1142 Table 2.

Star Date (UT) HD 88913

R. F. Griffin and A. P. Cornell Radial velocities of stars in Clube Area 6.

Velocity (km s-1)

Star Date (UT)

Velocity (km s-1) Velocity (km s-1)

Spectroscopic Binary Orbit in Paper XVII HD 88973* 1992 Jan. 17.05 +60.0 HD 88992

1989 Feb. 23.15 1990 Feb. 14.22 -14.1 -13.8

HD 90793 (continued) 1993 Dec. 25.12 +34.9 1994 Dec. 10.16 +35.1 HD 91064

1989 Feb. 23.17 1990 Feb. 14.25 +20.7 +20.1

Star Date (UT) HD 94441 1989 Feb. 23.20 1990 Feb. 14.27

+99.3 +98.9

Star Date (UT) HD 95940 1989 Feb. 23.23 1990 Feb. 13.14

Velocity (km s-1)

-21.6 -21.7

Star Date (UT) HD 97718 1989 Feb. 25.25 1990 Feb. 13.13

Velocity (km s-1)

+23.0 +21.9

Star Date (UT) HD 98827 1989 Feb. 25.27 1990 Feb. 13.18

Velocity (km s-1)

-20.1 -19.6

1992 Apr. 26.93 +99.0 1994 Dec. 10.18 +99.2

1995 Jan. HD 94563

2.19 +98.9

1992 Jan. 17.08 +20.5 HD 92256

1989 Feb. 23.17 1990 Feb. 14.25 1992 Jan. 17.08 HD 92309 1989 Feb. 23.18 1990 Feb. 14.25

+7.5 +7.1 +6.8

1992 Dec. 19.13 -22.1 HD 96005

1989 Feb. 23.23 1990 Feb. 13.14 1992 Dec. 19.13 HD 96402 -2.0 -2.8 -1.6

1992 Jan. 18.10 +21.5 HD 97718 B*

1989 Feb. 25.25 1990 Feb. 13.14 +21.9: +20.2:

1993 Dec. 29.11 -20.3 HD 98917

1989 Feb. 25.27 1990 Feb. 13.18 +27.4 +27.6

1992 Jan. 17.05 -14.1 HD 89003

1989 Feb. 23.15 1990 Feb. 14.22 +11.6 +11.6

1992 Jan. 17.05 +11.0 HD 89003 B*

1990 Feb. 14.22 HD 89003 C* 1990 Feb. 14.22 HD 89073 1989 Feb. 23.15 1990 Feb. 14.23

-2.0:

Spectroscopic Binary Orbit in Paper XVII HD 94577

1989 Feb. 23.20 1990 Feb. 14.29 1992 Apr. 26.93 -11.2 -12.1 -9.4

1992 Jan. 18.11 +22.6 HD 97750

1989 Feb. 25.25 1990 Feb. 13.16 -20.3 -20.4

1993 Dec. 29.11 +27.5 HD 99091

1989 Feb. 25.27 1990 Feb. 13.18 +12.0 +12.4

Spectroscopic Binary Orbit in Paper XVII HD 96402 B*

1993 Mar.22.97 Dec. 25.17 1996 Dec. 16.23 1997 Jan. 25.14 HD 96643 1989 Feb. 23.23 1990 Feb. 13.15 1993 Feb. 14.02 HD 96768 1989 Feb. 23.23 1990 Feb. 13.15 1993 Feb. 14.03 HD 96768 B* 1993 Feb. 14.03 HD 96818

+9.9 +8.6 +5.7 +4.5 +30.6 +30.4

+14.0

+66.6 +66.3

1992 Jan. 17.04 +65.8 HD 89073 B*

1990 Feb. 14.23 HD 89255 1989 Feb. 23.15 1990 Feb. 14.23

+2.7

1992 Jan. 17.08 +30.9 HD 92789 Spectroscopic Binary Orbit in Paper XVII HD 92789 B* 1993 Dec. 25.12 +10.5 HD 92830

1989 Feb. 23.18 1990 Feb. 14.25 +14.9 +14.7

30.87 -11.7 1993 Mar.22.98 -11.7 Dec. 25.16 -11.6 1994 May 3.87 -11.1 Dec. 10.19 -11.9 1996 Mar.29.96 -11.3 Dec. 16.22 -11.6 1997 Apr. 27.85 -11.9 HD 94656

1989 Feb. 23.21 1990 Feb. 14.29 -14.5 -14.7

1992 Jan. 17.09 +15.1 HD 92920

1989 Feb. 23.18 1990 Feb. 14.26 +16.0 +16.2

1992 Apr. 26.93 -14.2 1994 Dec. 11.18 -14.7 HD 94783

1989 Feb. 23.21 1990 Feb. 14.29 1992 Apr. 26.93 HD 94865 1989 Feb. 23.21 1990 Feb. 14.29 1992 Apr. 30.87 HD 94887 1989 Feb. 23.21 1990 Feb. 14.29 1992 Apr. 30.88 HD 95166

+6.8 +6.4 +7.4

+24.2 +23.6

1992 Jan. 17.06 +23.7 HD 89337

1989 Feb. 23.15 1990 Feb. 14.23 1992 Jan. 17.06 HD 89380 1989 Feb. 23.15 1990 Feb. 14.23 1992 Jan. 17.05 HD 89607 1989 Feb. 23.16 1990 Feb. 14.23 1992 Jan. 17.06 HD 90014 1989 Feb. 23.16 1990 Feb. 14.24

+3.0 +3.4 +2.9

1992 Jan. 17.09 +16.1 HD 92998

1989 Feb. 23.18 1990 Feb. 14.26 +55.0 +55.3

1992 Jan. 17.09 +54.6 HD 92998 B*

1992 Jan. 17.09 HD 93140 -28.4 +0.3 -0.2 -0.4

+6.4 +6.5 +6.4

Spectroscopic Binary Orbit in Paper XVII HD 93278

1989 Feb. 23.19 1990 Feb. 14.26 +15.4 +14.8

1992 Jan. 18.10 -19.9 HD 97977

1989 Feb. 25.25 1990 Feb. 13.16 +23.7 +24.1

1993 Dec. 29.12 +13.1 HD 99321

1989 Feb. 25.27 1990 Feb. 13.18 1993 Dec. 29.12 HD 99406 1989 Feb. 25.27 1990 Feb. 13.18

-1.9 -2.3 -1.4

-4.6 -5.0 -5.2 -3.6 -3.7 -3.6

1992 Jan. 18.10 +23.6 1993 Mar.22.97 +23.7 1994 Feb. 21.01 +24.4 HD 97977 B* 1990 Feb. 13.17 +25.8 1992 Jan. 18.10 +32.8 Apr. 24.90 +30.5 1993 Feb. 12.09 +30.1 Mar.22.98 +29.8 Dec. 25.18 +30.0 1994 Feb. 21.01 +30.8 Dec. 11.20 +26.1 1996 Dec. 16.24 +31.1 1997 Jan. 26.15 +30.8 Apr. 24.93 +31.7 24.94 +32.0 27.91 +32.5 1998 Apr. 28.93 +30.6 HD 98008

1995 Jan.

2.18 +29.3 7.21 +28.2

1989 Feb. 25.25 1990 Feb. 13.17 1992 Jan. 18.10 HD 98020 1989 Feb. 25.25 1990 Feb. 13.17

+0.5 +0.6 +0.7

+56.3 +56.2

1993 Dec. 29.12 +56.4 HD 99426

1989 Feb. 25.28 1990 Feb. 13.19 -13.0: -12.6:

1993 Dec. 29.13 -11.8: HD 99477

1989 Feb. 25.28 1990 Feb. 13.19 -20.7 -20.5 +4.9

-2.8 -3.1 -2.8

Spectroscopic Binary Orbit in Paper XVII HD 96839

1989 Feb. 25.22 1990 Feb. 13.15 1993 Feb. 14.03 HD 96873 1989 Feb. 25.23 1990 Feb. 13.15 1993 Feb. 14.04 HD 96889 1989 Feb. 25.23 1990 Feb. 13.15

+1.6 +1.6 +1.6

+6.7 +6.3 +5.7

Spectroscopic Binary Orbit in Paper XVII HD 95425

1989 Feb. 23.21 1990 Feb. 14.30 +13.7 +13.2

1993 Dec. 29.14 -19.8 HD 99551

1989 Feb. 25.28 1990 Feb. 13.19 1993 Dec. 29.14 HD 99552 1989 Feb. 25.28 1990 Feb. 13.19 1993 Dec. 29.14 HD 99584

+1.6 +1.7 +2.0

+6.7 +6.6 +7.0

+4.2 +4.5 +4.6

+39.8 +39.4

+12.6 +10.5

+23.6 +23.2

1992 Jan. 17.08 +15.2 HD 93801

1989 Feb. 23.19 1990 Feb. 14.26 +20.2 +19.7 1992 Jan. 17.07 +23.5 HD 90046

1989 Feb. 23.16 1990 Feb. 14.24 -11.6 -12.3

1992 Apr. 30.88 +14.3 1994 Dec. 11.19 +13.5 HD 95425 B*

1990 Feb. 14.30 HD 95533 1989 Feb. 23.21 1990 Feb. 14.31 1992 Apr. 30.89 HD 95714 1989 Feb. 23.22 1990 Feb. 14.31

+74.8

1992 Apr. 26.91 +20.0 HD 93996

1989 Feb. 23.19 1990 Feb. 14.26 1992 Apr. 26.91 1993 Feb. 12.05 Mar.22.96 Dec. 25.14 1994 May 3.86 Dec. 10.17 HD 93999 1989 Feb. 23.19 1990 Feb. 14.26

-6.8 -8.5 -6.5 -7.7 -8.1 -7.2 -6.9 -7.4

1992 Jan. 17.07 -11.8 HD 90167

1989 Feb. 23.16 1990 Feb. 14.24 -19.4 -18.7

1992 Jan. 17.07 -18.7 HD 90168

1989 Feb. 23.16 1990 Feb. 14.24 1992 Jan. 17.07 HD 90196 1989 Feb. 23.17 1990 Feb. 14.24 1992 Jan. 17.06 HD 90266 1989 Feb. 23.17 1990 Feb. 14.24 1992 Jan. 17.06 HD 90498 1989 Feb. 23.17 1990 Feb. 14.24

+0.4 +0.1 +0.5

1993 Feb. 12.09 +10.5 Dec. 25.18 +10.9 1994 May 3.91 +11.1 Dec. 11.19 +10.2 1995 June 4.87 +13.5 1996 Dec. 16.24 +10.6 1997 Jan. 26.14 +10.5

Apr. 27.89 HD 96908 1989 Feb. 25.23 1990 Feb. 13.15 1993 Feb. 14.04 HD 96940 1989 Feb. 25.23 1990 Feb. 13.15 1993 Feb. 14.04 HD 96959 1989 Feb. 25.23 1990 Feb. 13.16 1993 Feb. 14.04 Dec. 29.11 HD 97260 1989 Feb. 25.24 1990 Feb. 13.16

+9.6

1992 Jan. 18.09 +40.4 HD 98032*

1992 Jan. 18.09 HD 98121 1989 Feb. 25.25 1990 Feb. 13.17 1992 Jan. 18.09 HD 98122 1989 Feb. 25.26 1990 Feb. 13.17 1992 Jan. 18.09 HD 98250 1989 Feb. 25.26 1990 Feb. 13.17 1992 Jan. 18.09 HD 98251 1989 Feb. 25.26 1990 Feb. 13.17

-2.6

Spectroscopic Binary Orbit in Paper XVII HD 99637

1989 Feb. 25.28 1990 Feb. 13.19 -11.6 -11.1

+8.0 +8.2 +7.6

+16.3 +16.8

1992 Apr. 30.89 +15.7 HD 95852

1989 Feb. 23.22 1990 Feb. 14.31 1992 Apr. 30.89 HD 95871 1989 Feb. 23.22 1990 Feb. 13.14

-5.5 -6.0 -7.8 +19.6 +19.2

-6.7 -6.8 -7.1

1992 Apr. 26.91 +18.9 HD 94045

1989 Feb. 23.19 1990 Feb. 14.27 1992 Apr. 26.91 30.86 1994 Dec. 10.17

1995 Jan. HD 94126

2.19

-0.4 -0.9 -1.7 0.0 -0.2 -1.0

+0.7 +0.5 +0.5

+14.9 +14.8

1992 Dec. 19.14 +15.1 HD 95872

1989 Feb. 23.22 1990 Feb. 13.14 1992 Dec. 19.14 HD 95902 1989 Feb. 23.22 1990 Feb. 13.14 1992 Dec. 19.14 HD 95923 1989 Feb. 23.22 1990 Feb. 13.14

+1.1 +0.8 +1.1

+8.9 +9.0 +9.1

-4.9 -5.0 -4.3

+5.6 +6.0 +4.8 +6.2

-8.2 -7.8 -7.6

1993 Dec. 29.14 -11.8 HD 99691

1989 Feb. 25.28 1990 Feb. 13.19 1993 Dec. 29.14 HD 99724 1989 Feb. 25.29 1990 Feb. 13.20

+9.9 +9.9 +9.9

+1.4 +1.2 +1.6 -11.6 -11.7

-9.5 -9.3 -8.6

1993 Dec. 29.14 -11.5 HD 99755

1989 Feb. 25.29 1990 Feb. 13.20 -13.9 -14.0

+30.0 +29.3

1993 Dec. 29.15 -13.8 HD 100023

1989 Feb. 25.29 1990 Feb. 13.20 +31.2 +31.3

1992 Jan. 18.08 +29.9 HD 98492

1989 Feb. 25.26 1990 Feb. 13.18 +30.5 +30.6

1993 Dec. 29.15 +31.0 HD 100184

1989 Feb. 25.29 1990 Feb. 13.20 1993 Dec. 29.15 HD 100305 1989 Feb. 25.29 1990 Feb. 13.20

+0.4 -0.7 +1.6

+38.1 +38.0

+53.7 +53.2 1989 Feb. 23.19 1990 Feb. 14.27 +37.4 +37.4

1992 Jan. 17.07 +53.2 HD 90516

1989 Feb. 23.17 1990 Feb. 14.24 1992 Jan. 17.07 HD 90793 1989 Feb. 23.17 1990 Feb. 14.25

-1.9 -2.2 -2.1

1992 Apr. 26.92 +37.2 HD 94320

1989 Feb. 23.20 1990 Feb. 14.27 +10.3 +10.3

1992 Apr. 26.92 +10.0 HD 94428

1989 Feb. 23.20 1990 Feb. 14.27 1992 Apr. 26.92 -6.0 -6.0 -7.7

1993 Feb. 14.04 +37.9 HD 97464

1989 Feb. 25.24 1990 Feb. 13.16 1993 Feb. 14.05 HD 97480 1989 Feb. 25.24 1990 Feb. 13.16 1993 Feb. 14.04 HD 97574

-2.1 -2.2 -2.5

1992 Jan. 18.08 +30.6 HD 98507

1989 Feb. 25.26 1990 Feb. 13.18 1992 Jan. 18.08 HD 98541 1989 Feb. 25.26 1990 Feb. 13.18

+7.4 +7.5 +7.4

-4.0 -4.5 -2.5

+30.1 +30.2

+10.1 +9.9

-16.8 -17.0

+2.5 +2.5 +1.6 1992 Jan. 18.08 -16.9 HD 98738

1989 Feb. 25.27 1990 Feb. 13.18 +20.9 +21.1

1992 Jan. 18.12 +11.3 1993 Dec. 29.15 +10.8 HD 100306 Spectroscopic Binary Orbit in Paper XVII HD 100347

1989 Feb. 25.29 1990 Feb. 13.20 -14.1 -13.9 1992 Dec. 19.13 +29.5

+35.9 +35.8

1992 Jan. 17.08 +34.0 Dec. 18.16 +34.9

Spectroscopic Binary Orbit in Paper XVII 1993 Dec. 29.11 +21.5

1992 Jan. 18.11 -14.4 1993 Dec. 29.16 -13.8

*Non-Clube star  Observed at Haute-Provence

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


Photoelectric radial velocities, Paper XVI 1143

Table 3.

Star Date (UT) HD 111649 1989 Feb. 25.32 1990 Feb. 13.21 HD 111680 1989 Feb. 25.33 1990 Feb. 13.21 HD 111735 1989 Feb. 25.33 1990 Feb. 13.21 HD 111866 1987 July 18.00 1989 Feb. 25.33 1990 Feb. 13.21 HD 111964 1987 July 18.00 1989 Feb. 25.33 1990 Feb. 14.32 15.33

Radial velocities of stars in Clube Area 7.

Velocity (km s-1) Velocity (km s-1)

Star Date (UT) HD 117161

Velocity (km s-1)

+32.1 +31.6

-7.5 -7.4

-1.4 -1.5

+2.4 +2.2 +3.1

1993 Feb. 13.17 Mar.19.09 1994 Jan. 8.22 Apr. 29.96 1995 June 2.87 1996 Apr. 4.01 1997 Apr. 27.97 HD 112386 1989 Feb. 25.33 1990 Feb. 13.21 HD 112386 B* 1990 Feb. 13.21 HD 112402 1989 Feb. 25.33 1990 Feb. 13.22 HD 112434 1989 Feb. 25.33 1990 Feb. 13.22 HD 112488 1987 July 18.01 1989 Feb. 25.34 1990 Feb. 13.22 HD 112577 1987 July 18.02 1989 Feb. 25.34 1990 Feb. 13.22 14.32 HD 112656 1989 Feb. 25.34 1990 Feb. 13.22 HD 112877 1989 Feb. 25.34 1990 Feb. 13.22 HD 112877 B* 1989 Feb. 25.34 1990 Feb. 13.22 HD 112905 1989 Feb. 25.34 1990 Feb. 13.23 HD 113102 1987 July 18.02 1989 Feb. 25.35 1990 Feb. 13.23 HD 113310 1987 July 18.02 1989 Feb. 25.35 1990 Feb. 13.23 HD 113530 1989 Feb. 25.35 1990 Feb. 13.23 HD 113567 1989 Feb. 25.35 1990 Feb. 13.23 HD 113580 1989 Feb. 25.35 1990 Feb. 13.23 *Non-Clube star

+8.7 +8.0 +7.8 +7.5 +7.0 +8.3 +8.0 +8.7 +8.3 +9.3 +8.6

Star Date (UT) HD 113775 1987 July 18.02 1989 Feb. 25.35 1990 Feb. 13.23 HD 113909 1989 Feb. 25.36 1990 Feb. 13.24 HD 113926 1989 Feb. 25.36 1990 Feb. 13.24 HD 114181 1989 Feb. 25.36 1990 Feb. 13.24 HD 114384 1989 Feb. 25.36 1990 Feb. 13.24 HD 114483 1987 July 18.03 1989 Feb. 25.36 1990 Feb. 13.24 14.32

Star Date (UT) HD 119175

Velocity (km s-1)

-10.7 -11.3 -10.8 Spectroscopic Binary Orbit in Paper XVII HD 117205

1989 Feb. 25.39 1990 Feb. 13.26 HD 117321 1989 Feb. 25.39 1990 Feb. 13.26 HD 117392 1989 Feb. 25.39 1990 Feb. 13.26 HD 117393 1989 Feb. 25.39 1990 Feb. 13.26 HD 117518 1987 July 18.04 1989 Feb. 25.40 1990 Feb. 13.26 HD 117734 1989 Feb. 25.40 1990 Feb. 13.27 HD 117804 1989 Feb. 23.30 1990 Feb. 13.27 HD 117863 1989 Feb. 23.30 1990 Feb. 13.27 HD 117987 1989 Feb. 23.30 1990 Feb. 13.41 HD 118041 1987 July 18.04 1989 Feb. 23.30 1990 Feb. 13.27 HD 118116

-15.1 -15.3

Spectroscopic Binary Orbit in Paper XVII HD 119188

1989 Feb. 23.32 1990 Feb. 13.29 HD 119188 B* 1989 Feb. 23.32 1990 Feb. 13.29 HD 119294 1987 July 18.05 1989 Feb. 23.33 1990 Feb. 13.29 14.34 HD 119321 1987 July 18.05 1989 Feb. 23.33 1990 Feb. 13.29 HD 119451 No result HD 119522 1989 Feb. 23.33 1990 Feb. 13.29 HD 119591 1989 Feb. 23.34 1990 Feb. 13.30 1993 Feb. 14.17 1994 May 1.00 1995 Jan. 5.25 June 4.88 1997 Jan. 26.18 Apr. 28.02 1998 July 10.86 HD 119754 1987 July 18.05 1989 Feb. 23.34 1990 Feb. 13.30 HD 119854 1987 July 18.05 1989 Feb. 23.34 1990 Feb. 13.30 HD 120013 1989 Feb. 23.34 1990 Feb. 13.30 HD 120304 1989 Feb. 23.34 1990 Feb. 13.30 HD 120338 1989 Feb. 23.34 1990 Feb. 13.30 HD 120391 1987 July 18.06 1989 Feb. 23.34 1990 Feb. 13.30 HD 120503

+19.1 +19.1

-32.1 -32.5 -38.8 -39.1

+12.3 +13.2

-47.5 -47.4

+29.3 +28.8

-3.4:

-2.6: -1.6:

-18.5 -19.0

-12.1 -12.2 -12.6

-9.5 -9.2 -9.1 -9.5

-9.8 -9.8

+7.4 +7.4

-24.5 -24.7

+55.1 +54.5

-9.0 -9.2 -9.4

1993 Feb. 13.17 1994 Feb. 18.19 Apr. 29.96 Dec. 12.22 1995 Jan. 2.20 May 30.92 1996 Apr. 4.01 1997 Jan. 26.16 Apr. 24.97 27.98 HD 114524 1989 Feb. 25.36 1990 Feb. 13.24 HD 114893 1989 Feb. 25.36 1990 Feb. 13.24 HD 114936 1989 Feb. 25.37 1990 Feb. 13.25 HD 115203 1989 Feb. 25.37 1990 Feb. 13.25 HD 115250 1987 July 18.03 1989 Feb. 25.37 1990 Feb. 13.25 HD 115430 1989 Feb. 25.37 1990 Feb. 13.25 HD 115545 1989 Feb. 25.37 1990 Feb. 13.25 HD 116141 1989 Feb. 25.37 1990 Feb. 13.25 HD 116322 1989 Feb. 25.38 1990 Feb. 13.25 HD 116463

+0.3: +1.1: +3.0: +2.0: +2.9 +1.7 +0.4 -0.2 +0.6 +1.2 -0.1 +1.0 +0.5 +1.1

-26.9 -27.1

+16.4 +16.4

-2.1 -2.9

-21.1 -20.9

-9.4 -9.2

+47.1 +47.4

-42.3 -42.0 -42.1

-16.8 -16.4

+10.7 +10.5

-12.5 -12.4

-71.0 -72.0

+58.8 +58.1 +58.5

+77.3 +76.7

Spectroscopic Binary Orbit in Paper XVII HD 118236

1989 Feb. 23.30 1990 Feb. 13.27 HD 118282 1989 Feb. 23.31 1990 Feb. 13.27 HD 118597 1989 Feb. 23.31 1990 Feb. 13.28 HD 118853 1987 July 18.04 1989 Feb. 23.31 1990 Feb. 13.28 HD 118854 1989 Feb. 23.31 1990 Feb. 13.28 HD 118855 1989 Feb. 23.31 1990 Feb. 13.28 HD 118892 1989 Feb. 23.31 1990 Feb. 13.28 HD 119011

-25.6 -25.8

+44.6 +44.9 +45.1

-19.0 -18.6

-30.6 -30.8

-29.2 -28.9 -20.0 -20.1

+30.1 +29.1 +29.1

Spectroscopic Binary Orbit in Paper XVII HD 116482

1989 Feb. 25.38 1990 Feb. 13.25 HD 116661 1989 Feb. 25.38 1990 Feb. 13.25 HD 116858 1989 Feb. 25.38 1990 Feb. 13.26 HD 116920 1989 Feb. 25.38 1990 Feb. 13.26 

-17.9 -17.4

+0.5 +0.0

-10.4 -10.3

-6.7 -6.5

+70.6 +71.2

-25.5 -25.5

-24.6 -24.7 -25.0

-13.6 -13.8

-19.2: -21.3:

-49.4 -49.7 -49.6 -48.9

+17.1: +16.6 +16.7

-31.4 -31.0

-14.9 -13.9 -15.0 -14.8 -14.8 -14.9 -14.4 -14.7 -15.1

+25.6 +24.5 +24.4

-10.2: -10.4 -10.2

-1.3 -1.2

+14.7 +14.9

-22.4 -22.4

-20.6: -22.3 -21.7

-14.9 -14.7

Spectroscopic Binary Orbit in Paper XVII HD 120571

1989 Feb. 23.35 1990 Feb. 14.34 HD 120729 1989 Feb. 23.35 1990 Feb. 13.31 HD 120852

-31.7 -31.5

+23.8 +24.3

+29.2 +29.4

-12.2 -12.4

Spectroscopic Binary Orbit in Paper XVII HD 119087 Spectroscopic Binary Orbit in Paper XVII HD 119099

1987 July 18.05 1989 Feb. 23.32 1990 Feb. 13.29 HD 119134 1989 Feb. 23.32 1990 Feb. 13.29

-8.7 -9.6 -9.5

-29.4 -29.5

Spectroscopic Binary Orbit in Paper XVII HD 121202

1987 July 18.06 1989 Feb. 23.36 1990 Feb. 13.31 14.33 HD 121376 1987 July 18.07 1989 Feb. 23.36 1990 Feb. 13.31 14.33

-26.3 -25.9 -26.3 -26.2

Star Date (UT) HD 121379 1989 Feb. 23.36 1990 Feb. 13.31 HD 121426 1989 Feb. 23.36 1990 Feb. 13.31 HD 121552 1989 Feb. 23.36 1990 Feb. 13.41 HD 121593 1987 July 18.07 1989 Feb. 23.36 1990 Feb. 13.31 HD 121671 1987 July 18.07 1989 Feb. 23.37 1990 Feb. 14.35 HD 121687 1989 Feb. 23.37 1990 Feb. 13.32 HD 121885 1989 Feb. 23.37 1990 Feb. 13.32 HD 122011 1989 Feb. 23.37 1990 Feb. 13.32 HD 122055 1987 July 18.07 1989 Feb. 23.37 1990 Feb. 13.32 HD 122172 1987 July 18.08 1989 Feb. 23.37 1990 Feb. 13.32 HD 122207 1989 Feb. 23.38 1990 Feb. 13.32 HD 122350 1989 Feb. 23.38 1990 Feb. 13.32 HD 122509 1989 Feb. 23.38 1990 Feb. 14.35 HD 122521 1987 July 18.08 1989 Feb. 23.38 1990 Feb. 13.32 HD 122638 1987 July 18.08 1989 Feb. 23.38 1990 Feb. 13.33 HD 122734 1989 Feb. 23.38 1990 Feb. 14.35 HD 123052 1989 Feb. 23.38 1990 Feb. 13.33 HD 123108 1989 Feb. 23.39 1990 Feb. 13.33 HD 123368 1987 July 18.08 1989 Feb. 23.39 1990 Feb. 13.33 14.33

Velocity (km s-1)

+45.5 +45.4

-23.5 -23.7

-52.7 -53.4

+1.6: +0.7 +0.8

-42.5: -42.3 -43.0

-38.1 -39.2 -26.1 -26.9

-3.4 -4.0

+19.0 +18.9 +18.0

-10.1 -10.2 -10.8

+20.9 +20.9

-15.1 -15.3

-59.2 -60.2

-12.4: -12.7 -12.7

Star Date (UT) HD 123369 1987 July 18.09 1989 Feb. 23.39 1990 Feb. 13.33 14.35 HD 123414 1989 Feb. 23.39 1990 Feb. 13.33 HD 123427 1989 Feb. 23.39 1990 Feb. 13.33 HD 123525 1989 Feb. 23.39 1990 Feb. 13.34 HD 123620 1987 July 18.09 1989 Feb. 23.39 1990 Feb. 13.34 HD 123633 1987 July 18.10 1989 Feb. 23.39 1990 Feb. 13.34 HD 123648 1989 Feb. 23.40 1990 Feb. 13.34 HD 123810 1989 Feb. 23.40 1990 Feb. 13.34 HD 123812 1989 Feb. 23.40 1990 Feb. 13.34 HD 123988 1987 July 18.10 1989 Feb. 24.29 1990 Feb. 13.34 HD 124025 1987 July 18.10 1989 Feb. 24.29 1990 Feb. 13.34 14.35 HD 124038 1989 Feb. 24.29 1990 Feb. 13.35 HD 124190 1989 Feb. 24.29 1990 Feb. 13.35 HD 124536

Velocity (km s-1)

-29.0: -27.7 -28.0 -27.1

-35.6 -36.0

-11.2 -11.3 -13.7 -14.2

+4.4: +4.2 +3.2

+9.7 +10.0 +9.4

-3.0 -3.3

-0.6 -0.6

+23.5 +24.4

+42.3: +41.3 +40.9

-29.6: -30.5 -30.1 -30.1

-25.2 -25.3

-38.0 -37.4

+31.6: +32.2 +32.3

Spectroscopic Binary Orbit in Paper XVII HD 124558

1987 July 18.11 1989 Feb. 24.29 1990 Feb. 13.35 HD 124610 1987 July 18.11 1989 Feb. 24.30 1990 Feb. 13.35 HD 124685 1989 Feb. 24.30 1990 Feb. 13.35 HD 124779 1989 Feb. 24.30 1990 Feb. 13.35 HD 124871 1989 Feb. 24.30 1990 Feb. 13.41 14.35 1993 Feb. 14.18 1994 Feb. 18.20 May 1.03 1995 Jan. 5.25 May 30.94 1996 Apr. 4.05 1997 Jan. 26.19 Apr. 25.00 1998 July 10.87

-11.5 -11.5 -11.2

-58.9 -58.7

+18.7 +18.4

-14.2 -14.1

-12.6 -12.3

Observed at Haute-Provence

+59.5 +59.6

-9.9 -9.4 -9.9 -9.8

1993 Feb. 14.18 1994 Feb. 21.19 May 1.02 Dec. 13.24 1995 Jan. 7.23 May 30.93 1996 Apr. 4.04 1997 Jan. 26.18 Apr. 24.99 1998 July 10.87

+42.2: +45.5 +47.0 +47.2 +48.9 +49.6 +48.9 +48.8 +48.6 +49.1 +48.9 +49.2 +49.7 +47.0

-4.2 -4.3 -4.3

+10.3 +10.6

-0.5 -0.3

-45.2 -45.9 -44.6 -46.2 -45.3 -46.8 -46.3 -44.8 -45.3 -44.0 -45.5 -44.2

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


1144 R. F. Griffin and A. P. Cornell

Table 3  continued

Star Date (UT) HD 124918 1987 July18.11 1989 Feb.24.30 1990 Feb.13.41 HD 124958 1989 Feb.24.30 1990 Feb.13.35

Velocity (km s-1)

-64.7: -65.0 -65.4

-14.7 -14.4

Star Date (UT) HD 125132 1989 Feb.24.31 1990 Feb.13.36 HD 125168 1989 Feb.24.31 1990 Feb.13.36 HD 125169 1989 Feb.24.31 1990 Feb.13.36

Velocity (km s-1)

Star Date (UT) HD 125187

Velocity (km s-1)

-6.9 -7.0 -5.1 -5.3

Spectroscopic Binary Orbit in Paper XVII HD 125187 B*

1990 Feb.14.36 15.34 HD 125266 1989 Feb.24.31 1990 Feb.13.36

-10.1: -10.0:

+4.1 +4.2 +18.8 +18.8

Star Date (UT) HD 125266 B* 1989 Feb.24.31 1990 Feb.13.36 HD 125268 1989 Feb.24.32 1990 Feb.13.36 HD 125280 1989 Feb.24.32 1990 Feb.13.36

Velocity (km s-1)

Star Date (UT) HD 125341

Velocity (km s-1)

+18.3: +18.9:

Spectroscopic Binary Orbit in Paper XVII HD 125456

1989 Feb.24.32 1990 Feb.13.37 HD 125493 1989 Feb.24.32 1990 Feb.13.37

+4.0 +3.8

Star Date (UT) HD 125507 1989 Feb.24.32 1990 Feb.13.37

Velocity (km s-1)

-12.2 -12.3

+34.0 +33.6

-6.0 -5.9 +52.3 +52.6

*Non-Clube star

magnitudes are our own estimates. Relative positions are given in conventional double-star notation of separations () in seconds of arc and position angles in degrees, starting eastwards from the north point. We have added to Table 8 a column giving the mean velocities of the stars concerned. Those stars are not referred to again in this paper except in a few of the notes: they do not feature in any of the subsequent numerical tables or in the statistical discussions in Sections 4 and 6. In cases where companions were noted within one minute of arc of their respective primaries but were not measured, and the pairs do not already possess IDS notations, their existence is noted among the miscellaneous comments that constitute Table 11, later. Certain apparently single stars that were afterwards found from the literature to be already-known visual binaries are also noted in Table 11. We hardly need to point out that a momentary sighting on a monitor screen of a star image for the purpose of bringing it on to a spectrometer slit does not lend itself to the recognition of close double stars in the same way as a deliberate direct scrutiny of the image at the eyepiece could be expected to do.

Papers XIII and XVI are discussed together, an offset of 0.8 km s-1 should be applied with the appropriate sign to one or other set in the interest of homogeneity. The evidence suggests that the Coravel zero-point is nearer than the Cambridge one to an absolute scale, although such a scale is a somewhat nebulous concept at the sub-km s-1 level. Thus we recommend applying an offset of -0.8 km s-1 to the radial velocities in Paper XIII.

3 R A D I A L - V E L O C I T Y Z E RO - P O I N T We draw attention to the facts that the observations reported in this paper are derived from a source different from that used in Paper XIII for the ten northern Selected Areas, and that the zero-points are not expected to be the same. The velocities reported in Paper XIII were very largely made with the original Cambridge spectrometer (Griffin 1967) and were reduced to a zero-point established with that instrument (Griffin 1969) by reference to certain standard stars whose velocities had necessarily been obtained photographically. At the Coravels, standard stars were always observed at intervals of an hour or so. All the Coravel observations, including ours, are held in a data base that is maintained by the owners of the Coravels in Geneva and is not actually accessible to us, but the results are made available to us after they have been reduced by procedures determined upon at the Geneva Observatory. Those procedures have changed from time to time; in particular, after having long been suspected of producing a colour-dependent zero-point (Scarfe, Batten & Fletcher 1990; Griffin, unpublished), they were substantially revised on 2000 January 1 (Udry, Mayor & Queloz 1999). Direct comparisons between stellar radial velocities determined with the original Cambridge spectrometer (Griffin 1967) and measures of the same stars obtained with the ESO and OHP Coravels and reduced under the post-2000 procedures suggest that the colour dependence of the zero-point has largely gone, but there is a discrepancy of about 0.8 km s-1 in the sense that the Coravel zero-point is more negative by that amount. We have seen fit to publish the Coravel measurements here exactly as they were supplied to us. Therefore when the results from

4 R A D I A L - V E L O C I T Y E R RO R S This paper is fundamentally based upon radial-velocity measurements made at ESO. The ESO observations were all made with the same equipment and were of objects having nominally uniform magnitudes and spectral types. It might therefore be expected that the observational errors, too, would be consistent and would conform closely to a normal distribution with a standard deviation that would characterize by a single number everything that was worth knowing about the uncertainties of the data. All the same, we thought it prudent initially to treat the observations in each of the six Areas separately. For observations such as ours that were almost all made with a standard integration time, the brighter the star the greater will be the number of counts per bin in the trace and the more accurate the resulting velocity. Variations in observing conditions, however, can make the photon-counting rates obtained from any given star differ substantially from one occasion to another. When an observer has travelled a long way for a few nights on a telescope and has a programme of hundreds of stars to measure, he is inclined to try to observe even in conditions that otherwise might hardly be countenanced as usable observing time at all. That was particularly the case during the first observing run (1987 July) on the southern Clube stars. We could have decided to exclude those data, or to treat them separately, in the discussion of observational errors. As a matter of general principle, however, it seems best normally to take the rough with the smooth, on the basis that once one starts to exclude certain data from the statistics by recourse to special pleading it is hard to know where to stop. Moreover, if too many exclusions are made, the resulting statistics lose relevance to the data set that they are supposedly characterizing. Except for distinguishing between the ESO and OHP sources, we have accordingly elected to treat all the radial velocities as constituting a single distribution, first in each of the six Areas individually and eventually all together. A thorny problem that is inevitably encountered in an investigation such as this is where to draw the line between discrepancies arising from observational error and those caused by actual changes in the quantity being measured  in this case radial velocities. As another matter of principle we do not assert outright that any star is

2006 The Authors. Journal compilation C C 2006 RAS, MNRAS 371, 11401158


Photoelectric radial velocities, Paper XVI 1145

Table 4.

Star Date (UT) HD 26725 1987 Nov. 7.17 1989 Feb. 24.09

Radial velocities of stars in Clube Area 13.

Velocity (km s-1) Velocity (km s-1) Velocity (km s-1)

1994 Jan. 1.89 HD 26741 1987 Nov. 7.17 1989 Feb. 24.09 1994 Jan. 1.89 HD 26777 1987 Nov. 7.17 1989 Feb. 24.09 1993 Nov. 3.27 1994 Jan. 4.89 HD 26917

+22.7 +22.4 +21.7

Star Date (UT) HD 27890 1987 Nov. 8.14 1989 Feb. 24.11

+59.2 +59.5 +59.3

+92.7 +93.1 +92.4 +93.6

Spectroscopic Binary Orbit already published Griffin et al. 1995 HD 27077

1987 Nov. 7.17 1989 Feb. 24.09 1994 Jan. 4.89 HD 27116 1987 Nov. 7.17 1989 Feb. 24.10 1994 Jan. 1.90 HD 27206 1987 Nov. 7.17 1989 Feb. 24.10 1994 Jan. 4.90 HD 27229 1987 Nov. 7.18 1989 Feb. 24.10 1994 Jan. 4.90 HD 27300 1987 Nov. 7.18 1989 Feb. 24.10 1994 Jan. 4.90 HD 27412 1987 Nov. 7.18 1989 Feb. 24.10 1994 Jan. 1.90 HD 27529 1987 Nov. 8.13 1989 Feb. 24.10 1994 Jan. 1.90 HD 27538 1987 Nov. 8.14 1989 Feb. 24.10 1994 Jan. 4.90 HD 27600

-2.9 -3.2 -2.6 -0.2 -0.4 -1.0 -51.5 -51.3 -50.2

1994 Jan. 1.92 HD 27949 1987 Nov. 8.14 1989 Feb. 24.11 1994 Jan. 1.92 HD 28173 1987 Nov. 8.15 1989 Feb. 24.11 1994 Jan. 1.92 HD 28222 1987 Nov. 8.15 1989 Feb. 24.12 1994 Jan. 4.91 HD 28426

+11.2 +10.8 +11.6

Star Date (UT) HD 30118 1987 Nov. 8.32 1989 Feb. 24.14

-13.2 -14.0 -11.5

+17.8 +17.8 +19.7

+18.3 +18.4 +18.2

Spectroscopic Binary Orbit in Paper XVII HD 28559

1987 Nov. 8.15 1989 Feb. 24.12 1994 Jan. 4.91 HD 28683 1987 Nov. 8.15 1989 Feb. 24.12 1994 Jan. 4.91 HD 28753 1987 Nov. 8.15 1989 Feb. 24.12 1994 Jan. 1.93 HD 28971 1987 Nov. 8.15 1989 Feb. 24.12 1994 Jan. 4.92 HD 28997 1987 Nov. 8.16 1989 Feb. 24.12 1994 Jan. 4.92 HD 29217 1987 Nov. 8.16 1989 Feb. 24.13 1994 Jan. 1.93 HD 29229 1987 Nov. 8.16 1989 Feb. 24.13 1994 Jan. 4.92 HD 29358 1987 Nov. 8.16 1989 Feb. 24.13 1994 Jan. 4.92 Dec. 12.01 HD 29423 1987 Nov. 8.16 1989 Feb. 24.13 1994 Jan. 4.93 Dec. 12.02 HD 29791 1987 Nov. 8.16 1989 Feb. 24.13 1994 Dec. 12.02 HD 29800 1987 Nov. 8.17 1989 Feb. 24.13 1994 Dec. 12.02 HD 30010 1987 Nov. 8.17 1989 Feb. 24.14 1994 Dec. 12.02 HD 30024 1987 Nov. 8.17 1989 Feb. 24.14 1994 Jan. 1.93

+35.0 +34.5 +34.8

+68.3 +68.1 +68.4

-13.1 -13.4 -12.9

+58.3 +58.1 +59.5

+38.1 +37.8 +38.6

+92.0 +91.8 +92.6

Spectroscopic Binary Orbit in Paper XVII HD 27643

1987 Nov. 8.14 1989 Feb. 24.11 1992 Jan. 15.89 1993 Dec. 27.91 1994 Jan. 1.91 1997 Dec. 20.99 HD 27678 1987 Nov. 8.14 1989 Feb. 24.11 1994 Jan. 1.91 HD 27871

+34.0 +33.7 +33.7 +33.2 +34.4 +33.8

-10.1 -10.8 -10.4

Spectroscopic Binary Orbit in Paper XVII HD 27872

1987 Nov. 8.14 1989 Feb. 24.11 1994 Jan. 1.91 +11.0 +10.4 +11.3

+11.7 +10.9 +11.5

+43.8 +43.0 +44.0

+71.4 +70.9 +71.8

-1.1 -1.4 -0.7

+6.0 +6.0 +6.2

1994 Dec. 12.02 HD 30525 1987 Nov. 8.32 1989 Feb. 24.14 1994 Jan. 1.94 HD 30564 1987 Nov. 8.32 1989 Feb. 24.14 1994 Dec. 13.00 HD 30668 1987 Nov. 8.32 1989 Feb. 24.14 1994 Dec. 13.00 1995 Jan. 3.90 1996 Dec. 15.02 1997 Jan. 25.92 Dec. 21.01 HD 30745 1987 Nov. 8.32 1989 Feb. 24.14 1994 Dec. 13.00 HD 30785 1987 Nov. 8.32 1989 Feb. 24.14 1994 Dec. 13.00 HD 30903 1987 Nov. 8.33 1989 Feb. 24.15 1994 Dec. 13.01 HD 31259 1987 Nov. 8.33 1989 Feb. 24.15 1994 Dec. 13.01 HD 31341 1987 Nov. 8.33 1989 Feb. 24.15 1990 Feb. 14.14 1993 Feb. 11.85 Nov. 5.23 Dec. 27.91 1994 Feb. 19.80 HD 31341 B*

+1.7 +1.7 +0.6

Star Date (UT) HD 32759 1987 Nov. 9.28 1989 Feb. 24.16

Velocity (km s-1)

-7.5 -7.8 -8.5

+51.2 +50.5 +51.2

-2.2 -2.9 -7.1 -6.2 -8.6 -9.2 -9.4

+34.0 +34.5 +33.3

-4.2 -5.0 -3.5

1993 Dec. 27.95 HD 33196 1987 Nov. 9.29 1989 Feb. 23.06 1993 Dec. 27.95 HD 33757 1987 Nov. 9.29 1989 Feb. 23.06 1993 Dec. 27.95 HD 33758 1987 Nov. 9.29 1989 Feb. 23.07 1993 Dec. 27.95 1994 Jan. 4.93 Dec. 11.98 1995 Jan. 3.90 1996 Dec. 15.02 1997 Dec. 21.01 HD 33934 1987 Nov. 9.29 1989 Feb. 24.17 1993 Dec. 27.96 HD 33978

+48.6 +48.3 +49.4

Star Date (UT) HD 35371 1987 Nov. 9.31 1989 Feb. 23.09

Velocity (km s-1)

+70.6 +70.0 +71.8

+2.0 +1.5 +2.4

1994 Jan. 1.95 HD 35507 1987 Nov. 9.31 1989 Feb. 23.09 1994 Jan. 1.95 HD 35576 1987 Nov. 9.31 1989 Feb. 23.09 1994 Jan. 1.95 HD 35646

-0.8 -1.1 -0.6

Star Date (UT) HD 36544 1987 Nov. 7.20 1989 Feb. 23.12

Velocity (km s-1)

+65.0 +64.9 +65.3

1994 Jan. 1.96 Dec. 13.05 HD 36562

+64.1 +63.9 +64.6 +63.7

Spectroscopic Binary Orbit in Paper XVII HD 36632

1987 Nov. 7.20 1989 Feb. 23.12 1994 Dec. 13.05 HD 36657 1987 Nov. 7.20 1989 Feb. 23.12 1994 Dec. 13.05 HD 36730 1987 Nov. 7.20 1989 Feb. 23.12 1994 Dec. 13.05 1995 Jan. 4.94 1996 Dec. 15.04 1997 Jan. 25.94 Dec. 21.03 HD 36730 B* 1996 Dec. 15.05 1997 Dec. 21.03 HD 36744 1987 Nov. 7.20 1989 Feb. 23.12 1994 Dec. 13.05 HD 36745 1987 Nov. 7.21 1989 Feb. 23.12 1994 Dec. 13.06 HD 36924 1987 Nov. 7.21 1989 Feb. 23.13 1994 Dec. 13.06 HD 37044 1987 Nov. 7.21 1989 Feb. 23.13 1993 Feb. 11.89 Nov. 3.33 Dec. 27.93 1994 Feb. 19.84 Dec. 12.01 1995 Jan. 4.94 1996 Dec. 15.06 1997 Jan. 25.94 Dec. 21.04 23.98 25.03 HD 37064 1987 Nov. 7.21 1989 Feb. 23.13 1994 Dec. 13.06 HD 37222 1987 Nov. 7.21 1989 Feb. 23.13 1994 Dec. 13.06 HD 37494 1987 Nov. 7.21 1989 Feb. 23.14 1994 Dec. 13.06 HD 37595 1987 Nov. 7.21 1989 Feb. 23.14 1994 Dec. 13.07

+83.6 +83.2 +83.3 +18.8 +17.9 +18.9

+48.9 +47.8 +45.6 +45.9 +47.1 +47.8 +47.1 +46.3

Spectroscopic Binary Orbit in Paper XVII HD 35810

1987 Nov. 7.18 1989 Feb. 23.10 1994 Dec. 13.03 1995 Jan. 3.91 1996 Dec. 15.03 1997 Jan. 26.80 26.80 Dec. 21.02 HD 35852 1987 Nov. 7.18 1989 Feb. 23.10 1994 Dec. 13.04 1995 Jan. 3.91 1996 Dec. 15.03 1997 Jan. 25.92 26.80 Dec. 21.02 23.97 HD 35853 1987 Nov. 7.18 1989 Feb. 23.10 1994 Jan. 1.96 Dec. 13.04 HD 35871 1987 Nov. 7.18 1989 Feb. 23.10 1994 Dec. 13.04 HD 35992 1987 Nov. 7.18 1989 Feb. 23.10 1993 Dec. 27.93 1994 Dec. 13.04 HD 35993

+55.4 +55.6 +53.4 +53.9 +53.5 +52.5 +51.6 +51.8

+27.9 +27.4 +28.5

Spectroscopic Binary Orbit in Paper XVII HD 33978 B

1990 Feb. 15.11 1992 Jan. 15.91 HD 34014 1987 Nov. 9.29 1989 Feb. 23.07 1990 Feb. 14.16 1992 Jan. 14.92 1993 Feb. 11.88 Nov. 3.30 Dec. 27.92 1994 Feb. 19.83 Dec. 12.00 1995 Jan. 3.90 1996 Dec. 15.02 1997 Jan. 25.93 26.81 Dec. 21.01 HD 34166 1987 Nov. 9.30 1989 Feb. 23.08 1993 Dec. 27.96 HD 34659 1987 Nov. 9.30 1989 Feb. 23.08 1993 Dec. 27.96 HD 34659 B* 1987 Nov. 9.30 1989 Feb. 23.08 HD 34895 1987 Nov. 9.30 1989 Feb. 23.08 1994 Jan. 1.94 HD 35106 1987 Nov. 9.30 1989 Feb. 23.08 1994 Jan. 7.94 HD 35128 1987 Nov. 9.31 1989 Feb. 23.08 1994 Jan. 1.95 HD 35164 1987 Nov. 9.31 1989 Feb. 23.09 1994 Dec. 13.03

+15.5 +16.0

+0.1 -0.3 -1.0

+15.9 +16.2 +16.0

-5.7 -5.0 -4.9 -4.6 -5.5 -5.5 -5.5

+18.2 +17.2 +19.1

Spectroscopic Binary Orbit in Paper XVII HD 31406

1987 Nov. 8.33 1989 Feb. 24.15 1994 Jan. 1.94 HD 31637 1987 Nov. 8.33 1989 Feb. 24.15 1993 Dec. 27.94 HD 31638 1987 Nov. 8.33 1989 Feb. 24.16 1993 Dec. 27.94 HD 31927 1987 Nov. 8.34 1989 Feb. 24.16 1993 Dec. 27.94 HD 32121 1987 Nov. 8.34 1989 Feb. 24.16 1993 Dec. 27.94 HD 32360 1987 Nov. 9.28 1989 Feb. 24.16 1993 Dec. 27.94

+27.4 +27.4 +27.5

+8.6 +8.3 +8.6 +8.2

+14.8 +14.5 +15.8 +14.7

+8.4 +8.3 +7.9

+92.7 +92.5 +92.7

-4.5 -4.8 -5.0

+34.0 +34.2 +34.3

-4.1 -4.3 -4.1

+93.1 +93.1 +93.1

+47.6 +46.6 +47.7

-3.7 -3.6 -2.8

+41.2 +46.2 +43.5 +40.5 +39.5 +39.3 +38.9 +39.9 +37.7 +37.8 +36.9 +37.6 +35.9 +36.7

+33.9 +33.3 +33.2

+20.7 +20.5 +30.0 +28.1 +26.6 +34.1 +35.1 +20.9 +19.4

-7.7 -8.6 -8.2 -8.3

+31.2 +31.3 +30.8

+54.4 +54.0 +53.9 +54.5

-3.2 -3.5 -2.2

Spectroscopic Binary Orbit in Paper XVII HD 36004

1987 Nov. 7.19 1989 Feb. 23.11 1994 Jan. 1.96 HD 36140 1987 Nov. 7.19 1989 Feb. 23.11 1994 Jan. 1.96 Feb. 19.86 Dec. 13.04 HD 36186

+30.2 +29.8 +30.0

-3.9 -4.0

+53.8 +53.5 +53.2

+5.0 +5.1 +5.9 +4.5 +4.7

+19.6 +20.0 +20.2 Spectroscopic Binary Orbit in Paper XVII HD 36344

1987 Nov. 7.19 1989 Feb. 23.11 1994 Dec. 13.04 HD 36489 1987 Nov. 7.19 1989 Feb. 23.11 1994 Dec. 13.04 1997 Jan. 25.93 Dec. 21.03

+35.7 +35.7 +35.8

-27.2 -26.9 -26.4

+65.4 +64.9 +64.2

+34.3 +33.8 +34.4

+35.4 +35.4 +34.6

+25.4 +25.3 +20.2 +20.6 +21.7 +23.5 +23.5

+70.5 +71.6

+27.1 +27.2 +26.6

+25.9 +26.1 +26.9

+28.6 +28.2 +27.7

+5.1 +3.5 +5.6 +9.9 +8.3 +8.5 +10.5 +10.5 +16.8 +17.6 +19.1 +20.0 +18.9

+29.1 +29.2 +29.1

+74.7 +74.5 +74.1

+27.6 +27.7 +27.5

+12.5 +12.4 +12.9

+24.5 +24.6 +22.7 +24.2 +25.4

*Non-Clube star



Observed at Haute-Provence

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


1146 Table 5. R. F. Griffin and A. P. Cornell Radial velocities of stars in Clube Area 14.

Star Date (UT) HD 21188 1987 Nov. 8.22 1990 Feb. 13.04 1993 Nov. 6.27 HD 21189 1987 Nov. 8.22 1990 Feb. 13.04 1993 Nov. 6.27 HD 21255 1987 Nov. 8.22 1990 Feb. 13.04 1993 Nov. 6.27 HD 21516 1987 Nov. 8.22 1990 Feb. 13.04 1993 Nov. 6.27 HD 21721 1987 Nov. 8.23 1990 Feb. 13.04 1993 Nov. 6.27 HD 21827 1987 Nov. 8.23 1990 Feb. 13.04 1993 Nov. 6.27 HD 21989 1987 Nov. 8.23 1990 Feb. 13.05 1993 Nov. 4.27 HD 22436 1987 Nov. 8.23 1990 Feb. 13.05 1993 Nov. 6.28 HD 23072 1987 Nov. 8.23 1990 Feb. 13.05 1993 Nov. 6.28 HD 23266 1987 Nov. 8.23 1990 Feb. 13.05 1993 Nov. 6.28 HD 23332 1987 Nov. 8.24 1990 Feb. 13.05 1993 Nov. 5.23 HD 23497 1987 Nov. 8.24 1990 Feb. 13.05 1993 Nov. 5.24 HD 24363 1987 Nov. 8.24 1990 Feb. 13.05 1993 Nov. 5.24 HD 24618 1987 Nov. 8.24 1990 Feb. 13.06 1993 Nov. 5.24 HD 24930 1987 Nov. 8.24 1990 Feb. 13.06 1993 Nov. 5.24 HD 24956 1987 Nov. 8.24 1990 Feb. 13.06 1993 Nov. 5.24 HD 25018 1987 Nov. 8.24 1990 Feb. 13.06 1993 Nov. 5.24 HD 25119 1987 Nov. 8.25 1990 Feb. 13.06 1993 Nov. 5.25 HD 25405 1987 Nov. 8.25 1990 Feb. 13.06 1993 Nov. 5.25

Velocity (km s-1)

+12.4 +12.5 +12.8

+12.3 +12.2 +12.4

+32.4 +32.6 +32.6

+23.0 +23.8 +23.2

+13.8 +13.4 +13.5

+38.0 +37.3 +37.9

+13.3 +11.6 +9.1

+40.5 +40.0 +39.9

+12.1 +11.7 +11.8

+9.1 +8.7 +8.5

-1.8 -2.0 -1.3

+51.4 +51.7 +51.3

-14.6 -14.6 -14.0 -28.4 -28.6 -28.5

+13.2 +11.9 +11.7

+12.5 +12.4 +12.0

+21.4 +21.2 +21.2

+6.7 +6.6 +6.4

+4.3 +4.5 +4.9

Star Date (UT) HD 25831 1987 Nov. 8.25 1990 Feb. 13.06 1993 Nov. 5.25 HD 25875 1987 Nov. 8.25 1990 Feb. 13.07 1993 Nov. 5.25 HD 26046 1987 Nov. 8.25 1990 Feb. 13.07 1993 Nov. 5.25 HD 26098 1987 Nov. 8.25 1990 Feb. 13.07 1993 Nov. 5.25 6.28 HD 26191 1987 Nov. 8.25 1990 Feb. 13.07 1993 Nov. 5.25 6.28 HD 26247 1987 Nov. 8.25 1990 Feb. 13.07 1993 Nov. 4.27 HD 26318 1987 Nov. 8.26 1990 Feb. 13.07 1993 Nov. 6.28 HD 26523 1987 Nov. 8.26 1990 Feb. 13.07 1993 Nov. 6.29 HD 26530 1987 Nov. 8.26 1990 Feb. 13.07 1993 Nov. 6.29 HD 26615 1987 Nov. 8.26 1990 Feb. 13.07 1993 Nov. 6.29 HD 26788 1987 Nov. 8.26 1990 Feb. 13.08 1993 Nov. 6.29 HD 26834 1987 Nov. 8.26 1990 Feb. 13.08 1993 Nov. 6.29 HD 26891 1987 Nov. 8.26 1990 Feb. 13.08 1993 Nov. 6.29 HD 27010 1987 Nov. 8.27 1990 Feb. 13.08 1993 Nov. 6.29 HD 27011 1987 Nov. 8.27 1990 Feb. 13.08 1993 Nov. 6.29 HD 27068 1987 Nov. 8.27 1990 Feb. 13.08 1993 Nov. 6.30 HD 27099 1987 Nov. 8.27 1990 Feb. 13.08 1993 Nov. 5.25 HD 27201 1987 Nov. 8.27 1990 Feb. 13.09 1993 Nov. 5.25 HD 27319 1987 Nov. 8.28 1990 Feb. 13.09 1993 Nov. 5.26

Velocity (km s-1)

-33.0 -32.3 -32.9

+11.7 +12.1 +11.3

+4.3 +4.8 +4.5

+33.5 +33.0 +37.9 +37.9

+20.1 +20.3 +22.1 +21.8

+50.8 +45.3 +48.4

+32.8 +33.4 +33.1

+7.2 +7.9 +7.0

+23.1 +23.8 +23.1

+22.9 +22.7 +22.6

-12.6 -12.4 -12.1

+11.8 +11.8 +11.5

+9.0 +8.8 +9.2

+12.3 +12.0 +12.1

-0.1 -0.3 +0.3

+30.3 +30.8 +30.9

+34.5 +34.6 +34.6

-0.2 -0.2 +0.0

+41.9 +42.2 +42.5

Star Date (UT) HD 27555 1987 Nov. 8.28 1990 Feb. 13.09 1993 Nov. 4.28 HD 27853 1987 Nov. 8.28 1990 Feb. 13.09 1993 Nov. 5.26 6.30 HD 28002 1987 Nov. 8.28 1990 Feb. 13.09 1993 Nov. 5.26 HD 28330 1987 Nov. 8.28 1990 Feb. 13.09 1993 Nov. 5.26 HD 28340 1987 Nov. 8.28 1990 Feb. 13.09 1993 Nov. 5.26 HD 29016 1987 Nov. 8.28 1990 Feb. 13.10 1993 Nov. 5.26 HD 29067 1987 Nov. 8.28 1990 Feb. 13.10 1993 Nov. 5.27 HD 29168 1987 Nov. 8.29 1990 Feb. 13.10 1993 Nov. 4.28 HD 29657 1987 Nov. 8.29 1990 Feb. 13.10 1993 Nov. 4.29 HD 29825 1987 Nov. 8.29 1990 Feb. 13.10 1993 Nov. 4.29 HD 29845 1987 Nov. 8.29 1990 Feb. 13.10 1993 Nov. 4.30 HD 30253 1987 Nov. 8.29 1990 Feb. 13.10 1993 Nov. 5.27 HD 30253 B* 1990 Feb. 13.11 1993 Nov. 5.27 HD 31029 1987 Nov. 8.29 1990 Feb. 13.11 1993 Nov. 5.27 HD 31462 1987 Nov. 8.29 1990 Feb. 13.11 1993 Nov. 5.27 HD 31484 1987 Nov. 8.29 1990 Feb. 13.11 1993 Nov. 5.27 HD 31645 1987 Nov. 8.30 1990 Feb. 13.11 1993 Nov. 5.28 6.30 HD 31804 1987 Nov. 8.30 1990 Feb. 13.11 1993 Nov. 5.28 HD 32107 1987 Nov. 8.30 1990 Feb. 13.11 1993 Nov. 5.28

Velocity (km s-1)

+11.3 +15.1 +14.3

+54.6 +55.5 +53.8 +54.8

+42.2 +42.8 +42.5

-17.8 -17.9 -17.9

+83.6 +83.8 +83.6

+22.0 +21.9 +22.0

-1.2 -1.1 -1.6

+19.5 +19.9 +19.7

+36.6 +36.6 +36.7

-10.9 -10.9 -11.1

+6.7 +7.6 +7.6

+19.7 +20.6 +19.8

+72.8 +72.4

+47.4 +47.1 +47.0

+22.3 +22.2 +23.1

+35.8 +35.4 +35.6

+10.7 +10.2 +21.9 +21.6

+4.6 +5.2 +5.1

+36.7 +37.0 +37.0

Star Date (UT) HD 32140 1987 Nov. 8.30 1990 Feb. 13.12 1993 Nov. 4.28 HD 32244 1987 Nov. 8.30 1990 Feb. 13.12 1993 Nov. 5.28 HD 32823 1987 Nov. 8.30 1990 Feb. 13.12 1993 Nov. 5.28 HD 33380 1987 Nov. 8.30 1990 Feb. 13.12 1993 Nov. 5.28 HD 33456 1987 Nov. 8.31 1989 Feb. 25.07 1993 Nov. 5.28 HD 33516 1987 Nov. 7.29 1989 Feb. 25.07 1993 Nov. 5.29 HD 33700 1987 Nov. 7.29 1989 Feb. 25.07 1993 Nov. 4.30 6.30 HD 33895 1987 Nov. 7.29 1989 Feb. 25.07 1993 Nov. 5.29 HD 33954 1987 Nov. 7.29 1989 Feb. 25.07 1993 Nov. 5.29 HD 34230 1987 Nov. 7.30 1989 Feb. 25.07 1993 Nov. 5.29 HD 34396 1987 Nov. 7.30 1989 Feb. 25.07 1993 Nov. 5.29 6.30 HD 34821 1987 Nov. 7.30 1989 Feb. 25.07 1993 Nov. 5.29 HD 34830 1987 Nov. 7.30 1989 Feb. 25.08 1993 Nov. 5.29 HD 34915 1987 Nov. 7.30 1989 Feb. 25.08 1993 Nov. 5.29 HD 35167 1987 Nov. 7.30 1989 Feb. 25.08 1993 Nov. 4.31 5.30 HD 35445 1987 Nov. 7.31 1989 Feb. 25.08 1993 Nov. 5.30 HD 35529 1987 Nov. 7.31 1989 Feb. 25.08 1993 Nov. 4.32 5.30 HD 35740 1987 Nov. 7.31 1989 Feb. 25.08 1993 Nov. 5.30

Velocity (km s-1)

+48.5 +46.0 +39.0

-8.5 -8.3 -8.4

+3.0 +3.6 +3.8

+25.7 +26.2 +26.5

+16.9 +17.2 +17.1

+33.0 +33.0 +33.0

-43.5 -45.5 -29.2 -30.3

+16.2 +16.3 +16.4

+63.0 +62.4 +63.0

+39.5 +40.3 +40.1

+64.9 +65.3 +64.0 +64.6

+39.8 +40.9 +40.5

+15.0 +14.6 +15.0

+12.2 +12.7 +12.0

-25.0 -4.4 -17.2: -17.4

+27.8 +28.2: +27.8

+24.9 +19.1 +23.6 +24.0

+14.5 +14.3 +13.9

Star Date (UT) HD 37336 1987 Nov. 7.31 1989 Feb. 25.09 1993 Nov. 5.30 HD 37721 1987 Nov. 7.31 1989 Feb. 25.09 1993 Nov. 5.30 HD 37730 1987 Nov. 7.31 1989 Feb. 25.09 1993 Nov. 5.30 HD 37730 B* 1987 Nov. 7.32 1989 Feb. 25.09 1993 Nov. 5.31 6.31 HD 38112 1987 Nov. 7.32 1989 Feb. 25.09 1993 Nov. 5.31 HD 39446 1987 Nov. 7.32 1989 Feb. 25.10 1993 Nov. 5.31 HD 39609 1987 Nov. 7.32 1989 Feb. 25.10 1993 Nov. 5.31 HD 40293 1987 Nov. 7.32 1989 Feb. 25.10 1993 Nov. 5.31 HD 40342 1987 Nov. 7.32 1989 Feb. 25.10 1993 Nov. 5.32 HD 40484 1987 Nov. 7.32 1989 Feb. 25.10 1993 Nov. 5.32 6.31 HD 40560 1987 Nov. 7.33 1989 Feb. 25.10 1993 Nov. 5.32 6.31 HD 40768 1987 Nov. 7.33 1989 Feb. 25.10 1993 Nov. 5.32 HD 41023 1987 Nov. 7.33 1989 Feb. 25.11 1993 Nov. 5.32 HD 41094 1987 Nov. 7.33 1989 Feb. 25.11 1993 Nov. 5.32 6.31 HD 41540 1987 Nov. 7.33 1989 Feb. 25.11 1993 Nov. 5.32 HD 42010 1987 Nov. 7.33 1989 Feb. 25.11 1993 Nov. 5.32 HD 42027 1987 Nov. 7.33 1989 Feb. 25.11 1993 Nov. 5.32 HD 42193 1987 Nov. 7.34 1989 Feb. 25.11 1990 Feb. 15.17

Velocity (km s-1)

+90.4 +90.2 +89.9

+4.7 +5.2 +4.2

+18.2 +18.3 +18.3

-18.1: +6.5: +56.4: +64.3:

+16.9 +16.8 +16.8

+9.0 +9.0 +8.7

-4.8 -3.9 -5.3

+36.7 +36.8 +36.3

+94.3 +94.7 +94.2

-32.8 -32.3 -32.6 -32.7

+22.7 +22.7 +21.7 +22.2

-0.3 -0.2 +0.1

+9.9 +9.8 +9.5

+75.0 +75.1 +74.1 +74.7

+64.0 +65.2 +63.8

-23.4 -23.0 -23.3

+49.4 +49.6 +49.3

+31.4 +31.3 +31.2

*Non-Clube star

Star Date (UT) HD 42228 1987 Nov. 7.34 1989 Feb. 25.11 1990 Feb. 15.18 HD 42307* 1989 Feb. 25.12 1990 Feb. 15.18 HD 42328 1987 Nov. 7.34 1989 Feb. 25.12 1990 Feb. 15.18 1993 Nov. 5.33 HD 42451 1987 Nov. 7.34 1989 Feb. 25.12 1990 Feb. 15.18 HD 42505 1987 Nov. 7.34 1989 Feb. 25.12 1990 Feb. 15.18 HD 43182 1987 Nov. 7.34 1989 Feb. 25.12 1990 Feb. 15.18 HD 43493 1987 Nov. 7.35 1989 Feb. 25.12 1990 Feb. 15.18 HD 43792 1987 Nov. 7.35 1989 Feb. 25.12 1990 Feb. 15.18 HD 43977 1987 Nov. 7.35 1989 Feb. 25.13 1990 Feb. 15.18 1993 Nov. 5.33 HD 44013 1987 Nov. 7.35 1989 Feb. 25.13 1990 Feb. 15.19 HD 44121 1987 Nov. 7.35 1989 Feb. 25.13 1990 Feb. 15.19 HD 44325 1987 Nov. 7.35 1989 Feb. 25.13 1990 Feb. 15.19 HD 44384 1987 Nov. 7.35 1989 Feb. 25.13 1990 Feb. 15.19 HD 44627 1987 Nov. 7.36 1989 Feb. 25.14 1990 Feb. 15.19 1993 Nov. 5.33 HD 44777 1987 Nov. 7.36 1989 Feb. 25.14 1990 Feb. 15.19 HD 44790 1987 Nov. 7.36 1989 Feb. 25.14 1990 Feb. 15.19 HD 44879 1987 Nov. 7.36 1989 Feb. 25.14 1990 Feb. 15.19 HD 45037 1987 Nov. 7.36 1989 Feb. 25.14 1990 Feb. 15.20 HD 45186 1987 Nov. 7.36 1989 Feb. 25.14 1990 Feb. 15.20

Velocity (km s-1)

+16.3 +16.7 +16.6

+24.3 +24.3

+35.8 +34.5 +32.9 +28.4

+9.1 +9.0 +9.4

+23.9 +24.0 +23.7

+14.1 +13.2 +13.4

-0.8 -0.4 -0.5

+48.0 +48.9 +47.8

+42.7 +37.6 +37.4 +43.4

-0.1 0.0 -0.2

+18.9 +18.4 +18.8

+87.6 +87.6 +87.7

+25.5 +25.3 +25.9

+22.9 +22.6 +22.7 +21.9

+7.4 +6.7 +6.9

+8.9 +8.7 +8.5

+1.5 +1.6 +1.0

+14.0 +13.9 +13.6

+37.9 +38.1 +38.0

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


Photoelectric radial velocities, Paper XVI 1147

Table 5  continued

Star Date (UT) HD 46506 1987 Nov. 7.36 1989 Feb. 25.14 1990 Feb. 15.20 HD 47027 1987 Nov. 7.36 1989 Feb. 25.15 1990 Feb. 15.20 HD 47027 B* 1989 Feb. 25.15 1990 Feb. 15.20 HD 47028 1987 Nov. 7.37 1989 Feb. 25.15 1990 Feb. 15.21 HD 47191 1987 Nov. 7.37 1989 Feb. 25.15 1990 Feb. 15.21 HD 47234 1987 Nov. 7.37 1989 Feb. 25.16 1990 Feb. 15.21 HD 47235 1987 Nov. 7.37 1989 Feb. 25.16 1990 Feb. 15.21 *Non-Clube star

Velocity (km s-1)

+15.0 +15.4 +15.0

+15.6 +15.7 +15.4

+35.3: +33.9:

+13.3 +13.3 +13.2

+19.2 +18.8 +19.0

-18.7 -18.7 -18.5

+14.1 +14.3 +14.2

Star Date (UT) HD 47476 1987 Nov. 7.37 1989 Feb. 25.16 1990 Feb. 15.21 HD 47519 1987 Nov. 8.34 1989 Feb. 25.16 1990 Feb. 15.21 HD 47951 1987 Nov. 8.34 1989 Feb. 25.16 1990 Feb. 15.21 HD 48359 1987 Nov. 8.34 1989 Feb. 25.16 1990 Feb. 15.21 HD 48732 1987 Nov. 8.34 1989 Feb. 25.16 1990 Feb. 15.21 HD 48928 1987 Nov. 8.34 1989 Feb. 25.17 1993 Nov. 6.35 HD 49033 1987 Nov. 8.35 1989 Feb. 25.17 1993 Nov. 6.35

Velocity (km s-1)

+3.0 +3.0 +2.8

+23.6: +24.3: +23.0:

+98.0 +97.7 +97.5

+4.0 +3.9 +3.4

+14.1 +13.9 +13.8

-1.8 -1.3 -1.1

-12.6 -12.5 -12.4

Star Date (UT) HD 49171 1987 Nov. 8.35 1989 Feb. 25.17 1993 Nov. 6.35 HD 49265 1987 Nov. 8.35 1989 Feb. 25.17 1993 Nov. 6.35 HD 49266 1987 Nov. 8.35 1989 Feb. 25.17 1993 Nov. 6.35 HD 49670 1987 Nov. 8.35 1989 Feb. 25.17 1993 Nov. 6.36 HD 50159 1987 Nov. 8.35 1989 Feb. 25.17 1993 Nov. 6.36 HD 50504 1987 Nov. 8.35 1989 Feb. 25.18 1993 Nov. 6.36 HD 51556 1987 Nov. 8.36 1989 Feb. 25.18 1993 Nov. 6.36

Velocity (km s-1)

+3.3 +3.0 +3.1

+6.2 +6.1 +6.5

+28.8 +28.9 +28.9

+45.6 +45.2 +44.4

+9.0 +9.3 +9.9

+24.4 +24.4 +24.5

+11.4 +11.1 +11.6

Star Date (UT) HD 51863 1987 Nov. 8.36 1989 Feb. 25.18 1993 Nov. 6.36 HD 51950 1987 Nov. 8.36 1989 Feb. 25.18 1993 Nov. 6.36 HD 52119 1987 Nov. 8.36 1989 Feb. 25.18 1993 Nov. 6.36 HD 52251 1987 Nov. 6.39 1989 Feb. 25.18 1993 Nov. 6.36 HD 53103 1987 Nov. 6.38 1989 Feb. 25.18 1993 Nov. 6.37 HD 53167 1987 Nov. 6.38 1989 Feb. 25.19 1993 Nov. 6.37 HD 53707 1987 Nov. 6.36 1989 Feb. 25.19 1993 Nov. 6.37

Velocity (km s-1)

+34.2 +34.4 +34.2

+34.5 +34.9 +34.6

+8.7 +8.9 +8.7

+23.9 +24.1 +23.9

+39.4 +39.8 +39.9

+9.1 +9.3 +9.3

+9.3 +8.9 +9.2

Star Date (UT) HD 53787 1987 Nov. 6.36 1989 Feb. 25.19 1993 Nov. 6.37 HD 53841 1987 Nov. 6.36 1989 Feb. 25.19 1993 Nov. 6.37 HD 54506 1987 Nov. 6.36 1989 Feb. 25.19 1993 Nov. 6.37 HD 55048 1987 Nov. 6.36 1989 Feb. 25.19 1993 Nov. 6.38 HD 55432 1987 Nov. 6.36 1989 Feb. 25.19 1993 Nov. 6.38 HD 55546 1987 Nov. 6.38 1989 Feb. 25.19 1993 Nov. 6.38 HD 55644 1987 Nov. 6.37 1989 Feb. 25.20 1993 Nov. 6.38

Velocity (km s-1)

+36.5 +36.3 +36.8

+47.3 +47.1 +44.2

-20.3 -24.5 -23.9

+5.1 +4.7 +4.6

+0.3 +0.1 -0.1

+13.6 +13.7 +13.3

+29.5 +29.0 +29.4

Star Date (UT) HD 56319 1987 Nov. 6.37 1989 Feb. 25.20 HD 56440 1987 Nov. 6.38 1989 Feb. 25.20 HD 56706 1987 Nov. 6.37 1989 Feb. 25.20 HD 56706 B* 1989 Feb. 25.20 HD 56838 1987 Nov. 6.37 1989 Feb. 25.21 HD 57041 1987 Nov. 6.37 1989 Feb. 25.21 1993 Nov. 6.38 HD 57097 1987 Nov. 6.37 1989 Feb. 25.21 HD 57622 1987 Nov. 6.38 1989 Feb. 25.21 HD 57696 1987 Nov. 6.38 1989 Feb. 25.21

Velocity (km s-1)

-23.2 -23.4

+3.8 +4.2

+13.7 +13.8

+54.6:

+38.3 +37.9

+6.2 +8.6 +10.4

+22.1 +21.8

+62.0 +63.3

+81.6 +81.6

a spectroscopic binary (hereinafter SB) unless we obtained either (a) at least three velocities that are all mutually discrepant beyond the plausible bounds of observational error, or (b) two definitely discrepant velocities that are each attested by observations made on more than one night. In that way premature assertions of variability are avoided in cases where apparent discrepancies might be due to qualitative errors such as, notably, misidentification of the object on a particular occasion. Owing to the paucity of observations of any given star on the Clube programme, especially in the three farsouthern Areas for which re-observation from OHP was impossible, there are many objects for which we have obtained discordant velocities but without the proof that we require in order to claim them positively as SBs. Those that exhibit major discordances that could be due only to real variation or to out-and-out mistakes of some sort are regarded as `probable SBs'; those where the discordances might be marginally within observational error are `possible SBs'.

4.1 Errors of the ESO observations To assess the errors of the ESO observations, which number two for a large proportion of the stars on this programme, we have ignored any further measurements of any star and considered only the discrepancy between the first two observations of each one. Stars that are certainly SBs and are so identified in this paper were omitted from the outset. The distribution of the discrepancies showed in each Area a tight core and inevitably a number of outliers. Discrepancies as large as 2 km s-1 clearly belonged to the population of outliers. Unsupported discrepancies as large as that were deemed to merit the assignment of `probable SB' status to the stars concerned. We inspected individually the circumstances of the small number of discrepancies between 1.5 and 2.0 km s-1. In most cases they had to be regarded as true outliers and the rel-

evant stars to be `probable SBs', but in a few cases, particularly where the initial observation had been made in very bad conditions in the first observing run, we were content to regard them as conceivably arising from observational error and the stars as `possible SBs'. For the purposes of error assessment we adopted a uniform cut-off of 1.5 km s-1 for all six Areas. The rms values for each individual Area are given in Table 9. The values are seen to range from 0.39 to 0.55 km s-1, indicating retrospectively that the adopted cut-off ranged between 3.8 and 2.7 times the `sigma' of the distribution. The proportion of a normal distribution that is outside 2.7 is about 0.7 per cent, so we are reassured that even in the two `worst' Areas only about half a star in each might be expected to be rejected from the distribution when really it ought to be included; in the other Areas the incidence of improper exclusions would be altogether negligible. It must be emphasized that the numbers in Table 9 are not the rms errors of individual observations but are the rms differences between pairs of observations: the uncertainties of individual observa0.39 km s-1. Expressed as variances (mean-square uncertainties) they run from 0.075 to 0.15 (km s-1)2, ranging over a factor of almost exactly 2. Recourse to tables of the variance ratio, F, e.g. Lindley & Miller (1953), shows that such a large difference between variances established from populations of the order of 60 or more (as here) is significant at the 1-per-cent level. It is not obvious to us what is responsible for any such difference between Areas. We should point out, however, that in looking at the extreme range between six quantities we have implicitly tried 6C2 = 6!/2!4! = 15 pairs of comparisons, thereby multiplying the probability of obtaining an unusually large ratio by a factor of 15, so the significance is not so great after all.

tions are smaller by

 2. They accordingly range between 0.28 and

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


1148 R. F. Griffin and A. P. Cornell

Table 6.

Star Date (UT) HD 191 1987 Nov. 6.23 1993 Nov. 6.17 HD 526 1987 Nov. 6.23 1993 Nov. 6.17 HD 3096 1987 Nov. 6.23 1993 Nov. 6.17 HD 3182 1987 Nov. 6.24 1993 Nov. 6.18 HD 3615 1987 Nov. 6.24 1993 Nov. 6.18 HD 4547 1987 Nov. 6.24 1993 Nov. 6.18 HD 5004 1987 Nov. 6.24 1993 Nov. 6.18 HD 5193 1987 Nov. 6.24 1993 Nov. 6.18 HD 5489 1987 Nov. 6.24 1993 Nov. 6.18 HD 6674 1987 Nov. 6.25 1993 Nov. 6.18 HD 6940 1987 Nov. 6.25 1993 Nov. 6.18 HD 7262 1987 Nov. 6.25 1993 Nov. 6.19 HD 7403 1987 Nov. 6.25 1993 Nov. 6.19 HD 160484 1987 July 20.26 1993 Nov. 6.01 HD 170325 1987 July 20.26 1993 Nov. 6.02

Radial velocities of stars in Clube Area 15.

Velocity (km s-1) Velocity (km s-1) Velocity (km s-1)

-19.3 -19.3

+16.9 +16.8

+2.4 +1.9

+47.2 +47.2

-21.8 -15.5

+43.3 +43.3

+11.8 +12.4

+22.5 +22.6

+9.2 +8.8

+54.3 +62.9

+24.1 +23.4

+11.2 +11.8

+0.4 +0.7

-13.2 -13.8

Star Date (UT) HD 170692 1987 July 20.27 1993 Nov. 6.02 HD 172497 1987 July 20.27 1993 Nov. 6.02 HD 173414 1987 July 20.27 1993 Nov. 6.02 HD 174101 1987 July 20.27 1993 Nov. 6.02 HD 174826 1987 July 20.27 1993 Nov. 6.02 HD 174929 1987 July 20.28 1993 Nov. 6.03 HD 176772 1987 July 20.28 Nov. 9.06 1993 Nov. 6.03 HD 178736 1987 July 20.28 1993 Nov. 6.03 HD 181140 1987 July 20.28 1993 Nov. 6.03 HD 182073 1987 Nov. 9.07 1993 Nov. 6.04 HD 182073 B* 1987 July 20.29 Nov. 9.07 1993 Nov. 6.03 HD 182235 1987 July 20.29 1993 Nov. 6.07 HD 182439 1987 July 20.29 1993 Nov. 6.07 HD 186425 No result

+7.9 +7.0

-13.7 -13.0

-39.4 -46.9

-0.2 -0.7

-18.0 -18.9

+65.1 +63.7

+87.5: +87.0: +86.0:

+20.0 +19.1

+10.1 +9.4

-42.9: -48.4:

+23.7: +22.9 +23.2

+67.8 +67.1

+1.4 +1.5

Star Date (UT) HD 188925 1987 July 20.29 1993 Nov. 6.07 HD 192552 1987 July 20.30 1993 Nov. 6.08 HD 192695 1987 July 20.30 1993 Nov. 6.08 HD 192906 1987 July 20.30 1993 Nov. 6.08 HD 195477 1987 July 20.30 1993 Nov. 6.08 HD 197767 1987 July 20.30 1993 Nov. 6.08 HD 198944 1987 July 20.31 1993 Nov. 6.08 HD 200815 1987 July 20.31 1993 Nov. 6.08 HD 202460 1987 July 20.31 1993 Nov. 6.09 HD 203589 1987 July 20.31 1993 Nov. 6.09 HD 205037 1987 July 20.31 1993 Nov. 6.09 HD 205834 1987 July 20.31 HD 206693 1987 July 20.32 1993 Nov. 6.09 HD 206693 B* 1993 Nov. 6.09 HD 206951 1987 July 20.32 1993 Nov. 6.10

+54.3: +54.6

+91.2: +91.0:

+8.7 +7.9

-18.2 -19.0

+23.1 +23.4

+5.0 +4.5

0.0 -0.8

+38.5 +38.8

-6.3 -7.0 -0.5: -1.2

+15.5 +15.4

-47.8

+10.4 +10.7

+12.0:

-11.8 -12.5

-15.2 -15.0

Star Date (UT) HD 207046 1987 July 20.32 1993 Nov. 6.10 HD 207307 1987 July 20.32 1993 Nov. 6.10 HD 207444 1987 July 20.32 1993 Nov. 6.10 HD 207527 1987 July 20.32 1993 Nov. 6.10 HD 208929 1987 July 20.33 1993 Nov. 6.10 HD 209003 1987 July 20.33 1993 Nov. 6.11 HD 209620 1987 July 20.33 1993 Nov. 6.11 HD 210009 1987 Nov. 6.17 1993 Nov. 6.11 HD 210057 1987 Nov. 6.17 1993 Nov. 6.11 HD 210164 1987 Nov. 6.17 1993 Nov. 6.11 HD 210332 1987 Nov. 6.17 1993 Nov. 6.11 HD 210603 1987 Nov. 6.18 1993 Nov. 6.11 HD 210713 1987 Nov. 6.18 1993 Nov. 6.12 HD 212264 1987 Nov. 6.18 1993 Nov. 6.12 HD 212555 1987 Nov. 6.18 1993 Nov. 6.12

Velocity (km s-1)

-8.2 -8.7

+1.7 +2.0

-4.8 -4.2

+16.2 +16.1

+33.6 +35.9

-14.4 -14.9

+25.3 +25.1

-16.3: -12.9

-26.4 -26.3

+15.0 +15.3

+10.5 +10.2

+15.4 +14.6

+55.2 +55.3

-31.3 -33.1

-42.8 -43.1

Star Date (UT) HD 212663 1987 Nov. 6.18 1993 Nov. 6.12 HD 213158 1987 Nov. 6.19 1993 Nov. 6.12 HD 213289 1987 Nov. 6.19 1993 Nov. 6.12 HD 213289 B* 1993 Nov. 6.13 HD 213743 1987 Nov. 6.19 1993 Nov. 6.13 HD 214309 1987 Nov. 6.19 1993 Nov. 6.13 HD 214792 1987 Nov. 6.19 1993 Nov. 6.13 HD 215370 1987 Nov. 6.19 1993 Nov. 6.13 HD 215587 1987 Nov. 6.20 1993 Nov. 6.13 HD 215832 1987 Nov. 6.20 1993 Nov. 6.14 HD 215987 1987 Nov. 6.20 1993 Nov. 6.14 HD 217978 1987 Nov. 6.20 1993 Nov. 6.14 HD 218077 1987 Nov. 6.20 1993 Nov. 6.14 HD 218109 1987 Nov. 6.20 1993 Nov. 6.14 HD 218842 1987 Nov. 6.21 1993 Nov. 6.15

Velocity (km s-1)

+12.8 +12.9

-11.7 -11.2

+71.3 +71.3

+18.1:

+26.7 +26.1

+46.5 +46.7

+30.3 +33.7

-27.8 -27.0

+2.1 +2.8

+55.9 +56.6

+14.6 +14.2

-32.5 -32.7

-0.4 -0.7

+4.8 +3.9

Star Date (UT) HD 218864 1987 Nov. 6.21 1993 Nov. 6.15 HD 219090 1987 Nov. 6.21 1993 Nov. 6.15 HD 219357 1987 Nov. 6.21 1993 Nov. 6.15 HD 221033 1987 Nov. 6.21 1993 Nov. 6.15 HD 221331 1987 Nov. 6.21 1993 Nov. 6.15 HD 222261 1987 Nov. 6.22 1993 Nov. 6.15 HD 222513 1987 Nov. 6.22 1993 Nov. 6.16 HD 222899 1987 Nov. 6.22 1993 Nov. 6.16 HD 222973 1987 Nov. 6.22 1993 Nov. 6.16 HD 223445 1987 Nov. 6.22 1993 Nov. 6.16 HD 223614 1987 Nov. 6.22 1993 Nov. 6.16 HD 223646 1987 Nov. 6.23 1993 Nov. 6.16 6.17 HD 223845 1987 Nov. 6.23 1993 Nov. 6.17 HD 224248 1987 Nov. 6.23 1993 Nov. 6.17

Velocity (km s-1)

+1.8 +2.4

-38.5 -38.0

-54.5 -54.3

+30.5 +30.5

-8.1 -8.0

+1.4 +1.3

+38.6 +38.8

+15.5 +17.9

-27.4 -28.1 -12.4 -11.6

+8.4 +8.8

-39.8 -37.8 -38.1

-22.6 -22.6 -11.0 -10.5

-9.4 -8.3

*Non-Clube star

We conclude this section by pooling the distributions in the six Areas, producing the summation that is plotted in Fig. 1. We consider that the figure provides ample visual justification for our cut-off of the distribution of observational discrepancies at 1.5 km s-1, and indeed may suggest that we have erred (if at all) on the side of conservatism. The rms discrepancy for the whole ensemble of 550 stars within 1.5 km s-1 is 0.47 km s-1, so the finally derived global value for the rms uncertainty of a single observation is 0.33 km s-1.

4.2 Errors of the OHP observations Multiple observations of programme stars were not undertaken systematically at OHP except in the cases of known or suspected spectroscopic binaries. Many stars that had already been observed twice at ESO were, however, observed for a third time at OHP. Since, in general, they were observed for a fourth or subsequent time only if there was evidence of variation, any assessment of errors by appeal to cases where multiple measurements were made at OHP is certain to be severely biased. We have therefore looked at the discrepancy

of the first OHP observation of stars not specifically noted as certain or probable binaries from the means of the two ESO velocities (the last two, if there are more) of the same stars; we have added to Table 9 a column giving the rms values of those discrepancies for each of the two Areas for which adequate data exist. On the basis of considerations similar to those applied to the ESO measurements, we set the cut-off of the distribution at 2.0 km s-1; both Areas yielded rms discrepancies near 0.7 km s-1, and after pooling them and allowing for the contribution to the resulting value of the mean of the two ESO measures we are left with an estimate of 0.65 km s-1 for the uncertainty of a single OHP velocity. As a gloss on this discussion, we remark that although the OHP measurements are shown to have something like twice the errors of the ESO ones, and make only a modest contribution to the precision of the mean velocities of the constant stars on the programme, they (a) identify as SBs several stars that had given accordant velocities when observed from ESO, (b) verify with certainty the SB nature of many stars that could have been listed only as `probable SBs' on the basis of the ESO observations alone, and (c) enable the derivation

2006 The Authors. Journal compilation C C 2006 RAS, MNRAS 371, 11401158


Photoelectric radial velocities, Paper XVI 1149

Table 7.

Star Date (UT) HD 184581 1987 Nov. 6.00 6.06 1993 Nov. 4.02 6.04 HD 184626 1987 Nov. 6.01 1993 Nov. 4.02 HD 184650* 1993 Nov. 4.02 HD 184712 1987 Nov. 6.02 1993 Nov. 4.03 HD 186043 1987 July 18.14 Nov. 6.02 1993 Nov. 4.03 6.04 HD 186058 1987 Nov. 6.03 1993 Nov. 4.03 6.04 HD 186245 1987 Nov. 6.03 1993 Nov. 4.03 HD 186321 1987 July 18.14 Nov. 6.04 1993 Nov. 4.03 HD 186581 1987 Nov. 6.04 1993 Nov. 4.03 6.05 HD 187010 1987 Nov. 6.04 1993 Nov. 4.04 6.05 HD 188159 1987 Nov. 6.04 1993 Nov. 4.04 HD 188202 1987 Nov. 6.05 1993 Nov. 4.04 6.05

Radial velocities of stars in Clube Area 16.

Velocity (km s-1) Velocity (km s-1) Velocity (km s-1)

-19.1 -18.9 -21.9 -22.1

-0.2 +0.1

+43.5:

-6.3 -7.2

-29.5 -29.7 -29.7 -29.4

+16.2 +13.9 +13.8

+28.6 +27.8

+21.4: +21.3 +21.4

-9.1: -7.8 -8.1

-31.4: -38.4 -38.7

+12.7 +12.8

-11.5: -4.0 -5.3

Star Date (UT) HD 188245 1987 Nov. 6.05 1993 Nov. 4.04 6.05 HD 188316 1987 Nov. 6.05 1993 Nov. 4.04 6.05 HD 189120 1987 Nov. 6.05 1993 Nov. 4.04 HD 189584 1987 Nov. 6.05 1993 Nov. 4.04 HD 189855 1987 Nov. 6.06 1993 Nov. 4.04 HD 190288 1987 Nov. 6.06 1993 Nov. 4.05 6.05 HD 191503 1987 Nov. 6.06 1993 Nov. 4.05 HD 191847 1987 Nov. 6.06 1993 Nov. 4.05 HD 191865 1987 Nov. 6.06 6.07 1993 Nov. 4.05 HD 191990 1987 Nov. 6.07 1993 Nov. 4.05 HD 191991 1987 Nov. 6.07 1993 Nov. 4.05 HD 192488 1987 Nov. 6.07 1993 Nov. 4.06 HD 192570 1987 Nov. 6.07 1993 Nov. 4.06

-25.7 -25.0 -25.0

-64.3 -62.4 -62.7

-12.5 -12.4 -7.1 -7.2

-24.5 -24.6

-65.3 -65.4 -65.5

+3.1 +3.1

+1.1 +1.0

+15.7 +15.8 +15.5

+24.0 +23.9

+10.2 +10.7

+4.5 +3.9

-31.0 -31.3

Star Date (UT) HD 192631 1987 Nov. 6.07 1993 Nov. 4.06 HD 193570 1987 Nov. 6.08 1993 Nov. 4.06 HD 193604 1987 Nov. 6.08 1993 Nov. 4.06 HD 193805 1987 Nov. 6.08 1993 Nov. 4.06 HD 193806 1987 Nov. 6.08 1993 Nov. 4.06 HD 193867 1987 Nov. 6.08 1993 Nov. 4.07 HD 194185 1987 Nov. 6.08 1993 Nov. 4.07 HD 194327 1987 Nov. 6.09 1993 Nov. 4.07 HD 194369 1987 Nov. 6.09 1993 Nov. 4.07 HD 194462 1987 Nov. 6.09 1993 Nov. 4.07 HD 194606 1987 Nov. 6.09 1993 Nov. 4.07 HD 194749 1987 Nov. 6.09 1993 Nov. 4.08 HD 194945 1987 Nov. 6.09 1993 Nov. 4.08 HD 195081 1987 Nov. 6.10 1993 Nov. 4.08

-4.4 -4.6

+39.4 +40.4

-22.3 -22.6

-14.6 -14.7

+30.9 +31.1

-49.1 -49.3

-45.9 -45.9

-26.4 -27.0

+39.7 +39.6

-39.6 -40.3

-10.8 -10.9

-20.6 -20.2

+0.1 +0.2

+76.0 +76.7

Star Date (UT) HD 195415 1987 Nov. 6.10 1993 Nov. 4.08 HD 195416 1987 Nov. 6.11 1993 Nov. 4.09 HD 195660 1987 Nov. 6.11 1993 Nov. 4.09 6.06 HD 195885 1987 Nov. 6.11 1993 Nov. 4.09 6.06 HD 196047 1987 Nov. 6.11 1993 Nov. 4.10 HD 196082 1987 Nov. 6.11 1993 Nov. 4.10 6.06 HD 196082 B* 1993 Nov. 4.10 HD 196103 1987 Nov. 6.12 1993 Nov. 4.10 HD 196315 1987 Nov. 6.12 1993 Nov. 4.10 HD 196399 1987 Nov. 6.12 1993 Nov. 4.10 HD 196533 1987 Nov. 6.12 1993 Nov. 4.11 HD 197000 1987 Nov. 6.12 1993 Nov. 4.11 6.06 HD 197113 1987 Nov. 6.12 1993 Nov. 4.11

Velocity (km s-1)

+0.5 +1.3

-16.3 -16.3

+6.3 +9.2 +9.7

+45.0 +42.1 +41.9

+8.7 +8.6

-74.0 -73.8 -73.5

-68.4:

-55.3 -55.5

-35.0 -34.6 -58.7 -59.5

+11.0 +11.2

+48.9 +47.8 +48.6

Star Date (UT) HD 197501 1987 Nov. 6.13 1993 Nov. 4.11 HD 197613 1987 Nov. 6.13 1993 Nov. 4.11 HD 197890 No result HD 198764 1987 Nov. 6.14 1993 Nov. 4.11 HD 199118 1987 Nov. 6.14 1993 Nov. 4.11 HD 199174 1987 Nov. 6.14 1993 Nov. 4.11 6.06 HD 199242 1987 Nov. 6.14 1993 Nov. 4.12 HD 199387 1987 Nov. 6.14 1993 Nov. 4.12 HD 199474 1987 Nov. 6.14 1993 Nov. 4.12 HD 199674 1987 Nov. 6.14 1993 Nov. 4.12 HD 200055 1987 Nov. 6.15 1993 Nov. 4.12 HD 200096 1987 Nov. 6.15 1993 Nov. 4.12 6.06 HD 200143 1987 Nov. 6.15 1993 Nov. 4.13

Velocity (km s-1)

+14.0 +14.0

-32.6 -32.8

+9.8 +9.1

-33.4 -33.7 -5.0 +1.1 +1.3

-16.0 -16.6

+4.0 +4.5

-13.4 -13.9

+27.7 +28.9:

+55.6 +55.6:

Star Date (UT) HD 200144 1987 Nov. 6.15 1993 Nov. 4.13 HD 200382 1987 Nov. 6.15 1993 Nov. 4.13 6.06 HD 200420 1987 Nov. 6.15 1993 Nov. 4.13 HD 200853 1987 Nov. 6.16 1993 Nov. 4.13 6.07 HD 200854 1987 Nov. 6.16 1993 Nov. 4.13 HD 200902 1987 Nov. 6.16 1993 Nov. 4.14 HD 200954 1987 Nov. 6.16 1993 Nov. 4.14 HD 201410 1987 Nov. 6.16 1993 Nov. 4.14 HD 201441 1987 Nov. 6.17 1993 Nov. 4.14 HD 201885 1987 Nov. 6.17 1993 Nov. 4.14 6.07 *Non-Clube star

Velocity (km s-1)

+2.5 +2.6

+17.2: +16.0 +16.1

-45.2 -45.3

-47.4 -47.1 -47.4

+6.8 +6.0

+53.5 +53.5

-13.4 -12.8

-40.8 -40.5

-9.7 -9.6 -10.5 -9.0 -9.0

-33.7 -32.7 -32.7

-20.3 -20.7

-21.4 -21.1

of at least preliminary orbits (Griffin 2006, Paper XVII) for as many as 30 of the stars.

5 T H E S TA R S A N D T H E I R R E S P E C T I V E M E A N V E L O C I T I E S In taking mean values of the velocities for each individual star, we have attributed to the OHP measurements (if any) one-third of the weight of the ESO ones. The few observations that are marked with colons in Tables 27 have been given one-third as much weight as their respective sources (ESO or OHP) would normally warrant. Although we down-weight them now in forming the means, in order to avoid casting too rosy a light on the error estimates we treated them on a par with all the other data in the discussion of that topic above. The mean velocities for all the stars are set out in Table 10. Since practically all of the stars have, as a minimum, two ESO measurements, which we have shown globally to have standard deviations of 0.33 km s-1, the standard error of a mean stellar velocity is normally of the order of 0.25 km s-1 or better. In the cases where we have reason to suppose that the uncertainty is as much as 0.5 km s-1, we have placed a colon after the mean velocity. Such cases may arise either because all of the measurements are indi-

vidually uncertain (usually because the star concerned is of particularly early spectral type and gives `feeble dips'), or because the measures are not in mutual agreement, as in the cases of SBs for which the observational material is inadequate to support an orbit determination. Where the radial velocity of a star has proved to be variable, the best that we can do is still to give the mean velocity. Where orbits can be derived, the  -velocities (identified in Table 10 by the note SBO, the conventional designation for `spectroscopic binary with orbit') should be at least as accurate as any of the other mean velocities. In other cases the discrepancies between different measurements of the same star are never large in comparison with the real velocity dispersion among the stars in a particular Area. The poor accuracy of the mean velocities of such stars is therefore not likely significantly to inflate (or for that matter to diminish) the velocity dispersions that are among the ultimate objectives of this observing programme. We have explained at the end of Section 4 (the paragraph immediately before the start of Section 4.1) the careful distinction that we make between the unqualified use of the label `SB' and the progressively less certain `probable SB' and `possible SB'. We identify those respective cases in Table 10 by the notes SB, SB: and SB::.

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


1150 R. F. Griffin and A. P. Cornell

Table 8. Positions of measured companion stars in relation to their primaries, and their velocities.

Star `HD' Area 6



mV mag  arcsec PA



RV km s-1

Star `HD' Area 13 31341 B 34659 B 36730 B Area 14 30253 B 37730 B

 

42307 47027 B 56706 B

mV mag  arcsec



88973 89003 B 89003 C 89073 B 92789 B 92998 B 95425 B 96402 B 96768 B 97718 B 97977 B 98032 9.14 11 11 101/2 10.9 11.0 11.4 10.7 12.1 111/2 10.8 8.50 259 12 19 56 146 60 30 111 101 16 74 161 204 201 3 10 350 335 85 114 171 353 317 89 +60.0: -2.0: +14.0: +2.7: +10.5: -28.4: +74.8: +7.2: SB +4.9: +21.6 +28.8: SB -2.6

PA  RV km s-1

10.68 9.3 11.0 18 4.12 127 129 93 171 -5.3 SBO -4.0 +71.0:

10.7 11.1 8.89 10.5 11 37 26 96 34 20 327 8 339 255 292 +72.6 +20 :: SB +24.3 +34.6: +54.6:

Area 7 112386 B 112877 B 119188 B 125187 B 125266 B

 

11.3 11.6 10.5 111/2 111/2 50 58 62 54 10 87 73 163 102 340 -3.4: -24.6 -20.3: -10.1: +18.6:

Area 15 182073 B 206693 B 213289 B Area 16



184650 196082 B

 

11 10.6 11.4 11 3 71 343 90 130 +23.1 +12.0: +18.1:

9.33 12 81 11 151 259 +43.5: -68.4:

`Primary' is HD 89003. `Primary' is HD 98020. `Primary' is HD 42328. B is itself a close double.



`Primary' is HD 184626.

Table 9. Results of investigation of observational errors.

Area

6 7 13 14 15 16

ESO km s-1 0.39 0.48 0.43 0.43 0.54 0.55 OHP km s-1 0.63  0.72   

NB. the quantity tabulated is not the standard deviation of a single velocity measurement but is the rms discrepancy between the first two ESO measurements of standard deviation of an observation. ancy between the first OHP measurement of the star and the mean of the last two ESO velocities, and so is somewhat larger than the actual OHP standard deviation.

each star; it is therefore

 2 times the actual

 The quantity tabulated is the rms discrep-

Figure 1. Distribution of discrepancies between the first two radial-velocity measurements made with the ESO Coravel of each of 555 stars not known to vary in velocity.

In the cases of `certain' and `probable' SBs, the uncertainty created in the mean velocities by the variability is much greater than that caused by any errors of measurement, so in those cases any OHP values have been weighted on a par with the ESO ones in forming the means. The same consideration has impelled us to avoid giving undue weight to a particular epoch: mutually confirmatory measurements made within a single observing run have been averaged and treated as a single value in forming the mean. For `possible' SBs, we simply cannot tell whether the relatively small discrepancies between different observations are real or of instrumental origin; we

have used the normal reduced weight for any OHP measures, but to be on the safe side, and with acknowledged inconsistency, we have attached colons to the relevant mean velocities in Table 10. Table 10 lists the 628 stars Area by Area rather than in the global order of their HD numbers. In an effort to increase further the utility of Table 10, we have added to it the V magnitudes, (B - V) colour indices and spectral types of all the stars. The great majority of those data have simply been copied from SIMBAD. In the few cases where magnitudes are given in SIMBAD only to one decimal place, we have retrieved the missing data from the Tycho catalogue as presented by VizieR and identified them with daggers. The Michigan classifications of late-type stars sometimes include an extra component of the form `CNII', which indicates the luminosity class that

2006 The Authors. Journal compilation C C 2006 RAS, MNRAS 371, 11401158


Photoelectric radial velocities, Paper XVI

Table 10. Magnitudes, colour indices, spectral types and mean velocities. See end of table for key to superscripts. HD V (B-V) Type n SB? HD V (B-V) Type n SB? HD V (B-V)

mag. mag. Area 6

9.20 9.31 1.17 0.88

Vel. km s-1

mag. mag.

9.07 9.83

1.14 G8/K0III/IV

1.05 1.07 1.10 1.33 0.30 1.21 1.06 1.09 0.97 1.00 0.89

G8IV K0III K1III K1IV: G3/G5 K0III K0III K0III

Vel. km s-1

mag. mag.

8.74 9.46 9.54 9.21 9.19

1151

Type n

98827 98917

88913 88992 89003S

G8/K0III 27 +41.2 SBO

G8III K0V G8III/IV G8IV G8III G8III/IV K0III G8III K0/K1III K0II K0III G8/K0IV G8III K0V G8/K0III: K0V G8III G8IV

3 -14.0 3 +11.5 3 +66.4 3 +23.9

3 3 3 +3.2 0.0 +6.5

99091H 9.17

99321 99406 9.19 9.50 9.17 0.79

89073H 8.55

89255 89337 89380 89607 8.67 9.11 9.07 8.71

90014H 8.86 90046 9.12 *90167H 8.39

90168 90196 90266 9.03 9.12 9.14

90498R 9.33 90516 9.90 90793PS 9.23

*91064 92256 92309 *92789 *92830 *92920S 92998 93140 8.72 8.65 8.49 8.70 8.61 9.42 9.47 9.45

1.20 1.02 0.93 0.86 1.05 0.94 1.02 0.97 0.98 1.00 0.96 0.81 1.09 0.78 0.90 0.92

*99426 10.68

99477 99551 *99552 99584 99637S 9.58 8.65 8.16 9.08 9.55

3 +23.4 3 -12.0 3 -19.0

3 3 3 +0.3 -6.8 +0.6

99691H 9.21

99724 99755 100023

3 -19.9 3 +27.5 3 +12.3 3 -2.0 3 +56.3 3 -12.6: 3 -20.5

3 3 +1.7 +4.4

119099 119134 119175 *119188 119294

*119321R 9.63 119451 10.14 119522 9.30 119591H 8.96 119754 8.96 119854PS 9.34 *120013H 8.94 *120304H 9.07 120338 9.42 120391H 9.46 120503 9.82 *120571H 9.25

120729 120852 8.69 9.50

G8III/IV 15 +27.2 SBO

K1V G8/K0IV K3III K0III K2/K3III K0III K1III 3 -11.4 3 +9.9 3 -11.6 3 -13.9 3 +31.2 3 +0.1 4 +10.2

8.72 1.38

9.03 8.99

100184 10.09

100305 100306 9.57 8.95

3 +53.4 3 -2.0 6 +35.4 3 +20.4 3 +7.3 3 +30.6

100347H 8.68

1.07 1.42 1.04 1.07 1.12 0.93

K0III 16 +14.8 SBO G8III 4 -14.0

121202H 8.96

121376 121379 9.37 8.96

Area 7 0.88 G6/G8IV

0.98 G8/K0III/IV

0.77 1.10 1.00 1.30 0.86 1.17 1.11 1.42 1.20 0.92 0.70 1.06 1.01 0.89 0.89 1.10 1.14 0.95 1.25 0.97 0.70 1.24

111649 9.06 2 +31.8

93278H 8.73

93801 93996 8.66 9.15

93999H 8.64 94045H 8.73 94126R 8.74

94320 *94428 94441S 94563S 94577 8.23 9.13 9.44 8.57 9.05

94656H 9.00 94783R 8.38

94865 94887 95166S 95425 9.18 9.14 9.70 8.74

G3/G5III 19

-6.0 SBO

*111680H 9.13

111735 111866 9.34 9.83

1.13 K1/K2IIICN+ 2

0.95 1.05 0.76 0.97 0.56 1.16 0.88 1.02 1.07 0.98 0.91 1.01 1.24 1.06 1.04 1.07 0.97 0.83 1.15 0.96 0.90 1.12 1.14 1.01 0.98

K0III K0/K1III 2 3

K1IIICN+ 3 +14.9

G8V G8IV 3 +16.1 3 +55.1

111964R 9.66

112386 112402S 112434 112488 112577 9.42 9.84 9.49 9.66 8.96

K0III/IV 19

K0/K1III K0III M2/M3III:

+4.8 SBO

3 +15.1 3 +20.0 8 -7.5

K1IIICN+ 3 +19.3

G6/G8III G8IV K0III K0III G8V

6

-0.7

3 +37.3 3 +10.2 3 -6.3 5 +99.1

112656R 8.96 112877 9.37 112905H 9.51

113102 113310 113530 113567 113580 113775 113909S 113926 114181 114384 *114483 9.08 8.57 9.09 9.54 9.44 9.56 9.87 8.84 9.21 9.46 9.35

G5V 24 -11.4 SBO K0III 11 -11.5 K1III 4 -14.6

K0IV/VCN+ 3 K1III 3 K0IVCN+ 3 +6.7 -2.9 +6.4

K0V 22 +12.7 SBO

K1/K2III G8/K0V G8/K0V G6IV:

4 +13.6 3 +8.0 3 +16.4 3 -6.0 3 +14.9

3 3 +1.0 -4.0

95533R 9.16 0.80

95714S 95852 95871 9.91 9.92 8.59

0.89 0.68

114524H 9.46

114893 114936 115203 9.68 8.72 8.98

0.96 G8/K0III/IV

0.89 0.68 1.07 1.08 0.98 1.02 0.99 1.10 1.12

K0V G8V G8IV G8III G8IV

95872PS 9.89

95902S 95923 95940 9.42 9.98 9.08

96005H 8.89

96402 96643 *96768 96818 9.04 9.31 9.24 9.98

G8/K0V 11

G8III F6V K1/K2III G8III/IV G8IV K0IV K0III G8V K0III K0III K0III G8III K0III G8IV G8V K1III G8/K0IV G6/G8IV

-7.4 -1.5 +2.6 +8.1

121426H 8.59

*121552S 121593 121671 121687S 9.34 9.07 9.64 9.49

2 +29.0 2 -2.1: 2 -18.8 3 -12.3

4 2 2 -9.3 -9.8 +7.4

121885H 8.97 122011 9.72 *122055H 8.75

122172 122207 9.35 9.30

2 +54.8 3 -9.2 3 +29.4 2 +0.2 2 -10.4 2 -6.6 3 -10.9 2 -32.3 2 -38.9 2 +12.8 2 -47.5

122350H 9.60 122509H 9.79

122521 122638 122734 123052 123108 123368 123369 123414 123427 123525 123620 123633 123648 123810

9.92 9.28 9.77

K0/K1III 14

G8/K0III K0III K0III

+1.1

2 -27.0 2 +16.4 2 -2.5 2 +77.0 3 +44.9 2 -18.8 2 -30.7 2 -29.0 2 -20.0

1.06 1.01 1.17 1.21 1.30 0.72 0.31 1.18 0.98 0.91 0.84 1.20 1.13 0.94 0.79 1.03 1.25 1.06 1.21 0.99 0.96 1.19 1.00 1.01 1.13 1.19 0.71 1.02 0.95 1.24 0.92 1.57 0.83 1.20 0.95 1.09 1.03

K0III G8IV

3

Vel. km s-1 -9.3 SB?

2 +59.5

K2III 19 +20.4 SBO

K2/K3III: K1/K2III K0V A7/A8III K0III/IV G8III G8IV K1V K1III K0III K0III G6/G8V

2 +19.1 4 -49.4 3 +16.7 0 -- 2 -31.2 9 -14.6 3 +24.8 3 -10.3 2 -1.2 2 +14.8 2 -22.4 3 -21.8

G8 13

K0II K0III

+1.4 SBO

2 -31.6 2 -29.5

K1III 14

K0III K0IV K0III/IV K0III G8V K0/K1III

+3.5 SBO

4 -26.2 4 -9.8 2 +45.5 2 -23.6 2 -53.1 3 +0.9

G8IVCN+ 3 -42.6

G5V G8III K0III K1/K2III G8IV K4III: G8/K0V G8V G8III: K0III G8IV K2III K1/K2III

2 -38.7 2 -26.5 2 -3.7 3 +18.6 3 -10.4 2 +20.9 2 -15.2 2 -59.7 3 -12.7 3 +32.2 2 -58.8 2 +18.5 2 -14.1

9.72 1.01

8.77 9.48 9.53 8.68 9.20 9.26 9.65 9.26 9.12 9.71

1.13 1.00 0.88 1.09 0.97 1.00

K0III 14 +48.0: SB

K0IV K0III G8/K0III K0III

4 -27.7 2 -35.8 2 -11.2 2 -13.9

3 3 2 2

+3.8 +9.7 -3.2 -0.6

1.29 K0/K1II/III

1.01 1.06 1.02 0.97 1.21 1.44 1.28 0.92 1.08 1.35 1.30

G8III/IV K0/K1III K0III K0V K1III K1/K2III K1III: G8IV

0.90 G8/K0III/IV

1.22 1.18 1.19 0.91 0.87 1.19 1.18 0.64 0.93 0.91 0.93 1.02 0.95 1.02 1.18

K1III K0III K1III/IV G8/K0IV --

115250H 9.19

115430 115545 116141 116322 *116463 116482 116661S 8.70 9.40 9.23 9.84 9.13 9.33 9.84

3 +30.0 3 -21.7 3 -2.3

G8IV 16 +88.1 SBO

G8III/IV K1III 3 3

K0III: 13

F7V K0III 3 3

96839S 10.14 0.54

*96873H 9.26 96889PS 9.51

96908S 96940 96959 9.86 9.98 8.94

97260P 9.99 97464H 9.05

97480 97574S 9.74 9.79

97718PS10.07

97750 97977 8.84 8.85

98008H 9.11 98020P 8.81

98121 98122 98250 98251 98492 98507 98541 98738 9.58 9.23 9.50 9.24 8.69 8.75 9.05 9.59

1.12 0.54 0.77 0.92 0.99 0.89 0.90 1.03 0.89 0.68 1.31 1.41 1.21 1.00 1.02 1.10 0.92 1.29 1.31 1.07 1.36 0.94

-4.9 -3.6 +2.6 SBO +1.6 +6.7

*116858R 8.78 *116920R 8.73

117161 117205 9.85 9.11

G3/G5V 10 +11.2

K0V K0III: G6III K0/K1III G8IV G8III/IV

3 3 4 +9.0 -4.9 +5.7

117321H 9.00 117392 9.50 117393H 8.95

117518S 117734 117804 117863 9.37 9.14 9.26 9.30

3 +38.0

3 3

-2.2 +2.4

123812R 9.62

123988 124025 124038 124190 124536 124558 9.02 8.94 9.33 9.23 9.47 8.92

K1III 19 -44.5 SBO

K1III G3V K3V K3V

2 -17.6 2 +29.3 2 -12.3 2 -12.5

124610H 8.92

124685 124779 124871 8.92 9.03 8.96

2 +24.0 3 +41.3 4 -30.2 2 -25.2 2 -37.7

K1III 13 -38.6 SBO

K3III: K1/K2III

3 -11.4 3 -4.3 2 +10.5 2 -0.4

1.29 K1/K2III/IV

1.08 1.13 0.97 0.74 1.04

G8III

G6III/IV 15

K0III G8IV K0III K1III

+0.3 SBO 124918 10.00

124958S 125132 125168 9.79 9.33 9.40

2 -15.2 2 -21.0 2 -9.3 2 +47.2 3 -42.1 2 -16.6 2 +10.6 2 -12.4 2 -71.5 3 +58.5

K1III 12 -45.3

K1III G8IV/V K1III 3 -65.1 2 -14.5

2 2 2 -6.9 -5.2 +4.1

1.40 K1/K2III/IV 1.39 K2III

G8V 18 +44.2 SBO

G8V K2III K2/K3III K1III/IV K1III K1III K1III G6/G8IV K2III K3III K0III K1III K0III

3 +22.3 3 -20.3 5 +23.9 3 +0.6 3 +39.7

3 3 3

-7.9 +1.3 -9.3

0.96 G6/G8IV/V

1.29 0.94 1.02 0.99 1.12 0.95 1.09

G8III/IV G8IV K0III K2V K1III

*117987R 9.26

118041 118116 8.69 9.68

118236H 9.00

*125169H 8.98

125187 10.29 0.88 125266 10.41 0.69

*125268 125280 125341 125456 *125493 125507

9.44 9.33 1.21 1.42

8.83 1.07

9.57 8.97 9.68 1.06 0.94 0.97

G8/K0 15 -37.6 SBO

G8/K0III: K0III K2III 2 +18.8 2 +33.8 2 -5.9

G8III/IV 15 +20.9 SBO

K1III K0V K0III K0III K1III K0III K0III

2 -25.7 2 +70.9 2 -25.5 3 -24.8 2 -13.7 2 -14.8 2 +24.0

118282R 9.75 0.83

*118597 118853 118854 118855 8.74 9.10 8.79 9.29

3 +29.7 3 +30.6 3 +7.4 3 -16.9 3 +21.1

118892H 8.78

119011S 119087 9.72 8.97

1.02 1.00 1.06 0.99 1.09 0.69 1.03

K0III 17 -30.8 SBO

K0/K1III G8IV G8/K0IV

2 +3.9

2 +52.4 2 -12.2

Area 13

0.91 1.15 1.39 0.95 1.33

G6III/IV K0III K1III:

26725 9.01

26741H 8.90 *26777H 9.08 26917 9.49 27077H 9.36

G6IV/V 24 +13.3 SBO G8IV 20 +35.3 SBO

3 +22.4 3 +59.3 4 +92.8

K1III 35 +37.4 SBO K2III 3 -3.0

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


1152 R. F. Griffin and A. P. Cornell

Table 10  continued HD V (B-V) Type mag. mag.

27116H 8.98

27206 27229 9.66 9.40

n

27300H 9.24 27412 9.10 27529H 8.87

27538 27600 9.56 8.90

27643H 8.62 27678P 8.52 27871 9.53 27872H 8.49 27890H 8.88

27949 28173 8.96 8.48

28222H 9.32 28426H 8.91 28559H 9.18 28683 9.25 *28753H 8.28 28971 9.02 28997H 8.78 29217H 8.57

29229 29358 29423 8.56 8.89 9.40

29791H 8.99 29800H 8.80

30010 30024 8.86 8.47

30118H 9.21 30525PS 8.95

30564 30668 30745 30785 30903

1.29 1.01 1.26 1.41 0.95 1.07 0.99 1.31 1.24 1.00 0.90 1.38 1.10 1.07 1.02 1.17 1.10 1.06 0.92 1.02 1.51 1.20 1.21 1.39 1.09 1.05 1.08 1.11 1.20 1.05 0.95

K1/K2III G8III: K1III/IV K1III G8III/IV K0III G8IV 3

Vel. km s-1 -0.4 SB?

HD V

(B-V) Type n

mag. mag.

9.49

Vel. km s-1 SB? HD

V

(B-V) Type n

mag. mag.

35445 10.11 35529H 8.33 35740H 9.30

37336 37721 37730 38112 9.20 9.47 9.26 9.39

1.09 1.09

Vel. km s-1 SB?

36924

3 -51.2 3 +68.2 3 -13.2 3 +58.4 3 +38.0 3 +92.0

37044H 9.11

37064 37222 37494 37595 9.75 8.34 9.70 9.25

1.04 1.00 1.07 1.36 1.27 1.55

K0IV 3 +28.3

K0III 13 +10.5: SB

G8III: K2III K0III: K3/K4III: 3 +29.1 3 +74.5 3 +27.6 3 +12.5

G8III/IV 3 +27.9

K1IIICN+ 4 +22.9: SB:

0.76 G8/K0III/IV

0.96 1.43 1.22 1.12 1.20 0.93 0.70 0.95 1.39 1.08 1.22 1.14 1.00 0.88 0.91 0.96 1.03 1.05 1.04 1.26 1.15 1.07 1.13 K0/K1III K3III: K1III K0II/III K1III G8III G6V K0IV K2III K1III K2III K0III K0II/III G8wG2: G8IV G8IV K0III K1III K0III K2/K3III: K4V K0III K2III

K2III 15 +13.5 SBO

K1/K2III K1III 6 +33.8 3 -10.4

K0/K1III 15 +19.6 SBO

K3III K1III K0III K0III K1/K2III 3 +10.8 3 +11.1 3 -13.3 3 +18.1 3 +18.4

21188 21189 9.10 8.89

21255H 8.98 21516H 8.92 21721H 9.03 21827H 9.06 *21989H 8.16

22436 23072S 23266 9.18 9.75 8.76

Area 14 1.04 1.09 1.12 1.17

1.09 1.08 1.29 1.29 0.70 1.10 0.87 1.12 1.22 1.02 0.88 0.94 1.22 1.17 1.34 0.85 1.00 1.05 1.10 1.34 0.92 1.40 0.86 1.00 1.05 1.14 0.97 1.29 1.23 1.42 0.97 0.86 1.43 1.36 1.33 1.18 0.91 0.89 0.79 0.70 0.86 1.06 1.22 1.23 1.20 1.15 1.08 0.98 1.28 1.39 1.15 1.22 1.30 1.15 1.29

39446H 8.83 39609 9.43 *40293R 9.10 40342R 8.40

40484 40560 40768 7.88 9.40 8.58

K0III 13 +54.8 SBO

K0III G8III K0IV K3III: K1III K1III K2III K0III K1III G8/K0III K1III K1/K2III K0III G8IV

3 +34.8 3 +11.3 3 +43.5 3 +71.2

3 3

-1.2 +6.0

*23332H 8.88 23497H 8.57 24363 8.48 24618H 9.00

24930 24956 8.94 8.65

3 +17.9 4 +8.4 4 +14.8 3 +8.3 3 +92.6 3 -4.7 3 +34.1

3 3

+1.5 -7.8

25018H 8.29 25119H 8.34 25405H 8.25

25831 25875 9.27 9.47

1.01 K0/K1IV/V

*26046H 8.62

26098 26191 9.28 8.68 9.46 0.95

9.17 9.23 9.51 9.29

31259H 8.92 *31341H 8.95 31406H 8.43

31637 31638 31927 32121 9.19 9.50 9.30 9.57

32360H 9.29

32759 33196 33757 33758 33934 9.36 9.27 9.13 8.80 9.23

*33978H 8.34

34014 34166 9.19 8.94

*34659R 9.14

34895 35106 35128 *35164 35371S 8.91 9.60 8.31 9.5 8.99

35507H 9.18

35576 35646 35810 35852 9.09 9.60 9.19 9.09

35853H 8.46

35871 35992 9.29 8.70

*35993H 9.55

36004 36140 36186 36344 36489 36544 8.02 8.91 8.86 8.89 9.33 8.97

36562H 9.17

36632 36657 36730 36744 9.09 8.89 8.76 8.99

*36745R 9.14

0.97 1.01 1.02 1.07 1.06 1.03 1.21 1.12 0.98 1.18 0.95 1.19 1.05 0.90 1.08 1.22 0.82 1.01 1.27 1.38 1.01 1.06 0.95 1.48 1.3 0.94 1.03 1.09 1.02 1.12 1.13 1.19 1.04 1.21 1.09 1.50 1.14 1.54 0.97 0.97 1.14 1.21 1.27 1.02 1.11 1.15 0.86

K1III G8/K0IV G8IV G8III/IV K1III K0III K0II K1III K1III G8/K0III K0/K1III: G8IV K0III: G8IV G8IV G8III K1/K2III G3IV

3 +50.9 7 -6.5: SB 3 +34.2

3 3

-4.4 -0.2

26247H 8.98 26318H 8.88 26523R 9.55 26530H 8.75 *26615 9.49 26788H 8.81 26834H 9.04

26891 27010 27011 27068 27099 27201 8.67 9.14 8.53 9.57 9.18 7.91

3 +16.1 7 -5.3 3 +27.4 3 +34.1 3 -4.2 3 +93.1 3 +47.2 3 -3.5 3 +48.6 3 +70.5 3 +1.9 8 +47.1: SB 3 +27.8

27319H 8.72 27555H 8.16 27853 9.04 28002R 8.76 28330 9.66 28340H 9.25 29016R 9.71 29067H 9.30

29168 29657 29825 29845 8.93 8.32 8.35 8.87

K1III 42 +26.5 SBO K2III 14 +39.6: SB

K2III: K5V K1III G8/K0III: K4/K5III K2/K3III: K0V G8IV G8IV 3 +33.5 3 -3.2 3 +53.6 3 +19.9 3 -27.0 3 +65.0 3 -0.9 3 +65.0 3 +18.4

30253H 8.48

31029 31462 8.78 8.47

G8III 14 +24.5 SBO

K0III K1III K1III K0III K1III 8 +53.7: SB 9 +25.8: SB 4 -8.2 3 +31.2 4 +54.2

Kp Ba 13 +17.7 SBO

K4/K5III K2III: 3 +30.0 5 +5.0

*31484H 8.87 31645H 7.97 31804H 8.43 32107H 8.84 32140H 8.19 32244H 8.85 32823H 8.97 33380 9.32 33456H 9.34 33516H 8.90 33700H 9.02

33895 33954 9.33 9.53

K0III K0III K1III K2III K0/K1III K0III K1p Ba K3III G5V K0II/III G6wG0III K1III K1III K0III G8III K0III K2III K0III K2III G8III K1III K0III K1/K2III K2/K3III G8III/IV K3III K0IV/V G8III K1III K2III K0III K2III

3 +12.6 3 +12.3 3 +32.5 3 +23.3 3 +13.6 3 +37.7 3 +11.3: SB 3 +40.1 3 +11.9

3 3 +8.8 -1.7

41023H 9.08 41094P 8.44 41540H 9.33

42010 42027 9.18 9.14

42193H 8.55 42228 8.87 42328H 8.44 42451 9.35 42505R 9.41 43182 9.39 43493H 8.90

43792 43977 9.52 9.57

3 +51.5 3 -14.4 3 -28.5 3 +12.3 3 +12.3 3 +21.3 3 -32.7 3 +11.7 3 +4.5 4 +34.8: SB 4 +20.8: SB 3 +48.2: SB 3 +33.1 3 +7.4 3 +23.3 3 +22.7 3 -12.4 3 +11.7 3 +9.0

3 3 +6.6 +4.6

3 +14.2 3 +90.2 3 +4.7 3 +18.3 3 +16.8

3 3

+8.9 -4.7

3 +36.6 3 +94.4 4 -32.6 4 +22.3

3 3

-0.1 +9.7

4 +74.7 3 +64.3 3 -23.2 3 +49.4 3 +31.3 3 +16.5 4 +32.9: SB 3 +9.2 3 +23.9 3 +13.6 3 -0.6 3 +48.2 4 +40.3: SB 3 -0.1 3 +18.7 3 +87.6 3 +25.6 4 +22.5

3 3 3 +7.0 +8.7 +1.4

1.01 G8/K0III/IV

0.98 1.36 0.99 1.00 0.96 0.84 1.24 0.91 0.93 1.33 1.32 0.97 0.89 1.35 1.18 0.93 1.28 1.01 0.51 1.50 G6III K3/K4III K0/K1III K1III G8III K2V K1III G6III G8/K0III K3III K1/K2III G8III K0III K1/K2III K1III G6III/IV K2III K0III F6V M2III

44013H 8.87 44121 8.72 44325R 8.71 44384 9.45 44627R 9.16 44777H 9.10

44790 44879 45037 45186 46506 47027 9.24 9.61 8.35 8.91 9.45 9.26

47028H 8.81

47191 47234 47235 9.39 8.91 9.40

K1IIICN+ 3 +12.1

K3III K1/K2III K0IV K3III K3III K3III G8III/IV G8III G5/G8III: G8IV G5V G6III K1III K1III K1III K1III K2II/III K2III G8III K2III K4III K2III K2III K2III K1III K2/K3III

3 0.0

3 +30.7 3 +34.6 3 -0.1 3 +42.2 3 +13.6: SB: 4 +54.7 3 +42.5 3 -17.9 3 +83.7 3 +22.0 3 -1.3 3 +19.7 3 +36.6 3 -11.0 3 +7.3 3 +20.0 3 +47.2 3 +22.5 3 +35.6 4 +14.2: SB 3 +5.0 3 +36.9 3 +44.5: SB

3 3

-8.4 +3.5

47476H 9.09 *47519S 9.65 *47951H 8.76

48359 48732 48928 49033 49171 49265 8.70 9.17 9.61 9.12 8.71 9.39

3 +13.8 3 +38.0 3 +15.1 3 +15.6 3 +13.3 3 +19.0 3 -18.6 3 +14.2 3 +2.9 3 +23.6: 3 +97.7

1.26 K0/K3IIICN+ 3

0.90 1.01 1.08 1.68 1.09 1.12 1.16 0.98 1.14 1.19 1.05 1.09

+3.8

49266H 8.62 49670 9.25 50159H 8.40

50504 51556 51863 9.18 9.13 8.78

51950H 9.26

52119 8.98 1.19

52251H 8.60 53103H 8.71 53167H 8.63 53707H 8.07

53787 53841 8.40 8.95

54506H 8.79 55048 9.02 55432H 8.73 55546H 8.15 55644 8.96 56319H 8.92 56440H 8.69 56706 8.92 56838 10.09 57041R 9.82 57097 9.25 57622R 9.11 57696 9.43

1.23 K2III/IVCN+ 3 +26.1

0.96 1.21 K0III K1III 3 +17.1 3 +33.0

K4III 13 +82.0 SBO

G8/K0III G8/K0III K0/K1III 3 +35.7 5 +24.4 4 +64.0

1.10 G8/K0IIICN- 4 -39.6: SB

1.23 1.26 0.78 1.21 1.30 1.48 1.34 0.77 K2III K1III G8IV K0/K1III K2III K3III K3III G5III 3 +16.3 3 +62.8 3 +40.0 4 +64.7 3 +40.4 3 +14.9 3 +12.3 4 -15.6: SB

K1III 12

K1III/IV K0III/IV K0III K0/K1III K2V

+1.6 SBO 34230R 9.16

34396 34821 9.73 9.49

3 +83.4 3 +35.3 7 +22.9: SB 3 +27.0 3 +26.1

34830H 7.84 34915H 8.27 35167H 9.31

1.19 1.17 1.39 1.37 1.24 0.91 0.96 1.24 1.31 1.16 1.23 0.98 1.00 0.97 0.82 0.84 1.21 0.79 1.12

G8/K0III G6III G8III M1III K0III K0III K2/K3 G8III/IV K0/K1III K2III K0III K0/K1III K0III/IV K1III

3 +13.9 3 -1.4 3 -12.5

3 3 +3.1 +6.3

3 +28.9 3 +45.1 3 +9.4 3 +24.4 3 +11.4 3 +34.3 3 +34.7 3 +8.8 3 +24.0

K1IIICN+ 3 +39.7

K3III K4III K2III K0III K0III/IV K1III K2III K0III K2III G8III K0III K0III G5/G6 K1/K2IV K1/K2III G8IV/V K0III

3 3 +9.2 +9.1

3 +36.5 3 +46.2: SB: 3 -22.9: SB:

3 3 +4.8 +0.1

3 +13.5 3 +29.3 2 -23.3 2 +4.0 2 +13.8 2 +38.1 3 +8.4: SB 2 +22.0 2 +62.7 2 +81.6

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


Photoelectric radial velocities, Paper XVI 1153

Table 10  continued HD V (B-V) Type mag. mag. Area 15

160484 9.20 170325H 9.04 170692H 9.08

172497 173414 9.17 8.84

n

Vel. km s-1 SB? HD

V

(B-V) Type n

mag. mag.

9.45 8.13 9.11 9.39 9.23

1.04 1.50 1.42 1.15

174101H 8.96 174826 8.50 174929H 9.04 *176772P 9.54 178736P 9.51

181140 *182073S 182235 8.91 9.99 8.97

1.07 1.17 1.02 1.13 1.51 1.57 0.97 0.92 0.86 0.79 1.07 0.59 1.11

182439P 9.60 0.87

186425 9.92 188925R 9.72 192552S 9.78 192695H 9.18

192906 *195477 9.50 9.82

197767R 9.35 198944 9.66 200815H 8.67

202460 203589 8.66 9.73

205037H 7.82

205834 206693 206951

8.12

0.52 0.86 0.63 1.31 0.94 1.14 0.71 1.13 1.00 1.06 1.12 1.40 1.24

9.31 0.68

9.04

207046R 8.16

207307 207444 207527 9.29 9.35 9.40

208929H 8.23

209003 209620 *210009 210057 210164 9.09 8.69 9.24 9.46 9.44

210332H 8.98 210603 9.00 210713H 8.84 212264H 8.97

212555 212663 213158 213289 9.66 9.44 9.68

1.16 0.88 1.18 1.16 1.12 1.37 1.08 1.30 1.19 1.24 1.24 1.18 1.09 1.14 1.20 1.20 1.12 1.08

9.34 1.11

213743H 8.58 214309H 9.00 214792 9.38 215370H 8.85 215587R 8.40 215832H 9.01

215987 217978 9.10 9.09

218077H 9.26

*218109 218842 9.09 9.12

1.02 1.46 1.34 1.24 0.94 0.90 1.21 1.05 1.10 1.37 1.37

K0III K0/K1III G6/G8III: K1III -- K3: G8IV G8III/IV G6/K0 G8/K1 K1III F8/G2IV/V K0III G8IV F0/F2IIIm G8IV/V G5V K1III G6/G8III G6/K0III: G8V K0/K2III: K0III G8/K0III G8/K0III: K1/K2III K0III G8/K0IV K0III G6/G8III K1III G8/K0III G8/K0III K1III G8III K0III G8III K1/K2III: K1III: K2III G8III/IV K2III K1/K2III: G8III: K0III G8III: G6/G8 G8/K0III K2III K2III K0III K0III K0III K0III: G8III G8/K0III K3III K2III

2 -13.5 2 -15.1 2 +7.4 2 -13.4 2 -43.2: SB: 2 -0.4 2 -18.5 2 +64.4 3 +86.8: 2 +19.5 2 +9.8 2 -45.7: 2 +67.4

2 0 +1.5 --

218864 219090 219357 221033 221331

-- K2/K3III K2III: K2/K3III: 2

Vel. km s-1 +2.1 SB?

HD V

(B-V) Type n

mag. mag. 8.87 1.26

Vel. km s-1 SB?

194185

2 -38.2 2 -54.4 2 +30.5

2 2

-8.1 +1.3

*194327R 8.63 0.89

194369H 8.44

194462 194606 194749 194945 195081 195415 195416 *195660 195885 196047 9.24 8.68 9.28 8.75 8.95 9.30 8.53 9.02 9.12 8.97

0.77 G5/G6III/IV

1.49 1.12 1.17 1.03 0.99 1.19 1.19 1.23 1.41 K3III: G8/K0III K2III G6III K0III K1III K0/K2p Ba K1III K1III 222261H 8.76 222513H 8.78 *222899H 8.50 222973H 8.89 223445 9.32 *223614H 8.56 *223646H 9.21 *223845 8.40 224248H 7.92

191 526 3096 3182 3615 9.11 9.01 9.01 9.24 9.21

2 +38.7 2 +16.7: SB: 2 -27.8 2 -12.0 2 +8.6 3 -38.6: SB:: 2 -22.6 2 -10.8

2 +54.5 2 +91.1: 2 +8.3 2 -18.6 2 +23.2

2 2

+4.8 -0.4

1.20 K1/K2IIICN+ 2 -19.3

1.20 1.25 1.09 0.95 1.45 G8III K1/K2III: K0/K1III G6/G8III K1/K2III: 2 +16.8 2 +2.2 2 +47.2 2 -18.6: SB: 2 +43.3

196082H 9.02 196103R 9.26 196315 8.96 196399H 8.87 196533H 8.52 197000H 8.85 197113H 8.51 197501H 9.30 197613 9.28 *197890R 9.44 198764R 8.94

199118 199174 9.33 9.01

4547H 8.80 5004 8.59

1.32 K0/K2IIICN+ 2 +12.1

*5193R 9.89 0.96

5489H 9.12

6674 6940 7262 7403 9.59 9.51 9.15 9.20

1.23 1.11 1.23 0.88 1.15

2 +38.7

2 2

-6.7 -1.0

K2III: K2III K0/K1III: K1/K2III G8/K0IV: K0III 2 +22.5 2 +9.0 2 +58.6: SB: 2 +23.8 2 +11.5 2 +0.6

2 +15.4 1 -47.8: 2 +10.5 2 -12.1

2 2 2

-8.4 +1.9 -4.5

*199242H 9.14 199387H 8.90

199474 199674S 200055 8.98 9.41 9.02

184581 *184626 184712 8.91 8.86 8.77

Area 16 1.14

1.47 1.04 1.11 0.94 1.07 1.10 1.14 1.42 1.18 1.32 1.05 0.99 0.85 0.97 1.06 1.14 1.19 0.86 1.48 1.22 1.14 1.13 1.05 1.05 0.98 1.30 1.24 1.10 0.94

2 +16.2 2 +34.8: SB: 2 -14.6 2 +25.2 2 -14.6: SB: 2 -26.3 2 +15.1 2 +10.4 2 +15.0 2 +55.2 2 -32.2: SB:: 2 -42.9 2 +12.9 2 -11.4 2 +71.3 2 +26.4 2 +46.6 2 +32.0: SB: 2 -27.4 2 +2.4 2 +56.2 2 +14.4 2 -32.6

2 2 2 -0.6 +4.4 -8.9

*186043H 8.93 *186058H 9.49

186245 186321 186581 187010 188159 *188202 9.15 9.64 9.66 9.26 8.91 9.05

188245H 8.63

188316 189120 9.36 9.25

189584H 8.78 *189855H 8.34

190288 191503 9.06 9.33

191847R 9.48 191865 8.62 191990H 9.04 191991H 8.71 192488H 8.92

192570 192631 193570 193604 193805 193806 193867 8.70 9.16 8.87 9.00 8.70 9.03 9.16

K0III K2/K3III G8/K0III K1III K1III K1III: G8/K0IV G8/K0III K2III K1III K2III K0III K0III/IV G8IV K0III K0III K1III/IV K1III K1/K2V K3III

4 -20.5: SB 4 -29.6 3 +15.0: SB: 2 +28.2 3 +21.4 3 -8.1 3 -35.0: SB: 2 +12.8 3 -5.1: SB: 3 -25.2 3 -63.1: SB:: 2 -12.4 2 -7.1 2 -24.5 3 -65.4

2 2 -0.1 -6.8

2 2 +3.1 +1.0

200096H 9.07

1.09 1.33 1.00 1.03 1.10 1.12 1.19 1.14 1.07 0.85 1.23 1.09 0.85 1.00 1.11 0.97 1.22 1.19 1.14 0.86 0.94 0.85 1.00 0.98 1.21 1.03 1.21 1.12 1.06 1.15

K1III K0V K0III/IV K2III K0III G8III K0III K1/K2III K2III K1III K0III G6/G8III G8/K0IV K0III K0V K0III K0III K0III K1III K2III K1III/IV G8III K0V K0V K1III G8/K0IV K1III K0III 2 -45.9 2 -26.7 2 +39.7 2 -39.9 2 -10.9 2 -20.4 2 +0.2 2 +76.3 2 +0.9 2 -16.3 3 +7.9: SB: 3 +43.5: SB: 2 +8.6 3 -73.8 2 -55.4 2 -34.8 2 -59.1 2 +11.1 3 +48.4 2 -21.2 2 +14.0 2 -32.7 2 -33.6 3 -1.9: SB: 2 -16.3 2 +4.2

0 2 -- +9.5

K1IIICN+ 2 -13.6

K3V K1III K1/K2III G8V K1III K1/K2III: K0IV G8III G8IV G8IV K3III K0III/IV G8III K0III 2 +28.0 2 +55.6 3 -33.0 2 -20.5 2 +2.5 3 +16.2 2 -45.2 3 -47.3 2 +6.4 2 +53.5 2 -13.1 2 -40.7

2 3 -9.6 -9.5

200143R 9.74 0.90

200144H 8.71

*200382 200420 9.77 9.17

200853H 8.47 200854H 8.94 200902H 8.94 200954H 8.44 201410H 8.79

201441 201885 9.40 8.83

1.15 0.79 0.96 1.02 1.00 1.00 1.52 1.05 0.90 0.97

*Note in Table 11



H or R

Magnitude from Tycho, not SIMBAD Hipparcos star

3 +15.7

K2IIICN+ 2 +24.0 K1III 2 +10.4 K2IIICN+ 2 +4.2

K0III G8III G8III K1III K1/K2III G8III K0III

2 -31.1 2 -4.5 2 +39.9 2 -22.5 2 -14.6 2 +31.0 2 -49.2

P

Stars rejected from pruned sample on account of: Proper motion > 0 .1 per annum

R Hipparcos parallax

S

 >

0 .006

Spectrum of class IVV or V

the star would be judged to possess if the classification were based solely on `the CN break and CN band strength'. It has long been known (e.g. Griffin & Redman 1960) that CN strength is not very well correlated with luminosity, so the extra component in some of the Michigan classifications does not represent additional information about luminosities but only about `CN anomalies'; we have abbreviated it in Table 10 by writing `CN+' where the luminosity class that would be judged from the CN strength would be brighter than the actual class assigned to the spectrum, and writing `CN-' where it would be fainter. It has come to our attention that SIMBAD does not always faithfully transcribe the spectral classifications from the Michigan catalogues. We have noticed cases in which a spread of types has been arbitrarily truncated or averaged into a single type, thereby conveying an incorrect impression of its certainty. We could quote as examples three out of four successive stars in Area 15: the Michigan types of HD 176772, 178736 and 182073 are G6/K0, G8/K1 and F8/G2 IV/V, but they are rendered in SIMBAD as G8, K0 and G0/G1 IV/V. There are also outright errors (or possibly omissions to substitute the modern types for the HD ones), as in the case of HD 47519 in Area 14, which is given as type K0 by SIMBAD but whose Michigan type of F6 V sits much more comfortably with its (B - V) colour index of 0.51 mag. Table 11, which runs continuously in HD order, contains what amounts to a set of footnotes to Table 10. Asterisks in Table 10 draw attention to the existence of entries in Table 11. One class of entry has already been noted at the end of Section 2 above  to point out close visual double stars; the components of such systems, if

C 2006 The Authors. Journal compilation C 2006 RAS, MNRAS 371, 11401158


1154 R. F. Griffin and A. P. Cornell

Table 11. Notes on individual stars.

HD 5193 (Area 15). as  Cen, etc. HD 21989 (Area 14).

Large bibliography in SIMBAD refers in fact to the bright Be star HR 5193; some of the entries do not even refer to it by that name but

Barium star, discovered by MacConnell, Frye & Upgren (1972), and classified as such by Houk & Cowley (1975). We had

opportunities to make only three radial-velocity measurements, but they are all mutually discordant and thereby confirm positively that it is an SB, as barium stars are expected to be. HD 23332 (Area 14). Metal-weak giant, recognized first by Bidelman & MacConnell (1973) and classified as such in the revision of the HD Catalogue (Houk & Cowley 1975).

HD 26046 (Area 14). HD 26615 (Area 14). HD 26777 (Area 13). HD 28753 (Area 13). HD 31341 (Area 13). v sin i = 6.9  1.1 km s-1. Faint companion seen at 3 arcsec, 340; previously recorded by Rossiter (1955). The 1970 SIMBAD bibliographic entry appears to refer to a different star (38 Ori). See (1898) 37, ADS 3282 A, companion 11.6 mag, 13 arcsec, 34. Discovered to be a `marginal barium star' by MacConnell et al. (1972) and repeatedly reaffirmed as such since. The barium character

was not recognized in the revision of the HD Catalogue (Houk 1982) and led to the assignment of a luminosity class that is too bright. Seven radial-velocity observations reasonably distributed over an interval of more than six years show no significant variation, and one measurement by Beavers & Eitter (1986) accords well with our value. The star has a 10.7-mag visual companion (cf. Table 8) whose velocity we have measured and which has proved to be a spectroscopic binary with a  -velocity identical with the mean radial velocity of the visual primary.

HD 31484 (Area 14). HD 33978 (Area 13). Faint companion seen at 22 arcsec, 276. Discovered early in our observations to be a short-period spectroscopic binary system; with the assistance of ESO observers we have

been able to establish a good double-lined orbit (described in Paper XVII, Griffin 2006) with a period of some 10 d. The folded light-curve (ESA 1997, vol. 12, p. A100) of the Hipparcos photometry shows a variation, doubtless arising from ellipticity of the primary star, at exactly half the orbital period. That was recognized by Koen, Laney & van Wyk (2002), who also discovered the corresponding radial-velocity variations. The system has received the variable-star designation VV Lep. It is also a visual double star, van den Bos (1928) 81, ADS 3804; the companion has been estimated at 13 mag and is only 2 arcsec away from the primary. HD 34659 (Area 13). Double star, Coo 29 (Innes 1905), ADS 3892, with almost equal K-dwarf components 4 arcsec apart, both measured by us (cf. Tables 4 and 8) and found to have similar radial velocities. Hipparcos found substantial photometric variations; the period and type of variability were not determined by Hipparcos itself, but in the Inf. Bull. Variable Stars name-list (Kazarovets et al. 1999) in which it was designated VW Col it is listed as type EA (`Algol type eclipsing variables'). A plot of its (Hp) magnitude against time looks most unusual: there is an upper limit to the envelope at about 9.2 mag, but the majority of points are not clustered just near it as might be expected for an Algol system  the distribution thins out only gradually towards fainter magnitudes, with the faintest one being at 11.6 mag and having only a small error bar. Especially in the context of the apparent constancy of radial velocity, the photometry presents an interesting puzzle. If any periodicity could be found, it would be likely to have been reported by Koen & Eyer (2002). HD 35164 (Area 13). ADS 3954 C, distant optical companion at 58 arcsec, 104 to HR 1771 (which is called 41 Lep in ADS; it is in Lepus, but the RA is between those of 7 and 8 Lep and the numbering in that constellation goes only to 19). HD 35993 (Area 13). Barium star, discovered by MacConnell et al. (1972), classified as such by Houk & Smith-Moore (1988), and duly found by us to be a spectroscopic binary, whose orbit is given in Paper XVII (Griffin 2006).

HD 36745 (Area 13). recently. HD 37730 (Area 14). Very close visual binary, ADS 4153, not resolved in our observations; visual orbit very eccentric, P  70 yr, periastron passage just Visual companion (cf. Table 8) is a binary of short period and large amplitude; it has a v sin i of 10  3 km s-1. Regrettably the

authors have had no opportunity to determine the orbit.

HD 40293 (Area 14). HD 41023 (Area 14). HD 44627 (Area 14). HD 47519 (Area 14). HD 47951 (Area 14). HD 90167 (Area 6). Classified M3.5 III by Frishberg (1975); presumably misidentified. IDS lists 13-mag companion (Herschel 1847, p. 186) at 21.2 arcsec, 354. Small-amplitude variable star AB Pic, possibly of BY Dra type; now known to possess a low-mass companion (Chauvin et al. 2005). Very blue (F6 V), feeble radial-velocity dip, v sin i = 7.5  2.5 km s-1. All velocities rather uncertain. M giant with seemingly irregular photometric variations; V446 Car. Discovered to be a `marginal barium star' by MacConnell et al. (1972) and repeatedly reaffirmed as such since. The barium character

was not recognized in the revision of the HD Catalogue (Houk & Smith-Moore 1988) and led to the assignment of a luminosity class that is too bright. Three radial-velocity observations in different years show no discordance.

HD 91064 (Area 6). HD 92789 (Area 6). ADS 7806 A; 13-mag companion (Herschel 1847, p. 203) at 14 arcsec, 100. v sin i = 10.3  0.7 km s-1.

HD 92830, 92920 (Area 6). Although the stars are only 10 arcmin apart and have similar radial velocities, they are unrelated, having quite different

spectroscopic parallaxes and proper motions.

HD 94428 (Area 6). HD 96768 B (Area 6). HD 96873 (Area 6). HD 99426 (Area 6). HD 99552 (Area 6). IDS lists 15-mag companion (Donner 1955) at 5.7 arcsec, 300. v sin i = 12  5 km s-1. IDS lists 11.5-mag companion (van den Bos 1951) at 0.5 arcsec, 222. Particularly faint, and early type; all observations rather poor. IDS lists 15-mag companion (van den Bos 1929) at 3.2 arcsec, 16.

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Table 11  continued HD 111680 (Area 7).

Identified as a `strong-CN' star by Houk (1982). Adopted by Keenan (Keenan & Yorka 1988; Keenan & McNeil 1989) as an MK

standard star of type K1 III Fe 1, although he had previously (Keenan 1987) noted it as K1 III CN 1 and remarked (Keenan, Yorka & Wilson 1987) that for only a few of the Houk strong-CN stars is an abnormal strength of the iron lines so noticeable that they need to be distinguished by positive indices.

HD 112402 (Area 7). HD 114483 (Area 7). HD 116463 (Area 7). Early type; feeble radial-velocity dips, so poor accuracy. v sin i = 14.1  0.6 km s-1; velocities therefore rather poor. IDS lists 12.5-mag companion (van den Bos 1930) at 8.4 arcsec, 10.

HD 116858, 116920 (Area 7). HD 116858 long recognized as a nearby dwarf, Gliese 511 (Gliese 1969). Van den Bergh (1958) pointed out, from the entries

in the Yale Zone Catalogues, the common-proper-motion companion HD 116920 about 5 arcmin distant, which he reported as having also a similar radial velocity, as indeed we confirm here.

HD 117987 (Area 7). HD 118597 (Area 7). HD 119188 B (Area 7). HD 119321 (Area 7). HD 120013 (Area 7). HD 120304 (Area 7). HD 120571 (Area 7). Known as a `proper-motion star',  almost 0.6 arcsec per annum. Companion at 25 arcsec, 127, with no dip in radial-velocity trace, presumably early type. v sin i = 10  4 km s-1. Crifo et al. (1992) pointed out an error in the SAO proper motion. ADS 9024, wide optical double (Hough 1894), companion approx. 18 arcsec, 171. Type B7B9, evidently misidentified (Sundman, Loden & Nordstrom 1974). Discovered to be a `certain barium star' by MacConnell et al. (1972) and repeatedly reaffirmed as such since. The barium character

was not recognized in the revision of the HD Catalogue (Houk & Smith-Moore 1988) and led to the assignment of a luminosity class that is too bright. Our two radial-velocity observations show no change but were taken only one year apart; two measurements by Catchpole, Robertson & Warren (1977) show a 14 km s-1 mutual discordance that may be significant.

HD 121552 (Area 7). HD 122055 (Area 7). IDS lists 11.7-mag companion (van den Bos 1931) at 1.7 arcsec, 176. Discovered by Hipparcos to be a photometric variable, now designated MQ Vir, type LB (`slow irregular variable of late spectral

type'). Koen & Eyer (2002) claimed to find a 120-d periodicity that had escaped Hipparcos. v sin i = 8.9  1.1 km s-1.

HD 125169 (Area 7). HD 125268 (Area 7). HD 125493 (Area 7). HD 176772 (Area 15). HD 182073 (Area 15). Wide visual double (Herschel 1847, p. 216), 11.9-mag companion at 18 arcsec, 23. The SIMBAD bibliographic entry appears to refer to a different star (HD 122563). Rossiter (1955) discovered a very faint companion at 4 arcsec, 82. Feeble radial-velocity dip, weaker than would normally correspond to its colour index and spectral type. Velocities uncertain. Very weak and unquantifiably wide radial-velocity dip.

HD 184650 (= `HD 184626 B') (Area 16).

HD 186043 (Area 16). 325. HD 186058 (Area 16).

v sin i = 17  3 km s-1.

See (1898) listed a 12-mag companion at about 10 arcsec, 130. There is a brighter star (HD 186032, 8.26 mag, A1 V) at 135 arcsec, Wilhelmina Fleming (Pickering & Fleming 1896) noted this star as type B2p with H in emission, but it has since appeared to be a

normal K star. Hoffleit (1975) managed to retrieve the very plate which was the basis for Fleming's classification and found it to show almost nothing.

HD 188202 (Area 16). HD 189855 (Area 16). Stoy (1962). HD 194327 (Area 16). HD 195477 (Area 15). HD 195660 (Area 16). HD 197890 (Area 16). Type O9.5 III (Peton et al. 1972), evidently misidentified. Several mentions in the literature arising from its adoption as a photometric standard in one of the Cape `E regions' by Cousins & Close (0.3 arcsec) and nearly equal visual double star (Innes 1948), motion 2 per year. Faint companion seen at 17 arcsec, 116. Faint companion seen at 47 arcsec, 59. Variable star BO Mic, `Speedy Mic', very rapid rotation, very large literature (more than 60 items in SIMBAD since 1992 when its

rotational velocity was first recognized). See text, end of Section 5.

HD 199242 (Area 16). HD 200382 (Area 16). HD 210009 (Area 15). HD 218109 (Area 15). HD 222899 (Area 15). HD 223614 (Area 15). HD 223646 (Area 15).

Listed as a subdwarf by Carney (1978). Much too blue for its classification of K1/K2 III; listed by Nordstrom Faint companion seen at 42 arcsec, 350. Very faint companion seen at 17 arcsec, 327.

et al. (2004) as having MV = 6.18 mag.

May be SB2  discrepancies in width and depth of dip as well as in velocity. Very unequal Hipparcos double star; 12.3-mag companion at 0.43 arcsec, 184. Discovered as a barium star in the revision of the HD Catalogue by Houk & Cowley (1975). Our radial velocities are modestly

discordant but represent only two epochs, so in the spirit of the third paragraph of Section 4 above we can note the object only as a `possible SB', although in the light of the barium nature of the star the discordance could be seen as confirming the expectation that it is a spectroscopic binary. HD 223845 (Area 15). Faint companion seen at 43 arcsec, 339.

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1156 R. F. Griffin and A. P. Cornell

not themselves binaries, are likely to have radial velocities that are so similar to one another that the measured velocity is some sort of a mean between the velocities of the two components, weighted according to their brightnesses and the characters of their respective spectra. We have retrieved the SIMBAD entries, including bibliographies, for all the stars observed on this programme; the total amount of astrophysically interesting information about them is remarkably small, and that makes it altogether practicable to note it in Table 11. Rotational velocities above 5 km s-1 are exceptional for late-type stars, and in cases where they do occur they are often indicators of duplicity, with (pseudo-)synchronized orbital and rotational periods, and/or the cause of BY Dra or RS CVn variability that arises from star-spots. Projected rotational velocities are routinely derived from all Coravel radial-velocity traces, and where the mean value for any star exceeds 5 km s-1 by more than its standard error the v sin i value is noted in Table 11. Table 10 includes three stars for which we were unable to measure any velocity at all. We knew that there must be something very odd about HD 197890, whose spectral type of K0 V was supported by its colour index, but whose radial-velocity trace showed no dip. At our request, therefore, a South African Astronomical Observatory observer obtained spectra of the star in 1988, and reported that they showed a normal K-star spectrum  but the enormous rotational velocity that had smeared out the lines in radial-velocity traces into invisibility and was later recognized by Bromage et al. (1992) was overlooked. The failures on HD 119451 and 186425 are readily explained by their A7/A8 and F0/F2 spectral types, which are far too early to give good correlation dips with the Coravel, whose mask was designed on the basis of the spectrum of Arcturus (K2 III), and are probably compounded with rapid rotation. Additionally, HD 182073 was barely measurable, with very weak and wide dips, owing to its rather early type (F8/G2) and high rotational velocity. 6 M E A N V E L O C I T I E S A N D V E L O C I T Y D I S P E R S I O N S B Y A R E A Although there is much of interest in the radial velocities of the individual stars, yet we must recall that the original motivation for the Clube programme was to establish the mean velocities and their dispersions in the 16 systematically selected Areas, of which in fact only six feature in the present paper. Those final results are presented in Table 12. They are given, first, with all the measured Clube stars being included, and secondly, with the exclusion of those stars that we believe to be near the main sequence or at any rate to have substantially lower luminosities (and therefore to be a lot nearer to us) than they would if they were giants. The first method is analogous to the one that was necessarily adopted, in the absence of two-dimensional spectral types, for the 10 northern Areas treated in Paper XIII, but the second is considered to be more in keeping with the underlying intention of the project, which is to do with the statistical kinematics of groups of stars at a significant distance from us in the various directions. The omission of the rejected stars is seen not to make a great deal of difference to the final results, so it can confidently be expected that the principal results given in Paper XIII for the 10 northern Areas, too, are not significantly jeopardized by the inevitable inclusion there of a minority of relatively nearby stars. The mean velocities of all stars have been given equal weight in the derivations of the means and dispersions given in Table 12, because (as remarked in Section 5 above) the uncertainties in any of the stellar velocities, even those marked with a colon in Table 10, are trivial in comparison with the actual velocity dispersions within any Area. We have not specified individually the standard errors of the quoted velocity dispersions, but, provided that the distributions of the underlying velocities do not depart too much from the`normal', each of them is assessed statistically to be the fraction 1/ 2n of the dispersion itself. With the dispersions and numbers of stars reported here, the standard errors are all within quite a small range centred near 2 km s-1. In deciding which stars to omit in the second method, our initial inclination was to reject all those whose luminosity classifications are Class IV or fainter. We noticed, however, that where Hipparcos parallaxes are available stars classified as Class IV appear in many instances not to be significantly nearer to us than many of those called Class III. Class V stars, however, really are relatively nearby in most cases, so we decided in the end to reject on the basis of their Michigan types only the stars with luminosity classes given as IV/V and V. We have, however, tried to improve the segregation of the programme stars into giant and dwarf groups by considering other criteria, as described in the next two paragraphs. In the first place, we have regarded the Hipparcos parallaxes as superseding the luminosity classifications, so in the few instances where a `Class III' star is found to have a parallax more appropriate to a dwarf it has been omitted from the statistics in the second assessment, whereas the few `Class V' stars whose parallaxes show them not really to be dwarfs are restored to favour and retained in the second set of statistics. That form of vetting can, of course, be applied only to those of our stars, in number 206, that feature in the Hipparcos catalogue. Further to assist the interested reader, we have flagged with a superscript H (or R, as we shall shortly explain) all the Hipparcos stars in Table 10. We gave consideration to tabulating explicitly the parallaxes of all those stars, but decided against it, because typical values are only two or three milliseconds of arc and their standard deviations are typically one millisecond, so there is not a lot of information in the individual values for the giant stars, although it is satisfactory to see that statistically those stars evidently have distances (and therefore absolute magnitudes) close to the expected values. Where the parallaxes begin to become individually reliable, above values of say 0.005 arcsec, is also

Table 12. Synopsis of radial-velocity results  mean velocities and velocity dispersions by Area.

Dwarfs excluded

No. of obs.

Area b 

+35 +35 -35 -35 -35 -35

l 

270 315 225 270 315 360

No. of stars No. of obs.

6 7 13 14 15 16 97 130 91 151 84 72 485 510 480 460 169 166

All stars Mean velocity km s-1 +10.1  2.3 -4.9  2.5 +27.2  3.1 +20.1  2.0 +6.9  3.4 -7.1  3.6

Vel. disp. km s-1 22.2 28.4 29.0 24.6 30.6 30.4

No. of stars

76 113 86 137 74 66 355 442 465 417 148 154

Mean velocity km s-1 +7.4  2.4 -4.4  2.6 +28.7  3.1 +18.1  2.0 +4.7  3.3 -6.8  3.8 Vel. disp. km s-1 20.5 27.6 28.9 23.3 28.3 30.7

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Table 13. Stars that we believe to have erroneous Michigan luminosity classes.

Area HD Sp. Type

1157

6

7

13 14

15

90167 97260 98020 112905 120391 122350 122509 27678 28002 41094 44325 5193 207046 215587 K0 II K0/K1 III K1 III G8 V G6/G8 V G8/K0 V G8 V K1 III G8 III K0 II/III K1 III K2 III: G6/G8 III K0 III

V mag 8.39 9.99 8.81 9.51 9.46 9.60 9.79 8.52 8.76 8.44 8.71 9.89 8.16 8.40 (B - V ) mag 0.97 0.89 1.00 0.91 0.79 0.83 1.20 1.00 0.91 1.00 1.00 0.96 0.88 0.94

 (0.001 arcsec) 3.60 m - M mag 7.2 MV mag 1.2

1.32 3.78 4.77 1.34 6.26 8.58 16.93 6.99 8.54 9.4 7.11 6.60 9.4 6.01 5.33 3.85 5.78 5.34 0.1 2.35 3.00 0.4 2.75 3.38 6.04 2.38 3.06

 (0.001 arcsec yr-1) 26 105 116 38 84 13 29 212 11 104 90 219 74 42

where they indicate that the stars concerned are nearer than the Clube selection criteria would ideally have accepted for this programme. We have therefore flagged with an R (for `Rejected'), instead of with an H, such stars as have Hipparcos parallaxes such that  - () > 0.005 arcsec. There are 34 of them  almost one-sixth of the whole number of Hipparcos stars on the Clube programme. It does not follow, however, that that proportion is typical of the whole programme, because the stars observed by Hipparcos were specifically selected, many of them individually, before the start of the mission, and one major reason why known dwarfs would have been selected would have been to determine good distances and luminosities for them. The second auxiliary means of vetting the programme stars for dwarf interlopers is by proper motions, which are available for all the stars from Tycho and/or ground-based measurements, and usually very accurately from a combination of both in Tycho 2 (Hg et al. 2000). A giant star with MV  +1 and an apparent magnitude about 9 must be at a distance of 400 pc, at which an annual proper motion of 0.1 arcsec implies a transverse motion of nearly 200 km s-1. There is not even one star among those observed here that has a radial velocity as high as 100 km s-1.1 Accordingly, we can deem without fear of significant error that any star with an annual proper motion as high as 0.1 arcsec is extremely likely to be a lot nearer to us than the 400 pc expected for giants, and is therefore to be rejected from our pruned sample. Stars thus rejected on the basis of their proper motions are flagged in Table 10 with a superscript P. In order to make it quite clear which stars have been rejected from our pruned sample, we have also used the superscript S in Table 10 to identify stars omitted on the basis that their Michigan spectral classifications are in luminosity classes IV/V or V; where the proper motions and the spectral types both warrant rejection, both superscripts (P and S) are given. In many cases where stars are rejected on account of their parallaxes, rejection is supported by their dwarf classifications and/or proper motions, but we have not thought it necessary to indicate such support since the parallax speaks quantitatively for itself. For convenience of reference to stars that we regard as having distinctly erroneous luminosity classifications in the Michigan catalogues, we list in Table 13 (an inadvertent but not inappropriate coincidence!) those stars that are attributed luminosity class III but whose parallaxes show, or whose proper motions indicate, them to be of significantly lower luminosity, and also those stars that have dwarf classifications but whose parallaxes show them to be brighter. Among the stars with Hipparcos parallaxes, three `giants' and two `dwarfs' are demonstrated to be subgiants (luminosity class IV), one `giant' is shown to be a main-sequence star, and two `dwarfs' are shown really to be giants. Proper motions in excess of 0.1 arcsec per annum cast serious doubts on the luminosity classifications of a few additional `giants'. There are actually only four of them, three of which are only just over the 0.1-arcsec limit; one additional one that is well above that limit belongs to a star (HD 5193) that is also shown definitely by its parallax to be a main-sequence star and whose luminosity class is in any case qualified by a colon in the Michigan catalogue (Houk & Cowley 1975). We have refrained from reading decisive significance into very small proper motions, even for stars supposed to be dwarfs, because there is always some possibility of a fortuitously small value of the transverse velocity. We nevertheless harbour our own suspicions about several stars. For example, HD 121552 is classified as G8 V, but it is much too red for such a type: its (B - V) of 1.01 mag would be much more accordant with a type of G8 III, at which its annual proper motion of only 0.013 arcsec, too, would be unremarkable. It must, however, be commented that, although we consider that we have pinpointed a few errors in the Michigan classifications and have some grounds for questioning a few others, perhaps more significant even than the content of Table 13 is its brevity, which underlines the general reliability of the published luminosity classes.

1

The highest, without regard to sign, is the +99.1 km s-1 of HD 94428,

and there are nine others with  > +90 km s-1, but the distribution of high velocities is very skew, the highest negative one being the -73.8 km s-1 of HD 196082. It may be recalled that the solar apex is at a considerable northern declination, so it is not surprising if radial velocities of southernhemisphere stars tend to be positive.

AC K N OW L E D G M E N T S We are most grateful to ESO for providing observing time and technical support on the 61-inch Danish telescope at La Silla for this project, and to Dr M. Mayor and the Observatoire de Genev` e for allowing the use of their excellent `Coravel' radial-velocity spectrometers. We thank Dr B. D. Mason of the US Naval Observatory for his prompt amd willing assistance in connection with the literature on visual double stars. We would never have been able to submit

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1158 R. F. Griffin and A. P. Cornell

this paper without the kind assistance of Dr L. Jardine-Wright in complying with the technical requirements of the submission procedure. RFG is indebted to the SERC and its successor PPARC for defraying the costs of the observing visits, and is pleased to acknowledge the assistance of Dr R. E. M. Griffin on two of the five visits. Although both the authors have been acting in a voluntary capacity in the writing of this paper, we acknowledge with thanks the facilities that have been accorded to us at the Cambridge Observatories.

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