#1), 4.90(Soubiran08), 4.91(Prugniel07#2). [Fe/H]=-0.43(Prugniel07#1), -0.43(Soubiran08), -0.49(Prugniel07#2). Boyajian12 reports tetLD=0.764+-0.017mas. Boyajian12+HIP2 => 0.398Rsun. GJ 514 = HIP 65859 = LHS 352 = G 063-034 = LFT 1012 (J1330+1022) *M1V: JM53(non-stan),Henry94,Henry02,Kirkpatrick12,Lepine13,Gaidos14 M1.1: Mann15 M1.62: Terrien15 M0.5V: Hawley97 V=9.05(HIP), V=9.048+-0.008(Mermilliod91), U-B=1.228+-0.017(Mermilliod91), B-V=1.493+-0.017(HIP), B-V=1.497+-0.013(Mermilliod91), V-I=2.04+-0.00(HIP), J=5.902+-0.018(2MASS), H=5.300+-0.033(2MASS), Ks=5.036+-0.027(2MASS), V-J=3.148(HIP & 2MASS), (V-Ks)=4.014(HIP & 2MASS). Plx = 130.62+-1.05 mas (vanLeeuwen07). Mv = 9.63+-0.02 (Mermilliod91,vanLeeuwen07), M_Ks = 5.62+-0.03 (2MASS,vanLeeuwen07). mbol = 7.534+-0.014(JHK=>Casagrande08) => BC_K = 2.498, BCv = -1.514, Mbol = 8.11(w/vanLeeuwen07 plx), logL = -1.35(w/vanLeeuwen07 plx). Teffs: 3243+-160K(Berger06; CHARA/2MASS), 3377K(Berger06; CHARA/BC), 3512+-50K(Houdebine10), 3544K(V-K=>Casagrande08), 3578K(Jenkins09), 3630K(Lepine13), 3700K(V-K=>Mozurkewich03), 3720K(Morales08), 3727+-61K(Mann15#1), 3727+-69K(Gaidos14), 3755+-30K(Mann15), 3896K(Terrien15,median) => median Teff = 3670K. Rad=0.483+-0.016Rsun(Yee17). # Tertiary Standard GJ 424 = SZ UMa = LHS 41 = BD+66_717 = HIP 55360 = TYC 4152-272-1 M0: Hawley97 M0.5: Lepine13 *M1V: Adams35,Morgan38,JM53(non-standard),Herbig60,Bidelman85,Delfosse98,Jenkins09,Kirkpatrick10(pri.stan),McLean12,Reiners12,Gaidos14,Newton14(near-IR) M1.5: Joy74 M2: Vyssotsky43,Stephenson86 M3: Lee47 A few knocks: it is a tight binary, and it is metal poor (and high velocity), and slightly bluer than the other standards, but there is good modern agreement on M1V type and Kirkpatrick10 considers it a standard. WDS reports it as binary star TAM 1 (Tamazian), 0.1" separation mag1=9.36, mag2=13.06 M0V+M4.5. V=9.31(HIP),V=9.32(Morel78), V=9.314+-0.015(Mermilliod91), U=11.82(Morel78), B=10.74(Morel78), R_J=7.95(Morel78), I_J=6.94(Morel78), J_J=6.68(Morel78), K_J=5.43,5.52(Morel78), L=5.30(Morel78), H=5.71(Morel78). B-V=1.412+-0.018(HIP), B-V=1.419+-0.009(Mermilliod91), U-B=1.080+-0.000(Morel78), V-I=1.70+-0.05(HIP), J=6.306+-0.018(2MASS), H=5.730+-0.020(2MASS), Ks=5.534+-0.017(2MASS). V-Ks=3.780+-0.023, Hp=9.3513+-0.0025. plx=112.13+-1.03(vanLeeuwen07), plx=109.65+-0.79 (GaiaDR1) => Mv=9.514+-0.022(Mermilliod91,GaiaDR1), M_Ks=5.734+-0.023(2MASS,GaiaDR1). logL=-1.38+-0.06(Newton15), R=0.485+-0.028(Newton15), R=0.56+-0.05(Gaidos14), M=0.60(Gaidos14), [Fe/H]=-0.52, -0.70(Newton14). Motion is ~3"/year! Teffs: 3348K(Leger15), 3576K(Alonso96), 3586+-51K(Ramirez05), 3640K(Lepine13), 3729+-79K(Newton15), 3800K(Stelzer13), 3888+-105K(Gaidos14) => Teff=3640K. # Exemplars GJ 212 = HD 233153 = HIP 26801 = BD+53 935 K7: Cannon27 *M1V: Joy74,Bidelman85(M1),Stephenson86,Rojas-Ayala12(M1),Lepine13(M1.0),Gaidos14(M1),Newton14(near-IR),Alonso-Floriano15,Mann15(M1.0) M0.5: Hawley97 M2V: Lee47(M2),Vyssotsky56 9 independent estimates as M1V since 1974, and only modern classification that differs is PMSU (at 0.5 level). Notably the last 6 classifications since 2010 are all exactly M1V. Star unfortunately does not appear in DwarfArchives. plx=78.0+-9.1mas(Finch16), plx=80.40+-1.69mas (vanLeeuwen07). B-V=1.473+-0.011(Mermilliod91), V=9.779+-0.022(Mermilliod91), U-B=1.165(Mermilliod91), J=6.586+-0.021(2MASS), H=5.963+-0.016(2MASS), Ks=5.759+-0.016(2MASS), V-Ks = 9.779 - 5.759 = 4.02. Teff: 3500K(Lepine13), 3531+-50K(Houdebine10), 3733+-90K(Gaidos14), 3765+-40K(Mann15), 3768+-96K(Gaidos14#2), 3832K(Alonso96), 3851+-17K(RojasAyala12) => 3765K. GJ 887 = Lacaille 9352 = HD 217987 = LHS 70 = HIP 114046 M0.5: Bidelman85,Hawley97,Kirkpatrick12(Hawley97),Rieners12 *M1.0V: Dieterich12 M1.1: Mann15 M2V: Adams26,Evans57(M2Ve),Upgren72,Walker83,Burnashev85,Torres06,Bonfils13 M2.5V: Joy84 M2/3V: Houk82 Probably adopt M1V from Dieterich12/Mann15, and indeed its Teff and (B-V) are right in amongst the other M1V stars. Most of the M2V types are old and predate Kirkpatrick system. One of the brightest M dwarfs on the sky, but a surprisingly huge dispersion in types from M0.5 to M2.5. The 2nd largest angular diameter for an M dwarf in the compilation of Rabus19 (Table1), with diameter measured to 0.3% accuracy. [Fe/H]=-0.06+-0.08(Mann15), Teffs: 3688+-86K(Mann15), 3695+-35K(Newton15) => 3690K. B-V=1.476+-0.012(Mermilliod91), V=7.356+-0.014(Mermilliod91), U-B=1.175+-0.048(Mermilliod91). 2MASS photometry is poor (flags=DDC). Rabus19: tetLD=1.328+-0.004mas, fbol=(10.916+-0.657)e-8 erg/s/cm2 (=> mbol = 5.906+-0.065 IAU2015 scale), Rad=0.470+-0.001Rsun, Teff=3692+-57K. plx = 304.2190+-0.0451mas(GaiaDR2). BCv = mbol - V = 5.906 - 7.356 = -1.450. GJ 809 = HD 199305 = HIP 103096 = LHS 3595 (J2053+6209) M0V: Kirkpatrick92PhD,Henry94,Henry02,Kirkpatrick12 M0.5V: Hawley97 *M1: Gaidos14,Lepine13(M1.0),Mann15 M4: Lee47 M2V: Keenan46 Kirkpatrick12 lists the primary as "M0 V" (joint type, cites Kirkpatrick92(PhD)) and calls the companion "M? V?" (cites "this paper"). However, four recent surveys (Gaidos, Lepine, Hawley) place it 0.5-1 subtype later. Lepine13 used multiple spectral indices which gave M0.84. V=8.55(HIP), V=8.554+-0.037(Mermilliod91), B-V=1.483+-0.012(HIP), B-V=1.483+-0.012(Mermilliod91), V-I=1.97+-0.07(HIP), U-B=1.237+-0.009(Mermilliod91), J=5.429+-0.029(2MASS), Ks=4.618+-0.024(2MASS), V-J=3.121(HIP,2MASS), (V-Ks)=3.932(HIP,2MASS). Teff= 3400K(Lepine13), 3630K(Alonso96), 3646+-53K(Ramirez05), 3692+-22K(Boyajian12), 3715+-14K(Pecaut13), 3720+-50K(Woolf05), 3791+-60K(Mann15#1), 3843K(Gaidos14), 3846+-37K(Mann15) => Teff = 3715K. 3791K. R=0.54Rsun(Gaidos14), R=0.515+-0.01 Rsun(Mann15), mass=0.58Msun(Gaidos14), Mass = 0.546+-0.013 Msun (Mann15). Boyajian12 reports tetLD=0.722+-0.008mas. plx=142.0341+-0.0305mas(GaiaDR2). Boyajian12+GaiaDR2 => Rad=0.547Rsun. Rad=0.547+-0.007Rsun(Yee17). # Deprecated Standards GJ 15A = BD+43_44A = GX And = HD 1326A *M1.5V: GrayAtlas,Boeshaar94,Henry94(not standard),Henry02 M1V: JM53(non-standard),Hawley97,Reid04 M2V: Keenan85,Keenan88,Keenan99,Sozetti02 Keenan repeatedly classified GJ 15A as M2, but everyone else considers it M1 or M1.5. Segranson03 VLTI study: M=0.414+-0.021 Msun, R=0.383+-0.02 Rsun, Teff = 3698+-95 K, logg=4.89+-0.06 dex. GJ 908 = LHS 550 = BR Psc = HIP 117473 = Lal 46650 M0V: Newton14(near-IR) M1V: Stephenson86,Henry94,Hawley97,Henry02 M1V Fe-1: Keenan89 M1.4: Mann15 *M1.5V: Bidelman85(M1.5),Lepine13 M2V: Vyssotsky43,JM53(non-stan),Cowley82(M2Ve),Torres06,Gaidos14 M2.5Ve: Joy74 M3: Lee47 Type has mostly oscillated between ~M1 and ~M2 over the years. : [Fe/H]=-0.95+-0.19, as does Mann15 [Fe/H]=-0.45+-0.08. V=8.983+-0.012(Mermilliod91), B-V=1.464+-0.028(Mermilliod91), U-B=1.104+-0.025(Mermilliod91), J=5.827+-0.023(2MASS), H=5.282+-0.031(2MASS), Ks=5.043+-0.020(2MASS). V-Ks=3.940(Mermilliod91,2MASS). mbol = 7.503+-0.025 (JHK => Casagrande08 calib.) => BCv = -1.48, BC_K = 2.46. Plx = 167.29+-1.23 mas. Mv=10.10+-0.02(Mermilliod91, vanLeeuwen07), M_Ks=6.16+-0.03(2MASS,vanLeeuwen07). This star was also modeled by Leggett96: flux = 2.50e-11 W/m^2, logL=-1.59, mbol=7.53, Mbol=8.74, BCv=-1.45, BC_K=2.48. Teffs: 3646+-60K(Mann15#1), 3700+-150K(Leggett96), 3704+-29K(Mann15), 3712+-85K(Gaidos14) => adopt Teff=3700K. Nice to see the Leggett96 and Casagrande08-derived mbol agree at the +-0.03 mag level! GJ 1191B = MCC 277B = StKM 2-690 [B?] = LDS 917B = HIP 53947 = 2MASS J11021804+1630333 (V=11.35) *M1V: Stephenson86(A+B?),Hawley97(M1),Hawley02(stan,Reid95) M0V: Vyssotsky52 I've only included it here since it was used by Hawley02 as the M1V template for an analysis of Sloan survey M dwarf spectra. AB separation 18.6" in WDS - listed as LDS 917. Hipparcos split the system as HIP 53947 [comp. B] and 53953 [comp. A]. Sloan brown dwarf 2MASS J11021199+1629393 is 103" away. No DwarfArchives classification. Clearly there are other stars with better classification pedigrees than this one. Given that Hawley97 classified the three best Kirkpatrick and Henry M1V standards (GJ 229A, 412A, 514) *all* as M0.5, then chances are GJ 1191B is probably also ~M0.5 on a grid of Kirkpatrick and Henry standards. So it would not shock me if the Sloan M1V "template" is ~0.5 subtype hotter/earlier than other well-characterized local M1V star, on average. GJ 570BC = LHS 386 = HD 131976 = BD-20 4123 = Lalande 27173BC M1.0V: Walker83,Henry94(Kirkpatrick12),Hawley97,Henry02("joint"),Geballe02,Houdebine12(dM1) *M1V+M3:V: Kirkpatrick12 M1.0V+M1.0V: Reid04 M1.5V: Keenan89(stan),Gray06 M1.5V+M3V: Pourbaix/SB9 M2V: Vyssotsky56,Cowley67,Joy74,Stephenson86,Gaidos14,Newton14 M2III: Houdebine10(prob. because of poor parallax) M0.5: Bidelman85 Unfortunately Keenan considered M1.5, but Henry considers M1. I deprecate the Keenan type as the Henry types have become modern standards. 0.0437" binary according to Tokovinin15, with delta(y)=1.6, and SB orbit from Forvielle99 (Period 308 days). 25" away from primary HR 5568 (HD 131977). Forveille99 splits the BC components, with M_J(B) = 6.213+-0.033, M_J(C) = 7.403+-0.039, and M_K(B) = 5.396+-0.033, M_K(C) = 6.576+-0.039, so delta(K) = 1.18. Given this delta(mag), it likely that the companion is >2 subtypes later, similar to what Pourbaix reports. Forvielle99 section 4 discusses the IR photometry for the pair in more detail. Magnitudes are unresolved unless specifically stated: V=8.065(Koen10), B-V=1.494(Koen10), U-B=1.200(Koen10), V-Rc=0.990(Koen10), V-Ic=2.122(Koen10). Mass=0.586+-0.007Msun(Torres10), R=0.52+-0.05Rsun(Gaidos14). Teffs: 3454+-50K(Houdebine12), 3500+-100K(Torres10), 3506K(Cenarro01,Sanchez-Blazquez06,Cenarro07), 3650K(Stelzer13), 3788+-88K(Gaidos14) => 3506K. [Fe/H]=0.10+-0.13, 0.12+-0.02(Newton14). Note that GJ 570A appears to roughly solar metallicity. Forvielle99 derives dynamical masses of M(B) = 0.586+-0.007 Msun, M(C) = 0.390+-0.005. # Variants GJ 617A = LHS 3175 = HD 147379 = Lalande 29917 = HIP 73182 M1-Ve: Keenan88 GJ 191 = Kapteyn's star sdM1.0: Hawley97(Koen10) *M1pVI: KeenanMcNeil76(stan; "M1p", Keenan89(stan) M2.0V: Henry(RECONS) (B-V)=1.580 (Koen10). Segransan03 VLTI study reports: M = 0.281+-0.014 Msun, R = 0.291 +- 0.025 Rsun, Teff = 3570+-156 K, logg = 4.96+-0.13 dex. The caption to plate 19 of KeenanMcNeil76 discusses the classification of Kapteyn's star as a "M1 subdwarf (class VI)". # Other Stars GJ 825 = HD 202560 = AX Mic = Lacaille 8760 = UGP 518 = LHS 66 (J2117-3852) K7.0: Hawley97(Kirkpatrick12) K9.0V: Isaacson17 M0V: Evans57(M0Ve),Upgren72,Bidelman85(M0),Torres06 *M0.5V: Walker83 M1V: Adams26,Joy74,Keenan89(non-stan),Gaidos14(M1) M1/2V: Houk82 Brightest southern M dwarf (V=6.7), and the one "pure" M1V in Keenan89 (although not a standard, although there are two M1V variants). Not really good enough agreement to consider a standard. Note that Joy74's M1V corresponds roughly to M0.5(+-1.0) on the Kirkpatrick91 system (see notes in M0V.txt), and Teff (below) is most similar to M0.5V-ish. Teffs: 3592K(Alonso96), 3599+-52K(Ramirez05), 3776+-80K(Gaidos14), 3796+-18K(Koleva12), 3912K(Moro-Martin15), 3930K(Morales08) => = 3786K. [Fe/H]=-0.62+-0.07(Koleva12), logg=4.55+-0.08(Kovleva12). # Non-standard stars YY Gem: Torres02 finds that the eclipsing binary YY Gem consists of nearly identical M1V stars with T = 3820 +- 100 K. Keenan89 called them "M0.5Ve Fe-2", however Hill75 and JoyAbt74 called it "M1Ve" also. The "mean" value of the components has M = 0.5992 +- 0.0047 Msun, R = 0.6191 +- 0.0057 Rusn, logg = 4.6317 +- 0.0083, L = 0.0733 +- 0.0015 Lsun, Mv = 8.950 +- 0.029, Mbol = 7.569 +- 0.020.