NGC 2547

Last updated
NGC 2547
Star cluster NGC 2547.jpg
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 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
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
Constellation Vela
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]

Contents

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]

Related Research Articles

<span class="mw-page-title-main">Proplyd</span> Dust ring surrounding large stars thousands of solar radii wide

A proplyd, short for ionized protoplanetary disk, is an externally illuminated photoevaporating protoplanetary disk around a young star. Nearly 180 proplyds have been discovered in the Orion Nebula. Images of proplyds in other star-forming regions are rare, while Orion is the only region with a large known sample due to its relative proximity to Earth.

<span class="mw-page-title-main">Rogue planet</span> Planets not gravitationally bound to a star

A rogue planet, also termed a free-floating planet (FFP) or an isolated planetary-mass object (iPMO), is an interstellar object of planetary mass which is not gravitationally bound to any star or brown dwarf.

Photoevaporation is the process where energetic radiation ionises gas and causes it to disperse away from the ionising source. The term is typically used in an astrophysical context where ultraviolet radiation from hot stars acts on clouds of material such as molecular clouds, protoplanetary disks, or planetary atmospheres.

<span class="mw-page-title-main">HD 107146</span> Star in the constellation Coma Berenices

HD 107146 is a star in the constellation Coma Berenices that is located about 90 light-years (28 pc) from Earth. The apparent magnitude of 7.028 makes this star too faint to be seen with the unaided eye.

<span class="mw-page-title-main">Rho Coronae Borealis</span> Star in the constellation Corona Borealis

Rho Coronae Borealis is a yellow dwarf star 57.1 light-years away in the constellation of Corona Borealis. The star is thought to be similar to the Sun with nearly the same mass, radius, and luminosity. It is orbited by four known exoplanets.

HD 210277 is a single star in the equatorial constellation of Aquarius. It has an apparent visual magnitude of 6.54, which makes it a challenge to view with the naked eye, but it is easily visible in binoculars. The star is located at a distance of 69.6 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −20.9 km/s.

<span class="mw-page-title-main">Flame Nebula</span> Emission nebula in the constellation Orion

The Flame Nebula, designated as NGC 2024 and Sh2-277, is an emission nebula in the constellation Orion. It is about 1350 light-years away. At that distance, the Flame Nebula lies within the Orion B cloud of the larger Orion Molecular Cloud Complex.

<span class="mw-page-title-main">NGC 2244</span> Open cluster within the Rosette nebula, in the constellation Monoceros

NGC 2244 is an open cluster in the Rosette Nebula, which is located in the constellation Monoceros. This cluster has several O-type stars, super hot stars that generate large amounts of radiation and stellar wind.

HD 98800, also catalogued as TV Crateris, is a quadruple star system in the constellation of Crater. Parallax measurements made by the Hipparcos spacecraft put it at a distance of about 150 light-years away. The system is located within the TW Hydrae association (TWA), and has received the designation TWA 4.

HD 210277 b is an extrasolar planet orbiting the star HD 210277. It was discovered in September 1998 by the California and Carnegie Planet Search team using the highly successful radial velocity method. The planet is at least 24% more massive than Jupiter. The mean distance of the planet from the star is slightly more than Earth's distance from the Sun. However, the orbit is very eccentric, so at periastron this distance is almost halved, and at apastron it is as distant as Mars is from the Sun.

HD 23514, is a star in the Pleiades. It is a main-sequence star of class F6, and has been seen to have hot dust particles orbiting around it. These materials, otherwise known as planetesimals which orbit within a circumstellar disc, are evidence of possible planetary formation. The debris disk shows evidence of being rich in silica.

<span class="mw-page-title-main">HD 61005</span> Star in the constellation Puppis

HD 61005, also known as HIP 36948 and The Moth, is a young star located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 8.22, making it readily visible in binoculars, but not to the naked eye. The object is located relatively close at a distance of 119 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of 22.6 km/s.

HD 219623 is a solitary star in the northern circumpolar constellation of Cassiopeia. HD 219623 is its Henry Draper Catalogue designation. It has an apparent visual magnitude of 5.59, which lies in the brightness range that is visible to the naked eye. According to the Bortle scale, it can be observed from dark suburban skies. Parallax measurements place it at an estimated distance of around 67.2 light years. It has a relatively high proper motion, advancing 262 mas per year across the celestial sphere.

<span class="mw-page-title-main">NGC 4298</span> Galaxy in the constellation Coma Berenices

NGC 4298 is a flocculent spiral galaxy located about 53 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4302</span> Galaxy in the constellation Coma Berenices

NGC 4302 is an edge-on spiral galaxy located about 55 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

A Peter Pan disk is a circumstellar disk around a star or brown dwarf that appears to have retained enough gas to form a gas giant planet for much longer than the typically assumed gas dispersal timescale of approximately 5 million years. Several examples of such disks have been observed to orbit stars with spectral types of M or later. The presence of gas around these disks has generally been inferred from the total amount of radiation emitted from the disk at infrared wavelengths, and/or spectroscopic signatures of hydrogen accreting onto the star. To fit one specific definition of a Peter Pan disk, the source needs to have an infrared "color" of , an age of >20 Myr and spectroscopic evidence of accretion.

<span class="mw-page-title-main">Tucana-Horologium association</span> Large stellar association

The Tucana-Horologium association (Tuc-Hor), or Tucana Horologium moving group, is a stellar association with an age of 45 ± 4 Myr and it is one of the largest stellar associations within 100 parsecs. The association has a similar size to the Beta Pictoris moving group (BPMG) and contains, like BPMG, more than 12 stars with spectral type B, A and F. The association is named after two southern constellations, the constellation Tucana and the constellation Horologium.

HD 46588 is a star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.44, allowing it to be faintly seen with the naked eye. The object is relatively close at a distance of only 59 light years but is receding with a heliocentric radial velocity of 15 km/s.

HD 194012 is a star in the equatorial constellation Delphinus. It has an apparent magnitude of 6.15, making it visible to the naked eye under ideal conditions. The star is relatively close at a distance of only 85 light years but is receding with a heliocentric radial velocity of 4.5 km/s.

References

  1. 1 2 3 4 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.


This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.