Table 2
Spectroscopic stellar parameters and iron abundance derived with MOOG for low-rotating stars observed at high resolution.
| Star | Teff | log g | ξ | [Fe i/H]* | # Lines | [Fe ii/H]** | # Lines |
| (K) | (dex) | (km s-1) | (dex) | (dex) | |||
|
|
|||||||
| X-Clump 0534+22 | |||||||
| 2MASS J05263833+2231546 | 4750 | 4.4 | 2.0 | −0.08 ± 0.15 | 43 | −0.08 ± 0.15 | 3 |
| 2MASS J05263826+2231434 | 4750 | 4.0 | 1.9 | −0.07 ± 0.12 | 42 | −0.06 ± 0.11 | 5 |
| 2MASS J05214684+2400444 | 5000 | 4.3 | 2.2 | −0.04 ± 0.11 | 44 | −0.02 ± 0.06 | 4 |
|
|
|||||||
| X-Clump 0430−08 | |||||||
| 2MASS J04431640−0937052 | 6000 | 4.6 | 1.4 | + 0.22 ± 0.08 | 66 | + 0.22 ± 0.10 | 9 |
| " | 6050 | 4.6 | 1.4 | +0.26 ± 0.08 | 78 | +0.22 ± 0.10 | 9 |
| 2MASS J04443859−0724378 | 5900 | 4.4 | 1.5 | + 0.03 ± 0.09 | 64 | + 0.03 ± 0.08 | 11 |
|
|
|||||||
| Strip | |||||||
| 2MASS J03494386 − 1353108 | 5400 | 4.5 | 1.4 | + 0.00 ± 0.09 | 64 | −0.01 ± 0.12 | 9 |
| " | 5500 | 4.6 | 1.6 | +0.05 ± 0.09 | 70 | + 0.03 ± 0.13 | 10 |
| 2MASS J05274490+0313161 | 5000 | 4.3 | 1.7 | −0.02 ± 0.17 | 51 | −0.01 ± 0.23 | 3 |
| 2MASS J06134773+0846022 | 5050 | 3.6 | 1.6 | −0.25 ± 0.13 | 59 | −0.24 ± 0.13 | 9 |
| 2MASS J06203205+1331125 | 5350 | 4.4 | 0.3 | −0.23 ± 0.17 | 44 | −0.24 ± 0.25 | 4 |
| 2MASS J06350191+1211359 | 6100 | 4.3 | 1.5 | + 0.01 ± 0.13 | 45 | + 0.00 ± 0.19 | 9 |
| 2MASS J06513955+1828080 | 5100 | 4.7 | 1.5 | −0.07 ± 0.09 | 60 | −0.07 ± 0.13 | 5 |
|
|
|||||||
| Alcalá et al. (2000) Sample | |||||||
| RX J0515.6 − 0930 | 5650 | 4.5 | 2.3 | −0.04 ± 0.12 | 41 | −0.06 ± 0.23 | 4 |
| RX J0517.9 − 0708 | 5100 | 4.2 | 1.8 | + 0.06 ± 0.13 | 47 | + 0.05 ± 0.14 | 4 |
| RX J0531.6 − 0326 | 5250 | 4.3 | 1.7 | −0.02 ± 0.09 | 53 | −0.03 ± 0.08 | 5 |
| RX J0538.9 − 0624 | 5550 | 4.4 | 1.3 | + 0.01 ± 0.11 | 58 | + 0.02 ± 0.20 | 10 |
| RX J0518.3+0829 | 5300 | 4.2 | 2.0 | −0.04 ± 0.11 | 21 | −0.02 ± 0.15 | 3 |
| RX J0510.1 − 0427 | 4950 | 4.6 | 1.9 | −0.10 ± 0.12 | 34 | −0.00 ± 0.24 | 2 |
| RX J0520.0+0612 | 4750 | 4.1 | 2.2 | −0.17 ± 0.12 | 45 | −0.17 ± 0.30 | 5 |
| RX J0520.5+0616 | 4900 | 4.1 | 2.4 | −0.08 ± 0.17 | 29 | −0.07 ± 0.04 | 3 |
Notes. The two stars observed with FEROS are indicated in italics.
The iron abundances are relative to the Sun. Adopting 
K, log g ⊙ = 4.44, and ξ ⊙ = 1.1 km s-1, we obtain log n ⊙ (Fe i) = 7.53 ± 0.04 and log n ⊙ (Fe ii) = 7.53 ± 0.06 from a FOCES spectrum, and log n ⊙ (Fe i) = 7.50 ± 0.05 and log n ⊙ (Fe ii) = 7.50 ± 0.06 from a FEROS spectrum.
The listed errors are the internal ones in EW, represented by the standard deviation on the mean abundance determined from all lines. The other source of internal error includes uncertainties in stellar parameters (Biazzo et al. 2011a). Taking into account typical errors in Teff (~70 K), log g (~0.2 dex), and ξ (~0.2 dex), we derive an error of ~0.05 dex in [Fe/H] due to uncertainties on stellar parameters.
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