Homogeneous abundance analysis of FGK dwarf, subgiant, and giant stars with and without giant planets

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Table 7

Same as Table 4 but showing photometric and evolutionary parameters with the population membership.

Star	B − V	M _V	Dist. [pc]	BC	log L	Mass [M_⊙]	Age [Gyr]	Population group	Remarks	Ref.

HD 10145	0.691	4.84	37.3	−0.106	0.005 ± 0.026	0.94 ± 0.03	10.1 ^{+ 2.5} _-1.8	thin
HD 10476	0.836	5.82	7.5	−0.239	−0.331 ± 0.006	0.78 ± 0.04	17.1 ^{+ 8.2} _-7.7	thin	^a
HD 106116	0.701	4.79	34.9	−0.100	0.025 ± 0.015	1.00 ± 0.03	7.1 ^{+ 2.5} _-1.4	thin/thick
HD 106516	0.470	4.36	22.4	0.011	0.150 ± 0.016	1.05 ± 0.05	0.2 ^{+ 1.3} _-0.2	thick
HD 108954	0.568	4.53	21.8	−0.010	0.092 ± 0.008	–	–	thin	^b
HD 124292	0.733	6.18	22.1	−0.143	−0.516 ± 0.011	–	–	thin	^e	3
HD 128311	0.973	6.38	16.6	−0.126	−0.603 ± 0.015	–	0.50	thin	^c^,^d (U)	1, 2
HD 206860	0.587	4.74	17.9	−0.020	0.017 ± 0.008	–	0.10	thin	^c^,^d (P)	1, 2
HD 25825	0.593	4.50	45.9	−0.021	0.108 ± 0.052	–	0.65	thin	^d (H)	4
HD 42807	0.663	5.17	18.0	−0.070	−0.140 ± 0.008	–	2.70	thin	^d (W)	5
...	...	...	...	...	...	...	...	...

Notes.

^(a)

Not considered in the abundance analysis because the age uncertainties are larger than 4 Gyr (see Sect. 4.1);

^(b)

mass and age not derived because the star is located outside the evolutionary tracks and isochrones used;

^(c)

star hosting at least one giant planet;

^(d)

member of a stellar moving group (U: Ursa Major; P: Pleiades; H: Hyades; W: Wolf 630);

^(e)

subdwarf candidate.

Reference. (1) http://exoplanet.eu; (2) Montes et al. (2001); (3) Sandage & Fouts (1986); (4) Eggen (1950); (5) Bubar & King (2010).

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