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Table A.1:

Pleiades spectroscopic sample of 45 low-mass stars and brown dwarfs.

Object 		SpT $\alpha$a  $\delta$a $I_{\rm C}$ Zb Yb Jb Hb Kb Ref.c
      (mag) (mag) (mag) (mag) (mag) (mag)  
HHJ 2 M6.5 03 38 27.52   25 30 18.1 17.30 16.591 $\pm$ 0.011 15.938 $\pm$ 0.007 15.284 $\pm$ 0.007 14.747 $\pm$ 0.005 14.355 $\pm$ 0.006 1,-,1,7
HHJ 3 M6.0 03 48 50.45   22 44 29.9 17.51 16.562 $\pm$ 0.010 15.825 $\pm$ 0.006 15.098 $\pm$ 0.006 14.531 $\pm$ 0.005 14.141 $\pm$ 0.004 1,-,1,7
HHJ 6 M6.5 03 41 42.41   23 54 57.1 17.00 16.171 $\pm$ 0.007 15.464 $\pm$ 0.006 14.709 $\pm$ 0.004 14.124 $\pm$ 0.004 13.760 $\pm$ 0.050 1,-,1,7
HHJ 7 M6.0 03 57 49.37   22 08 31.0 17.00 16.149 $\pm$ 0.007 15.498 $\pm$ 0.005 14.831 $\pm$ 0.005 14.286 $\pm$ 0.005 13.884 $\pm$ 0.003 1,-,1,7
PPl 1 M6.5 03 45 41.27   23 54 09.8 18.21 17.166 $\pm$ 0.014 16.189 $\pm$ 0.008 15.360 $\pm$ 0.006 14.782 $\pm$ 0.005 14.305 $\pm$ 0.006 4,8,7,5
PPl 14 M5.5 03 44 34.30   23 51 24.6 17.43 16.920 $\pm$ 0.011 16.157 $\pm$ 0.007 15.438 $\pm$ 0.007 14.884 $\pm$ 0.005 14.478 $\pm$ 0.006 4,2,7,1
PPl 15 M6.5 03 48 04.66   23 39 30.2 17.91 17.014 $\pm$ 0.012 16.054 $\pm$ 0.007 15.283 $\pm$ 0.006 14.704 $\pm$ 0.005 14.256 $\pm$ 0.006 4,2,7,2
Calar 3 M8.0 03 51 25.57   23 45 21.3 19.00 ... ... 16.083 $\pm$ 0.010 15.478 $\pm$ 0.009 15.009 $\pm$ 0.011 4,3,5,3
Teide 1 M8.0 03 47 17.92   24 22 31.7 19.26 18.174 $\pm$ 0.029 17.067 $\pm$ 0.013 16.215 $\pm$ 0.010 15.591 $\pm$ 0.009 15.096 $\pm$ 0.011 4,3,5,2
PIZ 1 M9.0 03 48 31.52   24 34 37.3 20.00 19.218 $\pm$ 0.065 17.883 $\pm$ 0.025 16.715 $\pm$ 0.015 15.977 $\pm$ 0.012 15.357 $\pm$ 0.014 5,-,7,6
Roque 4d M9.0 03 43 53.55   24 31 11.6 20.25 18.970 $\pm$ 0.054 17.709 $\pm$ 0.025 16.649 $\pm$ 0.016 15.942 $\pm$ 0.016 15.260 $\pm$ 0.040 6,-,-,5
Roque 11 M8.0 03 47 12.08   24 28 31.7 19.06 ... 16.988 $\pm$ 0.013 16.174 $\pm$ 0.087 15.505 $\pm$ 0.009 15.048 $\pm$ 0.012 6,-,8,2
Roque 13 M7.5 03 45 50.66   24 09 03.5 18.67 17.478 $\pm$ 0.017 16.582 $\pm$ 0.010 15.705 $\pm$ 0.008 15.095 $\pm$ 0.006 14.580 $\pm$ 0.008 6,8,7,5
Roque 14 M7.0 03 46 42.98   24 24 50.7 18.27 17.484 $\pm$ 0.018 16.403 $\pm$ 0.009 15.550 $\pm$ 0.066 14.890 $\pm$ 0.006 14.391 $\pm$ 0.007 6,-,8,7
Roque 16 M6.0 03 47 39.02   24 36 22.2 17.91 17.112 $\pm$ 0.013 16.271 $\pm$ 0.008 15.548 $\pm$ 0.007 14.992 $\pm$ 0.006 14.570 $\pm$ 0.008 6,8,7,3
Roque 17 M6.5 03 47 23.97   22 42 37.4 17.87 ... 16.123 $\pm$ 0.008 15.354 $\pm$ 0.007 14.809 $\pm$ 0.006 14.402 $\pm$ 0.007 6,-,2,7
Teide 2 M6.0 03 52 06.72   24 16 00.5 18.02 17.079 $\pm$ 0.013 16.255 $\pm$ 0.009 15.515 $\pm$ 0.008 14.971 $\pm$ 0.008 14.507 $\pm$ 0.008 7,7,7,3
CFHT 9 M6.5 03 49 15.12   24 36 22.5 17.71 16.847 $\pm$ 0.011 16.059 $\pm$ 0.007 15.371 $\pm$ 0.006 14.890 $\pm$ 0.005 14.433 $\pm$ 0.007 8,8,7,3
CFHT 10 M6.5 03 44 32.32   25 25 18.0 17.78 16.994 $\pm$ 0.012 16.209 $\pm$ 0.009 15.450 $\pm$ 0.008 14.883 $\pm$ 0.007 14.476 $\pm$ 0.007 8,8,7,3
CFHT 12 M8.0 03 53 55.12   23 23 36.2 17.97 16.947 $\pm$ 0.012 16.027 $\pm$ 0.007 15.172 $\pm$ 0.006 14.569 $\pm$ 0.005 14.088 $\pm$ 0.005 8,8,3,3
CFHT 15 M7.0 03 55 12.60   23 17 37.3 18.62 17.842 $\pm$ 0.022 16.877 $\pm$ 0.012 15.977 $\pm$ 0.010 15.348 $\pm$ 0.009 14.842 $\pm$ 0.010 8,8,3,3
MHObd 3 M8.0 03 41 54.16   23 05 04.7 18.27 17.349 $\pm$ 0.016 16.376 $\pm$ 0.010 15.522 $\pm$ 0.008 14.975 $\pm$ 0.007 14.415 $\pm$ 0.007 8,8,7,4
NPL 26 M5.0 03 47 07.89   24 23 37.9 15.70 15.094 $\pm$ 0.004 14.598 $\pm$ 0.003 13.954 $\pm$ 0.003 13.415 $\pm$ 0.002 13.080 $\pm$ 0.002 9,-,4,2
NPL 34 M6.0 03 48 55.65   24 21 40.1 17.05 16.220 $\pm$ 0.007 15.636 $\pm$ 0.005 14.963 $\pm$ 0.005 14.416 $\pm$ 0.004 14.055 $\pm$ 0.005 9,-,1,2
NPL 36 M7.5 03 48 19.02   24 25 12.7 18.66 17.655 $\pm$ 0.020 16.668 $\pm$ 0.011 15.930 $\pm$ 0.009 15.365 $\pm$ 0.008 14.935 $\pm$ 0.011 9,-,7,2
NPL 38 M8.0 03 47 50.41   23 54 47.9 19.18 18.179 $\pm$ 0.028 17.138 $\pm$ 0.014 16.311 $\pm$ 0.011 15.622 $\pm$ 0.009 15.093 $\pm$ 0.012 9,-,8,2
MHObd 1 M7.0 03 44 52.42   24 36 49.5 17.95 17.147 $\pm$ 0.014 16.294 $\pm$ 0.008 15.487 $\pm$ 0.059 14.948 $\pm$ 0.006 14.525 $\pm$ 0.007 10,10,-,4
Roque 5 M9.0 03 44 22.44   23 39 01.3 20.19 19.107 $\pm$ 0.064 17.857 $\pm$ 0.025 16.874 $\pm$ 0.017 16.254 $\pm$ 0.016 15.666 $\pm$ 0.018 11,-,7,5
CFHT 1 M4.9 03 51 51.56   23 34 49.1 16.10 15.431 $\pm$ 0.005 14.857 $\pm$ 0.004 14.260 $\pm$ 0.003 13.768 $\pm$ 0.003 13.385 $\pm$ 0.003 12,-,3,3
CFHT 2 M4.9 03 52 44.29   23 54 15.0 16.61 15.738 $\pm$ 0.005 15.184 $\pm$ 0.004 14.554 $\pm$ 0.004 14.000 $\pm$ 0.004 13.654 $\pm$ 0.004 12,-,3,3
CFHT 5 M5.5 03 48 44.69   24 37 23.5 17.02 16.260 $\pm$ 0.008 15.584 $\pm$ 0.005 14.911 $\pm$ 0.005 14.419 $\pm$ 0.004 14.002 $\pm$ 0.005 12,-,7,3
CFHT 7 M5.6 03 52 05.83   24 17 31.0 17.34 16.512 $\pm$ 0.009 15.860 $\pm$ 0.007 15.176 $\pm$ 0.006 14.618 $\pm$ 0.006 14.251 $\pm$ 0.007 12,-,7,3
CFHT 16 M9.3 03 44 35.16   25 13 42.8 18.66 17.656 $\pm$ 0.020 16.584 $\pm$ 0.010 15.662 $\pm$ 0.007 14.985 $\pm$ 0.006 14.448 $\pm$ 0.008 12,12,7,3
CFHT 17 M7.9 03 43 00.17   24 43 52.3 18.80 17.791 $\pm$ 0.021 16.841 $\pm$ 0.013 16.022 $\pm$ 0.010 15.425 $\pm$ 0.010 15.070 $\pm$ 0.060 12,-,3,3
CFHT 25 M9.0 03 54 05.35   23 33 59.3 19.69 18.651 $\pm$ 0.041 17.573 $\pm$ 0.024 16.647 $\pm$ 0.018 15.964 $\pm$ 0.016 15.434 $\pm$ 0.017 12,-,3,3
NPL 40 M9.8 03 48 49.03   24 20 25.4 20.55 19.222 $\pm$ 0.069 18.227 $\pm$ 0.035 17.237 $\pm$ 0.023 16.569 $\pm$ 0.020 16.059 $\pm$ 0.029 12,-,8,2
Roque 7 M8.3 03 43 40.31   24 30 11.2 19.50 18.552 $\pm$ 0.038 17.490 $\pm$ 0.021 16.494 $\pm$ 0.014 15.853 $\pm$ 0.015 15.470 $\pm$ 0.020 12,-,3,3
Roque 25 L0.1 03 48 30.75   22 44 50.4 21.80 20.389 $\pm$ 0.193 18.936 $\pm$ 0.065 17.714 $\pm$ 0.039 16.861 $\pm$ 0.035 16.251 $\pm$ 0.027 12,-,9,5
BPL 327 M7.1 03 55 23.08   24 49 04.9 18.07 17.087 $\pm$ 0.014 16.311 $\pm$ 0.009 15.528 $\pm$ 0.008 15.013 $\pm$ 0.007 14.595 $\pm$ 0.008 13,-,6,5
BRB 17 L0.0 03 54 07.98   23 54 27.9 20.92 19.841 $\pm$ 0.111 18.451 $\pm$ 0.050 17.408 $\pm$ 0.033 16.628 $\pm$ 0.030 16.028 $\pm$ 0.029 14,-,5,6
PLIZ 28 L0.0 03 54 14.06   23 17 52.0 21.20 20.028 $\pm$ 0.136 18.873 $\pm$ 0.062 17.601 $\pm$ 0.035 16.818 $\pm$ 0.031 16.138 $\pm$ 0.030 14,-,5,6
PLIZ 35 L2.0 03 52 39.16   24 46 29.5 21.46 20.292 $\pm$ 0.030 19.271 $\pm$ 0.100 18.066 $\pm$ 0.055 17.106 $\pm$ 0.042 16.509 $\pm$ 0.042 14,-,5,6
BRB 21 L3.0 03 54 10.27   23 41 40.2 21.68 20.215 $\pm$ 0.030 19.260 $\pm$ 0.101 18.143 $\pm$ 0.062 17.171 $\pm$ 0.046 16.393 $\pm$ 0.040 14,-,5,6
BRB 23 L3.5 03 50 39.54   25 02 54.7 22.03 ... 19.786 $\pm$ 0.112 18.225 $\pm$ 0.044 17.358 $\pm$ 0.038 16.563 $\pm$ 0.043 14,-,5,6
BRB 29 L4.5 03 54 01.43   23 49 57.7 22.84 ... ... 18.686 $\pm$ 0.103 17.711 $\pm$ 0.081 16.999 $\pm$ 0.070 14,-,5,6

Notes. (a) Coordinates from UKIDSS Galaxy Cluster Survey DDR6. (b) ZYJHK-band photometry from UKIDSS Galaxy Cluster Survey DDR6, except for the measurements at Z band of PLIZ 35 and BRB 21 (Casewell et al. 2007), MKO K band of HHJ 6, Roque 4, CFHT 17, and Roque 7 (Pinfield et al. 2003), and J band of MHObd 1 (2MASS, converted to UKIDSS photometric system). (c) References for the quadruplet (SpT,Li,$\mu $,$I_{\rm C}$): Spectral type or lithium test: 1) Steele & Jameson (1995); 2) Basri et al. (1996); 3) Rebolo et al. (1996); 4) Martín et al. (1996); 5) Cossburn et al. (1997); 6) Zapatero Osorio et al. (1997); 7) Martín et al. (1998a); 8) Stauffer et al. (1998b); 9) Festin (1998b); 10) Stauffer et al. (1998a); 11) Martín et al. (1998b); 12) Martín et al. (2000); 13) Pinfield et al. (2003); 14) this study. Spectral type uncertainties for our L-type targets are listed in Table 1; for the other objects the uncertainties are typically of half a subclass. Proper motion: 1) Hambly et al. (1993); 2) Pinfield et al. (2000); 3) Moraux et al. (2001); 4) Deacon & Hambly (2004); 5) Bihain et al. (2006); 6) Casewell et al. (2007); 7) Lodieu et al. (2007); 8) Stauffer et al. (2007); 9) this study. $I_{\rm C}$-band photometry: 1) Stauffer et al. (1994); 2) Festin (1998a); 3) Bouvier et al. (1998); 4) Stauffer et al. (1998a); 5) Jameson et al. (2002); 6) Bihain et al. (2006); 7) Stauffer et al. (2007). Magnitude errors are of 0.05-0.1 mag. (d) Roque 4 has radial velocity and spectral features consistent with cluster membership (Zapatero Osorio et al. 1997; Kirkpatrick et al. 2008).


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