Context : Kepler produces a large amount of data used for asteroseismological analyses , particularly of solar-like stars and red giants .
The mode amplitudes observed in the Kepler spectral band have to be converted into bolometric amplitudes to be compared to models .

Aims : We give a simple bolometric correction for the amplitudes of radial modes observed with Kepler , as well as the relative visibilities of non-radial modes .

Methods : We numerically compute the bolometric correction c _ { \mathrm { K - bol } } and mode visibilities for different effective temperatures T _ { \mathrm { eff } } within the range 4000–7500 K , using a similar approach to a recent one from the literature .

Results : We derive a law for the correction to bolometric values : c _ { \mathrm { K - bol } } = 1 + a _ { 1 } ( T _ { \mathrm { eff } } - T _ { \mathrm { o } } ) + a _ { 2 } ( T _ { \mathrm { % eff } } - T _ { \mathrm { o } } ) ^ { 2 } , with T _ { \mathrm { o } } = 5934 K , a _ { 1 } = 1.349 \times 10 ^ { -4 } K ^ { -1 } , and a _ { 2 } = -3.120 \times 10 ^ { -9 } K ^ { -2 } or , alternatively , as the power law c _ { \mathrm { K - bol } } = ( T _ { \mathrm { eff } } / T _ { \mathrm { o } } ) ^ { \alpha } with \alpha = 0.80 .
We give tabulated values for the mode visibilities based on limb-darkening ( LD ) , computed from ATLAS9 model atmospheres for T _ { \mathrm { eff } } \in [ 4000 , 7500 ] K , \log g \in [ 2.5 , 4.5 ] , and [ M/H ] \in [ -1.0 , +1.0 ] .
We show that using LD profiles already integrated over the spectral band provides quick and good approximations for visibilities .
We point out the limits of these classical visibility estimations .

Conclusions :