NGC 4349 is an
open cluster in the constellation
Crux. It was discovered by
James Dunlop in 1826. It is located approximately 7,000
light years away from Earth.
Characteristics
There are 390 probable member stars within the angular radius of the cluster and 129 within the central part of the cluster. The tidal radius of the cluster is 17.8 - 22.8 parsecs (58 - 75 light years) and represents the average outer limit of NGC 4349, beyond which a star is unlikely to remain gravitationally bound to the cluster core.[4] One
blue straggler has been detected in the cluster.[5] There are four
Cepheid variables in the direction of the cluster, among them
R and
T Crucis, which, however, are not members of the cluster.[6] R Crucis lies 16 arcminutes from the centre of the open cluster NGC 4349, which is beyond the outer limit of the cluster, and is estimated to be nearly 1 kpc closer to Earth than the cluster.[7] The cluster has subsolar
metallicity (−0.12 ± 0.06).[8]
A
brown dwarf with minimum mass 19.8 times that of
Jupiter has been detected orbiting
star no. 127 (vmag. 10.88 and with mass 3.9
M☉) every 678 days. At the time of discovery, star NGC 4349 No. 127 was the heaviest star with an accurate mass determination around which a substellar companion had been detected, and also one of the youngest systems known.[9] However, this star's
radial velocity variations were later shown to result from stellar activity rather than a substellar companion.[10][11]