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Open cluster in the constellation Vela From Wikipedia, the free encyclopedia
NGC 2547 is a southern open cluster in Vela, discovered by Nicolas Louis de Lacaille in 1751[2][3] from South Africa. The star cluster is young with an age of 20-30 million years.[4]
NGC 2547 | |
---|---|
Observation data (J2000.0 epoch) | |
Right ascension | 8h 09m 52.360s |
Declination | −49° 10′ 35.01″ |
Distance | 1.19 kly (364.0+46.8 −37.9[1] pc) |
Apparent magnitude (V) | 4.7 |
Apparent dimensions (V) | 20′ |
Physical characteristics | |
Mass | 201[1] M☉ |
Radius | 2.61[1] ly |
Estimated age | 37.7+5.7 −4.8[1] Myr |
Other designations | NGC 2547, Cr 177, Mel 84, Dunlop 410, Lacaille III.2 |
Associations | |
Constellation | Vela |
Observations with the Spitzer Space Telescope showed a shell around the B3 III/IV-type star HD 68478. This could be a sign of recent mass loss in this star.[5]
A study using Gaia DR2 data showed that NGC 2547 formed about 30 million years ago together with a new discovered star cluster, called [BBJ2018] 6.[6][7] The star cluster NGC 2547 has a similar age compared with Trumpler 10, NGC 2451B, Collinder 135 and Collinder 140. It was suggested that all these clusters formed in a single event of triggered star formation.[8]
NGC 2547 shows evidence for mass segregation down to 3 M☉.[9]
Observations with the Spitzer Space Telescope have shown that ≤1% of the stars in NGC 2547 have infrared excess in 8.0 μm and 30-45% of the B- to F-type stars have infrared excess at 24 μm.[10]
The system 2MASS J08090250-4858172, also called ID8 is located in NGC 2547 and showed substantial brightening of the debris disk at a wavelength of 3 to 5 micrometers, followed by a decay over a year. This was interpreted as a violent impact on a planetary body in this system.[11]
NGC 2547 contains nine M-dwarfs with 24 μm excess. These could be debris disks and the material could be orbiting close to the snow line of these stars, indicating that planet-formation is underway in these systems.[12] Later it was suggested that these M-dwarfs might contain Peter Pan Disks.[13] 2MASS 08093547-4913033, which is one of the M-dwarfs with a debris disk in NGC 2547 was observed with the Spitzer Infrared Spectrograph. In this system the first detection of silicate was made from a debris disk around an M-type star.[14]
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