For the rotating evolved stars, one of the best known properties is that these ones rotate slowly, but little is known in detail. Herbig & Spalding ([1953], [1955]) have shown that a cutoff in the distribution of rotational velocities seems to be present in subgiant and giant stars, near the spectral type G0. Essentially, these authors pointed out that rotation rates decrease from late F-type toward early G-type stars in those luminosity classes.
In general, the pioneering works could only predict upper limits for the
rotation rates of evolved stars. Uesugi & Fukuda ([1982])
have compiled
102 sources of data for 6472 stars. Although, among the stars quoted by
these authors, there are for about 10% of G and K-type evolved stars with
rotational velocity values, the vast majority of these measurements are
unreliable, since the techniques used for these observations presented modest
resolution, larger than what we know today to be the mean rotational velocities for
these stars. In some cases, such as Herbig & Spalding
([1953], [1955]), Oke &
Greenstein ([1954]), Huang ([1953]) and Alschuler ([1975]),
the limits are typically
near 20 km s-1. Kraft ([1965]) predicted limits
to 6.0 km s-1 for the
Hyades giants and to 10.0 km s-1 for the yellow giants of NGC 2281 and
NGC 6633. Most recently, D. Gray and co-workers obtained rotational
velocities for about 170 stars of luminosity classes IV through Ib, from
high-resolution spectroscopic observations (Gray [1989]; Gray
& Nagar [1985]; Gray & Toner [1986], [1987]),
by using the Fourier deconvolution technique on single
line profiles. These authors have obtained very accurate
values, with
typical velocity resolution of about 0.5 to 2.0 km s-1.
These observations
concern mostly stars of spectral types G and K. Fekel (1997) has also obtained
rotational velocity
for about 60 evolved stars into the luminosity
classes IV, III and II. As one can see from the works by D. Gray and co-workers,
M. Mayor and co-workers and F. Fekel, rotation rates of the large majority of
G and K stars are actually several times smaller than the
20 kms-1 upper limits
set by the early works.
Admittedly, extensive surveys of at high resolution are needed for the
best comprehension of the rotational behaviour of evolved stars because, up to
the present, the paucity of the samples have prevented a complete statistical
analysis.
HD | ![]() |
![]() |
remark |
(Gray) | (COR) | ||
87 | 3.8 | 3.8 | SB |
2114 | 3.9 | 3.2 | |
2507 | 4.2 | 4.4 | |
3546 | 2.5 | 4.2 | SB |
3817 | 3.2 | 1.7 | |
7672 | 4.5 | 2.9 | SB |
10761 | 2.9 | 2.1 | |
12929 | 3.1 | 1.0 | SB |
17878 | 3.6 | 2.6 | SB |
20825 | 7.9 | 8.0 | |
21120 | 4.8 | 5.9 | SB |
27348 | 3.1 | 1.8 | |
27371 | 2.4 | 1.0 | |
27697 | 2.5 | 1.2 | SB |
28305 | 2.5 | 2.4 | |
28307 | 3.4 | 1.5 | |
51000 | 4.7 | 4.0 | |
62509 | 2.5 | 1.0 | |
65448 | 2.4 | 2.5 | SB |
71369 | 2.4 | 4.3 | SB |
72561 | 3.8 | 6.0 | |
74485 | 6.0 | 6.6 | |
79452 | 4.6 | 4.5 | |
82210 | 4.9 | 5.5 | |
82328 | 6.4 | 8.3 | SB? |
85945 | 6.2 | 6.2 | |
89485 | 2.7 | 1.1 | |
94481 | 3.9 | 2.8 | |
95689 | 2.6 | 1.6 | SB |
113994 | 1.8 | 1.0 | |
119445 | 6.0 | 6.9 | |
119458 | 4.9 | 4.0 | SB |
124850 | 15 | 14.8 | |
124897 | 2.4 | 1.0 | |
130259 | 5.6 | 4.9 | |
133208 | 3.4 | 2.5 | |
135722 | 1.1 | 1.2 | SB |
140573 | 0.0 | 1.6 | |
142980 | 1.1 | 1.0 | SB |
144608 | 3.5 | 1.4 | |
147266 | 2.5 | 1.2 | |
148387 | 2.2 | 1.6 | |
148856 | 3,4 | 4,8 | SB |
150997 | 2.2 | 1.7 | |
151627 | 4.7 | 4.1 | SB |
153751 | 24 | 23 | SB |
157910 | 3.6 | 4.1 | |
160781 | 4.5 | 4.5 | |
161096 | 1.6 | 1.0 | |
161239 | 5.4 | 5.9 | |
161797 | 1.2 | 1.7 | SB? |
163993 | 3.5 | 3.2 | |
165760 | 3.9 | 2.2 | |
167768 | 4.6 | 3.9 | |
168656 | 2.6 | 1.0 | |
173920 | 7.7 | 8.0 |
HD | ![]() |
![]() |
remark |
(Gray) | (COR) | ||
182572 | 2.3 | 1.7 | |
185758 | 5.8 | 7.1 | SB |
185958 | 9.1 | 9.9 | |
186675 | 3.1 | 1.7 | |
188119 | 1.1 | 1.2 | |
188512 | 1.8 | 1.2 | |
194577 | 4.7 | 3.3 | |
196524 | 40.0 | 49.8 | SB |
196755 | 3.3 | 3.3 | |
197964 | 2.8 | 1.0 | |
197989 | 3.0 | 1.4 | SB |
198149 | 1.5 | 1.4 | |
198809 | 5.9 | 4.7 | |
200039 | 2.8 | 1.0 | |
200253 | 4.7 | 3.0 | |
202109 | 3.4 | 1.0 | |
203574 | 2.4 | 1.0 | |
205435 | 2.7 | 1.9 | |
208110 | 4.0 | 3.3 | |
210220 | 3.4 | 1.8 | |
214558 | 4.1 | 1.4 | |
215665 | 7.8 | 7.5 | |
216131 | 2.6 | 1.2 | |
218658 | 4.7 | 5.5 | |
219615 | 0.0 | 1.6 | |
220858 | 2.6 | 1.0 | |
221115 | 3.1 | 1.5 | |
222404 | 0.0 | 1.0 | SB? |
Since March 1986 we have undertaken at Geneva Observatory a vast observational program to obtain rotational velocities for a well-defined sample of evolved stars of luminosity classes IV, III, II and Ib/Ib-II large enough to allow a reliable study of their rotational characteristics. This paper presents the results of the survey, concerning essentially the observations for the subgiant, giant and bright giant stars. The results for the supergiants Ib/Ib-II will be published in a forthcoming supplement catalog. Although the initial aim of the present work is the study of the rotational behaviour of evolved stars our observational procedure has produced about 4000 radial velocity measurements. When this survey was planned, there were still some 30% of class II giant and Ib supergiant stars from our selected sample for which no radial velocity measurements were available. The present paper brings such information for these stars.
This catalog is arranged as follows. Section 2 presents the definition of the
sample, the observational procedure used throughout this survey, the
calibration
of rotation rate values, with a discussion of their probable errors and a
comparison of our measurements with those obtained by using other high
resolution techniques. The list of the individual
measurements and the
mean radial velocity values are presented in Sect. 3.
Copyright The European Southern Observatory (ESO)