Searching for the signatures of terrestrial planets in F-, G-type main-sequence stars

J. I.  González Hernández; E. Delgado-Mena; S. G. Sousa; G. Israelian; N. C. Santos; V. Zh. Adibekyan; S. Udry

doi:10.1051/0004-6361/201220165

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Volume 552 (April 2013)

A&A, 552 (2013) A6

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Table 4

Slopes of the linear fit to the mean values Δ [X/Fe] _{SUN − STARS} versus T_C.

Sample^a	Non-GCE^b	GCE^b	N_stars^c

sSA	−0.378 ± 0.033	−0.060 ± 0.029	62
pSA	−0.302 ± 0.047	+ 0.014 ± 0.040	33
smrSA	−0.235 ± 0.055	−0.062 ± 0.053	16
pmrSA	−0.194 ± 0.048	−0.027 ± 0.047	16
sHA	−0.160 ± 0.046	−0.086 ± 0.041	32
pHA	−0.404 ± 0.048	−0.242 ± 0.046	29
smrHA	−0.111 ± 0.062	−0.106 ± 0.061	13
pmrHA	−0.506 ± 0.066	−0.379 ± 0.063	13
smrHAh	−0.330 ± 0.069	−0.258 ± 0.070	10
pmrHAh	−0.419 ± 0.068	−0.289 ± 0.067	10
pSAlp	−0.099 ± 0.067	+ 0.125 ± 0.059	13
pSAmp	−0.370 ± 0.075	−0.044 ± 0.062	14
pSAsp	−0.404 ± 0.114	−0.103 ± 0.092	6
pSAlm	−0.348 ± 0.059	−0.077 ± 0.050	21
pSAmm	+ 0.236 ± 0.114	+ 0.383 ± 0.097	4
pSAsm	−0.223 ± 0.084	+ 0.199 ± 0.065	8

Notes.Slopes of the linear fit of the mean abundance ratios, Δ [X/Fe] _{SUN − STARS}, as a function of the condensation temperature, T_C, using the whole T_C interval, for different stellar samples.

^(a)

Stellar samples: “single” solar analogs, “sSA”, planet-host solar analogs, “pSA”, “single” metal-rich solar analogs, “smrSA”, planet-host metal-rich solar analogs, “pmrSA”. “HA” refers to “hot” analogs and “HAh” refers to very high S/N data (S/N > 550). Planet-host solar analogs with the most massive planet in an orbital period P_orb < 25 days, “pSAsp”, 100 < P_orb < 600 days, “pSAmp”, 900 < P_orb < 4250 days, “pSAlp”. Planet-host solar analogs with the minimum mass, m_psini, of the least massive planet in the ranges: m_p < 14 M_⊕, “pSAsm”, 14 < m_p < 30 M_⊕, “pSAmm”, m_p > 30 M_⊕, “pSAlm”.

^(b)

“Non-GCE” and “GCE” refers to the mean abundances before and after being corrected for galactic chemical evolution effects.

^(c)

Total number of stars in the sample.

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