Star in the constellation Centaurus
! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000.0      Equinox J2000.0
! style="text-align:left" | Constellation
! style="text-align:left" | Right ascension
! style="text-align:left" | Declination
! style="text-align:left" | Apparent magnitude (V)
! style="background-color: #FFFFC0; text-align: center;" colspan="2"| Characteristics
! style="text-align:left" | Evolutionary stage
! style="text-align:left" | Spectral type
! style="text-align:left" | U−B 
! style="text-align:left" | B−V 
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HD 113703, also known by the Bayer designation f Centauri, is a multiple star system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association.
The primary of f Centauri is a blue-white hued B-type main-sequence star with a stellar classification of B4V. It is a young star with an age estimated at around 92 million years, and is spinning rapidly with a projected rotational velocity of 140 km/s. A close companion with a K magnitude of 9.16, designated component C, was detected in 2002 at an angular separation of . In 2013, a spectroscopic companion to the primary was observed using long baseline interferometry, with the two being designated components Aa and Ab.
A faint, magnitude 10.8 companion, component B, was first reported by J. F. W. Herschel in 1836. As of 2015, it was located at a separation of along a position angle of 78°. This is a K-type star with a class of K0Ve, showing emission in the Calcium H and K lines. It is a known BY Draconis variable star with the designation V1155 Centauri. It shares a common space motion with the primary, indicating a probable physical relationship, and its Gaia Data Release 3 parallax of suggests a distance of 409 light years. The star shows a strong overabundance in lithium, which demonstrates its young age. It is about 0.8 magnitudes above zero age main sequence and thus is still contracting as a post-T Tauri star. X-ray emission has been detected from this star.
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