B3V Garrison94 lists two B3V anchor standards: eta UMa and eta Aur MK43 standard: eta Aur - B3V eta UMa - B3V JM53 standards: eta Aur - B3V eta Hya - B3V eta UMa - B3V HD 6300 - B3V 35 Ari - B3V nu Ori - B3V HD 178849 - B3V HD 191236 - B3V 16 Peg - B3V HD 218537 - B3V Garrison67 standard: eta Aur - B3V Lesh68 standard: eta Aur - B3V (secondary is HD 178329) Hiltner69 standard: eta Aur - B3V Schild71 standard: eta Aur - B3V Walborn71 standards: eta Aur & eta UMa - B3V Cowley72 standards: eta Aur & iot Her - B3V MK73 dagger standards: eta Aur & eta UMa - B3V Houk75 standard: nu Ori - B3V (primary standard) Garrison77 standard: eta Aur - B3V MK78 standards: 29 Per - B3V Keenan85 standard: 29 Per - B3V Walborn90 standards: eta Hya (= HD 74280) - B3V WiegertGarrison98 stan: eta Hya - B3V GrayAtlas standard: 29 Per - B3V GrayNstars standards: 29 Per & iot Her - B3V Skiff08 flaged three B3V standards: HD 120315 (MK73), HD 32630 (MK73), & HD 20365 (MK78). All dereddening via the Q-method in this file has been updated with the revised calibration (10/9/2011). B-V(B3V) = -0.167 ; EEM dereddened prim. stan. HD 142883 (via Q-method) B-V(B3V) = -0.171 ; EEM dereddened prim. stan. 29 Per (via Q-method) B-V(B3V) = -0.180 ; EEM dereddened anchor stan. eta Aur (via Q-method) B-V(B3V) = -0.181 ; EEM dereddened N=101 HIP B3V stars (Q-method, E(B-V)<0.1) B-V(B3V) = -0.190 ; EEM dereddened anchor stan. eta UMa (zero reddening) B-V(B3V) = -0.198 ; Crawford76 B-V(B3V) = -0.199 ; EEM dereddened prim. stan. eta Hya (via Q-method) B-V(B3V) = -0.20 ; JohnsonMorgan53, Morgan53, Johnson63, Johnson66 B-V(B3V) = -0.20 ; Garrison67, Fitzgerald70, Morgan71, SchmidtKaler82 The bluest B-V I can find for a B3V star is HIP 115347 (B-V = -0.199+-0.008), so <(B-V)o> is near this value. U-B(B3V) = -0.623 ; EEM dereddened pri. stan. HD 142883 (via Q-method) U-B(B3V) = -0.638 ; EEM dereddened pri. stan. 29 Per (via Q-method) U-B(B3V) = -0.669 ; EEM dereddened pri. stan. eta Aur (via Q-method) U-B(B3V) = -0.673 ; EEM dereddened pri. stan. eta UMa (zero reddening) U-B(B3V) = -0.675 ; EEM dereddened N=101 HIP B3V stars (Q-method, E(B-V)<0.1) U-B(B3V) = -0.68 ; Fitzgerald70 U-B(B3V) = -0.71 ; Johnson63, Johnson66, Schmidt-Kaler82 U-B(B3V) = -0.737 ; EEM dereddened pri. stan. eta Hya (via Q-method) U-B(B3V) = -0.75 ; Bessell98 => adopt (U-B)(B3V) = -0.673 *** [updated 9/26/2019] => adopt (B-V)(B3V) = -0.178 => adopt Q(B3V) = -0.543 (=(U-B)-0.72*(B-V) = -0.673 - 0.72*-0.181) => adopt (V-I)(B3V) = -0.192 => adopt (V-R)(B3V) = -0.080 => adopt (R-I)(B3V) = -0.111 (V-Ks)(B3V) = -0.333 ; HIP_70248_ B3V d= 163.881pc, (B-V)=0.017 (dereddened from Kervella19) (V-Ks)(B3V) = -0.390 ; HIP_92989_ B3V d= 145.328pc, (B-V)=0.019 (dereddened from Kervella19) (V-Ks)(B3V) = -0.421 ; HIP_37450_ B3V d= 191.058pc, (B-V)=0.008 (dereddened from Kervella19) (V-Ks)(B3V) = -0.424 ; HIP_21881_ B3V d= 120.817pc, (B-V)=0.021 (dereddened from Kervella19) (V-Ks)(B3V) = -0.437 ; HIP_65271_ B3V d= 112.322pc, (B-V)=0.019 (dereddened from Kervella19) (V-Ks)(B3V) = -0.474 ; HIP_61199_ B3V d= 116.023pc, (B-V)=0.014 (dereddened from Kervella19) (V-Ks)(B3V) = -0.476 ; HIP_60710_ B3V(n) d= 135.612pc, (B-V)=0.015 (dereddened from Kervella19) (V-Ks)(B3V) = -0.485 ; HIP_29038_ B3V d= 183.722pc, (B-V)=0.009 (dereddened from Kervella19) (V-Ks)(B3V) =-0.492 ; from intrinsic color trend (U-B)=-0.673 (V-Ks)(B3V) = -0.507 ; HIP_59449_ B3V d= 80.0256pc, (B-V)=0.007 (dereddened from Kervella19) (V-Ks)(B3V) = -0.533 ; HIP_117315_ B3V d= 181.291pc, (B-V)=0.005 (dereddened from Kervella19) (V-Ks)(B3V) = -0.550 ; HIP_90200_ B3V d= 178.508pc, (B-V)=0.020 (dereddened from Kervella19) (V-Ks)(B3V) = -0.551 ; HIP_71865_ B3V d= 99.2654pc, (B-V)=0.014 (dereddened from Kervella19) (V-Ks)(B3V) = -0.553 ; HIP_99080_ B3V d= 145.943pc, (B-V)=0.012 (dereddened from Kervella19) (V-Ks)(B3V) = -0.558 ; HIP_42799_ B3V d= 155.569pc, (B-V)=0.009 (dereddened from Kervella19) (V-Ks)(B3V) = -0.567 ; HIP_43105_ B3V(n) d= 188.501pc, (B-V)=0.013 (dereddened from Kervella19) (V-Ks)(B3V) = -0.572 ; HIP_99824_ B3V d= 174.611pc, (B-V)=0.016 (dereddened from Kervella19) (V-Ks)(B3V) = -0.580 ; HIP_52633_ B3V d= 114.456pc, (B-V)=0.007 (dereddened from Kervella19) (V-Ks)(B3V) = -0.606 ; HIP_64004_ B3V d= 146.606pc, (B-V)=0.017 (dereddened from Kervella19) => adopt (V-Ks)(B3V) = -0.492 [updated 4/8/2022] => adopt (V-J)(B3V) = -0.373 [updated 4/8/2022] => adopt (V-H)(B3V) = -0.471 [updated 4/8/2022] => adopt (H-Ks)(B3V) = -0.021 [updated 4/8/2022] => adopt (J-H)(B3V) = -0.098 [updated 4/8/2022] (g-r)(B3V) = -0.46 ; Covey07 (Ks-W1)(B3V) = 0.026 ; EEM trend for d<30pc for B-V=-0.178 => adopt (Ks-W1)(B3V) = 0.026 [updated 12/29/2019] (Bp-Rp)(B3V) = -0.268 ; Evans18 trend for V-I=-0.192 (G-V)(B3V) = 0.00968 ; HIP_20543 B3V E(B-V)=0.003 (G-V)(B3V) = 0.001 ; fit for B dwarfs from Kervella19 corrected for E(B-V), eval for (V-Ks)=-0.492 => adopt (G-V)(B3V) = 0.001 [updated 4/8/2022 Teff(B3V) = 19000 K ; Bohm-Vitense81 Teff(B3V) = 18920 K ; Bertone04[ATLAS] Teff(B3V) = 18750 K ; Bessell98 Teff(B3V) = 18700 K ; Schmidt-Kaler82 Teff(B3V) = 18445 K ; Theodossiou90 Teff(B3V) = 18040 K ; B-V=-0.180 => Teff(Bessell98,logg=4.3) Teff(B3V) = 17899 K ; pri. stan. eta Hya (median Teff) Teff(B3V) = 17820 K ; median for Braganca12 B3V stars (N=101) Teff(B3V) = 17705 K ; mean photometric Teff Teff(B3V) = 17370 K ; mean photometric Teff Teff(B3V) = 17319 K ; EEM N=208 Teffs Teff(B3V) = 17200 K ; anchor stan. eta UMa (median Teff) Teff(B3V) = 17100 K ; Chavez95 (+-200K) Teff(B3V) = 17000 K ; Crowther97/Fig.3 Teff(B3V) = 17000 K ; anchor stan. eta Aur (median Teff) Teff(B3V) = 16785 K ; U-B=-0.673 => Teff(Bessell98) Teff(B3V) = 16500 K ; GrayCorbally09 Teff(B3V) = 16479 K ; B-V=-0.180 => Teff(Napiwotzki93) Teff(B3V) = 16445 K ; pri. stan. 29 Per (median Teff) Teff(B3V) = 16218 K ; Simon-Diaz17 for B3V (N=8) Teff(B3V) = 16030 K ; pri. stan. HD 142883 (median Teff) Teff(B3V) = 16000 K ; GrayCorbally94 => adopt Teff(B3V) = 17000 K (logT = 4.230) [updated 9/16/2019] Mv(B3V) = -0.51 mag ; pri. stan. HD 142883 (see below) Mv(B3V) = -0.6 mag ; HD 120315 (Jaschek98) Mv(B3V) = -0.66 mag ; anchor stan. eta UMa (see below) Mv(B3V) = -0.88 mag ; Upper Sco main sequence (B-V=-0.181, rms=+-0.39 mag) Mv(B3V) = -1.04 mag ; ONC main sequence (B-V=-0.181, rms=+-0.48 mag) Mv(B3V) = -1.1 mag ; HD 20365 (Jaschek98) Mv(B3V) = -1.1 mag ; HD 32630 (Jaschek98) Mv(B3V) = -1.19 mag ; anchor stan. eta Aur (see below) Mv(B3V) = -1.20 mag ; median Mv for B3V calc using Kervella19 HIP & Gaia DR2 Mv(B3V) = -1.47 mag ; pri. stan. 29 Per (see below) Mv(B3V) = -1.5 mag ; HD 74280 (Jaschek98) Mv(B3V) = -1.52 mag ; Bowen08 Mv(B3V) = -1.6 mag ; Schmidt-Kaler82 Mv(B3V) = -1.6 mag ; Russeil03 Mv(B3V) = -1.68 mag ; Wegner07 Mv(B3V) = -1.7 mag ; GrayCorbally09 Mv(B3V) = -1.99 mag ; pri. stan. eta Hya (see below) => adopt Mv(B3V) = -1.20 mag [updated 12/27/2020] => adopt M_Ks(B3V) = -0.708 mag = Mv - (V-Ks) = -1.20 - -0.492 [updated 12/30/2020] => adopt Mv(B3V)ZAMS = -0.96 mag BCv(B3V) = -1.81 mag ; Schmidt-Kaler82(BCv=-1.94 + 0.13 offset) BCv(B3V) = -1.674 mag ; Code76(Teff=17000K, set so BCv(5772K)=-0.085) BCv(B3V) = -1.621 mag ; Flower96(Teff=17000K, set so BCv(5772K)=-0.085 BCv(B3V) = -1.591 mag ; Nieva13(Teff=17000K) BCv(B3V) = -1.538 mag ; Bessell98(ATLAS9,logg=4.0,Teff=17000K, set so BCv(5772K)=-0.085) BCv(B3V) = -1.550 mag ; LanzHubeny07(Teff=17000K,logg=4.0,Z/Zsun=1) BCv(B3V) = -1.520 mag ; Balona94(Teff=17000K, set so BCv(5772K)=-0.085) BCv(B3V) = -1.471 mag ; Bertone04[Teff=17000K,ATLAS, set so BCv(5772K)=-0.085) => adopt BCv(B3V) = -1.54 [updated 9/16/2019, adjusted so that BCv(5772K)=-0.085] logL = 2.992 dex ; adopting Mv = -1.2, BCv = -1.54 => Mbol = -2.740 logL = 2.885 dex ; logL/Teff trend for OB dwarf EBs (Torres10; Teff=17000K) => adopt logL(B3V) = 2.992 dex [updated 4/4/2020] => adopt Mbol(B3V) = -2.740 mag [updated 4/4/2020] Mass(B3V) = 6.55+-0.42 Msun ; Hohle10 Mass(B3V) = 6.240+-0.066 Msun ; Eclipsing binary V539 Ara A (Torres10) Mass(B3V) = 6.07 Msun ; Harmanec88 Mass(B3V) = 5.6 Msun ; Pri. stan. Eta Aur (Maestro13) Mass(B3V) = 5.49 Msun ; Bertelli09 solar tracks Teff=17000,logL=2.992 Mass(B3V) = 5.43 Msun ; EEM logL vs. Mass fit for binaries (logL=2.992) Mass(B3V) = 5.39 Msun ; MIST/Choi16 solar tracks logT=4.230, logL=2.992 Mass(B3V) = 5.38 Msun ; Ekers18 ML calibration for logL=2.992 Mass(B3V) = 5.24 Msun ; EEM Teff vs. Mass fit for binaries (Teff=17000K) Mass(B3V) = 5.23 Msun ; EEM Mv vs. Mass fit for binaries (Mv=-1.2) Mass(B3V) = 5.16+-0.06 Msun ; Eclipsing binary V1388 Ori B (Torres10) => adopt Mass(B3V) = 5.4 Msun [updated 4/16/2022] Rad(B3V) = 3.64+-0.10 Rsun ; pri. stan. Eta Aur (Maestro13) Rad(B3V) = 3.12 Rsun ; logL=2.9, 92Teff=17000K => adopt Rad(B3V) = 3.612 Rsun [updated 4/4/2020] # Anchor Standards HD 32630 = Eta Aur = HR 1641 = ALS 8168 = HIP 23767 = Hoedus II (J0506+4114) *B3V: MK43,JM53,Garrison67(stan),Lesh68(stan),Hiltner69(stan),Walborn71,MK73,Garrison77(stan),Garrison94,Garrison96 M91: V=3.172+-0.008, B-V=-0.178+-0.009, U-B=-0.669+-0.005 => updated Q-method calibration (10/9/2011) => (B-V)o=-0.180, (U-B)o=-0.669, E(B-V)= 0.002, Av=0.005 (i.e. negligible reddening). Teffs: 16375 K (Adelman02/spec), 16712K(U-Bo=>Bessell98), 16800 K (Philip80), 16887 K (Adelman02/ubvy), 17379 K (Philip80), 17390 K (Zorec09#1), 17940 K (Zorec09#2), 18660+-230K (Maestro13) => median Teff ~ 17000 K. It is slightly alarming that the Maestro13 value (measured using CHARA) is so far at odds with previous estimates. Plx = 13.40+-0.20 mas (vanLeeuwen07) => D = 75+-1 pc. Welsh90 estimate logN_H = 18.840. Using Savage & Mathis (1979) logNH vs E(B-V) relation, this would suggest E(B-V) = 0.001 mag, i.e. negligible. Assume its unreddened. Mv = -1.19+-0.03. Maestro13 estimates Mass = 5.6+-0.1 Msun and age 41+-6 Myr. RV = +7.3+-0.7 km/s (Gontcharov06). XHIP catalog lists U,V,W = -13.6, -23.2, -5.5 km/s. HD 120315 = Eta UMa = Alcaid = HR 5191 *B3V: MK43,JM53,Walborn71,MK73,Walborn90,Garrison94,Garrison96 M91: V=1.860+-0.009, B-V=-0.190+-0.007, U-B=-0.673+-0.017 => Q-method consistent with negligible reddening (and d < 75 pc) => (B-V)o=-0.190, (U-B)o=-0.673, E(B-V)=Av=0. VanLeeuwen07 plx = 31.38+-0.24 mas => hence, probably negligible reddening. Mv = -0.66+-0.02 mag. Teffs: 16795K(U-Bo=>Bessell98), 16900K(Adelman02/spec), 16904K(Blackwell80), 17200K(Sokolov95), 17319K(Adelman02/ubvy), 17379K(Philip80), 17870K(Zorec09) => median Teff = 17200 K. # Primary Standards HD 20635 = 29 Per = Cl Melotte 20 383 (alpha Per cluster) *B3V: Cannon(B3),Roman50,Slettebak55,Heckmann58(B3),Jaschek64(major.),Lesh68,Petrie69,Morgan71,Jaschek78,MK78,Keenan85,Garcia89,GrayAtlas B4IV: Abt78 B3IV: Miczaika51 Appears to be an excellent standard. M91: V=5.145+-0.013, B-V=-0.056+-0.005, U-B=-0.557+-0.009 => updated Q-method calibration (10/9/2011) => (B-V)o=-0.171, (U-B)o=-0.638, E(B-V)= 0.115, Av=0.376. Adopting d=177+-4 pc (plx = 5.65+-0.13 mas) for alpha Per cluster (de Zeeuw et al. 1999), then Mv = -1.47+-0.05 mag. Teffs: 16090K(U-Bo=>Bessell98), 16800K(Philip80) => median Teff = 16445K. HD 142883 = HR 5934 = HIP 78168 (J1558-2058) *B3V: Bertiau58(B3:V),Morris61,Garrison67,Slettebak68,Hiltner69,Hill70,Garrison79(stan),Houk88 B5: Cannon Skiff09: all 6 references all call it B3V. deZeeuw+99 Upper Sco member. Excellent standard? M91: V=5.853+-0.007, B-V=0.021+-0.005, U-B=-0.489+-0.010 => updated Q-method (10/9/2011) => (B-V)o=-0.167, (U-B)o=-0.623, E(B-V)=0.188, Av=0.614. VanLeeuwen07 plx = 7.08+-0.33 mas => D = 141+-7 pc (agrees well with Upper Sco distance 145 pc). Mv = -0.51 +- 0.10 mag. Teffs: 15802K(U-Bo=>Bessell98), 16258K(Philip80) => median Teff = 16030K. HD 74280 = eta Hya = HR 3454 *B3V: JM53,Jaschek64(all),Jaschek78(JM53),Walborn90,Cannon(B3),Houk99(Garrison),Levenhagen06 B2V: Russeil07 B4V: Lesh68 Agreement among Morgan/Garrison/Walborn/Houk/Cannon. Good standard. M91: V=4.297+-0.008, B-V=-0.195, U-B=-0.735 => revised Q-method (10/9/2011) => (B-V)o=-0.199, (U-B)o=-0.737, E(B-V)=0.004, Av = 0.013 (lowest reddening among B3V standards). This star is one of the "Ten Primary Standards of the U, B, V System" in Johnson (1963), with V=4.30, B-V=-0.195, U-B = -0.74. Johnson (1966) lists V=4.30, B-V=-0.20, U-B=-0.74. Cousins (1971) adopts it as a standard and lists V=4.295+-0.009, B-V = -0.195+-0.005, and U-B = -0.74, so statistically identical to Johnson (1963, 1966). van Leeuwen (2007) lists parallax = 5.56+-0.24 mas (D = 180+-8 pc), however its reddening seems utterly negligible. Mv = -1.99+-0.09 mag. Teffs: 17482K(Prugniel07#3), 17502K(Prugniel07#2), 17899K(LeBorgne03), 17978K(Prugniel07#1), 18203K(U-Bo=>Bessell98) => median Teff = 17899K. logg=3.83(LeBorgne03). [Fe/H]=-0.09(LeBornge03). # Secondary Standards HD 6300 = HR 302 = SAO 91988 = BD+50_212 *B3V: Cannon(B3),JM53,Hoffleit91,Jaschek64(all),Jaschek78(Lesh68) All published types are B3 or B3V, but no types since Lesh68. M91: V=6.528+-0.013, B-V=-0.081+-0.010, U-B=-0.579+-0.061. HD 16908 = 35 Ari = HR 801 *B3V: Cannon(B3),JM53,Jaschek64(all but one),Jaschek78(Lesh68) All published types are B3 (excepting a 1931 source), but no types since Lesh68. M91: V=4.656+-0.012, B-V=-0.136+-0.005, U-B=-0.625+-0.005. HD 208057 = 16 Peg = HR 8356 *B3V: JM53,Jaschek64(most),Jaschek78(Lesh68),Slettebak82,Cannon(B3),Mendoza58(B3) B6V: : Herman59 In Jaschek82 catalog of Be stars, however only one published type (from 1949) uses "e" Good standard, but it might be a Be star? M91: V=5.073+-0.008, B-V=-0.169+-0.011, U-B=-0.680+-0.099 (big unc.). HD 178849 = HIP 94043 B3V: JM53,Jaschek78(Guetter68),Cannon(B3),O'Keefe41 B5V: Abt81 V=7.0, NErn of 14" common proper motion pair (companion is A0,V=8.40). M91: V=7.025+-0.025, B-V=-0.130+-0.010, U-B=-0.635+-0.005. # Weak Standards HD 191263 = HR 7700 = HIP 99234 B3V: JM53 B3IV: Jaschek78(Lesh68) B2.5V: Guetter68 B2IV: Crampton71 B5: Cannon Not great agreement after JM53 called this a standard. HD 218537 = HR 8808 B3V: JM53,Jaschek78(Lesh68),Abt81,Cannon(B3) B2V: Guetter68 B2.5V: Garrison70 JM53 B3V standard, but Garrison called B2.5V. HD 178329 = *B3V: JM53,Jaschek78(Lesh68(stan)),Hill77,Cannon(B3) B2V: Guetter68 V=6.5. Only Lesh68 considered it a standard, otherwise OK? HD 41753 = nu Ori = HR 2159 B3V: Houk,JM53 B3IV: Jaschek78(Lesh68) B2: Cannon B0(V): 1980ApJS...44..389B Jaschek64 types are mix of B3IV and B3V. Houk75 B3V primary standard. HD 160762 = iot Her B3V: JM53,Cowley72(stan),Jaschek64(most) *B3IV: MK43,Lesh68,MK78 B3: Cannon,Neubauer43 JM53 noted "SB". Consistently B3. Best considered "B3IV" standard (MK78). # Other Stars lam Tau A B2V: Hill75 *B3V: Slettebak55,Garrison96 B3IV+A: Levato75 B3.0 + A3/4: Olson68 B3: Cannon Eclipsing binary, p=3.95 days. "B" is A4IV according to Garrison96. Inappropriate as standard, and not considered a standard in the literature. HD 133955 = HR 5626 (Sco-Cen member) B3V: multiple sources including Hiltner69(see Skiff 2010) 29 Tau B3V: several references (see Skiff) mu Tau = HD 26912 B3V: Slettebak55,1955MmMtS..12....1W,Cucchiaro80 B3IV: Lesh68,Grenier99 B4: 1927MNRAS..86..364E B4III:: 1930MmMtS...2....1R V=4.280+-0.010(Mermilliod91), B-V=-0.060+-0.009(Mermilliod91), U-B=-0.522+-0.017(Mermilliod91) => Q-method(PecautMamajek13) => (B-V)o=-0.169, (U-B)o=-0.592, E(B-V)=0.099, Av=0.323, Teff=15930K. plx=6.6651+-0.3319mas(GaiaDR2), plx=7.16+-0.34mas (HIP2). age=37.8+-8.5 Myr(Tetzlaff11). Garrison96 listed 4 of the brightest stars as B3V (or variant): alf Eri (B3Vnp(shell)), lam Tau A (eclipsing SB2; B=A4IV), eta Aur, and eta UMa.