The White Dwarf Distance to the Globular Cluster NGC 6752 (and Its Age) with the [ITAL]HUBBLE SPACE TELESCOPE[/ITAL]

Renzini, A.; Bragaglia, A.; Ferraro, F. R.; Gilmozzi, R.; Ortolani, S.; Holberg, J. B.; Liebert, James; Wesemaël, F.; Bohlin, R. C.

doi:10.1086/310128

Cited by 167 publications

(192 citation statements)

References 30 publications

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“…With these constraints on the simulations, the relative number of stars in the different boxes, plus the magnitude and colour location of the HB were reproduced with E(B − V) = 0.03 (consistent with E(B − V) = 0.04 ± 0.005 and systematic error of ±0.011, as estimated by Gratton et al 2003), (m − M) 0 = 13.12 (consistent i.e. with the cluster white dwarf distance by Renzini et al 1996) and the mass distribution shown in Fig. 4.…”

Section: Synthetic Hb Simulationssupporting

confidence: 70%

On the missing second generation AGB stars in NGC 6752

Cassisi

Salaris

Pietrinferni

et al. 2014

A&A

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In recent years the view of Galactic globular clusters as simple stellar populations has changed dramatically, it is now thought that basically all globular clusters host multiple stellar populations, each with its own chemical abundance pattern and colour-magnitude diagram sequence. Recent spectroscopic observations of asymptotic giant branch stars in the globular cluster NGC 6752 have disclosed a low [Na/Fe] abundance for the whole sample, suggesting that they are all first generation stars, and that all second generation stars fail to reach the AGB in this cluster. A scenario proposed to explain these observations invokes strong mass loss in second generation horizontal branch stars -all located at the hot side of the blue and extended horizontal branch of this cluster -possibly induced by the metal enhancement associated to radiative levitation. This enhanced mass loss would prevent second generation stars from reaching the asymptotic giant branch phase, thus explaining at the same time the low value of the ratio between horizontal branch and asymptotic giant branch stars (the R 2 parameter) observed in NGC 6752. We have critically discussed this mass-loss scenario, finding that the required mass-loss rates are of the order of 10 −9 M yr −1 , significantly higher than current theoretical and empirical constraints. By making use of synthetic horizontal branch simulations, we demonstrate that our modelling correctly predicts the R 2 parameter for NGC 6752, without the need to invoke very efficient mass loss during the core He-burning stage. As a test of our stellar models we show that we can reproduce the observed value of R 2 for both M 3, a cluster of approximately the same metallicity and with a redder horizontal branch morphology, and M 13, a cluster with a horizontal branch very similar to NGC 6752. However, our simulations for the NGC 6752 horizontal branch predict however the presence of a significant fraction of second generation stars (about 50%) along the cluster asymptotic giant branch. We conclude that there is no simple explanation for the lack of second generation stars in the spectroscopically surveyed sample, although the interplay between mass loss (with low rates) and radiative levitation may play a role in explaining this puzzle.

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Section: Synthetic Hb Simulationssupporting

confidence: 70%

On the missing second generation AGB stars in NGC 6752

Cassisi

Salaris

Pietrinferni

et al. 2014

A&A

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“…Model estimates (Chaboyer et al 1996;Renzini et al 1996;Salaris, Degl'Innocenti & Weiss 1997). For each of the low-Ω0 flat models we choose the value of h that gives t ≈ 14Gyr.…”

Section: Cosmological Modelsmentioning

confidence: 99%

Mock 2dF and SDSS galaxy redshift surveys

Cole¹,

Hatton²,

Weinberg³

et al. 1998

Monthly Notices RAS

120

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We present a comprehensive set of mock 2dF and SDSS galaxy redshift surveys constructed from a set of large, high-resolution cosmological N -body simulations. The radial selection functions and geometrical limits of the catalogues mimic those of the genuine surveys. The catalogues span a wide range of cosmologies, including both open and flat universes. In all the models the galaxy distributions are biased so as to approximately reproduce the observed galaxy correlation function on scales of 1-10h −1 Mpc. In some cases models with a variety of different biasing prescriptions are included. All the mock catalogues are publically available at http://starwww.dur.ac.uk/˜cole/mocks/main.html . We expect these catalogues to be a valuable aid in the development of the new algorithms and statistics that will be used to analyse the 2dF and SDSS surveys when they are completed in the next few years. Mock catalogues of the PSCZ survey of IRAS galaxies are also available at the same WWW location.

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“…NGC 6752 is at a distance of 4:1 AE 0:2 kpc (Renzini et al 1996). The optically derived center is at (J2000.0) 19 h 10 m 519 8, À59 58 0 55 00 (Harris 1996).…”

Section: Introductionmentioning

confidence: 99%

Optical Identification of Multiple Faint X‐Ray Sources in the Globular Cluster NGC 6752: Evidence for Numerous Cataclysmic Variables1

Pooley

Lewin

Homer

et al. 2002

ApJ

142

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We report on the Chandra X-Ray Observatory ACIS-S3 imaging observation of the globular cluster NGC 6752. We detect six X-ray sources within the 10>5 core radius and 13 more within the 115 00 half-mass radius down to a limiting luminosity of L X % 10 30 ergs s À1 for cluster sources. We reanalyze archival data from the Hubble Space Telescope and the Australia Telescope Compact Array and make 12 optical identifications and one radio identification. Based on X-ray and optical properties of the identifications, we find 10 likely cataclysmic variables (CVs), one to three likely RS CVn or BY Dra systems, and one or two possible background objects. Of the seven sources for which no optical identifications were made, we expect that approximately two to four are background objects and that the rest are either CVs or some or all of the five millisecond pulsars whose radio positions are not yet accurately known. These and other Chandra results on globular clusters indicate that the dozens of CVs per cluster expected by theoretical arguments are being found. The findings to date also suggest that the ratio of CVs to other types of X-ray sources is remarkably similar in clusters of very different structural parameters.

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The White Dwarf Distance to the Globular Cluster NGC 6752 (and Its Age) with the [ITAL]HUBBLE SPACE TELESCOPE[/ITAL]

Cited by 167 publications

References 30 publications

On the missing second generation AGB stars in NGC 6752

On the missing second generation AGB stars in NGC 6752

Mock 2dF and SDSS galaxy redshift surveys

Optical Identification of Multiple Faint X‐Ray Sources in the Globular Cluster NGC 6752: Evidence for Numerous Cataclysmic Variables1

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