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
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)
<B-V>(M1V) = 1.438 ; 18 Gray03/06 stars (+-0.011 sem, +-0.035 stdev)
(B-V)(M1V) =   1.46  ; SchmidtKaler82
<B-V>(M1V) =   1.47  ; Fitzgerald70
<B-V>(M1V) =   1.47  ; ShayaOlling11
(B-V)(M1V) = 1.473 ; candidate stan. GJ 212
(B-V)(M1V) =  1.476  ; non-stan. GJ 887 
<B-V>(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)
<V-Ic>(M1V) = 1.841 (+-0.032 sem, +-0.117 stdev; Gray01/03/06 N=18)
(V-Ic)(M1V) = 1.96 ; Bessell91 "old disk"
<V-Ic>(M1V) = 2.020 (+-0.010 sem, +-0.017 stdev; N=3 standards) 
(V-Ic)(M1V) = 2.08 ; Hawley96
<V-I>(M1V)  = 2.45 ; Johnson66

(V-R)(M1V)  = 0.94 ; Bessell91 "old disk"

(R-I)(M1V)  = 1.02 ; Bessell91 "old disk"

<V-J>(M1V)  = 3.06 ; Johnson66
<V-J>(M1V)  = 3.159 (+-0.068 sem, +-0.118 stdev; N=3 standards) 
<V-J>(M1V)  = 3.19  (+-0.18 stdev) ; Lepine12

<V-K_CIT>(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)     =  3.95 ; 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  ; candidate stan. 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-K)(M1V)  = 4.02  [last updated (all) 9/25/2017]
=> adopt (B-V)(M1V)  = 1.475
=> adopt (U-B)(M1V)  = 1.172
=> adopt (V-I)(M1V)  = 2.019
=> adopt (V-R)(M1V)  = 0.959
=> adopt (R-I)(M1V)  = 1.060
=> adopt (V-J)(M1V)  = 3.184
=> adopt (V-H)(M1V)  = 3.797
=> adopt (V-Ks)(M1V) = 4.020
=> adopt (H-Ks)(M1V) = 0.223
=> adopt (J-H)(M1V)  = 0.613
=> adopt (K-W1)(M1V) = 0.137
=> adopt (G-V)(M1V)  = -0.800

<J-K_CIT>(M1V) = 0.85 ; Beuermann06

<H-K_CIT>(M1V) = 0.18 ; Beuermann06

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) =  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) = 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) = 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) = 3700 K (logT = 3.568)  [EEM: updated 2/16/2016]

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) =  -1.48 mag  ; BC_K=2.54, V-K=4.02
BCv(M1V) = -1.441 mag ; Mann15(V-J=3.184)
BCv(M1V) =  -1.434 +- 0.020 ; sec. stan. GJ 412A (Pecaut13)
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) = -1.48 mag [last updated 3/8/2018; BC_K = 2.54, V-K=4.02]

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_K(M1V) = 2.581 mag ; V-J=3.184 => Mann15 calibration
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) = 2.54 mag [last updated 3/8/2018]

Mv(M1V) =   9.3  mag ; Schmidt-Kaler82
Mv(M1V) =   9.33 mag ; pri. standard GJ 229A
Mv(M1V) =    9.33 mag ; Kirkpatrick94
Mv(M1V) =   9.51 mag ; ter. stan GJ 424
Mv(M1V) =   9.55 mag ; Wegner07
Mv(M1V) =   9.63 mag ; sec. standard GJ 514
Mv(M1V) =   9.66 mag ; Henry94
Mv(M1V) =  9.69 mag ; V-K=4.02, M_Ks=5.67
Mv(M1V) =   9.8  mag ; Reid04
Mv(M1V) =  10.39 mag ; sec. standard GJ 412 A
=> adopt Mv(M1V) = 9.69 mag  [updated 9/25/2017, V-K=4.02, M_Ks=5.67] see M_Ks below

M_Ks(M1V) = 6.34  ; sec. standard GJ 412 A
M_Ks(M1V) = 5.81  ; V-Ks=4.02 => Henry04
M_Ks(M1V) = 5.734 ; ter. stan. GJ 424
M_Ks(M1V) = 5.69  ; V-Ks=4.02 => EEM fit
M_Ks(M1V) = 5.69  ; V-Ks=4.02 => JohnsonApps09
M_Ks(M1V) = 5.67  ; V-Ks=4.02 => Dieterich14 
M_Ks(M1V) = 5.62  ; sec. standard GJ 514
M_Ks(M1V) = 5.59  ; V-Ks=4.02 => EEM fit to Jao16
M_Ks(M1V) = 5.50  ; V-Ks=4.02 => EEM fit to Ried CNS3 data
M_Ks(M1V) = 5.10  ; pri. standard GJ 229A 
=> adopt M_Ks(M1V) = 5.67 mag  [updated 9/25/2017]

logL(M1V) = -1.29 dex ; pri. stan. GJ 229 A
logL(M1V) = -1.35 dex ; sec. stan. GJ 514
logL(M1V) = -1.404 dex ; M_Ks=5.67, BC_Ks=2.58, Mbol=8.25
logL(M1V) = -1.404 dex ; Mv=9.69, BCv=-1.44, Mbol=8.25
logL(M1V) = -1.61 dex ; sec. stan. GJ 412A (calculated via JHK and Casagrande08 calib.)
=> adopt logL(M1V) = -1.404 dex
=> adopt Mbol(M1V) =  8.250 mag 

Mass(M1V) = 0.496 Msun ; Mv=9.69 => Benedict16 calibration
Mass(M1V) =  0.515 Msun ; Eker15 calibration for logL=-1.422
Mass(M1V) =  0.510 Msun ; M_Ks=5.70 => Delfosse10 calibration
Mass(M1V) =  0.53 Msun ; Mv=9.77 => HenryMcCarthy93 calibration
Mass(M1V) =  0.532 Msun ; Mv=9.69 => Delfosse10 calibration
Mass(M1V) =  0.548 Msun ; M_Ks=5.70 => Delfosse10 calibration
Mass(M1V) = 0.553 Msun ; M_Ks=5.67 => 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) =  0.623 Msun ; Mv=9.69 => Torres10 calibration
=> adopt Mass(M1V) = 0.54 Msun   [updated 3/8/2018]

Rad(M1V) = 0.474 Rsun ; Teff=3700K, logL=-1.422
Rad(M1V) = 0.3982 +- 0.0091 Rsun ; Boyajian12 (N=1) ***
*** note that N(star) = 1, and for M1.5V, they derive <R>=0.4979+-0.0026 Rsun.
    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 = LFT 757 = HIP 54211 = Lal 21258  = G 176-11 = LHS 38
 *M1V: Henry94,Henry02
  M0.5V: Hawley97

  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.  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).

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.

# Tertiary Standard

GJ 424 = SZ UMa = LHS 41 = BD+66_717 = HIP 55360 = TYC 4152-272-1
 *M1V: Adams35,Morgan38,JM53(non-standard),Herbig60,Bidelman85,Delfosse98,Jenkins09,Kirkpatrick10(pri.stan),McLean12,Reiners12,Gaidos14,Newton14(near-IR)
  M0.5: Lepine13
  M0: Hawley97
  M1.5: Joy74
  M2: Vyssotsky43,Stephenson86
  M3: Lee47

  A few knocks: it is a tight binary, and it is metal poor (and high
  velocity), 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.

# Candidate Standard

GJ 212 = HD 233153 = HIP 26801 = BD+53 935
 *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
  K7: Cannon27

  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.

# 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)".

# 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.

GJ 887 = Lacaille 9352
  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.  [Fe/H]=-0.06+-0.08(Mann15), Teffs: 3688+-86K(Mann15),
  3695+-35K(Newton15) => <Teff> 3690K.
  B-V=1.476+-0.012(Mermilliod91), V=7.356+-0.014(Mermilliod91),
  U-B=1.175+-0.048(Mermilliod91).

GJ 809 = 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).
  
GJ 825 = HD 202560 = AX Mic = UGP 518 = LHS 66 (J2117-3852)
  K7.0: Hawley97
  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) => <Teff> =
  3786K. [Fe/H]=-0.62+-0.07(Koleva12), logg=4.55+-0.08(Kovleva12).