HAZMAT. V. The Ultraviolet and X-ray Evolution of K Stars

TL;DR

This study provides the first detailed analysis of the ultraviolet and X-ray evolution of K stars, revealing they emit significantly less high-energy radiation than M stars, which impacts planetary habitability assessments.

Contribution

It offers the first comprehensive investigation into the UV and X-ray evolution of K stars, filling a gap in stellar activity research relevant to exoplanet habitability.

Findings

K stars have 5-50 times lower UV/X-ray flux than early-M stars.

K dwarf activity decreases earlier than M dwarfs.

Habitable zones around K stars receive much less high-energy radiation.

Abstract

Knowing the high-energy radiation environment of a star over a planet's formation and evolutionary period is critical in determining if that planet is potentially habitable and if any biosignatures could be detected, as UV radiation can severely change or destroy a planet's atmosphere. Current efforts for finding a potentially habitable planet are focused on M stars, yet K stars may offer more habitable conditions due to decreased stellar activity and more distant and wider habitable zones (HZ). While M star activity evolution has been observed photometrically and spectroscopically, there has been no dedicated investigation of K-star UV evolution. We present the first comprehensive study of the near-UV, far-UV, and X-ray evolution of K stars. We used members of young moving groups and clusters ranging in age from 10 - 625 Myr combined with field stars and their archived GALEX UV and ROSAT X-ray data to determine how the UV and X-ray radiation evolve. We find that the UV and X-ray flux incident on a HZ planet is 5 - 50 times lower than that of HZ planets around early-M stars and 50 - 1000 times lower than those around late-M stars, due to both an intrinsic decrease in K dwarf stellar activity occurring earlier than for M dwarfs and the more distant location of the K dwarf HZ.

Tables

Table 1. Table 1: Mass estimates based on the spectral type to effective temperature transformations of Pecaut & Mamajek ( 2013 ) and the evolutionary models of Baraffe et al. ( 2015 ) .

SpT	TW Hya	$\beta$ Pic	Tuc-Hor	AB Dor	UMa	Hyades	Field
	10 Myr	24 Myr	45 Myr	149 Myr	300 Myr	625 Myr	5 Gyr
K0	1.30	0.98	0.90	0.93	0.92	0.92	0.89
K1	1.26	0.96	0.88	0.89	0.89	0.89	0.86
K2	1.20	0.93	0.86	0.86	0.86	0.86	0.83
K3	1.10	0.89	0.83	0.80	0.80	0.80	0.79
K4	0.98	0.83	0.80	0.75	0.75	0.75	0.74
K5	0.90	0.78	0.77	0.71	0.71	0.71	0.70
K6	0.78	0.74	0.72	0.63	0.65	0.66	0.65
K7	0.75	0.72	0.69	0.59	0.62	0.62	0.61
K8	0.72	0.71	0.66	0.57	0.60	0.60	0.60
K9	0.68	0.68	0.63	0.54	0.57	0.57	0.57
M0	0.59	0.62	0.60	0.51	0.56	0.53	0.53
M1	0.49	0.52	0.52	0.45	0.50	0.47	0.47

Table 2. Table 2: Number of K stars in each group or cluster.

Group/Cluster	Age	Input	Observed in NUV	Detected in NUV	Observed in FUV	Detected in FUV	Detected in X-ray
	[Myr]	Sample	by GALEX	by GALEX	by GALEX	by GALEX	by ROSAT
TWA	10 $\pm$ 3aaNumber of data points used in each fit.	4	3	2	2	2	4
Beta Pic	24 $\pm$ 3bbfootnotemark:	30	21	19	16	15	27
Columba	42${}_{-4}{}^{}{}_{}{}^{+6}$aaNumber of data points used in each fit.	14	11	10	10	5	4
Carina	45${}_{-7}{}^{}{}_{}{}^{+11}$aaNumber of data points used in each fit.	3	1	1	1	1	3
Tuc-Hor	45 $\pm$ 4aaNumber of data points used in each fit.	26	25	24	24	22	20
AB Dor	149${}_{-19}{}^{}{}_{}{}^{+51}$aaNumber of data points used in each fit.	12	11	6	10	10	12
Ursa Major	414 $\pm$ 23ccfootnotemark:	12	7	3	7	7	8
Praesepe	600ddfootnotemark:	133	52	49	62	17	0
Hyades	625 $\pm$ 50eefootnotemark:	169	110	97	92	30	52
Field	$\sim$5000	310	229	169	211	152	107

Table 3. Table 3: Fits to log ​ ( y ) = m ∗ log ​ ( x ) + b log y m log x b \rm{log}(y)=m*log(x)+b in logarithmic space.

log(x)	log(y)	Subset	Slope (m)	Intercept (b)	R2	No.aaNumber of data points used in each fit.
[$\mu$Jy or Myr]	[$\mu$Jy]
NUV Excess	FUV Excess	0.5 - 0.6 M⊙	0.784 $\pm$ 0.177	-0.107 $\pm$ 0.594	0.399	6
NUV Excess	FUV Excess	0.6 - 0.7 M⊙	1.086 $\pm$ 0.039	-1.387 $\pm$ 0.120	0.493	61
NUV Excess	FUV Excess	0.7 - 0.8 M⊙	0.583 $\pm$ 0.025	0.033 $\pm$ 0.091	0.328	75
NUV Excess	FUV Excess	0.8 - 0.9 M⊙	0.463 $\pm$ 0.074	0.605 $\pm$ 0.297	0.124	27
NUV Excess	FUV Excess	0.9 - 1 M⊙	0.231 $\pm$ 0.123	1.750 $\pm$ 0.502	0.061	5
NUV Excess	FUV Excess	All	0.663 $\pm$ 0.016	-0.174 $\pm$ 0.056	0.418	174
X-ray	NUV Excess	All	0.360 $\pm$ 0.009	-6.888 $\pm$ 0.097	0.281	110
X-ray	FUV Excess	All	0.665 $\pm$ 0.012	-4.717 $\pm$ 0.130	0.745	130
Age	NUV Excess	10 Myr - 150 Myr	0.003 $\pm$ 0.472	-10.635 $\pm$ 0.836	0.000	3
Age	NUV Excess	150 Myr - 5 Gyr	-0.536 $\pm$ 0.343	-9.498 $\pm$ 0.976	0.877	3
Age	FUV Excess	10 Myr - 625 Myr	-0.266 $\pm$ 0.257	-11.280 $\pm$ 0.495	0.968	4
Age	FUV Excess	625 Myr - 5 Gyr	-0.987 $\pm$ 0.426	-9.275 $\pm$ 1.414	1.000	2
Age	X-ray	10 Myr - 150 Myr	-0.424 $\pm$ 0.467	-9.612 $\pm$ 0.746	0.981	3
Age	X-ray	150 Myr - 5 Gyr	-0.923 $\pm$ 0.285	-8.522 $\pm$ 0.881	0.999	3

Table 4. Table 4: Observed flux densities F 𝐹 F , fluxes f 𝑓 f , and model photospheric flux densities σ 𝜎 \sigma of the stars used in this analysis.

NameaaNames starting with J are 2MASS objects.	RA	Dec	Mass	Dist.	FJ	${\sigma }_J$	FNUV	${\sigma }_{NUV}$	FFUV	${\sigma }_{FUV}$	fX
	2MASS	2MASS	[M⊙]	[pc]	[$\mu$Jy]	[$\mu$Jy]	[$\mu$Jy]	[$\mu$Jy]	[$\mu$Jy]	[$\mu$Jy]	[erg cm-2 s-1]
TW Hydra, 10 Myr
J11015191-3442170	11 01 51.9052	-34 42 17.033	0.61	60.09	1.12E+07	6.13E+06	¿ 9.29E+03	6.79E+01	9.20E+04 $\pm$ 1.85E+03	5.13E-04	2.36E-10 $\pm$ 1.70E-11
J11482422-3728491	11 48 24.2227	-37 28 49.114	0.75	76.38	3.12E+07	2.03E+07	1.44E+04 $\pm$ 6.60E+02	9.29E+01	1.55E+03 $\pm$ 4.04E+02	6.47E-04	1.65E-10 $\pm$ 2.56E-11
J12153072-3948426	12 15 30.7230	-39 48 42.594	0.68	53.11	2.43E+07	1.80E+07	4.14E+03 $\pm$ 2.41E+02	7.05E+01	— $\pm$ —	—	8.16E-11 $\pm$ 1.32E-11
Beta Pictoris, 23 Myr
J00233468+2014282	00 23 34.6661	+20 14 28.637	0.71	63.15	3.53E+07	1.18E+07	7.73E+03 $\pm$ 4.20E+02	6.70E+01	— $\pm$ —	—	6.59E-11 $\pm$ 8.22E-12
J01373940+1835332	01 37 39.4099	+18 35 33.259	0.89	52.15	2.71E+07	3.24E+07	¿ 3.75E+03	3.07E+04	4.76E+04 $\pm$ 1.02E+03	7.19E-03	1.62E-10 $\pm$ 9.06E-12
J02272924+3058246	02 27 29.2543	+30 58 24.596	0.74	41.05	1.91E+07	1.29E+07	5.38E+03 $\pm$ 1.25E+02	8.24E+01	5.29E+02 $\pm$ 6.08E+01	1.10E-03	6.49E-11 $\pm$ 4.98E-12
J02303239-4342232	02 30 32.4110	-43 42 23.383	0.78	52.64	2.74E+07	1.44E+07	7.60E+03 $\pm$ 2.48E+02	1.10E+02	4.01E+02 $\pm$ 9.80E+01	8.41E-04	4.82E-11 $\pm$ 5.61E-12
J02304623-4343493	02 30 46.245	-43 43 49.55	0.72	52.84	9.75E+06	1.21E+07	1.20E+03 $\pm$ 1.10E+02	7.18E+01	1.81E+02 $\pm$ 6.84E+01	8.88E-04	— $\pm$ —
J02412589+0559181	02 41 25.88830	+05 59 18.4211	0.74	44.44	2.17E+07	1.29E+07	7.01E+03 $\pm$ 1.24E+02	8.24E+01	8.17E+02 $\pm$ 6.92E+01	1.10E-03	8.19E-11 $\pm$ 7.36E-12
CD-57 1054	05 00 47.1298	-57 15 25.453	0.52	26.90	1.68E+07	7.11E+06	2.60E+03 $\pm$ 6.68E+01	2.37E+01	4.22E+02 $\pm$ 4.68E+01	3.26E-05	3.19E-11 $\pm$ 1.56E-12
J05200029+0613036	05 20 00.291	+06 13 03.57	0.83	97.51	2.82E+07	1.71E+07	8.22E+03 $\pm$ 1.58E+03	1.92E+02	— $\pm$ —	—	5.55E-11 $\pm$ 1.12E-11
J05203182+0616115	05 20 31.8236	+06 16 11.589	0.83	97.26	3.02E+07	1.71E+07	7.59E+03 $\pm$ 1.80E+03	1.92E+02	— $\pm$ —	—	9.79E-11 $\pm$ 1.39E-11
J06182824-7202416	06 18 28.2077	-72 02 41.447	0.72	39.26	2.39E+07	1.21E+07	1.17E+04 $\pm$ 1.66E+02	7.18E+01	1.03E+03 $\pm$ 6.81E+01	8.88E-04	1.29E-10 $\pm$ 3.74E-12
HIP 50156	10 14 19.17664	+21 04 29.554	0.52	23.40	1.29E+07	7.11E+06	2.30E+03 $\pm$ 8.14E+01	2.37E+01	4.31E+02 $\pm$ 6.82E+01	3.26E-05	2.11E-11 $\pm$ 1.60E-12
J10593870+2526138	10 59 38.6780	+25 26 13.712	0.78	21.32	1.61E+07	1.44E+07	7.50E+03 $\pm$ 1.10E+02	1.10E+02	1.16E+02 $\pm$ 2.28E+01	8.41E-04	— $\pm$ —
J14142141-1521215	14 14 21.35665	-15 21 21.7551	0.78	28.96	1.43E+07	1.44E+07	4.29E+03 $\pm$ 9.54E+01	1.10E+02	8.51E+02 $\pm$ 9.19E+01	8.41E-04	4.81E-11 $\pm$ 3.15E-12
J16430128-1754274	16 43 01.2956	-17 54 27.539	0.52	71.05	1.34E+07	7.11E+06	3.34E+03 $\pm$ 2.41E+02	2.37E+01	¡ 1.19E+03	3.26E-05	4.06E-11 $\pm$ 8.69E-12
J19114467-2604085	19 11 44.670	-26 04 08.85	0.83	59.07	3.26E+07	1.71E+07	1.31E+04 $\pm$ 3.89E+02	1.92E+02	7.05E+02 $\pm$ 1.48E+02	7.19E-03	5.65E-11 $\pm$ 9.46E-12
J21100461-1920302	21 10 04.614	-19 20 30.21	0.74	34.27	7.96E+06	1.29E+07	7.67E+02 $\pm$ 5.52E+01	8.24E+01	2.89E+02 $\pm$ 4.78E+01	1.10E-03	4.71E-11 $\pm$ 4.28E-12
J21212446-6654573	21 21 24.49374	-66 54 57.3788	0.93	31.98	2.52E+07	2.47E+07	1.80E+04 $\pm$ 1.37E+02	5.94E+02	7.02E+02 $\pm$ 4.61E+01	2.10E-02	4.43E-11 $\pm$ 4.31E-12
TYC 2211-1309-1	22 00 41.5840	+27 15 13.535	0.62	35.56	7.62E+06	9.14E+06	2.81E+03 $\pm$ 8.17E+01	3.90E+01	¡ 5.77E+01	1.65E-04	2.18E-11 $\pm$ 2.13E-12
J22424896-7142211	22 42 48.9342	-71 42 21.190	0.78	36.66	1.64E+07	1.44E+07	5.77E+03 $\pm$ 4.24E+01	1.10E+02	7.36E+02 $\pm$ 6.36E+01	8.41E-04	7.73E-11 $\pm$ 6.37E-12
BD-13 6424	23 32 30.8613	-12 15 51.476	0.62	27.37	1.25E+07	9.14E+06	2.11E+03 $\pm$ 8.80E+00	3.90E+01	3.15E+02 $\pm$ 4.62E+00	1.65E-04	3.83E-11 $\pm$ 2.81E-12
Columba, 42 Myr
J03205070-1916086	03 20 50.70	-19 16 08.6	0.72	44.05	1.57E+07	1.10E+07	7.94E+03 $\pm$ 1.29E+02	1.73E+02	5.14E+02 $\pm$ 6.43E+01	5.79E-03	— $\pm$ —
J03405279-2231207	03 40 52.79	-22 31 20.7	0.86	80.57	2.00E+07	2.60E+07	1.68E+04 $\pm$ 4.61E+02	2.51E+03	¡ 1.65E+02	1.19E-01	— $\pm$ —
J04111512-5806479	04 11 15.12	-58 06 47.9	0.83	47.48	2.22E+07	2.18E+07	9.72E+03 $\pm$ 2.40E+02	2.34E+03	1.10E+02 $\pm$ 4.39E+01	1.17E-01	— $\pm$ —
J04325379-2736058	04 32 53.79	-27 36 05.8	0.72	56.02	1.06E+07	1.10E+07	1.96E+03 $\pm$ 1.25E+02	1.73E+02	¡ 9.58E+01	5.79E-03	— $\pm$ —
J04483160-1046496	04 48 31.60	-10 46 49.6	0.80	81.09	2.16E+07	1.78E+07	1.18E+04 $\pm$ 5.81E+02	5.22E+02	4.89E+02 $\pm$ 1.89E+02	1.76E-02	— $\pm$ —
J04590561-6325297	04 59 05.61	-63 25 29.7	0.72	86.99	5.52E+07	1.10E+07	8.35E+04 $\pm$ 1.06E+03	1.73E+02	6.01E+02 $\pm$ 1.75E+02	5.79E-03	1.40E-11 $\pm$ 3.15E-12
J05002847-2201400	05 00 28.47	-22 01 40.0	0.69	91.26	1.72E+07	9.62E+06	3.18E+03 $\pm$ 1.94E+02	6.15E+01	6.48E+02 $\pm$ 2.25E+02	9.19E-05	— $\pm$ —
J05275536-2743229	05 27 55.36	-27 43 22.9	0.86	101.50	5.04E+07	2.60E+07	5.10E+04 $\pm$ 1.04E+03	2.51E+03	¡ 3.12E+02	1.19E-01	— $\pm$ —
J05525904-0725278	05 52 59.04	-07 25 27.8	0.80	70.22	1.70E+07	1.78E+07	4.66E+03 $\pm$ 6.12E+02	5.22E+02	— $\pm$ —	—	— $\pm$ —
J06272781-3547244	06 27 27.81	-35 47 24.4	0.77	97.23	1.60E+07	1.46E+07	2.56E+03 $\pm$ 4.74E+02	3.45E+01	¡ 5.80E+02	5.80E-03	— $\pm$ —
Carina, 45 Myr
HIP 30034 A	06 19 12.91	-58 03 15.6	0.88	50.12	3.73E+07	3.03E+07	5.46E+04 $\pm$ 5.53E+02	9.78E+03	1.45E+03 $\pm$ 1.54E+02	6.68E-01	1.04E-10 $\pm$ 3.80E-12
Tucana Horologium, 45 Myr
HIP 1910	00 24 08.98105	-62 11 04.2982	0.69	44.23	1.38E+07	9.69E+06	2.83E+03     $\pm$ 1.47E+02	6.85E+01	6.39E+02   $\pm$ 1.11E+02	4.60E-04	2.52E-11 $\pm$ 7.10E-12
CT Tuc	00 25 14.6619	-61 30 48.251	0.72	44.16	1.11E+07	1.13E+07	2.23E+03 $\pm$ 9.59E+01	1.92E+02	2.79E+02 $\pm$ 5.23E+01	6.15E-03	— $\pm$ —
HD 3221	00 34 51.2018	-61 54 58.127	0.77	44.50	3.67E+07	1.53E+07	1.71E+04 $\pm$ 2.65E+02	1.29E+02	1.57E+03 $\pm$ 1.41E+02	6.44E-04	8.03E-11 $\pm$ 9.93E-12
CD-78 24	00 42 20.3154	-77 47 39.755	0.80	49.76	2.03E+07	1.89E+07	1.13E+04 $\pm$ 2.08E+02	8.44E+02	¡ 1.01E+02	3.11E-02	4.81E-11 $\pm$ 8.08E-12
J02000918-8025009	02 00 9.18	-80 25 00.9	0.80	74.65	2.98E+07	1.89E+07	1.09E+04 $\pm$ 2.99E+02	8.44E+02	¡ 1.79E+02	3.11E-02	— $\pm$ —
CD-60 416	02 07 32.2079	-59 40 21.054	0.80	45.46	1.54E+07	1.89E+07	¡ 7.31E+01	8.44E+02	8.04E+02 $\pm$ 1.17E+02	3.11E-02	8.13E-11 $\pm$ 8.31E-12
J02105538-4603588	02 10 55.38	-46 03 58.8	0.80	81.78	2.05E+07	1.89E+07	1.74E+04 $\pm$ 1.67E+02	8.44E+02	9.65E+02 $\pm$ 1.78E+02	3.11E-02	8.09E-11 $\pm$ 1.13E-11
J02372562-4912033	02 37 25.614	-49 12 03.32	0.60	50.68	6.48E+06	6.37E+06	1.75E+02 $\pm$ 4.83E+01	3.26E+01	¡ 7.80E+01	2.02E-04	— $\pm$ —
CD-53 544	02 41 46.8340	-52 59 52.376	0.77	43.81	2.84E+07	1.53E+07	8.59E+03 $\pm$ 1.90E+02	1.29E+02	1.35E+03 $\pm$ 1.08E+02	6.44E-04	1.27E-10 $\pm$ 6.36E-12
CD-58 553	02 42 33.0232	-57 39 36.812	0.77	49.72	1.48E+07	1.53E+07	3.86E+03 $\pm$ 1.29E+02	1.29E+02	5.54E+02 $\pm$ 8.40E+01	6.44E-04	2.11E-11 $\pm$ 4.91E-12
CD-35 1167	03 19 08.6657	-35 07 00.296	0.77	45.56	1.23E+07	1.53E+07	2.32E+03 $\pm$ 9.26E+01	1.29E+02	2.97E+02 $\pm$ 5.79E+01	6.44E-04	1.85E-11 $\pm$ 4.31E-12
CD-44 1173	03 31 55.6411	-43 59 13.549	0.60	45.28	1.56E+07	6.37E+06	3.60E+03 $\pm$ 4.66E+01	3.26E+01	4.75E+02 $\pm$ 8.24E+01	2.02E-04	3.73E-11 $\pm$ 4.58E-12
CD-44 1173	03 31 55.6411	-43 59 13.549	0.60	45.28	1.56E+07	6.37E+06	3.60E+03 $\pm$ 4.66E+01	3.26E+01	4.75E+02 $\pm$ 8.24E+01	2.02E-04	— $\pm$ —
J04000382-2902165	04 00 03.82	-29 02 16.5	0.77	49.38	2.54E+07	1.53E+07	1.45E+04 $\pm$ 3.59E+02	1.29E+02	1.90E+03 $\pm$ 2.03E+02	6.44E-04	1.17E-10 $\pm$ 7.52E-12
J04000395-2902280	04 00 03.95	-29 02 28.0	0.80	48.82	1.85E+07	1.89E+07	9.19E+03 $\pm$ 2.84E+02	8.44E+02	9.44E+02 $\pm$ 1.43E+02	3.11E-02	1.14E-10 $\pm$ 7.35E-12
J04021648-1521297	04 02 16.48	-15 21 29.7	0.83	54.84	2.45E+07	2.35E+07	2.83E+04 $\pm$ 6.16E+02	3.50E+03	1.36E+03 $\pm$ 2.02E+02	1.71E-01	5.61E-11 $\pm$ 6.44E-12
J04480066-5041255	04 48 00.6676	-50 41 25.663	0.72	59.60	1.81E+07	1.13E+07	3.24E+03 $\pm$ 2.37E+02	1.92E+02	5.57E+02 $\pm$ 1.39E+02	6.15E-03	5.22E-11 $\pm$ 5.45E-12
J05332558-5117131	05 33 25.58	-51 17 13.1	0.77	53.95	1.18E+07	1.53E+07	2.48E+03 $\pm$ 5.88E+01	1.29E+02	2.24E+02 $\pm$ 1.16E+02	6.44E-04	1.32E-11 $\pm$ 2.32E-12
HIP 107345	21 44 30.12081	-60 58 38.8797	0.69	46.36	1.08E+07	9.69E+06	2.42E+03 $\pm$ 6.83E+01	6.85E+01	3.74E+02 $\pm$ 5.18E+01	4.60E-04	2.33E-11 $\pm$ 3.78E-12
HIP 107345	21 44 30.12081	-60 58 38.8797	0.69	46.36	1.08E+07	9.69E+06	2.42E+03 $\pm$ 6.83E+01	6.85E+01	3.74E+02 $\pm$ 5.18E+01	4.60E-04	— $\pm$ —
J22021626-4210329	22 02 16.26	-42 10 33.0	0.52	44.35	8.44E+06	4.89E+06	1.52E+03 $\pm$ 5.85E+01	1.87E+01	3.52E+02 $\pm$ 5.09E+01	4.11E-05	2.78E-11 $\pm$ 4.05E-12
J23261069-7323498	23 26 10.7051	-73 23 49.895	0.66	46.29	9.94E+06	8.36E+06	2.43E+03 $\pm$ 1.58E+02	3.18E+01	7.65E+02 $\pm$ 1.34E+02	7.81E-04	4.19E-11 $\pm$ 5.85E-12
J23474694-6517249	23 47 46.95	-65 17 24.9	0.52	45.39	7.53E+06	4.89E+06	1.46E+03 $\pm$ 1.14E+02	1.87E+01	2.63E+02 $\pm$ 8.19E+01	4.11E-05	1.49E-11 $\pm$ 2.83E-12
J23585674-8339423	23 58 56.74	-83 39 42.3	0.72	55.63	1.11E+07	1.13E+07	2.09E+03 $\pm$ 4.60E+01	1.92E+02	1.79E+02 $\pm$ 7.47E+01	6.15E-03	— $\pm$ —
AB Doradus, 150 Myr
HIP 5191	01 06 26.14	-14 17 46.8	0.89	45.43	2.26E+07	2.68E+07	2.18E+04$\pm$ 4.19E+02	1.31E+04	1.67E+02 $\pm$ 6.05E+01	9.12E-01	2.23E-11 $\pm$ 3.73E-12
HIP 10272	02 12 15.35	+23 57 29.8	0.61	32.08	1.08E+07	6.13E+06	¿ 5.82E+04	6.79E+01	9.74E+02 $\pm$ 9.02E+01	9.12E-01	1.49E-11 $\pm$ 2.84E-12
HIP 12635	02 42 20.94	+38 37 21.2	0.75	49.33	1.73E+07	1.29E+07	¡ 3.05E+01	5.87E+02	4.33E+02 $\pm$ 3.09E+01	2.37E-02	3.34E-11 $\pm$ 3.83E-12
HIP 25647	05 28 44.84	-65 26 55.1	0.59	15.31	1.02E+07	5.30E+06	¿ 6.44E+04	5.70E+01	2.37E+03 $\pm$ 1.89E+01	9.12E-01	1.28E-10 $\pm$ 8.85E-13
HIP 26369	05 36 55.09	-47 57 48.1	0.59	24.64	1.02E+07	5.30E+06	¡ 1.33E+01	5.70E+01	4.94E+02 $\pm$ 5.58E+01	1.19E-03	9.46E-11 $\pm$ 2.32E-12
HIP 26373	05 36 56.85	-47 57 52.8	0.61	24.63	8.37E+06	6.13E+06	¿ 1.28E+04	6.79E+01	1.76E+03 $\pm$ 1.03E+02	3.03E+00	9.45E-11 $\pm$ 2.31E-12
HIP 31878	06 39 50.03	-61 28 41.7	0.59	22.24	9.47E+06	5.30E+06	1.42E+03 $\pm$ 3.36E+01	5.70E+01	1.20E+02 $\pm$ 1.56E+01	1.19E-03	5.91E-12 $\pm$ 5.40E-13
HIP 76768	15 40 28.40	-18 41 46.0	0.80	38.15	1.88E+07	1.66E+07	6.30E+03 $\pm$ 1.42E+02	1.78E+03	4.28E+02 $\pm$ 9.46E+01	8.81E-02	5.25E-11 $\pm$ 3.98E-12
HIP 106231	21 31 01.71	+23 20 07.4	0.57	24.25	1.39E+07	4.76E+06	7.59E+03 $\pm$ 1.88E+02	4.38E+01	— $\pm$ —	—	4.37E-11 $\pm$ 2.47E-12
HIP 113597	23 00 27.91	-26 18 43.1	0.57	31.77	2.44E+07	4.76E+06	3.61E+03 $\pm$ 5.37E+01	4.38E+01	3.61E+02 $\pm$ 4.20E+01	7.61E-04	2.35E-11 $\pm$ 4.39E-12
HIP 118008	23 56 10.67	-39 03 08.6	0.80	21.93	1.91E+07	1.66E+07	1.04E+04 $\pm$ 9.37E+01	1.78E+03	1.38E+02 $\pm$ 1.81E+01	8.81E-02	5.26E-12 $\pm$ 1.40E-12
Ursa Majoris, 414 Myr
HIP 35628	07 21 06.7319	+67 39 42.608	0.92	25.87	2.06E+07	3.15E+07	1.80E+04 $\pm$ 1.70E+02	3.05E+04	1.15E+02 $\pm$ 3.21E+01	2.57E+00	4.02E-12 $\pm$ 7.66E-13
HIP 37349	07 39 59.3286	-03 35 51.027	0.86	14.10	2.01E+07	2.31E+07	— $\pm$ —	—	1.05E+02 $\pm$ 1.08E+01	4.15E-01	2.33E-12 $\pm$ 2.84E-13
HIP 56337	11 32 57.0557	+52 31 25.354	0.75	46.02	3.12E+07	2.03E+07	¿ 2.55E+05	9.29E+01	2.69E+02 $\pm$ 1.90E+01	2.57E+00	— $\pm$ —
HIP 71395	14 36 00.56029	+09 44 47.4632	0.80	16.34	2.09E+07	1.74E+07	9.21E+03 $\pm$ 1.01E+02	1.87E+03	1.32E+02 $\pm$ 1.22E+01	9.08E-02	2.66E-12 $\pm$ 3.93E-13
HIP 74702	15 15 59.1669	+00 47 46.899	0.86	15.81	2.73E+07	2.71E+07	¿ 5.16E+04	1.34E+04	2.32E+02 $\pm$ 7.12E+00	2.57E+00	1.12E-12 $\pm$ 1.99E-13
HIP 92919	18 55 53.22506	+23 33 23.9349	0.83	21.35	2.15E+07	2.27E+07	¿ 1.55E+04	5.21E+03	1.15E+03 $\pm$ 4.16E+01	2.57E+00	— $\pm$ —
HIP 104383	21 08 45.46901	-04 25 36.9339	0.65	23.94	1.27E+07	7.53E+06	2.34E+03 $\pm$ 3.72E+01	1.09E+02	1.51E+02 $\pm$ 1.52E+01	3.01E-03	2.91E-11 $\pm$ 1.80E-12
Praesepe, 600 Myr
Cl* NGC 2632 JC 107	08 37 36.243	+19 15 54.30	0.71	189.05	1.53E+07	1.07E+07	3.43E+03 $\pm$ 1.07E+03	2.71E+02	¡ 1.70E+03	1.00E-02	— $\pm$ —
Cl* NGC 2632 KW 184	08 39 28.586	+19 28 25.13	0.92	184.62	5.26E+07	3.21E+07	— $\pm$ —	—	3.96E+02 $\pm$ 1.03E+02	2.60E+00	— $\pm$ —
Cl* NGC 2632 JC 163	08 39 29.407	+19 47 11.88	0.80	199.62	3.22E+07	1.74E+07	— $\pm$ —	—	6.25E+02 $\pm$ 1.78E+02	8.94E-02	— $\pm$ —
Cl* NGC 2632 JC 208	08 40 26.241	+19 13 09.92	0.80	186.89	2.04E+07	1.74E+07	9.44E+03 $\pm$ 1.41E+03	1.85E+03	¡ 1.41E+03	8.94E-02	— $\pm$ —
Cl* NGC 2632 JC 215	08 40 33.473	+19 38 00.97	0.89	187.36	2.92E+07	2.77E+07	— $\pm$ —	—	3.16E+02 $\pm$ 7.75E+01	1.02E+00	— $\pm$ —
Cl* NGC 2632 JS 395	08 40 54.879	+19 56 06.72	0.89	181.52	3.03E+07	2.77E+07	— $\pm$ —	—	1.51E+03 $\pm$ 2.29E+02	1.02E+00	— $\pm$ —
Cl* NGC 2632 JC 278	08 42 11.492	+19 16 37.36	0.89	188.93	3.10E+07	2.77E+07	¡ 1.79E+03	1.49E+04	4.62E+02 $\pm$ 1.67E+02	1.02E+00	— $\pm$ —
Cl* NGC 2632 WJJP 899	08 43 08.226	+19 42 47.55	0.75	186.38	1.68E+07	1.33E+07	— $\pm$ —	—	6.90E+02 $\pm$ 2.82E+02	2.35E-02	— $\pm$ —
J08431522+2003561	08 43 15.219	+20 03 56.062	0.77	185.06	1.56E+07	1.46E+07	4.40E+03 $\pm$ 1.10E+03	8.72E+02	2.08E+03 $\pm$ 2.54E+02	3.51E-02	— $\pm$ —
J08364182+2024400	08 36 41.817	+20 24 39.942	0.81	194.04	2.02E+07	1.85E+07	1.37E+04 $\pm$ 2.03E+03	2.42E+03	¡ 2.33E+03	1.27E-01	— $\pm$ —
J08414369+1957438	08 41 43.681	+19 57 43.675	0.89	192.83	2.93E+07	2.71E+07	— $\pm$ —	—	4.17E+02 $\pm$ 9.35E+01	8.86E-01	— $\pm$ —
J08393445+2057207	08 39 34.445	+20 57 20.602	0.75	187.25	1.48E+07	1.32E+07	1.42E+03 $\pm$ 6.67E+02	5.70E+02	¡ 2.84E+03	2.26E-02	— $\pm$ —
J08373624+1915543	08 37 36.240	+19 15 54.230	0.75	189.05	1.53E+07	1.31E+07	3.43E+03 $\pm$ 1.07E+03	5.53E+02	¡ 1.70E+03	2.20E-02	— $\pm$ —
J08424848+2034245	08 42 48.464	+20 34 24.315	0.88	256.46	5.05E+07	2.69E+07	4.10E+04 $\pm$ 4.18E+03	1.30E+04	¡ 3.37E+03	8.56E-01	— $\pm$ —
J08384610+2034364	08 38 46.098	+20 34 36.375	0.87	188.38	2.65E+07	2.51E+07	2.29E+04 $\pm$ 2.13E+03	9.24E+03	4.96E+02 $\pm$ 1.69E+02	5.63E-01	— $\pm$ —
J08353387+1855475	08 35 33.867	+18 55 47.478	0.61	184.96	6.72E+06	5.76E+06	3.70E+02 $\pm$ 1.33E+02	6.21E+01	¡ 2.91E+02	1.30E-03	— $\pm$ —
J08421665+2005325	08 42 16.640	+20 05 32.431	0.69	189.35	1.14E+07	9.26E+06	— $\pm$ —	—	4.46E+02 $\pm$ 1.48E+02	5.98E-03	— $\pm$ —
J08430823+1942476	08 43 08.217	+19 42 47.512	0.77	186.38	1.68E+07	1.49E+07	— $\pm$ —	—	6.90E+02 $\pm$ 2.82E+02	3.93E-02	— $\pm$ —
J08364270+1853429	08 36 42.685	+18 53 42.784	0.72	185.44	1.27E+07	1.14E+07	4.14E+03 $\pm$ 5.50E+02	3.39E+02	¡ 2.85E+02	1.30E-02	— $\pm$ —
J08423701+2008319	08 42 36.994	+20 08 31.804	0.72	186.80	1.23E+07	1.10E+07	¡ 1.87E+03	2.96E+02	1.65E+03 $\pm$ 2.12E+02	1.11E-02	— $\pm$ —
J08444871+2017260	08 44 48.702	+20 17 25.954	0.82	186.49	2.05E+07	1.89E+07	7.16E+03 $\pm$ 1.43E+03	2.66E+03	¡ 1.71E+03	1.43E-01	— $\pm$ —
J08444076+2011371	08 44 40.744	+20 11 37.053	0.67	185.56	9.68E+06	8.45E+06	¡ 1.72E+03	1.44E+02	5.09E+02 $\pm$ 1.29E+02	4.31E-03	— $\pm$ —
J08405531+1834593	08 40 55.305	+18 34 59.102	0.66	188.21	9.60E+06	7.91E+06	2.34E+03 $\pm$ 9.63E+02	1.23E+02	1.06E+03 $\pm$ 3.38E+02	3.46E-03	— $\pm$ —
J08341024+1948178	08 34 10.231	+19 48 17.762	0.69	186.78	1.12E+07	9.26E+06	1.56E+03 $\pm$ 2.09E+02	1.83E+02	¡ 2.17E+02	5.98E-03	— $\pm$ —
J08362269+1911294	08 36 22.683	+19 11 29.295	0.89	182.69	2.63E+07	2.71E+07	2.16E+04 $\pm$ 1.93E+03	1.35E+04	¡ 1.47E+03	8.93E-01	— $\pm$ —
J08342412+1947362	08 34 24.115	+19 47 36.24s	0.78	192.73	1.81E+07	1.58E+07	4.79E+03 $\pm$ 2.62E+02	1.23E+03	¡ 2.39E+02	5.29E-02	— $\pm$ —
J08435181+1954490	08 43 51.804	+19 54 48.949	0.69	186.39	1.04E+07	9.41E+06	1.24E+03 $\pm$ 6.00E+02	1.91E+02	— $\pm$ —	—	— $\pm$ —
J08355988+1931321	08 35 59.868	+19 31 31.929	0.80	174.61	1.59E+07	1.73E+07	4.01E+03 $\pm$ 1.08E+03	1.81E+03	¡ 1.40E+03	8.69E-02	— $\pm$ —
J08422009+1909058	08 42 20.079	+19 09 05.691	0.76	188.15	1.56E+07	1.43E+07	6.78E+03 $\pm$ 2.10E+03	8.03E+02	— $\pm$ —	—	— $\pm$ —
J08385723+2010537	08 38 57.216	+20 10 53.562	0.76	177.08	1.28E+07	1.39E+07	¡ 1.88E+03	7.09E+02	4.78E+02 $\pm$ 2.19E+02	2.81E-02	— $\pm$ —
J08375180+1924538	08 37 51.800	+19 24 53.708	0.78	213.49	2.45E+07	1.60E+07	7.88E+03 $\pm$ 1.95E+03	1.30E+03	¡ 2.10E+03	5.64E-02	— $\pm$ —
J08360865+1844509	08 36 08.638	+18 44 50.902	0.63	183.35	7.67E+06	6.64E+06	5.61E+02 $\pm$ 2.54E+02	8.38E+01	¡ 2.86E+02	2.03E-03	— $\pm$ —
J08441707+1844119	08 44 17.065	+18 44 11.756	0.88	187.20	2.76E+07	2.69E+07	2.80E+04 $\pm$ 2.26E+03	1.30E+04	¡ 1.65E+03	8.56E-01	— $\pm$ —
J08435468+1853369	08 43 54.667	+18 53 36.920	0.84	187.50	2.31E+07	2.18E+07	1.23E+04 $\pm$ 1.57E+03	4.91E+03	¡ 1.75E+03	2.88E-01	— $\pm$ —
J08441324+1849114	08 44 13.234	+18 49 11.380	0.70	197.84	1.25E+07	9.84E+06	2.30E+03 $\pm$ 9.79E+02	2.16E+02	¡ 1.90E+03	7.46E-03	— $\pm$ —
J08433106+1832548	08 43 31.047	+18 32 54.711	0.75	169.14	1.12E+07	1.34E+07	1.29E+03 $\pm$ 5.91E+02	6.09E+02	¡ 1.36E+03	2.42E-02	— $\pm$ —
J08463304+1854242	08 46 33.032	+18 54 24.188	0.79	187.03	1.68E+07	1.60E+07	1.99E+03 $\pm$ 7.73E+02	1.31E+03	¡ 1.97E+03	5.74E-02	— $\pm$ —
J08325224+1958359	08 32 52.225	+19 58 35.900	0.80	187.00	1.94E+07	1.75E+07	6.52E+03 $\pm$ 2.60E+02	1.92E+03	¡ 1.99E+02	9.37E-02	— $\pm$ —
J08370346+1910412	08 37 03.449	+19 10 41.134	0.75	176.32	1.32E+07	1.36E+07	9.27E+03 $\pm$ 2.55E+03	6.59E+02	¡ 1.45E+03	2.61E-02	— $\pm$ —
J08330290+1840575	08 33 02.889	+18 40 57.464	0.77	186.79	1.63E+07	1.47E+07	3.15E+03 $\pm$ 2.00E+02	9.06E+02	¡ 2.93E+02	3.66E-02	— $\pm$ —
J08461010+1931439	08 46 10.096	+19 31 43.813	0.62	187.58	7.16E+06	6.07E+06	2.76E+03 $\pm$ 3.29E+02	6.95E+01	1.30E+03 $\pm$ 1.79E+02	1.55E-03	— $\pm$ —
J08393752+1810134	08 39 37.514	+18 10 13.393	0.89	187.09	2.76E+07	2.79E+07	2.82E+04 $\pm$ 3.66E+02	1.54E+04	¡ 2.83E+02	1.06E+00	— $\pm$ —
J08365164+1904351	08 36 51.632	+19 04 35.014	0.72	187.35	1.31E+07	1.13E+07	1.78E+03 $\pm$ 9.53E+02	3.20E+02	¡ 1.64E+03	1.22E-02	— $\pm$ —
J08323342+2004483	08 32 33.413	+20 04 48.327	0.78	180.73	1.61E+07	1.58E+07	3.45E+03 $\pm$ 2.05E+02	1.25E+03	¡ 1.83E+02	5.37E-02	— $\pm$ —
J08434357+1904332	08 43 43.557	+19 04 33.175	0.74	196.46	1.64E+07	1.25E+07	4.50E+03 $\pm$ 1.26E+03	4.63E+02	¡ 2.17E+03	1.83E-02	— $\pm$ —
J08305102+1921089	08 30 51.018	+19 21 08.838	0.65	182.08	8.21E+06	7.36E+06	4.22E+02 $\pm$ 1.04E+02	1.04E+02	¡ 2.02E+02	2.75E-03	— $\pm$ —
J08370375+1840025	08 37 03.742	+18 40 02.510	0.71	184.29	1.14E+07	1.07E+07	— $\pm$ —	—	¡ 3.83E+02	1.02E-02	— $\pm$ —
J08492676+1831196	08 49 26.759	+18 31 19.542	0.61	187.60	7.12E+06	5.93E+06	8.85E+02 $\pm$ 1.65E+02	6.61E+01	¡ 1.52E+02	1.43E-03	— $\pm$ —
J08413600+1906256	08 41 35.991	+19 06 25.488	0.69	186.00	1.10E+07	9.37E+06	1.82E+03 $\pm$ 7.22E+02	1.89E+02	¡ 1.40E+03	6.25E-03	— $\pm$ —
J08343646+1823531	08 34 36.460	+18 23 53.037	0.61	193.09	7.19E+06	5.69E+06	9.64E+02 $\pm$ 1.76E+02	6.03E+01	¡ 2.77E+02	1.24E-03	— $\pm$ —
J08465012+2101129	08 46 50.116	+21 01 12.799	0.81	180.08	1.81E+07	1.79E+07	6.32E+03 $\pm$ 1.39E+03	2.12E+03	¡ 1.81E+03	1.07E-01	— $\pm$ —
J08331763+1925505	08 33 17.614	+19 25 50.458	0.72	185.95	1.28E+07	1.12E+07	1.63E+03 $\pm$ 1.62E+02	3.14E+02	¡ 2.01E+02	1.19E-02	— $\pm$ —
J08365375+1829451	08 36 53.737	+18 29 45.092	0.69	187.26	1.20E+07	9.74E+06	1.49E+03 $\pm$ 3.08E+02	2.10E+02	¡ 2.74E+02	7.21E-03	— $\pm$ —
J08383724+1901161	08 38 37.229	+19 01 16.046	0.79	187.26	1.61E+07	1.62E+07	1.54E+03 $\pm$ 9.90E+02	1.37E+03	¡ 1.95E+03	6.03E-02	— $\pm$ —
J08325566+1843582	08 32 55.656	+18 43 58.148	0.79	188.39	1.83E+07	1.64E+07	6.00E+03 $\pm$ 2.71E+02	1.47E+03	¡ 2.93E+02	6.60E-02	— $\pm$ —
J08330746+2007483	08 33 07.456	+20 07 48.244	0.70	186.80	1.18E+07	1.01E+07	2.04E+03 $\pm$ 1.71E+02	2.29E+02	3.72E+02 $\pm$ 1.07E+02	8.08E-03	— $\pm$ —
J08384973+1815572	08 38 49.727	+18 15 57.106	0.85	187.64	2.41E+07	2.23E+07	1.53E+04 $\pm$ 2.69E+02	5.44E+03	¡ 2.92E+02	3.21E-01	— $\pm$ —
J08461382+2051248	08 46 13.809	+20 51 24.753	0.72	176.01	1.07E+07	1.12E+07	1.44E+03 $\pm$ 5.76E+02	3.17E+02	— $\pm$ —	—	— $\pm$ —
J08365411+1845248	08 36 54.103	+18 45 24.706	0.83	181.70	2.09E+07	2.00E+07	1.69E+04 $\pm$ 8.79E+02	3.41E+03	¡ 3.21E+02	1.93E-01	— $\pm$ —
J08344714+1801162	08 34 47.138	+18 01 16.161	0.73	192.07	1.44E+07	1.17E+07	2.68E+03 $\pm$ 2.71E+02	3.65E+02	¡ 2.95E+02	1.42E-02	— $\pm$ —
Hyades, 625 Myr
HIP 13806	02 57 46.6727	+29 39 41.268	0.92	41.53	3.06E+07	3.21E+07	3.57E+04     $\pm$ 5.03E+02	3.11E+04	1.68E+02   $\pm$ 5.77E+01	2.60E+00	5.39E-12 $\pm$ 1.20E-12
HIP 13976	03 00 02.8119	+07 44 59.119	0.80	23.79	2.67E+07	1.74E+07	1.77E+04 $\pm$ 2.19E+02	1.85E+03	¡ 1.12E+01	8.94E-02	2.93E-12 $\pm$ 7.19E-13
HIP 15374	03 18 15.10184	+09 14 42.5704	0.71	61.51	1.08E+07	1.07E+07	— $\pm$ —	—	¡ 1.31E+02	1.00E-02	— $\pm$ —
HIP15563	03 20 29.1951	+08 27 16.025	0.71	31.77	1.54E+07	1.07E+07	3.18E+03 $\pm$ 8.83E+01	2.71E+02	1.75E+02 $\pm$ 3.32E+01	1.00E-02	— $\pm$ —
HIP 15720	03 22 28.1400	+27 09 21.792	0.62	31.75	8.06E+06	6.24E+06	5.92E+02 $\pm$ 5.19E+01	7.38E+01	¡ 5.27E+01	1.69E-03	— $\pm$ —
HIP 16548	03 33 05.2980	+04 57 29.240	0.71	54.99	8.83E+06	1.07E+07	8.34E+02 $\pm$ 1.24E+02	2.71E+02	¡ 1.63E+02	1.00E-02	— $\pm$ —
HIP17766	03 48 11.8636	+07 08 46.477	0.62	36.53	1.04E+07	6.24E+06	7.67E+02 $\pm$ 5.63E+01	7.38E+01	¡ 9.64E+01	1.69E-03	— $\pm$ —
HIP 17962	03 50 24.9669	+17 14 47.431	0.83	47.72	2.34E+07	2.27E+07	¿   4.20E+04	5.21E+03	¿ 1.65E+05	2.45E-01	1.70E-10 $\pm$ 7.35E-12
HD 283044	03 52 41.0090	+25 48 15.980	0.62	44.46	1.04E+07	6.24E+06	1.23E+03 $\pm$ 1.44E+02	7.38E+01	— $\pm$ —	—	— $\pm$ —
HIP 18327	03 55 06.5014	+16 59 54.520	0.92	40.98	2.90E+07	3.21E+07	2.75E+04 $\pm$ 6.62E+02	3.11E+04	¡ 2.51E+02	2.60E+00	5.18E-12 $\pm$ 1.76E-12
HIP18946	04 03 39.0405	+19 27 18.046	0.86	48.04	1.92E+07	2.38E+07	5.85E+03 $\pm$ 4.41E+01	7.28E+03	¡ 1.69E+02	4.32E-01	— $\pm$ —
HIP19263	04 07 43.1990	+16 31 07.644	0.92	46.56	1.98E+07	3.21E+07	8.15E+03 $\pm$ 1.07E+02	3.11E+04	3.05E+03 $\pm$ 2.91E+02	2.60E+00	— $\pm$ —
HIP19441	04 09 49.3492	+09 18 19.771	0.75	36.01	1.42E+07	1.33E+07	2.23E+03 $\pm$ 9.05E+01	5.92E+02	¡ 8.39E+01	2.35E-02	— $\pm$ —
V* V1313 Tau	04 18 10.7920	+23 17 04.765	0.92	54.01	4.30E+07	3.21E+07	4.07E+04 $\pm$ 1.38E+02	3.11E+04	2.30E+03 $\pm$ 9.82E+01	2.60E+00	1.29E-10 $\pm$ 8.25E-12
HIP20082	04 18 19.2717	+16 05 17.995	0.92	45.18	2.29E+07	3.21E+07	1.29E+04 $\pm$ 7.83E+01	3.11E+04	1.77E+02 $\pm$ 3.60E+01	2.60E+00	— $\pm$ —
HD 285773	04 29 31.6064	+17 53 35.459	0.92	45.79	3.27E+07	3.21E+07	4.65E+04 $\pm$ 6.57E+02	3.11E+04	— $\pm$ —	—	— $\pm$ —
HD 28462	04 29 57.7280	+16 40 22.226	0.89	45.67	2.98E+07	2.77E+07	3.92E+04 $\pm$ 3.38E+02	1.49E+04	1.76E+02 $\pm$ 4.45E+01	1.02E+00	— $\pm$ —
HD 29159	04 36 05.2667	+15 41 02.418	0.92	50.22	2.89E+07	3.21E+07	3.61E+04 $\pm$ 7.86E+01	3.11E+04	2.67E+02 $\pm$ 1.88E+01	2.60E+00	— $\pm$ —
HD 30505	04 49 03.5240	+18 38 28.480	0.89	45.73	3.38E+07	2.77E+07	4.60E+04 $\pm$ 4.68E+02	1.49E+04	2.02E+02 $\pm$ 7.24E+01	1.02E+00	8.06E-12 $\pm$ 2.47E-12
HIP23312	05 00 48.8864	+04 43 59.203	0.86	52.06	2.46E+07	2.38E+07	1.86E+04 $\pm$ 1.25E+02	7.28E+03	4.23E+02 $\pm$ 1.46E+02	4.32E-01	— $\pm$ —
HD 32347	05 03 07.6578	+13 43 50.413	0.92	53.76	4.09E+07	3.21E+07	9.39E+04 $\pm$ 8.12E+02	3.11E+04	4.10E+02 $\pm$ 1.18E+02	2.60E+00	2.65E-12 $\pm$ 9.40E-13
HD 240648	05 06 17.9892	+17 48 59.098	0.79	53.75	2.00E+07	1.82E+07	¿   1.10E+04	2.23E+03	7.33E+02 $\pm$ 1.48E+02	2.60E+00	7.83E-12 $\pm$ 2.16E-12
J04053965+1756156	04 05 39.596	+17 56 16.000	0.89	45.81	2.66E+07	2.77E+07	2.78E+04 $\pm$ 1.22E+02	1.49E+04	2.48E+02 $\pm$ 6.18E+01	1.02E+00	4.97E-12 $\pm$ 2.28E-12
J04083620+2346071	04 08 36.208	+23 46 06.996	0.89	47.52	2.63E+07	2.77E+07	2.06E+04 $\pm$ 2.60E+02	1.49E+04	2.70E+02 $\pm$ 7.00E+01	1.02E+00	3.22E-12 $\pm$ 1.45E-12
J04181926+1605181	04 18 19.199	+16 05 18.198	0.86	45.18	2.29E+07	2.38E+07	1.29E+04 $\pm$ 7.83E+01	7.28E+03	1.77E+02 $\pm$ 3.60E+01	4.32E-01	— $\pm$ —
J04464943+1744540	04 46 49.395	+17 44 54.261	0.89	48.09	2.80E+07	2.77E+07	— $\pm$ —	—	¡ 4.42E+02	1.02E+00	1.10E-11 $\pm$ 2.63E-12
J04431568+1704088	04 43 15.688	+17 04 08.688	0.87	45.93	2.12E+07	2.51E+07	1.01E+04 $\pm$ 7.01E+01	9.19E+03	3.16E+02 $\pm$ 8.45E+01	5.60E-01	1.26E-11 $\pm$ 2.56E-12
J04074319+1631076	04 07 43.124	+16 31 07.862	0.82	46.56	1.98E+07	1.93E+07	8.15E+03 $\pm$ 1.07E+02	2.91E+03	3.05E+03 $\pm$ 2.91E+02	1.60E-01	— $\pm$ —
J04094935+0918197	04 09 49.257	+09 18 19.817	0.75	36.01	1.41E+07	1.33E+07	2.23E+03 $\pm$ 9.05E+01	5.92E+02	¡ 8.39E+01	2.35E-02	— $\pm$ —
J04033902+1927180	04 03 38.964	+19 27 18.338	0.83	48.04	1.92E+07	2.04E+07	5.85E+03 $\pm$ 4.41E+01	3.67E+03	¡ 1.69E+02	2.09E-01	— $\pm$ —
J04250024+1659057	04 25 00.18s	+16 59 05.784	0.82	54.70	1.92E+07	1.93E+07	— $\pm$ —	—	¡ 4.86E+01	1.60E-01	— $\pm$ —
J04070122+1520062	04 07 01.150	+15 20 06.28s	0.77	45.09	1.46E+07	1.48E+07	2.57E+03 $\pm$ 7.94E+01	9.26E+02	¡ 7.79E+01	3.75E-02	— $\pm$ —
J04474178+2609009	04 47 41.726	+26 09 01.555	0.65	47.61	1.53E+07	7.53E+06	1.71E+03 $\pm$ 3.68E+01	1.10E+02	¡ 1.22E+02	2.95E-03	— $\pm$ —
J04333716+2109030	04 33 37.112	+21 09 03.468	0.75	43.80	1.30E+07	1.33E+07	1.58E+03 $\pm$ 7.74E+01	5.92E+02	¡ 1.15E+02	2.35E-02	— $\pm$ —
J04145191+1303178	04 14 51.864	+13 03 17.996	0.80	44.55	1.32E+07	1.74E+07	1.97E+03 $\pm$ 4.09E+01	1.85E+03	¡ 1.74E+02	8.94E-02	7.50E-12 $\pm$ 2.23E-12
J04500069+1624436	04 50 00.700	+16 24 43.488	0.76	49.40	1.57E+07	1.40E+07	3.22E+03 $\pm$ 5.52E+01	7.38E+02	¡ 1.50E+02	2.93E-02	— $\pm$ —
J04334192+1900504	04 33 41.865	+19 00 50.819	0.74	47.80	1.40E+07	1.26E+07	2.33E+03 $\pm$ 1.79E+02	4.78E+02	— $\pm$ —	—	— $\pm$ —
J04172512+1901478	04 17 25.14s	+19 01 47.388	0.74	47.86	1.33E+07	1.26E+07	1.77E+03 $\pm$ 3.89E+01	4.78E+02	¡ 9.74E+01	1.89E-02	— $\pm$ —
J04081110+1652229	04 08 11.020	+16 52 23.304	0.67	40.13	8.00E+06	8.48E+06	6.58E+02 $\pm$ 6.15E+00	1.45E+02	6.39E+01 $\pm$ 1.80E+01	4.38E-03	— $\pm$ —
J04052565+1926316	04 05 25.595	+19 26 32.032	0.68	47.30	9.92E+06	8.99E+06	9.83E+02 $\pm$ 2.79E+01	1.69E+02	¡ 1.27E+02	5.38E-03	— $\pm$ —
J04151038+1423544	04 15 10.339	+14 23 54.598	0.66	48.01	9.69E+06	8.00E+06	8.38E+02 $\pm$ 4.48E+01	1.26E+02	¡ 1.05E+02	3.58E-03	— $\pm$ —
J04510241+1458167	04 51 02.409	+14 58 16.5s	0.67	40.79	8.04E+06	8.48E+06	9.70E+02 $\pm$ 8.07E+01	1.45E+02	1.99E+02 $\pm$ 4.93E+01	4.38E-03	8.34E-12 $\pm$ 1.85E-12
J04471851+0627113	04 47 18.508	+06 27 11.592	0.65	40.59	9.10E+06	7.53E+06	6.07E+02 $\pm$ 1.06E+02	1.10E+02	— $\pm$ —	—	— $\pm$ —
J05110971+1548574	05 11 09.688	+15 48 57.492	0.79	57.00	1.33E+07	1.65E+07	1.43E+03 $\pm$ 1.56E+02	1.47E+03	¡ 2.29E+02	6.62E-02	1.76E-11 $\pm$ 4.15E-12
J04522385+1043099	04 52 23.860	+10 43 09.912	0.65	52.12	6.07E+06	7.53E+06	6.80E+02 $\pm$ 1.41E+02	1.10E+02	— $\pm$ —	—	— $\pm$ —
J04412780+1404340	04 41 27.808	+14 04 34.104	0.60	49.21	5.70E+06	5.49E+06	1.18E+03 $\pm$ 4.30E+01	5.55E+01	4.90E+02 $\pm$ 9.06E+01	1.08E-03	3.09E-11 $\pm$ 3.98E-12
J02185464+3513053	02 18 54.633	+35 13 05.632	0.64	43.60	7.67E+06	7.09E+06	4.40E+02 $\pm$ 2.23E+01	9.59E+01	¡ 9.06E+01	2.45E-03	— $\pm$ —
J02263361+1522245	02 26 33.645	+15 22 24.483	0.88	57.09	3.07E+07	2.63E+07	6.00E+04 $\pm$ 8.90E+02	1.17E+04	¡ 1.73E+02	7.47E-01	1.72E-11 $\pm$ 6.57E-12
J02523774-0913565	02 52 37.762	-09 13 56.381	0.72	33.97	7.79E+06	1.13E+07	4.14E+02 $\pm$ 1.13E+01	3.23E+02	2.08E+01 $\pm$ 5.53E+00	1.23E-02	— $\pm$ —
J03000280+0744590	03 00 02.811	+07 44 59.102	0.88	23.79	2.67E+07	2.63E+07	1.77E+04 $\pm$ 2.19E+02	1.17E+04	¡ 1.12E+01	7.47E-01	2.93E-12 $\pm$ 7.19E-13
J03181510+0914426	03 18 15.099	+09 14 42.538	0.68	61.51	1.08E+07	8.99E+06	— $\pm$ —	—	¡ 1.31E+02	5.38E-03	— $\pm$ —
J03183830+3239570	03 18 38.323	+32 39 56.859	0.67	25.71	5.39E+06	8.48E+06	1.64E+02 $\pm$ 2.24E+01	1.45E+02	¡ 3.41E+01	4.38E-03	— $\pm$ —
J03202921+0827161	03 20 29.195	+08 27 16.003	0.78	31.77	1.54E+07	1.56E+07	3.18E+03 $\pm$ 8.83E+01	1.17E+03	1.75E+02 $\pm$ 3.32E+01	4.93E-02	— $\pm$ —
J03222810+2709219	03 22 28.139	+27 09 21.795	0.65	31.75	8.06E+06	7.53E+06	5.92E+02 $\pm$ 5.19E+01	1.10E+02	¡ 5.27E+01	2.95E-03	— $\pm$ —
J03330528+0457291	03 33 05.302	+04 57 29.216	0.69	54.99	8.83E+06	9.52E+06	8.34E+02 $\pm$ 1.24E+02	1.97E+02	¡ 1.68E+02	6.63E-03	— $\pm$ —
J03481186+0708464	03 48 11.862	+07 08 46.466	0.69	36.53	1.04E+07	9.52E+06	7.67E+02 $\pm$ 5.63E+01	1.97E+02	¡ 9.64E+01	6.63E-03	— $\pm$ —
J03524101+2548159	03 52 41.011	+25 48 15.995	0.72	44.46	1.04E+07	1.13E+07	1.23E+03 $\pm$ 1.44E+02	3.23E+02	— $\pm$ —	—	— $\pm$ —
J03590972+2628340	03 59 09.735	+26 28 33.953	0.70	35.86	6.68E+06	1.01E+07	3.84E+02 $\pm$ 4.77E+01	2.31E+02	¡ 8.98E+01	8.15E-03	— $\pm$ —
J04084015+2333257	04 08 40.176	+23 33 25.620	0.61	46.08	5.99E+06	5.85E+06	2.36E+02 $\pm$ 4.61E+01	6.42E+01	¡ 8.85E+01	1.37E-03	— $\pm$ —
J04092011+0807436	04 09 20.127	+08 07 43.707	0.81	199.84	1.65E+08	1.83E+07	9.04E+04 $\pm$ 1.01E+03	2.32E+03	¡ 3.16E+03	1.20E-01	— $\pm$ —
J04150713-1132156	04 15 07.150	-11 32 15.523	0.70	43.82	8.41E+06	1.01E+07	1.44E+03 $\pm$ 6.14E+01	2.31E+02	¡ 3.08E+01	8.15E-03	— $\pm$ —
J04161310+1853042	04 16 13.122	+18 53 04.202	0.63	45.61	7.87E+06	6.66E+06	5.65E+02 $\pm$ 2.89E+01	8.42E+01	¡ 9.84E+01	2.04E-03	— $\pm$ —
J04174767+1339422	04 17 47.693	+13 39 42.392	0.62	47.45	6.21E+06	6.24E+06	2.84E+02 $\pm$ 2.53E+01	7.38E+01	¡ 1.33E+02	1.69E-03	— $\pm$ —
J04184702+1321585	04 18 47.037	+13 21 58.732	0.64	46.14	7.62E+06	7.09E+06	4.65E+02 $\pm$ 2.72E+01	9.59E+01	¡ 9.96E+01	2.45E-03	— $\pm$ —
J04201057-1445400	04 20 10.585	-14 45 39.852	0.74	29.32	1.30E+07	1.26E+07	1.82E+03 $\pm$ 8.21E+01	4.78E+02	¡ 5.72E+01	1.89E-02	— $\pm$ —
J04210411+0316074	04 21 04.11s	+03 16 07.564	0.83	37.08	1.90E+07	2.04E+07	6.87E+03 $\pm$ 4.45E+01	3.67E+03	1.86E+02 $\pm$ 6.50E+01	2.09E-01	— $\pm$ —
J04223004+1026046	04 22 30.036	+10 26 04.602	0.60	47.89	5.74E+06	5.49E+06	1.77E+02 $\pm$ 6.57E+01	5.55E+01	¡ 2.06E+02	1.08E-03	— $\pm$ —
J04240740+2207079	04 24 07.426	+22 07 07.930	0.72	45.78	1.18E+07	1.13E+07	1.21E+03 $\pm$ 1.96E+02	3.23E+02	— $\pm$ —	—	— $\pm$ —
J04252002+2306312	04 25 20.039	+23 06 31.115	0.60	53.48	5.84E+06	5.49E+06	2.57E+02 $\pm$ 8.72E+01	5.55E+01	¡ 9.67E+01	1.08E-03	— $\pm$ —
J04264760+2114059	04 26 47.618	+21 14 05.716	0.67	43.20	9.63E+06	8.48E+06	9.93E+02 $\pm$ 1.25E+02	1.45E+02	— $\pm$ —	—	— $\pm$ —
J04274170+4655395	04 27 41.719	+46 55 39.466	0.81	68.77	5.25E+07	1.83E+07	2.31E+04 $\pm$ 8.16E+02	2.32E+03	¡ 2.49E+02	1.20E-01	— $\pm$ —
J04293897+2252579	04 29 38.994	+22 52 57.812	0.74	59.35	1.29E+07	1.26E+07	1.99E+03 $\pm$ 1.63E+02	4.78E+02	¡ 2.60E+02	1.89E-02	2.36E-11 $\pm$ 4.35E-12
J04303819+2254289	04 30 38.194	+22 54 28.882	0.66	50.93	8.27E+06	8.00E+06	1.77E+03 $\pm$ 1.58E+02	1.26E+02	3.81E+02 $\pm$ 1.18E+02	3.58E-03	— $\pm$ —
J04324094+1906484	04 32 40.945	+19 06 48.534	0.78	52.53	1.64E+07	1.56E+07	4.51E+03 $\pm$ 2.56E+02	1.17E+03	— $\pm$ —	—	— $\pm$ —
J04331890+4951407	04 33 18.903	+49 51 40.705	0.80	46.37	1.08E+07	1.74E+07	1.36E+03 $\pm$ 8.84E+01	1.85E+03	¡ 1.72E+02	8.94E-02	— $\pm$ —
J04343992+1512325	04 34 39.936	+15 12 32.589	0.65	48.07	8.90E+06	7.53E+06	— $\pm$ —	—	3.72E+02 $\pm$ 2.26E+01	2.95E-03	2.41E-11 $\pm$ 3.79E-12
J04350255+0839304	04 35 02.550	+08 39 30.564	0.79	59.34	1.65E+07	1.65E+07	2.73E+03 $\pm$ 6.78E+01	1.47E+03	5.19E+02 $\pm$ 1.57E+02	6.62E-02	3.34E-11 $\pm$ 4.88E-12
J04375823+0440111	04 37 58.241	+04 40 11.199	0.70	48.32	9.70E+06	1.01E+07	6.91E+02 $\pm$ 9.75E+01	2.31E+02	¡ 2.15E+02	8.15E-03	— $\pm$ —
J04404249+0213522	04 40 42.484	+02 13 52.012	0.64	23.91	6.34E+06	7.09E+06	1.85E+02 $\pm$ 6.44E+00	9.59E+01	¡ 2.56E+01	2.45E-03	— $\pm$ —
J04431267+1518538	04 43 12.673	+15 18 53.753	0.60	52.52	3.50E+06	5.49E+06	3.06E+02 $\pm$ 5.97E+01	5.55E+01	¡ 2.56E+02	1.08E-03	— $\pm$ —
J04451961+1334274	04 45 19.614	+13 34 27.437	0.66	51.71	7.64E+06	8.00E+06	2.33E+03 $\pm$ 1.45E+02	1.26E+02	4.74E+02 $\pm$ 8.56E+01	3.58E-03	2.32E-11 $\pm$ 3.35E-12
J04470642+1543419	04 47 06.431	+15 43 41.787	0.90	60.34	2.40E+07	2.91E+07	3.29E+04 $\pm$ 1.30E+02	1.91E+04	¡ 1.23E+02	1.40E+00	— $\pm$ —
J04470892+2052564	04 47 08.933	+20 52 56.336	0.82	42.30	1.86E+07	1.93E+07	6.81E+03 $\pm$ 1.14E+02	2.91E+03	¡ 8.98E+01	1.60E-01	— $\pm$ —
J04470974+2401124	04 47 09.753	+24 01 12.131	0.61	46.15	6.58E+06	5.85E+06	3.45E+02 $\pm$ 8.88E+01	6.42E+01	— $\pm$ —	—	— $\pm$ —
J04473532+1453209	04 47 35.335	+14 53 20.725	0.67	47.84	9.95E+06	8.48E+06	8.74E+02 $\pm$ 2.27E+01	1.45E+02	¡ 1.53E+02	4.38E-03	— $\pm$ —
J04513356+1417109	04 51 33.578	+14 17 10.942	0.88	75.82	2.39E+07	2.63E+07	5.88E+03 $\pm$ 3.47E+02	1.17E+04	¡ 2.64E+02	7.47E-01	— $\pm$ —
J04514917+1716255	04 51 49.187	+17 16 25.394	0.73	54.47	1.17E+07	1.19E+07	1.41E+03 $\pm$ 5.10E+01	3.90E+02	¡ 2.20E+02	1.53E-02	— $\pm$ —
J04524755+2238503	04 52 47.561	+22 38 50.132	0.70	55.94	1.17E+07	1.01E+07	1.58E+03 $\pm$ 1.00E+02	2.31E+02	¡ 1.96E+02	8.15E-03	— $\pm$ —
J04543192-1154506	04 54 31.939	-11 54 50.515	0.81	35.49	1.82E+07	1.83E+07	5.88E+03 $\pm$ 1.70E+02	2.32E+03	6.44E+01 $\pm$ 4.19E+01	1.20E-01	5.01E-12 $\pm$ 1.60E-12
J04594949+1958003	04 59 49.508	+19 58 00.356	0.89	149.16	1.70E+08	2.77E+07	3.70E+05 $\pm$ 4.20E+03	1.49E+04	¡ 1.57E+03	1.02E+00	— $\pm$ —
J05004888+0443591	05 00 48.886	+04 43 59.21s	0.85	52.06	2.46E+07	2.26E+07	1.86E+04 $\pm$ 1.25E+02	5.80E+03	4.23E+02 $\pm$ 1.46E+02	3.43E-01	— $\pm$ —
J05012217+2955475	05 01 22.170	+29 55 47.596	0.90	90.51	5.34E+07	2.91E+07	3.90E+04 $\pm$ 8.34E+02	1.91E+04	¡ 5.24E+02	1.40E+00	— $\pm$ —
J05013765+1224589	05 01 37.665	+12 24 58.999	0.80	51.46	1.37E+07	1.74E+07	1.05E+03 $\pm$ 1.29E+02	1.85E+03	¡ 1.94E+02	8.94E-02	— $\pm$ —
J05030708+1901048	05 03 07.101	+19 01 04.779	0.62	53.34	9.26E+06	6.24E+06	7.51E+02 $\pm$ 3.58E+01	7.38E+01	¡ 1.73E+02	1.69E-03	— $\pm$ —
J05054038+0627545	05 05 40.377	+06 27 54.632	0.87	65.51	3.84E+07	2.51E+07	2.56E+04 $\pm$ 4.04E+02	9.19E+03	¡ 3.59E+02	5.60E-01	— $\pm$ —
J05073527+1841339	05 07 35.292	+18 41 33.807	0.75	68.78	1.47E+07	1.33E+07	2.89E+03 $\pm$ 2.45E+02	5.92E+02	¡ 2.61E+02	2.35E-02	— $\pm$ —
J05081333+2159250	05 08 13.336	+21 59 24.884	0.64	62.76	6.83E+06	7.09E+06	4.97E+02 $\pm$ 1.43E+02	9.59E+01	— $\pm$ —	—	— $\pm$ —
J05102443+1025047	05 10 24.438	+10 25 04.795	0.68	67.80	1.17E+07	8.99E+06	1.33E+03 $\pm$ 1.89E+02	1.69E+02	— $\pm$ —	—	— $\pm$ —
J05115547+0542578	05 11 55.474	+05 42 57.863	0.89	69.88	2.30E+07	2.77E+07	1.48E+04 $\pm$ 2.17E+02	1.49E+04	¡ 4.92E+02	1.02E+00	— $\pm$ —
J05122408+1824086	05 12 24.082	+18 24 08.641	0.61	53.09	7.32E+06	5.85E+06	5.21E+02 $\pm$ 1.15E+02	6.42E+01	¡ 2.10E+02	1.37E-03	— $\pm$ —
J05505408+0609242	05 50 54.091	+06 09 24.194	0.81	355.34	5.68E+08	1.83E+07	2.09E+05 $\pm$ 1.32E+04	2.32E+03	¡ 1.71E+04	1.20E-01	— $\pm$ —
Field, 5 Gyr
HD 55	00 05 17.6886	-67 49 57.322	0.70	16.39	1.14E+07	1.07E+07	2.01E+03 $\pm$ 1.79E+01	2.61E+02	¡ 1.79E+01	9.10E-03	— $\pm$ —
GJ 3008	00 08 27.2796	+17 25 27.459	0.61	21.74	5.68E+06	6.13E+06	3.24E+02 $\pm$ 1.65E+01	6.79E+01	4.07E+01 $\pm$ 1.11E+01	1.38E-03	— $\pm$ —
HD 870	00 12 50.2493	-57 54 45.395	0.89	20.63	3.10E+07	3.24E+07	¿ 5.12E+04	3.07E+04	1.62E+02 $\pm$ 1.97E+01	2.52E+00	— $\pm$ —
CD-46 76	00 21 19.6196	-45 44 47.109	0.61	17.59	5.35E+06	6.13E+06	1.83E+02 $\pm$ 1.17E+01	6.79E+01	8.94E+00 $\pm$ 4.00E+00	1.38E-03	— $\pm$ —
HD 2025	00 24 25.9333	-27 01 36.380	0.79	17.95	1.71E+07	1.82E+07	8.91E+03 $\pm$ 5.46E+01	2.23E+03	5.54E+01 $\pm$ 8.15E+00	1.22E-01	— $\pm$ —
54 Psc	00 39 21.80589	+21 15 01.7081	0.86	11.14	3.22E+07	2.71E+07	¿ 1.69E+04	1.34E+04	5.99E+01 $\pm$ 7.16E+00	9.74E-01	— $\pm$ —
HD 3765	00 40 49.26909	+40 11 13.8306	0.83	17.94	2.71E+07	2.27E+07	1.03E+04 $\pm$ 2.54E+01	5.21E+03	3.12E+01 $\pm$ 1.14E+00	2.45E-01	1.17E-12 $\pm$ 3.60E-13
CD-34 239	00 41 30.4739	-33 37 32.032	0.57	19.63	5.07E+06	4.78E+06	1.45E+02 $\pm$ 1.09E+01	3.70E+01	¡ 1.80E+01	5.14E-04	— $\pm$ —
HD 4256	00 45 04.8939	+01 47 07.878	0.79	22.43	2.41E+07	1.82E+07	8.47E+03 $\pm$ 1.85E+01	2.23E+03	3.80E+01 $\pm$ 2.32E+00	1.22E-01	— $\pm$ —
HD 4628	00 48 22.97665	+05 16 50.2129	0.79	7.43	1.57E+07	1.82E+07	— $\pm$ —	—	2.40E+01 $\pm$ 2.62E+00	1.22E-01	— $\pm$ —
CD-50 210	00 49 01.7119	-50 08 41.708	0.61	23.10	6.43E+06	6.13E+06	2.28E+02 $\pm$ 1.76E+01	6.79E+01	3.79E+01 $\pm$ 1.16E+01	1.38E-03	— $\pm$ —
HD 4913	00 51 21.7540	+18 44 21.293	0.65	22.24	1.31E+07	7.91E+06	1.17E+03 $\pm$ 4.19E+01	1.24E+02	2.68E+01 $\pm$ 1.02E+01	5.17E-03	8.45E-13 $\pm$ 3.07E-13
HD 4967	00 51 34.0200	-22 54 36.241	0.70	15.34	9.04E+06	1.07E+07	7.28E+02 $\pm$ 2.54E+01	2.61E+02	1.81E+01 $\pm$ 7.24E+00	9.10E-03	— $\pm$ —
HD 6101	01 02 24.57273	+05 03 41.2140	0.83	15.21	1.22E+07	2.27E+07	3.81E+03 $\pm$ 7.34E+00	5.21E+03	4.04E+01 $\pm$ 1.16E+00	2.45E-01	— $\pm$ —
BD+79 38	01 21 30.9120	+80 09 06.480	0.70	24.42	1.12E+07	1.07E+07	9.96E+02 $\pm$ 5.06E+01	2.61E+02	— $\pm$ —	—	— $\pm$ —
HD 7924	01 21 59.1136	+76 42 37.039	0.89	17.00	3.12E+07	3.24E+07	¿ 2.74E+04	3.07E+04	6.95E+01 $\pm$ 9.16E+00	9.74E-01	3.76E-13 $\pm$ 1.30E-13
HD 9540	01 33 15.8091	-24 10 40.654	0.89	19.27	3.12E+07	3.24E+07	— $\pm$ —	—	2.06E+02 $\pm$ 2.13E+01	2.52E+00	8.43E-13 $\pm$ 2.21E-13
HD 9770	01 35 01.03508	-29 54 37.0162	0.83	26.02	4.42E+07	1.71E+07	¿ 2.08E+05	1.92E+02	2.77E+03 $\pm$ 1.26E+02	9.74E-01	1.51E-10 $\pm$ 4.03E-12
GJ 68	01 42 29.76170	+20 16 06.6015	0.74	7.61	1.56E+07	1.36E+07	¿ 1.66E+05	5.87E+02	4.97E+01 $\pm$ 9.51E-01	2.52E+00	— $\pm$ —
HD 10853	01 46 38.7174	+12 24 42.385	0.74	24.06	1.56E+07	1.36E+07	4.36E+03 $\pm$ 6.55E+01	5.87E+02	6.83E+01 $\pm$ 2.17E+01	1.88E-02	— $\pm$ —
BD-21 397	02 13 12.1645	-21 11 47.232	0.61	23.75	1.08E+07	6.13E+06	8.13E+02 $\pm$ 3.08E+01	6.79E+01	7.55E+01 $\pm$ 1.62E+01	1.38E-03	1.11E-12 $\pm$ 4.77E-13
HD 14039	02 18 24.602	+56 33 35.72	0.86	31.93	3.74E+07	2.71E+07	1.51E+04 $\pm$ 2.20E+02	1.34E+04	— $\pm$ —	—	— $\pm$ —
GJ 105 A	02 36 04.89466	+06 53 12.7466	0.60	7.24	6.48E+06	6.37E+06	¿ 2.53E+05	3.26E+01	2.24E+01 $\pm$ 2.64E+00	1.22E-01	1.73E-13 $\pm$ 4.86E-14
BD+00 444	02 40 42.8731	+01 11 55.240	0.61	23.94	1.14E+07	6.13E+06	8.60E+02 $\pm$ 4.87E+01	6.79E+01	— $\pm$ —	—	— $\pm$ —
BD+02 418	02 42 32.5410	+03 22 26.063	0.70	24.61	8.54E+06	1.07E+07	7.16E+02 $\pm$ 4.63E+01	2.61E+02	— $\pm$ —	—	— $\pm$ —
HD 17230	02 46 17.2768	+11 46 30.855	0.65	16.15	1.27E+07	7.91E+06	1.09E+03 $\pm$ 2.66E+01	1.24E+02	1.83E+01 $\pm$ 5.38E+00	5.17E-03	— $\pm$ —
CD-23 1056	02 46 42.8871	-23 05 11.803	0.70	23.39	8.26E+06	1.07E+07	4.81E+02 $\pm$ 2.35E+01	2.61E+02	3.67E+01 $\pm$ 1.09E+01	9.10E-03	— $\pm$ —
BD+33 529	02 52 07.13773	+34 23 21.6702	0.70	14.76	5.24E+06	1.07E+07	2.23E+02 $\pm$ 3.35E+00	2.61E+02	¡ 8.76E+00	9.10E-03	— $\pm$ —
BD+19 451	03 03 49.0599	+20 06 39.126	0.70	21.37	1.65E+07	1.07E+07	3.12E+03 $\pm$ 5.88E+01	2.61E+02	2.93E+01 $\pm$ 9.49E+00	9.10E-03	— $\pm$ —
HD 20165	03 14 47.2268	+08 58 50.856	0.71	23.13	1.08E+07	1.07E+07	¿ 1.64E+05	2.71E+02	8.00E+01 $\pm$ 2.36E+01	9.74E-01	— $\pm$ —
HD 21209	03 23 17.1764	-49 59 30.914	0.74	19.30	1.38E+07	1.36E+07	3.07E+03 $\pm$ 1.85E+01	5.87E+02	2.17E+01 $\pm$ 3.49E+00	1.88E-02	2.06E-13 $\pm$ 8.63E-14
HD 21175	03 23 35.2704	-40 04 35.027	0.74	17.70	1.75E+07	1.36E+07	¿ 2.04E+04	5.87E+02	2.04E+03 $\pm$ 4.84E+01	2.52E+00	1.02E-11 $\pm$ 8.11E-13
HD 21197	03 24 59.7306	-05 21 49.518	0.74	15.35	1.75E+07	1.36E+07	2.72E+03 $\pm$ 9.85E+00	5.87E+02	5.21E+01 $\pm$ 2.84E+00	1.88E-02	7.17E-13 $\pm$ 2.13E-13
HD 21749	03 26 59.2225	-63 29 56.763	0.70	16.33	1.57E+07	1.07E+07	3.03E+03 $\pm$ 6.32E+01	2.61E+02	¡ 7.99E+00	9.10E-03	— $\pm$ —
GJ 144	03 32 55.84496	-09 27 29.7312	0.86	3.20	2.00E+07	2.60E+07	¿ 1.92E+06	2.51E+03	1.42E+02 $\pm$ 3.05E+00	2.45E-01	2.29E-12 $\pm$ 6.33E-14
BD+16 502	03 43 52.5642	+16 40 19.305	0.65	17.21	7.17E+06	7.91E+06	3.30E+02 $\pm$ 1.22E+01	1.24E+02	2.23E+01 $\pm$ 5.61E+00	5.17E-03	— $\pm$ —
HD 23356	03 43 55.3429	-19 06 39.232	0.62	13.96	1.04E+07	6.24E+06	¿ 7.37E+04	7.38E+01	3.39E+01 $\pm$ 5.98E+00	2.45E-01	1.13E-12 $\pm$ 2.02E-13
HD 23484	03 44 09.1730	-38 16 54.371	0.86	16.17	2.81E+07	2.38E+07	¿ 2.22E+05	7.28E+03	1.52E+02 $\pm$ 2.27E+01	2.45E-01	1.49E-12 $\pm$ 3.66E-13
HD 24238	03 55 03.8426	+61 10 00.505	0.83	21.01	2.54E+07	1.53E+07	¿ 1.06E+05	1.29E+02	¡ 2.98E+01	2.45E-01	— $\pm$ —
HD 24451	04 01 19.62185	+76 09 33.7332	0.74	16.23	1.46E+07	1.36E+07	2.90E+03 $\pm$ 4.87E+01	5.87E+02	8.41E+01 $\pm$ 1.28E+01	1.88E-02	2.97E-13 $\pm$ 8.88E-14
HD 25665	04 09 35.0401	+69 32 29.011	0.79	18.77	2.26E+07	1.82E+07	1.14E+04 $\pm$ 1.89E+01	2.23E+03	4.40E+01 $\pm$ 2.46E+00	1.22E-01	— $\pm$ —
BD-04 782	04 15 09.52878	-04 25 05.9763	0.70	35.09	2.91E+07	1.07E+07	3.26E+03 $\pm$ 1.20E+02	2.61E+02	¡ 7.59E+01	9.10E-03	— $\pm$ —
GJ 166 A	04 15 16.31963	-07 39 10.3404	0.89	5.04	4.30E+07	3.21E+07	¿ 5.90E+05	3.11E+04	¡ 2.55E+00	2.52E+00	— $\pm$ —
HD 26900	04 16 32.6550	+36 30 06.574	0.83	24.53	2.28E+07	2.27E+07	1.49E+04 $\pm$ 4.85E+01	5.21E+03	1.14E+02 $\pm$ 3.40E+01	2.45E-01	2.26E-12 $\pm$ 5.29E-13
CPD-20 550	04 21 31.6088	-19 45 23.345	0.70	24.61	6.71E+06	1.07E+07	3.86E+02 $\pm$ 2.61E+01	2.61E+02	¡ 1.96E+01	9.10E-03	— $\pm$ —
HD 29883	04 43 35.4358	+27 41 14.648	0.70	21.86	2.27E+07	1.07E+07	1.27E+04 $\pm$ 5.04E+01	2.61E+02	— $\pm$ —	—	— $\pm$ —
LHS 199	04 55 57.594	-61 09 45.91	0.61	24.00	2.22E+06	6.13E+06	4.50E+02 $\pm$ 2.78E+01	6.79E+01	¡ 2.03E+01	1.38E-03	— $\pm$ —
HD 32450	05 02 28.42030	-21 15 23.9203	0.61	8.38	7.39E+06	6.13E+06	2.74E+02 $\pm$ 4.22E+00	6.79E+01	5.44E+00 $\pm$ 1.10E+00	1.38E-03	1.83E-13 $\pm$ 5.78E-14
CD-23 2363	05 03 21.88545	-23 15 00.8542	0.65	23.20	1.79E+07	7.91E+06	1.12E+03 $\pm$ 2.88E+01	1.24E+02	3.88E+01 $\pm$ 1.05E+01	5.17E-03	— $\pm$ —
L 233-30	05 17 53.48	-53 40 52.5	0.79	89.12	5.18E+06	1.82E+07	— $\pm$ —	—	¡ 2.92E+02	1.22E-01	— $\pm$ —
CD-42 1943	05 26 36.0189	-42 20 17.514	0.83	19.88	4.93E+06	2.27E+07	1.41E+02 $\pm$ 1.77E+01	5.21E+03	¡ 2.21E+01	2.45E-01	— $\pm$ —
HD 36003	05 28 26.0955	-03 29 58.400	0.70	12.94	1.51E+07	1.07E+07	1.82E+03 $\pm$ 4.16E+01	2.61E+02	— $\pm$ —	—	— $\pm$ —
HD 37008	05 38 11.86172	+51 26 44.6719	0.86	20.51	2.37E+07	2.71E+07	— $\pm$ —	—	2.86E+01 $\pm$ 9.74E+00	9.74E-01	— $\pm$ —
BD+62 780	05 45 48.2757	+62 14 12.386	0.61	13.51	8.37E+06	6.13E+06	— $\pm$ —	—	2.08E+01 $\pm$ 3.73E+00	1.38E-03	— $\pm$ —
CD-48 1982	05 47 18.2143	-48 31 30.504	0.61	20.79	1.01E+07	6.13E+06	7.19E+02 $\pm$ 2.26E+01	6.79E+01	2.45E+01 $\pm$ 9.67E+00	1.38E-03	1.23E-12 $\pm$ 2.23E-13
HD 40307	05 54 04.23991	-60 01 24.4977	0.79	12.94	1.83E+07	1.82E+07	— $\pm$ —	—	1.24E+01 $\pm$ 3.95E+00	1.22E-01	— $\pm$ —
LHS 1865	06 44 45.69310	+71 53 15.4480	0.61	21.53	5.37E+06	6.13E+06	1.74E+02 $\pm$ 1.44E+01	6.79E+01	¡ 3.09E+01	1.38E-03	5.09E-13 $\pm$ 2.02E-13
HD 48948	06 49 57.0256	+60 20 07.961	0.70	16.91	1.33E+07	1.07E+07	1.31E+03 $\pm$ 7.38E+00	2.61E+02	2.08E+01 $\pm$ 2.78E+00	9.10E-03	— $\pm$ —
BD+40 1758	06 56 28.11811	+40 04 27.5872	0.70	25.15	1.56E+07	1.07E+07	— $\pm$ —	—	¡ 2.05E+01	9.10E-03	— $\pm$ —
HD 266611	06 57 04.68907	+30 45 23.3738	0.70	18.89	8.24E+06	1.07E+07	5.37E+02 $\pm$ 1.62E+01	2.61E+02	2.43E+01 $\pm$ 1.10E+01	9.10E-03	— $\pm$ —
MCC 484	07 01 06.1884	+59 49 59.830	0.70	22.14	4.38E+06	1.07E+07	1.90E+02 $\pm$ 1.63E+01	2.61E+02	¡ 2.81E+01	9.10E-03	— $\pm$ —
HD 53680	07 03 50.23558	-43 33 40.8161	0.65	17.30	1.25E+07	7.91E+06	1.10E+03 $\pm$ 4.40E+01	1.24E+02	— $\pm$ —	—	— $\pm$ —
HD 53927	07 08 04.2389	+29 50 04.185	0.79	23.01	1.86E+07	1.82E+07	1.20E+04 $\pm$ 7.76E+01	2.23E+03	5.43E+01 $\pm$ 9.34E+00	1.22E-01	— $\pm$ —
BD-14 1750	07 10 49.5790	-14 25 58.925	0.70	23.36	8.84E+06	1.07E+07	6.00E+02 $\pm$ 4.25E+01	2.61E+02	— $\pm$ —	—	— $\pm$ —
HD 59582	07 31 07.7116	+14 36 50.915	0.70	20.75	1.27E+07	1.07E+07	1.80E+03 $\pm$ 3.98E+01	2.61E+02	¡ 1.21E+01	9.10E-03	— $\pm$ —
HD 63991	07 52 47.4276	+25 55 35.344	0.74	21.88	1.65E+07	1.36E+07	4.09E+03 $\pm$ 2.19E+01	5.87E+02	3.95E+01 $\pm$ 4.19E+00	1.88E-02	— $\pm$ —
HD 68834	08 14 35.9143	+13 01 22.174	0.70	19.19	1.32E+07	1.07E+07	1.74E+03 $\pm$ 1.22E+01	2.61E+02	2.72E+01 $\pm$ 7.49E+00	9.10E-03	— $\pm$ —
BD+31 1781	08 18 10.7790	+30 36 02.944	0.70	22.86	1.62E+07	1.07E+07	2.37E+03 $\pm$ 1.21E+01	2.61E+02	3.44E+01 $\pm$ 2.97E+00	9.10E-03	— $\pm$ —
LHS 2018	08 29 56.3283	+61 43 32.738	0.61	20.31	5.96E+06	6.13E+06	2.76E+02 $\pm$ 1.36E+01	6.79E+01	¡ 3.09E+01	1.38E-03	— $\pm$ —
HD 72760	08 34 31.6500	-00 43 33.864	0.92	21.10	5.26E+07	3.21E+07	¿ 3.46E+06	3.11E+04	3.06E+02 $\pm$ 7.45E+00	2.52E+00	4.03E-12 $\pm$ 7.64E-13
HD 73667	08 39 50.7918	+11 31 21.618	0.83	18.46	2.19E+07	2.27E+07	¡ 1.25E+01	5.21E+03	1.43E+01 $\pm$ 5.87E+00	2.45E-01	— $\pm$ —
HD 74377	08 45 10.3963	+41 40 18.604	0.79	24.97	2.09E+07	1.82E+07	7.22E+03 $\pm$ 2.95E+01	2.23E+03	¡ 2.83E+01	1.22E-01	— $\pm$ —
HD 77175 A	09 01 17.478	+15 15 56.82	0.70	18.47	1.15E+07	1.07E+07	1.20E+03 $\pm$	2.61E+02	1.94E+01 $\pm$ 3.34E+00	9.10E-03	— $\pm$ —
HD 79210	09 14 22.79157	+52 41 11.7206	0.61	6.33	7.08E+06	6.13E+06	4.14E+02 $\pm$ 6.06E+00	6.79E+01	2.23E+01 $\pm$ 3.51E+00	1.38E-03	5.55E-13 $\pm$ 6.09E-14
GJ 338 B	09 14 24.6788	+52 41 10.919	0.61	6.33	7.83E+06	6.13E+06	4.02E+02 $\pm$ 5.97E+00	6.79E+01	2.24E+01 $\pm$ 3.49E+00	1.38E-03	5.54E-13 $\pm$ 6.09E-14
HD 79555	09 14 53.65814	+04 26 34.4517	0.74	17.80	2.18E+07	1.36E+07	7.61E+03 $\pm$ 2.73E+01	5.87E+02	1.73E+02 $\pm$ 5.90E+00	1.88E-02	9.44E-12 $\pm$ 7.59E-13
BD+27 1739	09 18 21.5230	+27 18 41.626	0.70	20.98	1.09E+07	1.07E+07	8.97E+02 $\pm$ 9.50E+00	2.61E+02	6.19E+01 $\pm$ 9.82E+00	9.10E-03	1.36E-12 $\pm$ 4.57E-13
HD 80632	09 20 44.3171	-05 45 14.302	0.74	24.18	1.52E+07	1.36E+07	1.92E+03 $\pm$ 5.56E+01	5.87E+02	4.44E+01 $\pm$ 1.45E+01	1.88E-02	— $\pm$ —
HD 80768	09 26 53.1297	+75 56 03.340	0.61	20.95	1.30E+07	6.13E+06	1.77E+03 $\pm$ 5.55E+01	6.79E+01	6.86E+01 $\pm$ 2.04E+01	1.38E-03	7.52E-13 $\pm$ 1.69E-13
BD+81 297	09 27 56.1794	+80 34 48.811	0.61	23.10	1.32E+07	6.13E+06	1.14E+03 $\pm$ 1.28E+01	6.79E+01	2.17E+01 $\pm$ 9.41E+00	1.38E-03	— $\pm$ —
BD-04 2639	09 29 35.05287	-05 22 21.7364	0.61	24.18	1.08E+07	6.13E+06	8.02E+02 $\pm$ 3.80E+01	6.79E+01	6.51E+01 $\pm$ 2.05E+01	1.38E-03	— $\pm$ —
HD 82106	09 29 54.8252	+05 39 18.472	0.79	12.78	1.75E+07	1.82E+07	— $\pm$ —	—	1.00E+02 $\pm$ 3.41E+00	1.22E-01	2.03E-12 $\pm$ 2.43E-13
BD+23 2121	09 37 11.3404	+22 41 38.910	0.70	22.55	1.25E+07	1.07E+07	9.82E+02 $\pm$ 2.17E+01	2.61E+02	2.15E+01 $\pm$ 7.59E+00	9.10E-03	— $\pm$ —
HD 84035	09 43 25.66143	+42 41 29.6141	0.74	18.03	1.89E+07	1.36E+07	2.79E+03 $\pm$ 1.58E+01	5.87E+02	1.70E+01 $\pm$ 7.67E+00	1.88E-02	1.14E-12 $\pm$ 3.23E-13
HD 85488	09 52 11.36258	+03 13 18.6347	0.70	20.54	1.41E+07	1.07E+07	1.59E+03 $\pm$ 1.44E+01	2.61E+02	¡ 1.89E+01	9.10E-03	— $\pm$ —
HD 87883	10 08 43.1400	+34 14 32.133	0.89	18.30	2.47E+07	3.24E+07	1.08E+04 $\pm$ 2.19E+01	3.07E+04	7.21E+01 $\pm$ 1.67E+01	2.52E+00	— $\pm$ —
BD+75 403	10 10 58.51301	+75 08 28.9261	0.65	21.07	1.24E+07	7.91E+06	7.33E+02 $\pm$ 3.82E+01	1.24E+02	¡ 3.14E+01	5.17E-03	— $\pm$ —
GJ 380	10 11 22.14051	+49 27 15.2567	0.61	4.87	9.76E+06	6.13E+06	6.42E+02 $\pm$ 5.11E+00	6.79E+01	2.89E+01 $\pm$ 2.36E+00	1.38E-03	2.84E-13 $\pm$ 2.86E-14
HD 233719	10 13 57.38220	+52 30 24.2141	0.65	22.97	9.53E+06	7.91E+06	1.21E+03 $\pm$ 1.33E+01	1.24E+02	¡ 2.44E+01	5.17E-03	— $\pm$ —
36 UMa B	10 30 25.3093	+55 59 56.850	0.61	12.92	9.49E+06	6.13E+06	¡ 5.21E+00	6.79E+01	3.25E+01 $\pm$ 7.96E+00	1.38E-03	— $\pm$ —
BD+46 1635	10 31 24.2177	+45 31 33.779	0.61	16.01	1.18E+07	6.13E+06	8.25E+02 $\pm$ 1.93E+01	6.79E+01	1.79E+01 $\pm$ 6.79E+00	1.38E-03	1.18E-12 $\pm$ 2.56E-13
BD+57 1274	10 31 43.2242	+57 06 57.107	0.70	17.56	7.93E+06	1.07E+07	5.25E+02 $\pm$ 1.08E+00	2.61E+02	2.14E+01 $\pm$ 5.83E-01	9.10E-03	8.71E-13 $\pm$ 2.04E-13
BD+76 404	10 54 26.5092	+76 03 56.709	0.65	23.01	1.00E+07	7.91E+06	1.12E+03 $\pm$ 4.92E+01	1.24E+02	¡ 2.56E+01	5.17E-03	— $\pm$ —
BD-18 3106	11 07 27.70340	-19 17 29.3321	0.70	18.73	5.86E+06	1.07E+07	3.97E+02 $\pm$ 1.99E+01	2.61E+02	8.93E+01 $\pm$ 1.69E+01	9.10E-03	— $\pm$ —
HD 96612	11 08 14.0146	+38 25 35.874	0.89	22.82	1.96E+07	3.24E+07	9.84E+03 $\pm$ 1.12E+02	3.07E+04	¡ 1.51E+01	2.52E+00	— $\pm$ —
HD 97101	11 11 05.1720	+30 26 45.663	0.61	11.89	1.12E+07	6.13E+06	6.67E+02 $\pm$ 1.60E+01	6.79E+01	2.25E+01 $\pm$ 5.09E+00	1.38E-03	— $\pm$ —
HD 97214	11 11 10.7008	-10 57 03.192	0.70	19.87	9.04E+06	1.07E+07	1.17E+03 $\pm$ 3.29E+01	2.61E+02	¡ 2.37E+01	9.10E-03	— $\pm$ —
HD 97503	11 13 13.2345	+04 28 56.437	0.70	18.36	1.29E+07	1.07E+07	2.14E+03 $\pm$ 1.23E+01	2.61E+02	4.34E+01 $\pm$ 1.27E+01	9.10E-03	5.40E-13 $\pm$ 1.29E-13
HD 97658	11 14 33.1613	+25 42 37.390	0.61	21.58	7.49E+06	6.13E+06	¿ 1.73E+04	6.79E+01	4.08E+01 $\pm$ 1.15E+01	9.74E-01	— $\pm$ —
HD 97782	11 14 48.17139	-23 06 17.7241	0.70	23.11	1.66E+07	1.07E+07	1.61E+03 $\pm$ 6.01E+01	2.61E+02	¡ 2.67E+01	9.10E-03	— $\pm$ —
BD-13 3333	11 16 22.1464	-14 41 36.155	0.61	18.27	6.51E+06	6.13E+06	3.63E+02 $\pm$ 1.04E+01	6.79E+01	3.48E+01 $\pm$ 1.02E+01	1.38E-03	— $\pm$ —
CD-27 7978	11 17 07.5069	-27 48 48.715	0.61	17.67	7.49E+06	6.13E+06	4.55E+02 $\pm$ 2.35E+01	6.79E+01	4.46E+01 $\pm$ 1.37E+01	1.38E-03	— $\pm$ —
GJ 3662	11 24 59.7800	+40 00 12.675	0.74	23.47	8.45E+06	1.36E+07	4.92E+02 $\pm$ 3.29E+01	5.87E+02	2.59E+01 $\pm$ 1.18E+01	1.88E-02	— $\pm$ —
BD+63 965	11 31 13.0920	+63 09 27.122	0.61	23.01	9.28E+06	6.13E+06	7.47E+02 $\pm$ 7.20E+00	6.79E+01	8.44E+01 $\pm$ 1.59E+01	1.38E-03	1.25E-12 $\pm$ 3.94E-13
BD+51 1697	11 47 03.4988	+50 58 18.500	0.74	23.57	1.20E+07	1.36E+07	1.23E+03 $\pm$ 3.80E+01	5.87E+02	6.85E+01 $\pm$ 2.08E+01	1.88E-02	1.40E-12 $\pm$ 5.31E-13
HD 104067	11 59 10.0090	-20 21 13.612	0.83	20.38	2.17E+07	2.27E+07	9.57E+03 $\pm$ 1.36E+02	5.21E+03	— $\pm$ —	—	— $\pm$ —
HD 238090	12 12 20.8595	+54 29 08.724	0.70	15.24	6.59E+06	1.07E+07	3.31E+02 $\pm$ 4.67E+00	2.61E+02	¡ 6.74E+00	9.10E-03	— $\pm$ —
BD+49 2126	12 15 08.8430	+48 43 57.258	0.65	22.46	7.27E+06	7.91E+06	4.30E+02 $\pm$ 2.39E+00	1.24E+02	3.08E+01 $\pm$ 1.27E+00	5.17E-03	— $\pm$ —
HD 107576	12 21 59.84698	-41 03 33.2576	0.74	24.44	2.00E+07	1.36E+07	4.69E+03 $\pm$ 7.82E+01	5.87E+02	¡ 4.29E+01	1.88E-02	— $\pm$ —
HD 107888	12 23 53.5526	+12 34 48.911	0.70	21.48	7.47E+06	1.07E+07	3.11E+02 $\pm$ 3.60E+00	2.61E+02	1.01E+01 $\pm$ 1.73E+00	9.10E-03	— $\pm$ —
HD 110315	12 41 06.4777	+15 22 36.006	0.70	14.11	1.47E+07	1.07E+07	1.69E+03 $\pm$ 6.18E+00	2.61E+02	¡ 1.08E+01	9.10E-03	— $\pm$ —
HD 110833	12 44 14.54514	+51 45 33.4882	0.74	15.00	1.15E+07	1.36E+07	¿ 2.35E+04	5.87E+02	8.05E+01 $\pm$ 3.95E+00	1.22E-01	1.98E-12 $\pm$ 2.72E-13
HD 112575	12 57 43.95596	-14 27 48.6288	0.70	25.64	1.50E+07	1.07E+07	2.62E+03 $\pm$ 4.57E+01	2.61E+02	¡ 4.19E+01	9.10E-03	— $\pm$ —
HD 113827	13 05 41.4079	+49 28 18.964	0.74	21.60	1.11E+07	1.36E+07	1.68E+03 $\pm$ 3.88E+00	5.87E+02	4.16E+01 $\pm$ 1.93E+00	1.88E-02	1.23E-12 $\pm$ 3.43E-13
BD+21 2486	13 06 15.39818	+20 43 45.2749	0.74	19.71	1.15E+07	1.36E+07	— $\pm$ —	—	9.78E+01 $\pm$ 1.95E+01	1.88E-02	3.90E-12 $\pm$ 4.28E-13
BD+35 2406	13 07 35.0630	+34 24 06.061	0.79	24.80	1.38E+07	1.82E+07	1.89E+03 $\pm$ 2.10E+01	2.23E+03	4.89E+01 $\pm$ 1.14E+01	1.22E-01	— $\pm$ —
HD 114783	13 12 43.78556	-02 15 54.1335	0.79	21.08	1.85E+07	1.82E+07	¿ 1.49E+04	2.23E+03	5.66E+01 $\pm$ 8.92E+00	9.74E-01	— $\pm$ —
HD 238224	13 23 23.29688	+57 54 22.1403	0.70	24.12	1.25E+07	1.07E+07	1.55E+03 $\pm$ 4.70E+01	2.61E+02	1.36E+02 $\pm$ 2.81E+01	9.10E-03	8.55E-12 $\pm$ 7.48E-13
HD 116443	13 23 40.8451	+02 43 30.987	0.70	16.57	8.67E+06	1.07E+07	¿ 2.10E+04	2.61E+02	4.11E+01 $\pm$ 1.14E+01	2.45E-01	5.61E-13 $\pm$ 2.27E-13
HD 117936	13 33 32.4004	+08 35 12.345	0.79	18.05	1.85E+07	1.82E+07	5.45E+03 $\pm$ 9.28E+01	2.23E+03	7.02E+01 $\pm$ 1.65E+01	1.22E-01	1.45E-12 $\pm$ 3.91E-13
HD 118096	13 34 03.2376	+33 13 42.211	0.74	22.68	1.10E+07	1.36E+07	2.24E+03 $\pm$ 1.24E+01	5.87E+02	2.74E+01 $\pm$ 8.37E+00	1.88E-02	— $\pm$ —
BD+05 2767	13 34 21.50204	+04 40 02.6362	0.70	20.44	8.67E+06	1.07E+07	4.75E+02 $\pm$ 7.54E+00	2.61E+02	2.29E+01 $\pm$ 1.07E+01	9.10E-03	4.97E-13 $\pm$ 2.10E-13
BD-17 3890	13 35 42.2032	-18 15 12.562	0.61	24.24	5.71E+06	6.13E+06	2.40E+02 $\pm$ 2.54E+01	6.79E+01	¡ 4.08E+01	1.38E-03	— $\pm$ —
HD 118926	13 40 07.13057	-04 11 09.9609	0.70	15.08	6.30E+06	1.07E+07	3.07E+02 $\pm$ 1.67E+01	2.61E+02	¡ 1.17E+01	9.10E-03	— $\pm$ —
HD 118972	13 41 04.17106	-34 27 50.9672	0.74	15.69	2.69E+07	1.36E+07	¿ 1.94E+04	5.87E+02	2.11E+02 $\pm$ 2.39E+01	2.52E+00	4.12E-12 $\pm$ 5.30E-13
HD 119332	13 41 13.4047	+56 43 37.821	0.89	23.90	2.85E+07	3.24E+07	— $\pm$ —	—	7.48E+01 $\pm$ 2.62E+01	2.52E+00	— $\pm$ —
HD 119291	13 42 26.0345	-01 41 10.577	0.61	24.59	1.45E+07	6.13E+06	1.79E+03 $\pm$ 4.67E+01	6.79E+01	3.66E+01 $\pm$ 1.35E+01	1.38E-03	— $\pm$ —
HD 120476 A	13 49 04.0023	+26 58 47.585	0.74	13.48	2.69E+07	1.36E+07	5.92E+03 $\pm$ 6.78E+00	5.87E+02	1.01E+02 $\pm$ 2.04E+00	1.88E-02	1.59E-12 $\pm$ 2.12E-13
HD 120780	13 52 35.8602	-50 55 18.124	0.70	16.66	1.59E+07	1.07E+07	¿ 3.54E+04	2.61E+02	7.90E+01 $\pm$ 2.16E+01	2.52E+00	4.48E-12 $\pm$ 1.42E-12
BD+13 2721	13 53 27.56205	+12 56 33.4172	0.61	21.92	1.28E+07	6.13E+06	7.18E+02 $\pm$ 4.67E+01	6.79E+01	8.42E+01 $\pm$ 2.64E+01	1.38E-03	— $\pm$ —
HD 122064	13 57 32.05750	+61 29 34.3012	0.79	10.08	1.59E+07	1.82E+07	— $\pm$ —	—	2.44E+01 $\pm$ 4.77E+00	1.22E-01	1.34E-13 $\pm$ 4.59E-14
HD 122120	13 59 19.4031	+22 52 11.104	0.70	23.80	1.59E+07	1.07E+07	2.02E+03 $\pm$ 5.06E+01	2.61E+02	¡ 2.58E+01	9.10E-03	— $\pm$ —
HD 124106	14 11 46.17230	-12 36 42.3544	0.86	23.02	2.41E+07	2.71E+07	— $\pm$ —	—	1.27E+02 $\pm$ 3.05E+01	9.74E-01	5.34E-13 $\pm$ 1.85E-13
HD 124642	14 13 57.0781	+30 13 01.872	0.74	17.21	1.74E+07	1.36E+07	4.62E+03 $\pm$ 1.61E+01	5.87E+02	7.03E+01 $\pm$ 1.02E+01	1.88E-02	1.50E-12 $\pm$ 3.16E-13
HD 125455	14 19 34.86361	-05 09 04.2965	0.61	20.46	8.96E+06	6.13E+06	¿ 1.33E+04	6.79E+01	6.52E+01 $\pm$ 1.39E+01	9.74E-01	— $\pm$ —
BD+30 2512	14 21 57.2163	+29 37 46.616	0.65	14.52	1.18E+07	7.91E+06	1.23E+03 $\pm$ 6.45E+00	1.24E+02	4.83E+01 $\pm$ 2.25E+00	5.17E-03	1.02E-12 $\pm$ 1.99E-13
HD 127506	14 30 44.9769	+35 27 13.501	0.74	22.54	1.61E+07	1.36E+07	4.27E+03 $\pm$ 5.59E+00	5.87E+02	3.78E+01 $\pm$ 1.67E+00	1.88E-02	8.56E-13 $\pm$ 2.98E-13
HD 127339	14 30 47.71785	-08 38 46.8144	0.61	15.78	8.96E+06	6.13E+06	4.06E+02 $\pm$ 1.15E+01	6.79E+01	2.31E+01 $\pm$ 1.05E+01	1.38E-03	— $\pm$ —
HD 128165	14 33 28.8678	+52 54 31.647	0.79	13.24	1.87E+07	1.82E+07	5.53E+03 $\pm$ 1.60E+01	2.23E+03	3.11E+01 $\pm$ 7.78E+00	1.22E-01	4.46E-13 $\pm$ 8.41E-14
BD+34 2541	14 34 57.8115	+33 44 48.218	0.65	20.04	9.19E+06	7.91E+06	7.47E+02 $\pm$ 1.17E+00	1.24E+02	1.85E+01 $\pm$ 2.69E+00	5.17E-03	— $\pm$ —
HD 130004	14 45 24.1829	+13 50 46.734	0.89	18.81	1.87E+07	3.24E+07	1.19E+04 $\pm$ 1.23E+02	3.07E+04	3.21E+01 $\pm$ 1.07E+01	2.52E+00	— $\pm$ —
BD+17 2785	14 46 23.2824	+16 29 48.115	0.70	17.76	9.39E+06	1.07E+07	8.55E+02 $\pm$ 4.52E+01	2.61E+02	¡ 2.46E+01	9.10E-03	— $\pm$ —
BD+39 2801	14 48 01.4254	+38 27 58.440	0.61	23.99	1.18E+07	6.13E+06	1.01E+03 $\pm$ 4.03E+01	6.79E+01	3.05E+01 $\pm$ 1.10E+01	1.38E-03	1.29E-12 $\pm$ 5.26E-13
HD 130992	14 51 40.46506	-24 18 14.8741	0.74	16.76	1.80E+07	1.36E+07	5.49E+03 $\pm$ 5.71E+01	5.87E+02	— $\pm$ —	—	— $\pm$ —
HD 131582	14 53 41.5706	+23 20 42.690	0.79	23.51	1.70E+07	1.82E+07	6.02E+03 $\pm$ 1.48E+02	2.23E+03	7.17E+01 $\pm$ 2.64E+01	1.22E-01	— $\pm$ —
HD 132142	14 55 11.0436	+53 40 49.246	0.86	23.55	2.75E+07	2.71E+07	— $\pm$ —	—	¡ 2.92E+01	9.74E-01	— $\pm$ —
BD+06 2986	15 04 53.5262	+05 38 17.160	0.60	19.02	7.16E+06	5.75E+06	3.88E+02 $\pm$ 5.08E+00	5.92E+01	7.77E+00 $\pm$ 1.35E+00	1.18E-03	— $\pm$ —
BD-04 3873	15 22 04.10086	-04 46 38.8234	0.74	19.18	9.40E+06	1.36E+07	7.70E+02 $\pm$ 4.09E+01	5.87E+02	3.32E+01 $\pm$ 1.32E+01	1.88E-02	— $\pm$ —
HD 137303	15 25 58.50235	-26 42 20.8264	0.74	22.16	1.41E+07	1.36E+07	2.97E+03 $\pm$ 3.74E+01	5.87E+02	¡ 5.39E+01	1.88E-02	— $\pm$ —
HD 137778	15 28 12.21068	-09 21 28.2944	0.86	20.67	5.01E+07	2.71E+07	¿ 2.75E+04	1.34E+04	2.40E+02 $\pm$ 2.97E+01	9.74E-01	4.52E-12 $\pm$ 6.20E-13
HD 139477	15 35 20.0438	+60 05 13.171	0.79	19.55	1.59E+07	1.82E+07	4.61E+03 $\pm$ 5.32E+01	2.23E+03	9.67E+01 $\pm$ 1.28E+01	1.22E-01	7.49E-12 $\pm$ 4.47E-13
HD 139323	15 35 56.5662	+39 49 52.027	0.79	22.47	3.17E+07	1.82E+07	1.72E+04 $\pm$ 1.29E+02	2.23E+03	5.74E+01 $\pm$ 1.15E+01	1.22E-01	2.06E-12 $\pm$ 4.81E-13
HD 139341	15 36 02.22306	+39 48 08.9141	0.86	22.32	5.01E+07	2.71E+07	— $\pm$ —	—	1.07E+02 $\pm$ 1.40E+01	9.74E-01	— $\pm$ —
HD 142709	15 57 40.74436	-42 37 27.2394	0.74	14.73	1.34E+07	1.36E+07	1.78E+03 $\pm$ 4.17E+01	5.87E+02	— $\pm$ —	—	— $\pm$ —
HD 144628	16 09 42.7946	-56 26 42.542	0.65	14.83	1.16E+07	7.91E+06	¿ 4.40E+04	1.24E+02	— $\pm$ —	—	— $\pm$ —
14 Her	16 10 24.3145	+43 49 03.522	0.65	17.94	1.17E+07	7.91E+06	¿ 3.16E+04	1.24E+02	6.55E+01 $\pm$ 4.26E+00	2.52E+00	— $\pm$ —
BD+41 2695	16 20 52.7395	+40 57 41.221	0.70	15.79	9.78E+06	1.07E+07	6.49E+02 $\pm$ 5.84E+00	2.61E+02	1.41E+01 $\pm$ 1.71E+00	9.10E-03	— $\pm$ —
HD 147555	16 24 27.28476	-43 39 23.7163	0.65	29.45	1.16E+07	7.91E+06	9.86E+02 $\pm$ 6.07E+01	1.24E+02	— $\pm$ —	—	— $\pm$ —
HD 148467	16 27 56.9072	+07 18 19.598	0.65	17.53	1.17E+07	7.91E+06	1.05E+03 $\pm$ 2.43E+01	1.24E+02	1.40E+01 $\pm$ 4.76E+00	5.17E-03	— $\pm$ —
HD 151541	16 42 38.5765	+68 06 07.792	0.61	24.25	4.51E+06	6.13E+06	¿ 3.00E+04	6.79E+01	5.48E+01 $\pm$ 1.09E+01	9.74E-01	— $\pm$ —
BD+39 3048	16 49 24.6974	+39 16 34.476	0.74	22.35	9.47E+06	1.36E+07	8.06E+02 $\pm$ 1.01E+01	5.87E+02	2.37E+01 $\pm$ 3.45E+00	1.88E-02	— $\pm$ —
Ross 644	16 54 12.0327	+11 54 52.857	0.61	20.08	4.51E+06	6.13E+06	1.21E+02 $\pm$ 1.51E+01	6.79E+01	¡ 1.79E+01	1.38E-03	— $\pm$ —
HD 154712B	17 03 19.78133	+59 35 15.9688	0.74	24.96	8.48E+06	1.36E+07	¡ 5.33E+00	5.87E+02	2.73E+01 $\pm$ 3.36E+00	1.88E-02	6.39E-13 $\pm$ 1.41E-13
BD+54 1862	17 10 12.3543	+54 29 24.506	0.60	21.24	1.12E+07	5.75E+06	1.26E+03 $\pm$ 5.13E+01	5.92E+01	6.10E+01 $\pm$ 2.02E+01	1.18E-03	1.65E-12 $\pm$ 2.16E-13
HD 155712	17 12 37.62262	+18 21 04.3072	0.79	20.84	2.22E+07	1.82E+07	1.07E+04 $\pm$ 5.69E+00	2.23E+03	2.66E+01 $\pm$ 2.24E+00	1.22E-01	— $\pm$ —
HD 156668	17 17 40.49053	+29 13 38.0243	0.79	24.35	2.18E+07	1.82E+07	6.28E+03 $\pm$ 3.40E+01	2.23E+03	¡ 5.12E+01	1.22E-01	— $\pm$ —
HD 156985	17 17 50.4236	+52 26 49.609	0.83	18.53	1.94E+07	2.27E+07	7.04E+03 $\pm$ 6.63E+01	5.21E+03	5.09E+01 $\pm$ 1.58E+01	2.45E-01	— $\pm$ —
BPM 78873	17 18 21.72350	-01 46 53.2502	0.61	22.51	7.68E+06	6.13E+06	3.58E+02 $\pm$ 1.89E+01	6.79E+01	1.08E+02 $\pm$ 3.31E+01	1.38E-03	7.31E-13 $\pm$ 2.07E-13
HD 158633	17 25 00.0975	+67 18 24.148	0.79	12.79	1.93E+07	1.82E+07	¿ 6.09E+04	2.23E+03	6.89E+01 $\pm$ 9.33E+00	2.52E+00	— $\pm$ —
GJ 673	17 25 45.2323	+02 06 41.122	0.61	7.71	1.01E+07	6.13E+06	6.82E+02 $\pm$ 7.17E+00	6.79E+01	2.74E+01 $\pm$ 4.04E+00	1.38E-03	4.11E-13 $\pm$ 7.45E-14
HD 162283	17 50 34.0331	-06 03 01.037	0.61	22.19	8.73E+06	6.13E+06	4.45E+02 $\pm$ 4.07E+01	6.79E+01	¡ 5.08E+01	1.38E-03	— $\pm$ —
BD+21 3245	17 53 29.9358	+21 19 31.053	0.79	24.52	1.93E+07	1.82E+07	1.16E+04 $\pm$ 8.23E+01	2.23E+03	2.33E+02 $\pm$ 2.31E+01	1.22E-01	1.90E-12 $\pm$ 4.11E-13
G 204-45	18 07 44.4478	+39 04 26.915	0.70	22.64	1.59E+07	1.07E+07	1.37E+03 $\pm$ 3.32E+01	2.61E+02	¡ 2.71E+01	9.10E-03	3.44E-13 $\pm$ 1.22E-13
Wolf 1409	18 07 51.3998	+52 47 54.658	0.70	28.36	1.87E+06	1.07E+07	3.08E+01 $\pm$ 1.14E+01	2.61E+02	¡ 2.76E+01	9.10E-03	— $\pm$ —
HD 166620	18 09 37.41626	+38 27 27.9960	0.61	11.10	9.21E+06	6.13E+06	¿ 2.54E+04	6.79E+01	2.55E+01 $\pm$ 5.08E+00	2.45E-01	— $\pm$ —
G 205-20	18 25 31.92818	+38 21 12.6762	0.65	23.60	4.31E+06	7.91E+06	1.40E+02 $\pm$ 2.24E+01	1.24E+02	¡ 2.92E+01	5.17E-03	— $\pm$ —
HD 171314	18 33 17.7601	+22 18 51.312	0.74	23.39	1.64E+07	1.36E+07	2.26E+03 $\pm$ 2.96E+01	5.87E+02	¡ 2.10E+01	1.88E-02	— $\pm$ —
HD 229590	18 48 51.8715	+17 26 20.208	0.61	16.68	9.21E+06	6.13E+06	5.44E+02 $\pm$ 1.16E+01	6.79E+01	2.60E+01 $\pm$ 9.84E+00	1.38E-03	— $\pm$ —
HD 178445	19 10 52.26921	-47 09 31.0178	0.61	20.78	1.26E+07	6.13E+06	7.78E+02 $\pm$ 3.09E+01	6.79E+01	¡ 1.75E+01	1.38E-03	— $\pm$ —
HD 183870	19 32 06.7042	-11 16 29.790	0.61	17.69	4.23E+06	6.13E+06	¿ 5.60E+04	6.79E+01	1.24E+02 $\pm$ 1.33E+01	2.45E-01	— $\pm$ —
sig Dra	19 32 21.5899	+69 39 40.236	0.89	5.77	2.28E+07	3.24E+07	— $\pm$ —	—	4.66E+01 $\pm$ 3.15E+00	2.52E+00	4.07E-13 $\pm$ 2.05E-14
HD 332518	19 45 35.6050	+30 00 36.784	0.70	20.93	1.19E+07	1.07E+07	1.15E+03 $\pm$ 4.92E+01	2.61E+02	— $\pm$ —	—	— $\pm$ —
LHS 3517	20 04 10.90	-45 39 09.9	0.61	36.88	4.23E+06	6.13E+06	1.10E+02 $\pm$ 2.50E+01	6.79E+01	¡ 4.37E+01	1.38E-03	— $\pm$ —
HD 193202	20 10 52.41565	+77 14 20.3031	0.61	16.82	1.23E+07	6.13E+06	8.38E+02 $\pm$ 5.90E+00	6.79E+01	3.73E+01 $\pm$ 6.03E+00	1.38E-03	1.24E-13 $\pm$ 3.58E-14
HD 192961	20 19 36.93546	-46 25 41.2315	0.65	18.47	1.34E+07	7.91E+06	1.32E+03 $\pm$ 3.19E+01	1.24E+02	2.01E+01 $\pm$ 6.44E+00	5.17E-03	— $\pm$ —
CD-52 9466	20 21 10.91759	-51 47 27.8274	0.61	28.66	1.54E+07	6.13E+06	9.07E+02 $\pm$ 2.97E+01	6.79E+01	8.17E+01 $\pm$ 2.45E+01	1.38E-03	— $\pm$ —
HD 196877	20 42 18.78232	-52 41 57.3427	0.61	12.33	7.49E+06	6.13E+06	3.69E+02 $\pm$ 1.20E+01	6.79E+01	¡ 7.32E+00	1.38E-03	— $\pm$ —
HD 352860	20 44 21.94494	+19 44 58.8712	0.65	20.60	7.70E+06	7.91E+06	5.29E+02 $\pm$ 2.54E+01	1.24E+02	2.51E+01 $\pm$ 9.30E+00	5.17E-03	— $\pm$ —
HD 198550	20 50 10.5456	+29 23 02.915	0.70	20.23	2.05E+07	1.07E+07	4.83E+03 $\pm$ 6.39E+01	2.61E+02	— $\pm$ —	—	— $\pm$ —
BD+52 2815	20 50 33.0757	+52 53 58.545	0.61	22.74	1.05E+07	6.13E+06	5.44E+02 $\pm$ 4.16E+01	6.79E+01	— $\pm$ —	—	— $\pm$ —
HD 200779	21 05 19.7460	+07 04 09.471	0.65	15.05	1.38E+07	7.91E+06	1.31E+03 $\pm$ 2.49E+01	1.24E+02	3.73E+01 $\pm$ 5.27E+00	5.17E-03	— $\pm$ —
HD 202575	21 16 32.4670	+09 23 37.776	0.79	16.16	1.56E+07	1.82E+07	5.29E+03 $\pm$ 1.82E+01	2.23E+03	9.13E+01 $\pm$ 6.92E+00	1.22E-01	9.17E-13 $\pm$ 2.83E-13
GJ 825	21 17 15.26879	-38 52 02.4958	0.61	3.97	6.05E+06	6.13E+06	3.05E+02 $\pm$ 2.59E+00	6.79E+01	9.85E+00 $\pm$ 7.86E-01	1.38E-03	1.04E-13 $\pm$ 1.41E-14
HD 203850	21 26 58.45314	-56 07 30.9477	0.79	23.06	1.41E+07	1.82E+07	7.86E+03 $\pm$ 7.28E+01	2.23E+03	— $\pm$ —	—	— $\pm$ —
HD 205390	21 36 41.24416	-50 50 43.3891	0.86	14.81	2.17E+07	2.71E+07	— $\pm$ —	—	9.71E+01 $\pm$ 9.80E+00	9.74E-01	9.07E-13 $\pm$ 1.85E-13
HD 207144	21 48 00.04545	-40 15 21.8898	0.79	24.50	1.77E+07	1.82E+07	6.59E+03 $\pm$ 6.86E+01	2.23E+03	¡ 1.31E+01	1.22E-01	— $\pm$ —
HD 207491	21 49 12.228	+05 43 22.29	0.79	22.56	1.57E+07	1.82E+07	4.50E+03 $\pm$ 6.62E+01	2.23E+03	4.35E+01 $\pm$ 1.11E+01	1.22E-01	— $\pm$ —
HD 208038	21 53 05.3533	+20 55 49.871	0.79	23.30	2.11E+07	1.82E+07	1.61E+04 $\pm$ 4.69E+01	2.23E+03	1.54E+02 $\pm$ 2.43E+01	1.22E-01	5.47E-12 $\pm$ 1.08E-12
LP 758-73	21 53 07.5400	-12 49 40.845	0.61	24.12	4.92E+06	6.13E+06	2.10E+02 $\pm$ 6.79E+00	6.79E+01	¡ 1.76E+01	1.38E-03	— $\pm$ —
CD-61 6651	21 59 32.09420	-60 55 58.7116	0.65	23.73	1.16E+07	7.91E+06	8.61E+02 $\pm$ 2.55E+01	1.24E+02	¡ 1.11E+01	5.17E-03	— $\pm$ —
G 127-28	22 24 45.53616	+22 33 04.0696	0.61	20.92	1.76E+07	6.13E+06	2.29E+03 $\pm$ 5.03E+01	6.79E+01	4.02E+01 $\pm$ 1.19E+01	1.38E-03	4.45E-13 $\pm$ 1.40E-13
HD 213042	22 29 15.23549	-30 01 06.2712	0.74	15.69	1.93E+07	1.36E+07	3.74E+03 $\pm$ 4.38E+01	5.87E+02	2.78E+01 $\pm$ 5.48E+00	1.88E-02	— $\pm$ —
HD 214731	22 40 58.70043	-46 12 07.1842	0.74	23.30	1.25E+07	1.36E+07	— $\pm$ —	—	¡ 1.44E+01	1.88E-02	— $\pm$ —
HD 215152	22 43 21.3028	-06 24 02.953	0.79	21.61	2.14E+07	1.82E+07	— $\pm$ —	—	1.92E+01 $\pm$ 9.49E+00	1.22E-01	— $\pm$ —
HD 216520	22 47 31.8769	+83 41 49.302	0.65	19.56	1.29E+07	7.91E+06	¿ 1.26E+04	1.24E+02	3.97E+01 $\pm$ 1.67E+01	2.52E+00	— $\pm$ —
HD 216259	22 51 26.3584	+13 58 11.941	0.79	22.54	1.83E+07	1.82E+07	— $\pm$ —	—	1.91E+01 $\pm$ 3.19E+00	1.22E-01	— $\pm$ —
GJ 879	22 56 24.05327	-31 33 56.0351	0.74	7.61	1.42E+07	1.36E+07	— $\pm$ —	—	9.91E+01 $\pm$ 4.82E+00	1.88E-02	1.86E-12 $\pm$ 2.07E-13
HD 218511	23 09 40.95125	-67 43 58.1682	0.65	14.84	1.29E+07	7.91E+06	1.73E+03 $\pm$ 3.65E+01	1.24E+02	7.44E+01 $\pm$ 1.41E+01	5.17E-03	4.01E-13 $\pm$ 9.14E-14
HD 219538	23 16 18.1577	+30 40 12.743	0.83	24.91	2.56E+07	2.27E+07	1.98E+04 $\pm$ 9.67E+01	5.21E+03	5.63E+01 $\pm$ 1.04E+01	2.45E-01	— $\pm$ —
HD 220339	23 23 04.8953	-10 45 51.277	0.83	19.18	1.94E+07	2.27E+07	— $\pm$ —	—	3.49E+01 $\pm$ 2.26E+00	2.45E-01	— $\pm$ —
HD 221503	23 32 49.3982	-16 50 44.321	0.65	14.56	1.08E+07	7.91E+06	1.28E+03 $\pm$ 1.76E+01	1.24E+02	7.26E+01 $\pm$ 6.00E+00	5.17E-03	— $\pm$ —
BD+00 5017	23 35 00.2759	+01 36 19.455	0.61	20.82	1.22E+07	6.13E+06	1.52E+03 $\pm$ 9.57E+00	6.79E+01	1.73E+02 $\pm$ 4.62E+00	1.38E-03	1.12E-11 $\pm$ 1.03E-12
CD-49 14193	23 36 18.27486	-48 35 17.0609	0.61	25.04	1.05E+07	6.13E+06	6.69E+02 $\pm$ 2.57E+01	6.79E+01	2.77E+01 $\pm$ 1.17E+01	1.38E-03	2.46E-11 $\pm$ 2.86E-12
BD-03 5691	23 42 10.62469	-02 34 36.6880	0.61	24.29	7.98E+06	6.13E+06	5.61E+03 $\pm$ 1.64E+01	6.79E+01	8.04E+01 $\pm$ 3.36E+00	1.38E-03	— $\pm$ —
G 130-9	23 45 49.5010	+36 15 18.179	0.74	19.82	7.39E+06	1.36E+07	4.46E+02 $\pm$ 1.24E+01	5.87E+02	¡ 1.00E+01	1.88E-02	— $\pm$ —
BD+29 5007	23 50 27.8618	+30 21 11.731	0.70	23.65	1.30E+07	1.07E+07	1.92E+03 $\pm$ 2.22E+01	2.61E+02	7.83E+01 $\pm$ 1.27E+01	9.10E-03	— $\pm$ —
BD+28 4660	23 53 08.5916	+29 01 05.034	0.65	19.91	8.57E+06	7.91E+06	6.82E+02 $\pm$ 3.85E+01	1.24E+02	¡ 1.00E+01	5.17E-03	— $\pm$ —
BD+45 4378	23 58 43.50974	+46 43 44.9540	0.61	17.12	1.01E+07	6.13E+06	3.68E+02 $\pm$ 1.75E+01	6.79E+01	— $\pm$ —	—	— $\pm$ —

Equations

$$f_{GALEX}=10^{\frac{23.9-m_{GALEX}}{2.5}}$$

$$d=(\frac{R^2\cdot T_{\mathrm{eff}}^4}{S_{\mathrm{eff}}}{)}^{0.5}\text{AU},$$

Full text

stars: evolution, stars: low-mass

††journal: ApJ††software: Astropy   (Price-Whelan et al., 2018),  Matplotlib (Hunter, 2007),  Numpy  (van der Walt et al., 2011),   Scipy   (Jones et al., 2001),  PHOENIX  (Hauschildt et al., 1997; Short & Hauschildt, 2005)

1 Introduction

Astronomers have discovered thousands of exoplanets, with an estimate for the occurrence rate of Earth-sized planets in the habitable zone (HZ) around GK stars of 22% (Petigura et al., 2013) from the Kepler mission statistics. The Transiting Exoplanet Survey Satellite (TESS) is expected to detect yet another 3,500 planetary candidates during its mission life (Ricker et al., 2009, 2014; Barclay et al., 2018; Huang et al., 2018). While TESS is expected to discover $\sim$700 new planets around K stars, none are expected to be in the HZ since TESS is optimized to find planets with short orbital periods, excluding the longer orbital periods of habitable zone planets around K stars (Barclay et al., 2018; Huang et al., 2018). However, the PLAnetary Transits and Oscillations of stars (PLATO) mission, which will be optimized to find habitable zone planets around K dwarfs, is expected to discover $\sim$30 HZ K dwarf planets in the next decade (PLATO Definition Study Report, 2017).

Further research is being conducted on what stellar characteristics increase the chances of HZ planets being in fact habitable (e.g. Cockell et al., 2016; Kaltenegger, 2017). This would require a balance of environmental factors such as stellar lifetime, ultraviolet (UV) radiation, stellar winds, and HZ width. Currently, the most promising candidates for potentially habitable planets are thought to be around M stars (2,400 – 3,700 K; 0.08 – 0.45 M*⊙; conservative HZ width 0.1AU, Kopparapu et al. 2013); over half of all known HZ planets are around M dwarfs. Rocky planets around these stars are more easily detectable than around Sun-like stars due to favorable star-planet radius ratios, mass ratios, and shorter periods (Charbonneau & Deming, 2007). However, these stars are typically the most active of all spectral types and HZ planets around them are close-in and most likely tidally locked (e.g. Checlair et al., 2017; Barnes & Rory, 2017). Planets around M stars that were initially expected to be likely habitable, such as Proxima Centauri b, are losing favorability due to excessive flaring (MacGregor et al. 2018). M stars have been shown to have the largest levels of stellar activity during their pre-main sequence, which lasts through the duration of the formation of the planet and both its primordial and secondary atmospheres (Schneider & Shkolnik, 2018; Shkolnik & Barman, 2014). Additionally, the large magnetic fields ($\sim$kG) of most M stars has been shown to potentially create magma oceans or partial melt the mantle of close-in planets, leading to increased volcanism and strong outgassing of greenhouse gases (Kislyakova et al., 2017, 2018). K stars (3,700 – 5,200K; 0.6 – 0.9M⊙*), with conservative HZ width of 0.4AU, (Kopparapu et al., 2013) may offer super-habitable conditions due to decreased stellar activity, lower magnetic field strengths, faster contraction onto the main sequence, and more distant and wider HZs. The highest potential of finding a truly habitable planet may lie with K stars.

The evolution of stellar activity as determined in the near-UV (NUV), far-UV (FUV), and X-ray wavelength regions has been studied in great detail for both GK stars (e.g. Findeisen et al., 2011) and M stars (e.g. Stelzer et al., 2013; Shkolnik & Barman, 2014; Schneider & Shkolnik, 2018) using archived Galaxy Evolution Explorer (GALEX; Martin et al. 2004) and RÖntgenSATellit (ROSAT; Truemper 1982) photometric data. However, a comprehensive investigation of the high-energy radiation environments of K-type stars has yet to be performed. The purpose of this study is to fill in this gap in our understanding of stellar evolution.

1.1 The Importance of UV Data

The UV radiation incident on a planet is a critical factor in determining if that planet is potentially habitable and if any biosignatures could be detectable. UV radiation ionizes and photodissociates some of the most important molecules for the development of life (e.g. H2O, H2, O2, CO2, H2S, and OCS) and signatures that would be indicative of life (e.g. CH4, NH3, and N2O) with potential for complete erosion of the atmosphere (e.g. Kasting et al., 1993; Lichtenegger et al., 2010; Segura et al., 2010; Hu et al., 2012). UV radiation can be split into three regimes: the extreme-UV (EUV, 100-912 Å), the far-UV (FUV, 912-1700 Å), and the near-UV (NUV, 1700-3200 Å) as defined in Linsky & Güdel (2015). The EUV heats and inflates a planets upper-atmosphere, exacerbating its erosion (Koskinen et al., 2010; Lammer et al., 2007). Other than very limited data from the former Extreme Ultraviolet Explorer (EUVE) satellite, no information in this wavelength regime exists for stars other than the Sun. Any missions observing in the EUV will exclude most of the ionizing flux due to absorption by the ISM. These values are crucial as photochemical atmospheric models of HZ planets and abundance rate models require an input of EUV stellar fluxes, currently being interpolated from a limited number of FUV and X-ray observations.

Realistic information regarding the evolution of the NUV, FUV, and EUV is of the utmost importance for using models to answer questions regarding planetary atmospheres. UV radiation, in particular the ratio of FUV/NUV, can impact the abundance rates and photochemistry of the atmospheres in the production of hazes in depleting atmospheres (Zerkle et al., 2012; Arney et al., 2017) and ozone in oxidizing atmospheres (Segura et al., 2003, 2005), both of which drastically alter the planetary spectrum. This affects not only the composition, but also the detectability and stability of the atmospheres of these planets. For future missions such as the James Webb Space Telescope (JWST) that will focus on spectra, a planet with a hazy or depleted atmosphere will not make a good target.

1.2 The K Star Advantage

While current popularity resides among M stars as the most likely to host identifiable habitable planets, stellar variability, excess flaring and tidal locking in the HZ is cause for concern (e.g. Shields et al., 2016). Early and mid-K spectral-type stars have been suggested by Heller & Armstrong (2014) to be “super-habitable”, i.e. the probability of life on a planet orbiting in the HZ of one of these super-habitable stars is higher than the probability of life on an Earth-sized planet orbiting in the HZ of a G2V star. Cuntz & Guinan (2016) analyzed several factors to determine the Habitable-Planetary-Real-Estate Parameter (HabPREP), which depends on the frequency of different stars, the rate of contraction onto the main sequence, the size and longevity of the HZ, UV and X-ray emission and flare frequency and power. They individually determined that the highest probability of having a habitable planet is in the early-K star regime. The longer lifetimes of the continuous HZ of these types of stars compared to F and G stars allow for life to tune their environment and develop a more favorable biosignature, whereas unmagnetized planets around M stars may lose their atmosphere within the first 100 Myr based on severe UV irradiance (Airapetian et al., 2017). Lingam & Loeb (2017) find that K6V stars around 0.67 M*⊙* would take the least amount of time for complex life to develop since increased oxygen levels from UV photolysis permit the emergence of complex life. Arney et al. (2018) have independently concluded that there is a similar “K star advantage” because a planet orbiting a K6V star has the potential to produce detectable CH4 and O2. However, the UV flux for most of these calculations was assumed to be constant throughout the timescale of the formation of life and could consequently lead to incorrect determinants. K star UV evolution is thus needed to determine the probability of planetary habitability. The highest potential of finding a truly habitable planet may lie with K stars.

2 The K Star Sample

We compiled K stars in young moving groups (YMG) and clusters ranging in age from 10 Myr to 625 Myr. The associations included are TW Hydra (10 $\pm$ 3 Myr, Bell et al. 2015), Beta Pictoris (24 $\pm$ 3 Myr, Shkolnik et al. 2017), Columba (42${}^{+6}_{-4}$ Myr, Bell et al. 2015), Carina (45${}^{+11}_{-7}$ Myr, Bell et al. 2015), Tucana-Horologium (45 $\pm$ 4 Myr, Bell et al. 2015), AB Doradus (149${}^{+51}_{-19}$ Myr, Bell et al. 2015), Ursa Majoris (414 $\pm$ 23 Myr; Jones et al. 2015, 2017), Praesepe (600 Myr, Kraus & Hillenbrand 2007), and Hyades (625 $\pm$ 50 Myr, Perryman et al. 1997). In addition, we define a field star sample as K stars within 30 pc to which we assign an age of 5 Gyr. The sample was drawn from SIMBAD and confirmed individually to not be close binaries or known association members.

Taking into account the wide range of ages in this study, we must consider how similar spectral types represent different masses over various ages. Using the effective stellar temperatures in Pecaut & Mamajek (2013) and the model isochrones from Baraffe et al. (2015), we determine mass estimates for the spectral types used in this work following Table 1. We used masses from 0.6 – 0.9 M*⊙* but allowed one spectral subtype lower and higher to account for spectral type uncertainty.

The YMG members were identified by Gagné et al. (2017) for TW Hydra; Shkolnik et al. (2017) for Beta Pictoris; Malo et al. (2013) for Carina, Columba, and AB Doradus; Kraus et al. (2014) for Tucana Horologium; Montes et al. (2001) for Ursa Major; Wang et al. (1995) for Praesepe; and Goldman et al. (2013) for the Hyades. Due to the low number of K star members in some of the age ranges, we combined groups of similar age ranges to calculate the median and inner quartiles for each age bin, as seen in Figures 1 and 2.

3 GALEX Photometry

We cross referenced proper motion corrected coordinates of our sample to GALEX using the GALEXview tool111http://galex.stsci.edu/galexview/ with a search radius of 10″. The NUV (1771 – 2831 Å) and FUV (1344 – 1786 Å) detectors have a non-linear response at 104 counts s*-1* and 34 counts s*-1*, respectively, equivalent to a magnitude of $\approx$15 for both NUV and FUV. Measured magnitudes less than 15 were thus taken as lower limits. Additionally, we excluded detections with photometric flags for bright star window reflection, dichroic reflection, detector run proximity, or bright star ghost. We visually inspected the GALEX tiles for each observation to ensure that there was no contamination that was not caught by the flags. A comparison of the number of objects that were in our input sample, observed by GALEX, and were then resolved with no photometric flags for each band can be seen in Table 1 and Figure 3.

In the NUV, the higher mass objects were less likely to have usable photometry, as they were too bright for reliable photometric measurements. This is due to the more massive stars being intrinsically brighter and saturating the detector. For the Hyades and Praesepe clusters, the low fraction of detections is most likely due to their distances (∼47 pc and 177 pc, respectively; van Leeuwen 2009).

For some objects there were multiple observations with multiple exposure times, in which case we took the weighted mean of the magnitude as our measurement and the weighted standard deviations as our uncertainty. All of the photometry can be seen in Table 4.

For the objects that were observed but not detected, we calculated an upper limit for the object by repeating the search with a 10′ radius and proceeding using the method described in Schneider & Shkolnik (2018). The objects that were measured with a magnitude $<$15 were taken as upper limits. These were then addressed in the same manner as the detections.

4 Evolution of the Photospheric UV Emission

One of the goals of the HAZMAT program is to provide measurements of FUV and NUV flux densities for low-mass stellar models. Most low-mass stellar atmosphere models predict photospheric emission only and do not contain contributions from the stellar upper-atmosphere, leading to an underestimate of stellar photospheric emission. Work is being carried out to include contributions from these regions (i.e. Peacock et al. 2015, Fontenla et al. 2016), but observations are needed to fully inform these models with empirical data in the NUV and FUV.

The PHOENIX stellar atmosphere models (Hauschildt et al. 1997, Short & Hauschildt 2005) were used to calculate the photospheric NUV and FUV flux densities of each K star in our sample using the stellar masses derived in Table 1 and the age of the star. The evolution of the NUV and FUV photospheric model flux densities for select masses from 0.6 to 0.9 M*⊙* with a reference 1 M*⊙* can be seen in Figure 4. As the mass increases, the photospheric contribution becomes greater. For each mass, the photospheric contributions become nearly constant after the age at which contraction onto the main sequence has ended, since the temperature of the star does not significantly change after the pre-main sequence evolution during the ages used in this study (Figure 5).

Figure 6 shows the fraction of the photospheric flux density compared to the absolute observed values for the YMG members and field stars as a function of both mass and age. The NUV has a higher fraction of photosphere compared to observed flux, with most of the contribution being between 10 and 100%. Values reported that were larger than 100% are due to uncertainties in both the mass and age of the star and were taken to be 100% photospheric. The photospheric FUV flux density was typically $<$1%. For both the NUV and the FUV we see a decrease in photospheric flux with decreasing mass, although this trend is much steeper for the FUV, where the photospheric contribution becomes negligible. With increasing age, we see an increase in photospheric contribution equally for both NUV and FUV flux densities.

For each of the YMG members and field stars, we subtract the photospheric contribution derived from the PHOENIX models from the absolute observed GALEX flux densities to calculate the excess emission, representative of upper-atmosphere activity.

5 Evolution of the Observed NUV and FUV Emission

With the second data release of Gaia (Gaia Collaboration et al., 2018), accurate distances to all objects in our sample are available. Therefore, we investigate the absolute GALEX NUV and FUV flux densities rather than analyzing them relative to the Two Micron All-Sky Survey (2MASS) J-band, such as in Shkolnik & Barman (2014) and Schneider & Shkolnik (2018).

To explore the evolutionary trends, we convert the GALEX reported magnitudes to flux densities in $\mu$Jy using

[TABLE]

where $m_{GALEX}$ is the GALEX FUV or NUV magnitude. These values were then translated to absolute fluxes using the known distances from Gaia Data Release 2 (Gaia Collaboration et al., 2018). Because we are interested in the excess UV contribution from the K stars, we calculated the photospheric contribution using the PHOENIX models as described in section 4 and subtracted these from the flux density calculations reported in GALEX.

Figure 7 shows the evolution of the excess NUV and FUV flux densities as a function of age. Both the NUV and FUV decrease in time. The slope of the decrease is much more gradual for the NUV than that of the FUV and the values obtained for early M stars in Shkolnik & Barman (2014) and mid- to late M stars in Schneider & Shkolnik (2018). Unlike both Shkolnik & Barman (2014) and Schneider & Shkolnik (2018) where the median values remain constant up until 625 Myr and then distinctly drop off, we see a more gradual decrease in time starting at 100 Myr in the FUV. The wide spread comes from intrinsic astrophysical variation and perhaps initial spin rate, which has been shown to cause large spreads in the X-ray due to the bimodal distribution of stellar rotation in young open clusters for solar-like stars (Gondoin, 2017, 2018). Additionally, the uncertainty in stellar ages beyond the age of the Hyades may cause increased variation among the field stars.

Figures 8 and 9 show the distribution of the NUV and FUV excess flux for the different age groups. The scatter in the FUV ranges from 1.5 – 3 orders of magnitude, similar to Shkolnik & Barman (2014). Shkolnik & Barman (2014) and Schneider & Shkolnik (2018) see a change in the median FUV value of about 1.5 orders of magnitude for stars with masses 0.35 – 0.6 M*⊙*, whereas for the K stars we see a shift of only 1 order of magnitude. For the NUV, the scatter ranges from 1 – 4 orders of magnitude, with the scatter increasing for the older age groups. The slopes of the NUV and FUV excess flux density vs age curves are found in Table 3. These trends can be used to predict flux densities and their ranges for K stars in the NUV and FUV bands.

5.1 Mass Distributions

Figure 10 is the same as Figure 7 but broken down by mass group. In both the NUV and FUV, we see that in general, all three mass groups follow the trends of each other. This is counter to the trends seen in Schneider & Shkolnik (2018), where the late M stars remain active much longer than early M stars. Even though the higher-mass stars have a larger contribution from the photosphere that is being subtracted off to yield the excess, the intrinsic flux of the higher-mass stars is large enough that the excess flux is still largest for higher-mass stars throughout most of the evolutionary period. However, once the stars reach field age, the photospheric contribution becomes so large that most of the excess flux for higher-mass stars approaches zero.

6 The Relationship Between GALEX FUV and NUV for K Stars

6.1 FUV $/$ NUV

The ratio of FUV to NUV is valuable in understanding the photochemistry of terrestrial planet atmospheres. Segura et al. (2005) showed that lifetimes of the biogenic gases CH4, N2O, and CH3Cl are actually increased, allowing a higher probability of being detected. However, the FUV to NUV ratio also sets the abundance rates of molecules such as CO2, O2, and O3, as the FUV will break down CO2, forming O2 and O3, the latter of which will be destroyed by the NUV. This abiotic oxygen and ozone can thus produce false-positive biosignatures (e.g. Domagal-Goldman et al., 2014; Tian et al., 2014; Harman et al., 2015).

We calculate FUV/NUV excess flux densities as a function of mass for stars with both NUV and FUV flux densities, as seen in Figure 11. The trends seen in Schneider & Shkolnik (2018) continue into the K-star regime, with increasing separation between the young and old stars as the stellar mass increases, demonstrating that the FUV/NUV ratio is both mass- and age-dependent.

6.2 NUV vs FUV

When comparing the NUV to FUV excess flux density, we do not see the same tight correlations as Shkolnik & Barman (2014) nor Schneider & Shkolnik (2018). Instead, we see in Figure 13 that with increasing mass (i.e. earlier spectral type), the scatter becomes greater and the correlation worsens. We calculated both a Pearson’s R2 statistic (Pearson, 1895) and a Spearman Rank correlation value (Spearman, 1904) for each K spectral type mass range. The results can be seen in Figure 14. In both tests we see a similar trend, where the highest mass (i.e. earliest spectral type) stars have correlations generally with $\rho$ $<0.5$ and lower mass (i.e. later spectral type) stars have correlations generally $\rho$ $>0.5$. This trend also appears in Miles & Shkolnik (2017).

The reason for this decrease in correlation with higher mass can most easily be seen in analyzing the model photospheric fluxes in Figure 4. In comparing the model values of a single mass from 10 Myr – 5 Gyr, the photospheric flux density of a 0.6 M*⊙* star changes by no more than a single order of magnitude. However, the photospheric flux density of a 0.9 M*⊙* star is much more prevalent and changes by as much as four orders of magnitude. The scatter in the FUV excess flux density vs NUV excess flux density then comes from differences in age, whereas the intrinsic scatter of a single age group is much smaller.

7 X-Ray Evolution

The X-ray flux has frequently been used as a stellar activity diagnosis (e.g. Jackson et al., 2012; Booth et al., 2017). X-ray wavelengths may be used in conjunction with the NUV and FUV to interpolate into the EUV, which is most powerful in understanding the photodissociation of molecules in a planet’s atmosphere. To compare X-ray and UV data, we cross-referenced our sample of K stars with the Second ROSAT All-Sky Survey Point Source Catalog (2RXS, 5-124 Å; Boller et al. 2016) with a search radius of 38″, which was determined by Voges et al. (1999) to be the 3$\sigma$ positional error. We then used the hardness ratio and the count rate to convert to flux $F_{X}$ in in erg s*-1* cm*-2* using the empirical fit of Schmitt et al. (1995). The number of detections can be seen in the last column of Table 1.

As can be seen in Figure 15, the X-ray flux remains steady through the age of Tucana-Horologium (45 Myr) and decreases by the age of AB Doradus (150 Myr), similar to the trend in FUV. These results are also seen in Jackson et al. (2012), who see that FGKM stars remain saturated in the X-ray until about 100 Myr. We derive a slope of $(-0.906\pm 0.079)$log$(t)$ from 150 Myr - 5 Gyr (Table 3).

A histogram of the range in X-ray values for each age can be seen in Figure 16. The flux for each age ranges from 1-3 orders of magnitude, similar to the NUV and FUV values. Again, the wide spread likely comes from the bimodal distribution of stellar rotation in young open clusters for solar-like stars (Gondoin, 2017, 2018) and uncertainty in stellar ages up to 10 Gyr among the field stars.

Unlike for the early-M stars in Shkolnik & Barman (2014), we do not see a clear distinction between young X-ray emitters and old emitters when looking at the UV flux compared to the X-ray flux (Figure 17). This may be due to larger spread in x-ray flux we see at the younger ages of K stars (Figure 16) and the more gradual decrease of the x-ray flux with age (Figure 18) as compared to the M stars in Shkolnik & Barman (2014), leading to an undefined distinction between young and old emitters.

Figure 18 shows both the K and M star NUV, FUV, and X-ray fluxes (as opposed to flux densities) from this work, Shkolnik & Barman (2014), and Schneider & Shkolnik (2018). The M-star work was done relative to the J band flux, as the distances to the stars were not all known. We have therefore redone this work relative to the J band flux for comparison with the M stars. The results are extremely similar except for the K dwarf NUV median value at 150 Myr, which is noticeably elevated. This is most likely due to small numbers in that age bin and uncertainties within the model photosphere, yet is still consistent within the inner quartiles seen in Figure 7

Comparing the K stars to the M stars, we see in both the FUV and the X-ray that at the age where a planet is forming its atmosphere (10 - 500 Myr; see Schaefer & Fegley, 2010, and references therein), the K star flux has dropped below that of the M stars, meaning that any primordial atmosphere has a lower chance of being destroyed. In comparing the X-ray medians to those of the NUV and FUV, we see that the X-ray flux dominates during the young ages of the stars, then falls below the NUV values after 650 Myr, a trend also seen in the M dwarfs of Shkolnik & Barman (2014).

8 UV and X-Ray Flux at the Habitable Zone

To better understand the habitability of planets around K stars, we need to understand what the UV and X-ray flux incident on a planet in the habitable zone would be. Using the radii and effective temperature estimates of Baraffe et al. (2015), we calculated the HZ distance as a function of age for a K star (0.8 M*⊙), an early-M star (0.4 M⊙), and a late-M star (0.1 M⊙*) using Equation 3 of Kopparapu et al. (2013):

[TABLE]

where the stellar radius $R$ and effective temperature $T_{\rm eff}$ are given in solar units and $S_{\rm eff}$ is the stellar photospheric flux at the HZ, which is strictly a function of the stellar temperature. The stellar flux at the HZ for each star was interpolated from the $S_{\rm eff}$ values given in Kopparapu et al. (2014) for temperatures from 2600 K - 7200 K. The HZ distances are shown in Figure 19a as a function of age. The opaque regions represent the conservative habitable zones and the translucent regions are the optimistic habitable zones. The size of the K-dwarf HZ is about twice as large as that of the M-stars and farther from the star by at least 0.4 AU.

We then calculated the range of NUV, FUV, and X-ray median values in the HZ at each age, as seen in Figures 19b, 19c, and 19d, respectively. In each of the plots, the K-star flux levels are below those of the M-stars by at least five times for the early-M stars and at least 50 times for the late-M stars. The initial rise in the NUV, FUV, and X-ray flux of all of the M stars is due to the HZ becoming closer-in to the star as the star ages, thus increasing the UV and X-ray flux in this region. For this reason, the UV and X-ray HZ flux of late-M stars is larger during the early stages of planet evolution than when the planet was initially formed. Conversely, the UV and X-ray HZ flux of K stars decreases from the time of planet formation, thus allowing more suitable conditions for the development and detectability of life, perhaps garnering K dwarfs the “superhabitable” label.

9 Implications and Conclusions

Because of their high-energy radiation environments, more frequent flaring, and tidally locked planets, M stars may not be the most suitable locations for finding habitable planets. Instead, if high UV emission is detrimental, then K stars offer a more favorable UV environment throughout the key evolutionary period of the planet and its atmosphere due to wider habitable zones and faster contraction onto the main sequence.

Using GALEX and ROSAT photometry, we calculated the NUV and FUV excess (i.e. photosphere subtracted to yield the emission from the upper-atmosphere) flux densities and X-ray flux levels from young moving group members, clusters, and field stars ranging from 10 Myr to 5 Gyr. We find that the FUV and X-ray fluxes remain constant for $\sim$100 Myr before decreasing, as compared to M stars, which remain constant until $\sim$650 Myr (Shkolnik & Barman, 2014; Schneider & Shkolnik, 2018). To determine the extent of the potential “super-habitability” of K stars, we also analyzed these results within the habitable zones of K and M stars. We find that the UV and X-ray flux incident on a planet is 5 - 50 times lower than that of early-M stars and 50 - 1000 times lower than that of late-M stars (depending on age). These UV and X-ray levels offer a much more suitable environment and a higher probability of planet habitability and the detection of any biomarkers.

These results should be used to advise estimations of the extreme-UV, for which very little data currently exist. The EUV fluxes are some of the most effective measures of chemical alteration, as the photodissociation cross-sections are the largest for most molecules in this regime. The EUV flux is expected to follow the trends of both the FUV and X-ray emission. Therefore, we would expect the EUV to decline as early as $\sim$100 Myr.

The ratio of FUV to NUV is an important determinate in the probability of detecting a habitable planet. Larger ratios allow for longer lifetimes of biogenic gases such as as CH4, N2O, and CH3Cl, leading to a higher probability of detection. However, this ratio also affects the abundances of abiotic molecules such as CO2, O2, and O3 that may lead to false positive signatures. We find that this ratio is both mass- and age-dependent for all K spectral types.

While these results are informative of median UV and X-ray fluxes incident on K star planets during the early stages of their evolution, this does not entail a higher probability of habitability in the case of all K dwarfs.

The authors would like to acknowledge support from the NASA Habitable Worlds grant NNX16AB62G. We wish to thank the anonymous referee for an insightful and helpful report. This work is based on observations made with the NASA Galaxy Evolution Explorer and the RÖntgenSATellit. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. This research utilized the public data from the second ROSAT All-Sky Survey (https://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass2rxs.html). This work makes use of data products from the Two Micron All-Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).