Langbahn Team – Weltmeisterschaft

NGC 2547

NGC 2547
This image from the Wide Field Imager on the MPG/ESO 2.2-metre telescope at ESO's La Silla Observatory in Chile, shows the bright open star cluster NGC 2547.
Observation data (J2000.0 epoch)
Right ascension8h 09m 52.360s
Declination−49° 10′ 35.01″
Distance1.19 kly (364.0+46.8
−37.9[1] pc)
Apparent magnitude (V)4.7
Apparent dimensions (V)20′
Physical characteristics
Mass201[1] M☉
Radius2.61[1] ly
Estimated age37.7+5.7
−4.8[1] Myr
Other designationsNGC 2547, Cr 177, Mel 84, Dunlop 410, Lacaille III.2
Associations
ConstellationVela
See also: Open cluster, List of open clusters

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]

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]

Cluster members with debris disks

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]

  • Asteroid collision - building planets near star NGC 2547-ID8 (artist concept)
    Asteroid collision - building planets near star NGC 2547-ID8 (artist concept)
  • Plot of IR brightness over time suggesting a collision of asteroids near star NGC 2547-0ID8 (2012–2013)
    Plot of IR brightness over time suggesting a collision of asteroids near star NGC 2547-0ID8 (2012–2013)
  • Zooming into the open star cluster NGC 2547 (in HD)
  • Pan sequence in the open star cluster NGC 2547 (in HD)
  • Infrared image of NGC 2547 taken with the Spitzer Space Telescope. Below the center HD 68478 and the shell around this star is seen.
    Infrared image of NGC 2547 taken with the Spitzer Space Telescope. Below the center HD 68478 and the shell around this star is seen.
  • Wide-field view of NGC 2547, created from DSS2 images.
    Wide-field view of NGC 2547, created from DSS2 images.

References

  1. ^ a b c d Bravi, L.; Zari, E.; Sacco, G. G.; Randich, S.; Jeffries, R. D.; Jackson, R. J.; Franciosini, E.; Moraux, E.; López-Santiago, J.; Pancino, E.; Spina, L. (July 2018). "The Gaia-ESO Survey: a kinematical and dynamical study of four young open clusters". Astronomy & Astrophysics. 615: A37. arXiv:1803.01908. Bibcode:2018A&A...615A..37B. doi:10.1051/0004-6361/201832645. ISSN 0004-6361. S2CID 119494247.
  2. ^ "Full name of NGC discoverers". NASA/IPAC Extragalactic Database. Archived from the original on 28 February 2011. Retrieved 5 September 2014.
  3. ^ Jones, K. G. (March 1969). "The search for the nebulae - VI". Journal of the British Astronomical Association. 79: 213–222. Bibcode:1969JBAA...79..213J.
  4. ^ "Young, Hot and Blue - Stars in the cluster NGC 2547". www.eso.org. Retrieved 2020-01-22.
  5. ^ Young, E. T.; Lada, C. J.; Teixeira, P.; Muzerolle, J.; Muench, A.; Stauffer, J.; Beichman, C. A.; Rieke, G. H.; Hines, D. C.; Su, K. Y. L.; Engelbracht, C. W. (September 2004). "Spitzer Observations of NGC 2547: The Disk Population at 25 Million Years". The Astrophysical Journal Supplement Series. 154 (1): 428. Bibcode:2004ApJS..154..428Y. doi:10.1086/422688. ISSN 0067-0049.
  6. ^ Beccari, Giacomo; Boffin, Henri M. J.; Jerabkova, Tereza; Wright, Nicholas J.; Kalari, Venu M.; Carraro, Giovanni; De Marchi, Guido; de Wit, Willem-Jan (November 2018). "A sextet of clusters in the Vela OB2 region revealed by Gaia" (PDF). MNRAS. 481 (1): L11–L15. arXiv:1807.07073. Bibcode:2018MNRAS.481L..11B. doi:10.1093/mnrasl/sly144. ISSN 0035-8711. S2CID 118974910.
  7. ^ "[BBJ2018] 6". sim-basic. Retrieved 2020-01-22.
  8. ^ Cantat-Gaudin, T.; Mapelli, M.; Balaguer-Núñez, L.; Jordi, C.; Sacco, G.; Vallenari, A. (January 2019). "A ring in a shell: the large-scale 6D structure of the Vela OB2 complex". Astronomy & Astrophysics. 621: A115. arXiv:1808.00573. Bibcode:2019A&A...621A.115C. doi:10.1051/0004-6361/201834003. ISSN 0004-6361. S2CID 119071750.
  9. ^ Littlefair, S. P.; Naylor, Tim; Jeffries, R. D.; Devey, C. R.; Vine, S. (November 2003). "Mass segregation in the young open cluster NGC 2547". MNRAS. 345 (4): 1205–1211. arXiv:astro-ph/0308320. Bibcode:2003MNRAS.345.1205L. doi:10.1046/j.1365-2966.2003.07035.x. ISSN 0035-8711.
  10. ^ Gorlova, N.; Balog, Z.; Rieke, G. H.; Muzerolle, J.; Su, K. Y. L.; Ivanov, V. D.; Young, E. T. (November 2007). "Debris Disks in NGC 2547*". The Astrophysical Journal. 670 (1): 516–535. arXiv:0707.2827. Bibcode:2007ApJ...670..516G. doi:10.1086/521671. ISSN 0004-637X. S2CID 7581125.
  11. ^ Meng, Huan Y. A.; Su, Kate Y. L.; Rieke, George H.; Stevenson, David J.; Plavchan, Peter; Rujopakarn, Wiphu; Lisse, Carey M.; Poshyachinda, Saran; Reichart, Daniel E. (August 2014). "Large impacts around a solar-analog star in the era of terrestrial planet formation" (PDF). Science. 345 (6200): 1032–1035. arXiv:1503.05609. Bibcode:2014Sci...345.1032M. doi:10.1126/science.1255153. ISSN 0036-8075. PMID 25170148. S2CID 206558302.
  12. ^ Forbrich, Jan; Lada, Charles J.; Muench, August A.; Teixeira, Paula S. (November 2008). "New M Dwarf Debris Disk Candidates in NGC 2547". The Astrophysical Journal. 687 (2): 1107–1116. arXiv:0807.3597. Bibcode:2008ApJ...687.1107F. doi:10.1086/592035. ISSN 0004-637X. S2CID 119215678.
  13. ^ Silverberg, Steven M.; Wisniewski, John P.; Kuchner, Marc J.; Lawson, Kellen D.; Bans, Alissa S.; Debes, John H.; Biggs, Joseph R.; Bosch, Milton K. D.; Doll, Katharina; Luca, Hugo A. Durantini; Enachioaie, Alexandru (2020-01-14). "Peter Pan Disks: Long-lived Accretion Disks Around Young M Stars". The Astrophysical Journal. 890 (2): 106. arXiv:2001.05030. Bibcode:2020ApJ...890..106S. doi:10.3847/1538-4357/ab68e6. S2CID 210718358.
  14. ^ Teixeira, Paula S.; Lada, Charles J.; Wood, Kenneth; Robitaille, Thomas P.; Luhman, Kevin L. (July 2009). "Infrared Spectrograph Characterization of a Debris Disk Around an M-Type Star in NGC 2547". Astrophysical Journal. 700 (1): 454–459. arXiv:0905.2469. Bibcode:2009ApJ...700..454T. doi:10.1088/0004-637X/700/1/454. ISSN 0004-637X. S2CID 8231130.



Quelle: https://en.wikipedia.org/wiki/NGC_2547