2003A&A...408..529G


Query : 2003A&A...408..529G

2003A&A...408..529G - Astronomy and Astrophysics, volume 408, 529-543 (2003/9-3)

Distances and ages of NGC 6397, NGC 6752 and 47 Tuc.

GRATTON R.G., BRAGAGLIA A., CARRETTA E., CLEMENTINI G., DESIDERA S., GRUNDAHL F. and LUCATELLO S.

Abstract (from CDS):

New improved distances and absolute ages for the Galactic globular clusters NGC 6397, NGC 6752, and 47 Tuc are obtained using the Main Sequence Fitting Method. We derived accurate estimates of reddening and metal abundance for these three clusters using a strictly differential procedure, where the Johnson B-V and Stroemgren b-y colours and UVES high resolution spectra of turn-off stars and early subgiants belonging to the clusters were compared to similar data for field subdwarfs with accurate parallaxes measured by Hipparcos. The use of a reddening free temperature indicator (the profile of Hα) allowed us to reduce the error bars in reddening determinations to about 0.005mag, and in metal abundances to 0.04 dex, in the scales defined by the local subdwarfs. Error bars in distances are then reduced to about 0.07mag for each cluster, yielding ages with typical random errors of about 1Gyr. We find that NGC 6397 and NGC 6752 have ages of 13.9±1.1 and 13.8±1.1Gyr respectively, when standard isochrones without microscopic diffusion are used, while 47 Tuc is probably about 2.6Gyr younger, in agreement with results obtained by other techniques sensitive to relative ages. If we use models that include the effects of sedimentation due to microscopic diffusion in agreement with our observations of NGC 6397, and take into account various sources of possible systematic errors with a statistical approach, we conclude that the age of the oldest globular clusters in the Galaxy is 13.4±0.8± 0.6Gyr, where the first error bar accounts for random effects, and the second one for systematic errors. This age estimate is fully compatible with the very recent results from WMAP, and indicates that the oldest Galactic globular clusters formed within the first 1.7Gyr after the Big Bang, corresponding to a redshift of z≥2.5, in a standard ΛCDM model. The epoch of formation of the (inner halo) globular clusters lasted about 2.6 Gyr, ending at a time corresponding to a redshift of z≥1.3. On the other hand, our new age estimate once combined with values of H0 given by WMAP and by the HST Key Project, provides a robust upper limit at 95% level of confidence of ΩM<0.57, independently of type Ia SNe, and strongly supports the need for a dark energy. The new cluster distances lead to new estimates of the horizontal branch luminosity, that may be used to derive the zero point of the relation between the horizontal branch absolute magnitude and metallicity: we obtain MV(HB)=(0.22±0.05)([Fe/H]+1.5)+(0.56± 0.07). This zero point is 0.03 mag shorter than obtained by Carretta et al. (2000ApJ...533..215C) and within the error bar it agrees with, but it is more precise than most of the previous individual determinations of the RR Lyrae absolute magnitude. When combined with the apparent average luminosity of the RR Lyrae stars in the LMC by Clementini et al. (2003AJ....125.1309C), this zero point provides a new estimate of the distance modulus to the LMC: (m-M)0=18.50±0.09.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: evolution - stars: Population II - Galaxy: globular clusters: general - Galaxy: formation - cosmology: distance scale

Simbad objects: 22

goto Full paper

goto View the references in ADS

Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20     4.09     ~ 3922 0
2 CD-35 360 Pe* 01 04 06.1284009928 -34 40 28.933235247   11.01 10.25     G8 64 0
3 BD-16 251 RG* 01 29 31.1311443552 -16 00 45.495314460 12.527 12.427 11.642 11.189 10.713 CEMP 292 0
4 V* RR Cet RR* 01 32 08.1731409309 +01 20 30.230098757 9.46 9.33 9.15     A9V 221 0
5 HD 25329 PM* 04 03 14.9979736362 +35 16 23.805785323 9.75 9.37 8.50 7.75 7.23 K1VbFe-2 367 0
6 HD 75530 PM* 08 50 21.0008103626 -05 32 09.700067362   9.93 9.19     G8/K0V 111 0
7 HIP 44949 * 09 09 17.116752 -81 09 48.47904   12.81 12.13 12.109   ~ 15 0
8 HD 103095 Pe* 11 52 58.7673387755 +37 43 07.254113125 7.38 7.20 6.45 5.80 5.35 K1V_Fe-1.5 803 1
9 HD 104006 PM* 11 58 28.0120446715 -41 55 19.236557718   9.70 8.91     K0.5V 95 0
10 HD 108564 PM* 12 28 19.1204752529 -16 54 39.777541659   10.43 9.502 9.676   K5Vmetalweak 103 0
11 HD 120559 PM* 13 51 40.3987847839 -57 26 08.350982731 8.679 8.647 7.982 7.605 7.217 G7VFe-1.4CH-1 155 0
12 HD 123505 PM* 14 10 02.6869201433 -61 31 18.395066327   10.46 9.68 9.22 8.963 G8(V) 70 0
13 HD 126681 PM* 14 27 24.9094012952 -18 24 40.454425566   9.939 9.535     G3V 189 0
14 HD 134440 PM* 15 10 12.9678589986 -16 27 46.522175847 10.69 10.217 9.426 8.913 8.441 K2V 281 0
15 HD 134439 PM* 15 10 13.0873110544 -16 22 45.877317625 10.03 9.837 9.066 8.604 8.160 sd:K1Fe-1 325 0
16 HD 145417 PM* 16 13 48.5588453721 -57 34 13.843989664 8.663 8.365 7.540 7.054 6.588 K3VFe-1.7 164 0
17 HD 145598 PM* 16 14 09.9313657304 -50 47 05.550472704   9.32 8.66     G8VFe-1.6CH-1.2 80 0
18 M 4 GlC 16 23 35.22 -26 31 32.7           ~ 1856 0
19 NGC 6397 GlC 17 40 42.09 -53 40 27.6     5.17     ~ 1979 0
20 NGC 6752 GlC 19 10 52.11 -59 59 04.4           ~ 2004 0
21 V* RR Lyr RR* 19 25 27.9129605304 +42 47 03.693258204   7.36   7.6   kA3hF0 926 0
22 BD+22 4454 PM* 21 39 36.4600575768 +23 15 55.885777992   10.27   9.0   G5 55 0

To bookmark this query, right click on this link: simbad:objects in 2003A&A...408..529G and select 'bookmark this link' or equivalent in the popup menu