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Table A.2

Basic stellar data of the sample of UMa group members.

Object HIP number α (2000.0) δ (2000.0) Parallax [mas] Spec. type V mag. Ks mag.

HD 11131 8486 01 49 23.36 –10 42 12.8 44.32± 3.02 G1V 6.727 5.149
HD 11171 8497 01 49 35.10 –10 41 11.1 43.13± 0.26 F3III 4.664 3.872
HD 22049 16537 03 32 55.84 –09 27 29.7 310.94± 0.16 K2V 3.730 1.776
HD 26913 19855 04 15 25.79 +06 11 58.7 47.49± 0.68 G5IV 6.960 5.271
HD 26923 19859 04 15 28.80 +06 11 12.7 46.88± 0.47 G0IV 6.314 4.903
HD 38393 27072 05 44 27.79 –22 26 54.2 112.02± 0.18 F7V 3.586 2.508
HD 41593 28954 06 06 40.48 +15 32 31.6 65.48± 0.67 K0V 6.762 4.822
HD 60491 36827 07 34 26.17 –06 53 48.0 40.73± 1.00 K2V 8.160 6.019
HD 61606 37349 07 39 59.33 –03 35 51.0 70.37± 0.64 K2V 7.200 4.885
HD 63433 38228 07 49 55.06 +27 21 47.5 45.45± 0.53 G5IV 6.930 5.258
HD 95650 53985 11 02 38.34 +21 58 01.7 84.95± 1.05 M0 9.690 5.688
HIP 57548 57548 11 47 44.40 +00 48 16.4 298.04± 2.30 M4V 11.080 5.654
HD 125451 69989 14 19 16.28 +13 00 15.5 38.32± 0.28 F5IV 5.400 4.394
HD 135599 74702 15 15 59.17 +00 47 46.9 63.11± 0.70 K0 7.000 4.958
HD 139006 76267 15 34 41.27 +26 42 52.9 43.46± 0.28 A0V+G5Va 2.210 2.206
HD 147584 80686 16 28 28.14 –70 05 03.8 82.53± 0.52 F9V+M4Vb 4.910 3.661
HD 165185 88694 18 06 23.72 –36 01 11.2 56.97± 0.48 G5V 5.949 4.469
HD 175742 92919 18 55 53.22 +23 33 23.9 46.74± 0.85 K0Vc 8.090 5.637
HIP 104383 104383 21 08 45.47 –04 25 36.9 36.92± 1.53 K6+M1d 9.430 6.398
HD 217813 113829 23 03 04.98 +20 55 06.9 40.46± 0.57 G5V 6.652 5.148

Notes. All parallaxes are Hipparcos parallaxes (van Leeuwen 2007). Ks band magnitudes were taken from 2MASS (Skrutskie et al. 2006) and are combined magnitudes for tight binaries. For spectroscopic binaries, the spectral type is displayed for both components.

Reference. References for spectral type.

(b)

HD 147584: mean value of M4 of the range given by Skuljan et al. (2004) (M1V-M7V);

(c)

HD 175742: SB1 (Tokovinin et al. 2006); literature not unanimous on the parameters (Eggleton & Tokovinin 2008);

(d)

HIP 104383: Balega et al. (2004).

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