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Table 2.

Atmospheric parameters and heliocentric velocities of the stars.

Cluster Star Teff log g M Status vhel nv vcluster Ref.
(K) (cm s−2) (M) (km s−1) (km s−1)
NGC 5139 UIT151 62 600 ± 2400 5.11 ± 0.10 −0.99 ± 0.08 0.24 peAGB +231.1 ± 12 9 +231.8 (1)
UIT644 18 000 ± 800 2.82 ± 0.10 −0.35 ± 0.06 0.29 pAGB +232.3 ± 13 26
UIT1275 17 200 ± 1100 3.34 ± 0.18 −1.27 ± 0.18 0.25 pHB +272.3 ± 6 14
UIT1425 11 700 ± 200 3.57 ± 0.08 −1.72 ± 0.36 0.23 pHB +213.6 ± 17 9
Dk3873 49 700 ± 1800 4.99 ± 0.12 −1.21 ± 0.12 0.28 peAGB +231.2 ± 26 11
ROA5342 52 000 ± 2000 4.79 ± 0.10 −1.17 ± 0.10 0.29 peAGB +227.6 ± 10 10
NGC 6121 UVBS2 (1) 46 600 ± 600 5.82 ± 0.12 +0.89 ± 0.18 0.85 WDM +74.6 ± 15 17 +71.5 (2)
NGC 6656 UVBS2 78 800 ± 9900 4.58 ± 0.20 +0.36 ± 0.16 0.18 pAGB −111.3 ± 4 3 −144.9 (2)
NGC 6712 C49 (2) 53 300 ± 4000 4.50 ± 0.12 −1.04 ± 0.12 0.31 pAGB −108.0 ± 8 8 −109.0 (3)
NGC 6779 ZNG2 21 500 ± 1800 3.07 ± 0.16 −0.85 ± 0.08 0.19 pAGB −123.5 ± 9 15 −138.1 (4)
NGC 7099 UVBS2 65 000 ± 2000 7.22 ± 0.12 −3.29 ± 0.12 WD +11.4 ± 8 3 −184.4 (2)

Unpublished data from Moehler et al. (1998)

NGC 5139 ROA542 10 600 ± 200 2.55 ± 0.10 −1.00 0.34 pHB
ROA3596 17 800 ± 1000 3.56 ± 0.16 −1.26 ± 0.18 0.41 pHB

New analysis of data from Moehler et al. (1998)

NGC 2808 C2946 24 900 ± 1800 4.78 ± 0.20 −1.88 ± 0.14 0.68 pHB
C2947 15 000 ± 1200 3.92 ± 0.24 −1.45 ± 0.44 0.41 pHB
C4594 19 900 ± 1600 3.79 ± 0.22 −1.63 ± 0.26 0.34 pHB
NGC 6121 Y453 54 900 ± 2000 5.62 ± 0.14 −1.25 ± 0.10 0.59 peAGB
NGC 6723 III60 43 000 ± 1400 4.72 ± 0.14 −1.19 ± 0.14 1.02 peAGB
IV9 25 900 ± 2000 4.02 ± 0.22 −1.06 ± 0.10 0.88 peAGB
NGC 6752 B2004 34 500 ± 800 5.18 ± 0.14 −2.45 ± 0.24 0.35 pHB

Notes. The status acronyms are p-AGB (post-AGB), post-early AGB (peAGB), post-HB (pHB), white dwarf merger (WDM), and white dwarf (WD). We have no velocity information for the data from Moehler et al. (1998).

(1)

Mochejska et al. (2002) refer to the star as B2 and describe its spectrum as helium rich.

(2)

Remillard et al. (1980) classified the star as sdO.

References. (1) Johnson et al. (2008); (2) Lane et al. (2010); (3) Yong et al. (2008); (4) Webbink (1981).

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