2003A&A...410..871C


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.14CEST14:37:42

2003A&A...410..871C - Astronomy and Astrophysics, volume 410, 871-878 (2003/11-2)

RR Lyrae variables in Galactic globular clusters. I. The observational scenario.

CASTELLANI M., CAPUTO F. and CASTELLANI V.

Abstract (from CDS):

In this paper we revisit observational data concerning RR Lyrae stars in Galactic globular clusters, presenting frequency histograms of fundamentalized periods for the 32 clusters having more than 12 pulsators with well recognized period and pulsation mode. One finds that the range of fundamentalized periods covered by the variables in a given cluster remains fairly constant in varying the cluster metallicity all over the metallicity range spanned by the cluster sample, with the only two exceptions given by M 15 and NGC 6441. We conclude that the width in temperature of the RR Lyrae instability strip appears largely independent of the cluster metallicity. At the same time, it appears that the fundamentalized periods are not affected by the predicted variation of pulsators luminosity with metal abundance, indicating the occurrence of a correlated variation in the pulsator mass. We discuss mean periods in a selected sample of statistically significant ``RR rich" clusters with no less than 10 RRab and 5 RRc variables. One finds a clear evidence for the well known Oosterhoff dichotomy in the mean period <Pab> of ab-type variables, together with a similarly clear evidence for a constancy of the mean fundamentalized period <Pf> in passing from Oosterhoff type II to type I clusters. On this basis, the origin of the Oosterhoff dichotomy is discussed, presenting evidence against a strong dependence of the RR Lyrae luminosity on the metal content. On the contrary, I) the continuity of the mean fundamentalized period, II) the period frequency histograms in the two prototypes M 3 (type I) and M 15 (type II), III) the relative abundance of first overtone pulsators, and iv) the observed difference between mean fundamental <Pab> and fundamentalized periods <Pf>, all agree in suggesting the dominant occurrence of a variation in the pulsation mode in a middle region of the instability strip (the ``OR" zone), where variables of Oosterhoff type I and type II clusters are pulsating in the fundamental or first overtone mode, respectively.

Abstract Copyright:

Journal keyword(s): stars: variables: RR Lyr - stars: evolution - stars: horizontal-branch

Simbad objects: 43

goto Full paper

goto View the reference in ADS

Number of rows : 43

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 288 GlC 00 52 45.24 -26 34 57.4   10 8.13     ~ 951 0
2 NGC 1261 GlC 03 12 16.21 -55 12 58.4     8.63     ~ 445 0
3 NGC 1851 GlC 05 14 06.76 -40 02 47.6   8.80 7.23     ~ 1279 0
4 M 79 GlC 05 24 10.59 -24 31 27.3   9.21 8.16     ~ 738 0
5 NGC 2298 GlC 06 48 59.41 -36 00 19.1   10.77 8.89     ~ 444 0
6 NGC 2419 GlC 07 38 08.51 +38 52 54.9     10.05     ~ 844 0
7 NGC 3201 GlC 10 17 36.82 -46 24 44.9           ~ 760 0
8 NGC 4147 GlC 12 10 06.149 +18 32 31.78   11.45 10.74     ~ 511 0
9 M 68 GlC 12 39 27.98 -26 44 38.6   10.26 7.96     ~ 906 0
10 NGC 4833 GlC 12 59 33.92 -70 52 35.4   8.72 7.79     ~ 369 0
11 M 53 GlC 13 12 55.25 +18 10 05.4   8.95 7.79     ~ 742 0
12 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2313 0
13 NGC 5286 GlC 13 46 26.81 -51 22 27.3   9.18 8.31     ~ 385 0
14 NGC 5466 GlC 14 05 27.29 +28 32 04.0   10.5 9.70     ~ 749 0
15 IC 4499 GlC 15 00 18.57 -82 12 49.6     8.56     ~ 320 0
16 NGC 5824 GlC 15 03 58.612 -33 04 06.70   10.28 9.56     ~ 356 0
17 NGC 5897 GlC 15 17 24.40 -21 00 36.4   10.16 8.52     ~ 349 0
18 M 5 GlC 15 18 33.22 +02 04 51.7   7.34 5.95     ~ 1815 0
19 NGC 5986 GlC 15 46 03.00 -37 47 11.1     6.92     ~ 322 0
20 M 80 GlC 16 17 02.41 -22 58 33.9           ~ 643 0
21 M 4 GlC 16 23 35.22 -26 31 32.7           ~ 1713 0
22 M 107 GlC 16 32 31.86 -13 03 13.6   9.96 8.85     ~ 727 0
23 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2047 0
24 NGC 6229 GlC 16 46 58.641 +47 31 36.38   9.38 9.86     ~ 325 0
25 NGC 6235 GlC 16 53 25.36 -22 10 38.8   11.99 7.20     ~ 165 0
26 M 62 GlC 17 01 12.60 -30 06 44.5   8.55 7.39     ~ 535 0
27 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 1943 0
28 M 9 GlC 17 19 11.78 -18 30 58.5   9.36 8.42     ~ 285 0
29 NGC 6362 GlC 17 31 54.99 -67 02 54.0   9.72 8.86     ~ 506 0
30 M 14 GlC 17 37 36.15 -03 14 45.3   9.55 5.73     ~ 328 0
31 NGC 6441 GlC 17 50 13.06 -37 03 05.2   9.26 8.00     ~ 793 0
32 NGC 6584 GlC 18 18 37.60 -52 12 56.8   10.32 8.17     ~ 256 0
33 M 28 GlC 18 24 32.89 -24 52 11.4           ~ 684 0
34 M 22 GlC 18 36 23.94 -23 54 17.1   7.16 6.17     ~ 1252 0
35 M 70 GlC 18 43 12.76 -32 17 31.6   9.76 9.06     ~ 344 0
36 M 54 GlC 18 55 03.33 -30 28 47.5           ~ 943 0
37 NGC 6723 GlC 18 59 33.15 -36 37 56.1           ~ 446 0
38 M 55 GlC 19 39 59.71 -30 57 53.1     6.49     ~ 780 0
39 NGC 6934 GlC 20 34 11.37 +07 24 16.1   10.48 9.75     ~ 374 0
40 NGC 7006 GlC 21 01 29.465 +16 11 16.49     10.46     ~ 493 0
41 M 15 GlC 21 29 58.33 +12 10 01.2   3       ~ 2958 0
42 M 2 GlC 21 33 27.02 -00 49 23.7     6.25     ~ 928 1
43 NGC 7492 GlC 23 08 26.68 -15 36 41.3     10.48     ~ 268 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2003A&A...410..871C and select 'bookmark this link' or equivalent in the popup menu


2021.05.14-14:37:42

© Université de Strasbourg/CNRS

    • Contact