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Table 2

Fluorine abundances and element ratios.

Star log ϵ(F)a Δlog ϵ(F)b C/O [Fe/H] [F/Fe] [s/Fe]

Sun 4.37 ± 0.04(10) 0.19 0.58 0.00 0.00 0.00
Arcturus 3.78 ± 0.02(3) 0.37 0.20 −0.53 −0.07 −0.01
N-type
AQ Sgr 4.34 ± 0.08 (5) 0.29 1.03 −0.10 0.08
BL Ori 4.62 ± 0.20 (5) 0.30 1.04 0.00 0.26 1.00
RT Cap 4.30 0.36 1.20 0.00 −0.06
RV Cyg 4.30 ± 0.00 (4) 0.40 1.09 0.00 −0.06 0.07
S Sct 4.37 ± 0.05 (5) 0.25 1.05 −0.10 0.11 0.40
ST Cam 4.45 ± 0.00 (4) 0.27 1.02 −0.10 0.19 0.45
TU Gem 4.63 ± 0.24 (5) 0.29 1.07 0.00 0.27
TW Oph 4.26 ± 0.06 (3) 0.35 1.12 −0.40 0.29
TX Psc 4.65 ± 0.07 (6) 0.18 1.03 −0.39 0.69 1.10
U Cam 4.20 ± 0.08 (4) 0.38 1.23 −0.10 −0.06 0.55
U Hya 4.70 ± 0.20 (6) 0.37 1.05 −0.05 0.39 1.10
UU Aur 4.55 ± 0.14 (7) 0.33 1.06 0.00 0.19 0.45
UX Dra 4.56 ± 0.18 (5) 0.29 1.05 −0.20 0.20 0.65
V460 Cyg 4.47 ± 0.12(4) 0.18 1.07 −0.05 0.15 0.80
V Aql 4.26 ± 0.05 (5) 0.36 1.05 −0.05 −0.05 0.20
VY UMa 4.50 ± 0.03 (5) 0.20 1.06 −0.10 0.24 0.90
W CMa 4.68 ± 0.13 (5) 0.27 1.07 0.20 0.12 0.60
W Ori 4.30 ± 0.00 (3) 0.12 1.07 0.05 −0.10 0.25
X Cnc 4.32 ± 0.08 (4) 0.61 1.03 −0.30 0.25
Y Hya 4.40 ± 0.00 (2) 0.50 1.18 −0.10 0.14
Y Tau 4.36 ± 0.17 (4) 0.21 1.04 0.00 0.00 0.05
Z Psc 4.80 ± 0.06 (5) 0.10 1.08 −0.01 0.44 0.97
SC-type
CY Cyg 4.62 ± 0.03 (4) 0.53 1.00 0.10 0.15 0.10
FU Mon 4.91 ± 0.07 (5) 0.24 1.00 0.00 0.55 0.40
GP Ori 4.70 ± 0.14 (5) 0.56 1.01 0.00 0.34 1.25
RZ Peg 4.80 ± 0.02 (7) 0.20 1.00 0.00 0.44 0.00
WZ Cas 5.31 ± 0.14 (7) 0.49 1.01 0.00 0.95 0.16
J-type
R Scl 4.07 ± 0.05 (4) 0.11 1.02 −0.30 0.01
RY Dra 3.80 0.68 1.12 −0.05 −0.51 <0.20
T Lyr 4.32 0.35 1.14 0.00 −0.04
VX And 4.30 ± 0.00 (2) 0.05 1.76 −0.10 0.04 0.2
Y Cvn <3.50 >0.85 1.12 0.00 < −0.86 <0.2
ExtraGalactic N-type
LMC TRM88 4.50 0.35 1.62 −0.60 0.74
SMC GM780 4.10 3.10 −0.80 0.53
SMC BMB B30 3.60 0.00 1.47 −1.10 0.34 0.90
Carina ALW6 3.50 0.20 12.0 −1.70 0.84 1.60
Carina ALW7 3.80 0.60 19.0 −1.90 1.34 1.74

Notes. [s/Fe] is the average s-element enhancement according to Abia & Isern (2000), Abia et al. (2002), de Laverny et al. (2006), and Abia et al. (2008).

(a)

The number in parenthesis indicates the number of HF lines used.

(b)

Abundance differences in Abia et al. (2010; Galactic stars) or Abia et al. (2011; extragalactic stars) minus this work. In the cases of the Sun and Arcturus, the differences are respect to that derived in Asplund et al. (2009) and Abia et al. (2009), respectively.

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