A proper motion study of the globular cluster M 10

Chen, L.; Geffert, M.; Wang, J. J.; Reif, K.; Braun, J. M.

doi:10.1051/aas:2000238

Cited by 11 publications

(15 citation statements)

References 18 publications

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“…Furthermore, we can compare our spectroscopic distance estimates with published globular cluster distances to perform a consistency check on our choice of atmospheric parameters. The programme stars have been previously identified as being members of their respective globular clusters based on radial velocity measurements and proper motion studies (see Strom et al 1970 andChen et al 2000 for M 10 ZNG-1; Cudworth 1976 for M 15 ZNG-1; and Cudworth 1988 for NGC 6712 ZNG-1). Radial velocity estimates obtained from our high-resolution spectra are presented in Table 5.…”

Section: Evolutionary Status Luminosity Mass and Distancementioning

confidence: 99%

High-resolution spectroscopy of globular cluster post-Asymptotic Giant Branch stars

Mooney

Rolleston

Keenan

et al. 2004

A&A

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Abstract. We present model atmosphere analyses of high resolution Keck and VLT optical spectra for three evolved stars in globular clusters, viz. ZNG-1 in M 10, ZNG-1 in M 15 and ZNG-1 in NGC 6712. The derived atmospheric parameters and chemical compositions confirm the programme stars to be in the post-Asymptotic Giant Branch (post-AGB) evolutionary phase. Differential abundance analyses reveal CNO abundance patterns in M 10 ZNG-1, and possibly M 15 ZNG-1, which suggest that both objects may have evolved off the AGB before the third dredge-up occurred. The abundance pattern of these stars is similar to the third class of optically, bright post-AGB objects discussed by van Winckel (1997). Furthermore, M 10 ZNG-1 exhibits a large C underabundance (with [C/O] ∼ −1.6 dex), typical of other hot post-AGB objects. Differential [α/Fe] abundance ratios in both M 10 ZNG-1 and NGC 6712 ZNG-1 are found to be approximately 0.0 dex, with the Fe abundance of the former being in disagreement with the cluster metallicity of M 10. Given that the Fe absorption features in both M 10 ZNG-1 and NGC 6712 ZNG-1 are well observed and reliably modelled, we believe that these differential Fe abundance estimates to be secure. However, our Fe abundance is difficult to explain in terms of previous evolutionary processes that occur on both the Horizontal Branch and the AGB.

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Section: Evolutionary Status Luminosity Mass and Distancementioning

confidence: 99%

High-resolution spectroscopy of globular cluster post-Asymptotic Giant Branch stars

Mooney

Rolleston

Keenan

et al. 2004

A&A

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“…The SNO+ physics programme will include measurements of low energy solar neutrino fluxes and a search for neutrinoless double beta decay using neodymium [2]. Sensitivity to both requires precise energy and position reconstruction, for which an accurate characterization of the scintillator timing is needed.…”

Section: Introductionmentioning

confidence: 99%

Scintillation decay time and pulse shape discrimination in oxygenated and deoxygenated solutions of linear alkylbenzene for the SNO+ experiment

O’Keeffe

O’Sullivan

Chen

2011

Nuclear Instruments and Methods in Physics Research Section A:

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The SNO+ liquid scintillator experiment is under construction in the SNOLAB facility in Canada. The success of this experiment relies upon accurate characterization of the liquid scintillator, linear alkylbenzene (LAB). In this paper, scintillation decay times for alpha and electron excitations in LAB with 2 g/L PPO are presented for both oxygenated and deoxygenated solutions. While deoxygenation is expected to improve pulse shape discrimination in liquid scintillators, it is not commonly demonstrated in the literature. This paper shows that for linear alkylbenzene, deoxygenation improves discrimination between electron and alpha excitations in the scintillator.

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“…Two of the remaining program stars (IV-44 & IV-87) were found to have wavelength shifts and Hα profiles inconsistent with being both cluster members and low surface gravity RGB stars. Comparison with the proper motion study by Chen et al (2000) reveals that both of these stars have proper motions inconsistent with other cluster members.…”

Section: Observations and Reductionsmentioning

confidence: 74%

Chemical Analysis of Five Red Giants in the Globular Cluster M10 (NGC 6254)

Haynes

Burks

Johnson

et al. 2008

PUBL ASTRON SOC PAC

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ABSTRACT. We have determined Al, α, Fe-peak, and neutron capture elemental abundances for five red-giant branch (RGB) stars in the Galactic globular cluster M10. Abundances were determined using equivalent width analyses of moderate-resolution (R ∼ 15; 000) spectra obtained with the Hydra multifiber positioner and bench spectrograph on the WIYN telescope. The data sample the upper RGB from the luminosity level near the horizontal branch to about 0.5 mag below the RGB tip. We find, in agreement with previous studies, that M10 is moderately metal-poor with ½Fe=H ¼ À1:45 (σ ¼ 0:04). All stars appear enhanced in Al with 〈½Al=Fe 〉 ¼ þ0:33 (σ ¼ 0:19), but no stars have ½Al=Fe ≳ þ0:55. We find the α elements to be enhanced by þ0:20 to þ0:40 dex and the Fe-peak elements to have ½el=Fe ∼ 0, which are consistent with predictions from type II SNe ejecta. Additionally, the cluster appears to be r-process rich with 〈½Eu=La 〉 ¼ þ0:41.

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A proper motion study of the globular cluster M 10

Cited by 11 publications

References 18 publications

High-resolution spectroscopy of globular cluster post-Asymptotic Giant Branch stars

High-resolution spectroscopy of globular cluster post-Asymptotic Giant Branch stars

Scintillation decay time and pulse shape discrimination in oxygenated and deoxygenated solutions of linear alkylbenzene for the SNO+ experiment

Chemical Analysis of Five Red Giants in the Globular Cluster M10 (NGC 6254)

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