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Home All issues Volume 672 (April 2023) A&A, 672 (2023) A56 Full HTML
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Table 1.

Spearman correlation coefficients (SCCs) between the log σ(Sph) residuals, when isolating each dependence, and the different observational and stellar properties.

Main sequence
M K G F Subgiant
N stars 426 13 499 20 235 7771 2674
⟨Sph⟩5 th 567.1 281.7 81.4 30.9 37.4
⟨Sph⟩95 th 5950.6 5125.5 4870.7 2031.6 4239.8
SCC Kp 0.07 0.07 0.15 0.28 0.21
tobs 0.00 −0.09 −0.12 −0.20 −0.17
Teff 0.11 0.10 −0.07 −0.14 −0.24
L −0.11 0.00 −0.11 −0.15 0.04
[Fe/H] 0.03 0.04 0.01 −0.06 −0.02
Prot −0.38 −0.36 −0.37 −0.15 −0.16
⟨Sph⟩ 0.84 0.91 0.94 0.88 0.88
FAST-ROTATING POPULATION
N stars 175 2848 2104
⟨Sph⟩5 th 507.8 378.8 138.7
⟨Sph⟩95 th 7624.7 9666.7 6800.0
SCC Kp 0.06 0.06 0.02
tobs −0.05 −0.15 −0.15
Teff 0.16 −0.03 −0.07
L −0.11 0.01 −0.07
[Fe/H] 0.12 0.07 0.01
Prot −0.46 −0.41 −0.19
Sph 0.91 0.93 0.93
SLOW-ROTATING POPULATION
N stars 251 10,651 18,131
⟨Sph⟩5 th 742.5 269.1 78.1
⟨Sph⟩95 th 4518.0 4465.6 4410.3
SCC Kp 0.08 0.08 0.16
tobs 0.01 −0.08 −0.12
Teff 0.18 0.07 −0.06
L −0.26 0.00 −0.12
[Fe/H] 0.03 0.04 0.02
Prot −0.18 −0.35 −0.33
⟨Sph⟩ 0.77 0.89 0.93

Notes. The first part of the table concerns all the stars in Fig. 2, which are split into slow- and fast-rotating populations (GKM) for the second and third parts of the table (Fig. 4). The top lines of each part indicate the number of stars and 5th and 95th percentiles of the ⟨Sph⟩ distribution.

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